# GCN_circulars

GRB_name: GRB190604B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24747
SUBJECT: GRB190604B: Swift/UVOT detection
DATE:    19/06/04 20:40:46 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and K. L. Page (U Leicester) report on behalf 
of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190604B 
128 s after the BAT trigger (Page et al., GCN Circ. 24742). A faint 
source is detected in the initial white UVOT exposure at a position 
consistent with the enhanced XRT source position (Evans et al., GCN 
Circ. 24746).

The preliminary detection and 3-sigma upper limits using the UVOT 
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for 
the early exposures are:

Filter      T_start(s) T_stop(s)    Exp(s)      Mag

white      128      276         146        19.90 Â± 0.24
white      618      812          39        >19.63
v          669      861          39        >17.95
b          594      787          39        >18.98
u          338      588         246        >19.71
uvw1       718      738          20        >17.44
uvw2       645      837          39        >18.09

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.15 in the direction of the 
  burst (Schlegel et al. 1998).


GRB_name: GRB190604B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24748
SUBJECT: GRB190604B: GROWTH-India telescope followup - no optical counterpart found
DATE:    19/06/04 21:31:40 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

M. Khandagale, H. Kumar, V. Karambelkar, V. Bhalerao(IITB), G. C. Anupama,
J. Stanzin (IIA) report on behalf of the GROWTH collaboration:

We observed the field of GRB190604B reported by K. L. Page et al., GCN
24742 at 2019-06-04 and 20:03:18.675 UT with the 0.7m GROWTH-India
telescope. We took 2 exposures of 600 seconds each in r filter. No source
was found within an uncertainty region of 3.6 arcseconds to RA(J2000) = 19h
50m 09.13s, Dec(J2000) = -32d 58' 35.9" (K. L. Page et al.,GCN 24742).

We obtained the following upper limits:

------------------------------------------------------------------

 JD(Start)| Exposure(sec) | Filter | lim_Mag |

------------------------------------------------------------------

2458639.335 | 600 | r | 20.33|

2458639.342 | 600 | r | 19.93|

------------------------------------------------------------------

The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government
of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).


GRB_name: GRB190604B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24749
SUBJECT: GRB 190604B: Swift-XRT refined Analysis
DATE:    19/06/05 02:39:36 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU),
A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne
(U. Leicester), M.G. Bernadini (INAF-OAB), E. Ambrosi  (INAF-IASFPA) ,
V. D'Elia (ASDC) and K.L. Page report on behalf of the Swift-XRT team:

We have analysed 7.7 ks of XRT data for GRB 190604B (Page et al. GCN
Circ. 24742), from 120 s to 34.4 ks after the  BAT trigger. The data
comprise 285 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN Circ. 24743).

The late-time light curve (from T0+4.9 ks) can be modelled with a
power-law decay with a decay index of alpha=0.94 (+/-0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.40 (+/-0.03). The
best-fitting absorption column is  1.49 (+0.16, -0.13) x 10^21 cm^-2,
consistent with the Galactic value of 1.4 x 10^21 cm^-2 (Willingale et
al. 2013). The PC mode spectrum has a photon index of 2.02 (+/-0.12)
and a best-fitting absorption column of 3.0 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (5.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.0 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 1.4 x 10^21 cm^-2
Excess significance: 5.7 sigma
Photon index:      2.02 (+/-0.12)

If the light curve continues to decay with a power-law decay index of
0.94, the count rate at T+24 hours will be 0.057 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.1 x
10^-12 (3.1 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00906654.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190604B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24750
SUBJECT: GRB 190604B: BOOTES-3 early optical limits
DATE:    19/06/05 05:52:15 GMT
FROM:    Alberto J. Castro-Tirado at IAA-CSIC  <ajct@iaa.es>

Y.-D. Hu, X.-Y.Li, E. Fernandez-Garcia, A. Ayala and A. J. Castro-Tirado 
(IAA-CSIC),
I. Carrasco and C. Perez del Pulgar (Univ. de Malaga), M. D. 
Caballero-Garcia (ASU-CAS, CZ)
and R. Querel (NIWA), on behalf of a larger collaboration,

report:

The 60cm BOOTES-3/YA robotic telescope at NIWA Lauder in Otago (New 
Zealand) automatically
responded to the Swift GRB 190604B (Page et al. GCNC 24742) only 35 s 
after the burst). At
the position of the Swift/XRT enhanced X-ray position (Evans et al. GCNC 
24746), no optical
afterglow is detected down to R = 15.5 (for the 1-s image gathered at 
14:57:50 UT) or down to
19.8 mag (for the co-added 9x10s unfiltered images at mid-time 15:05:56 
UT, i.e. 8.7 min after
trigger).

We thank the staff at NIWA for its excellent support.


GRB_name: GRB190530A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24751
SUBJECT: GRB 190530A: optical follow-up observations at Konkoly
DATE:    19/06/05 13:27:40 GMT
FROM:    Jozsef Vinko at Konkoly Observatory  <vinko@konkoly.hu>

J. Vinko, R. Szakats, A. Pal, L. Kriskovics, A. Ordasi, K. Sarneczky 
(MTA CSFK Konkoly Observatory) report:

We took follow-up observations on the optical afterglow (Lipunov et al., GCN 24680; 
Kann et al., GCN 24684; Heintz et al., GCN 24686;  Izzo et al., GCN 24687; 
Xin et al., GCN 24688; Watson et al., GCN 24690; Lipunov et al., GCN 24693; 
Xin et al., GCN 24697; Belkin et al.,  GCN 24698; Kann et al., GCN 24700; 
Siegel, GCN 24703; Moskvitin and Uklein, GCN 24708; Vinko et al., GCN 24709; 
Belkin et al., GCN 24712; Kumar et al., GCN 24729; Nandi et al., GCN 24745) 
of the bright GRB 190530A (Fermi GBM team, GCN 24676, Biltzinger et al., GCN 24677;  
Longo et al., GCN 24679; Lucarelli et al.,GCN 24678, Verecchia et al., GCN 24683). 

The source was clearly detected on the stacked Sloan-r band CCD frames (total exposure time 60 min)
taken with the 0.8m RC80 telescope at Konkoly Observatory, Piszkesteto (Hungary)
on 2019-06-01.85 UT, but only marginally detected on the frames taken 
on 2019-06-02.86 UT (2.42 and 3.43 days after burst, respectively).

We measured the brightness of the transient via aperture photometry on the stacked 
r-band frames using PS1 r-band magnitudes of 19 local comparison stars. The results, 
corrected for the contamination of the nearby faint source (r_PS1(AB) = 20.947 +/- 0.0565 mag),
are as follows:

# Date      UT(mid)    JD-2400000     r(AB)  unc.   Ref
#----------------------------------------------------------------
2019-05-31 20:23:35   58635.349711    20.36  0.37   GCN 24709
2019-06-01 20:23:56   58636.349953    20.15  0.11   this circular
2019-06-02 20:37:30   58637.359375    22.10  0.41   this circular
#----------------------------------------------------------------

Note that in Vinko et al. (GCN 24709) the UT date of the observation was 
reported incorrectly. The correct date was 2019-05-31.85 UT. Also, our 
previous photometry given in GCN 24709 was not corrected for the nearby 
contaminating source. The table above contains the updated, corrected 
magnitudes.

Our last photometric measurement (taken on 2019-06-02) is consistent with the
R-band magnitude reported by Kumar et al. (GCN 24729, R ~ 21.3 +/- 0.3 mag).


GRB_name: GRB190604B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24752
SUBJECT: GRB 190604B: Swift-BAT refined analysis
DATE:    19/06/05 14:50:33 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL),
K. L. Page (U Leicester), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+962 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 190604B (trigger #906654)
(Page et al., GCN Circ. 24742).  The BAT ground-calculated position is
RA, Dec = 297.546, -32.975 deg which is
   RA(J2000)  =  19h 50m 10.9s
   Dec(J2000) = -32d 58' 31.1"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 64%.

The mask-weighted light curve shows a multi-peaked structure that starts
from ~T-40 s and ends at ~T+240 s. There are two major peaks that occur
at ~T0 and ~T+158 s, respectively. T90 (15-350 keV) is 220.2 +- 4.7 sec
(estimated error including systematics).

The time-averaged spectrum from T-39.776 sec to T+239.504 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.81 +- 0.04. The fluence in the 15-150 keV band
is 1.77 +- 0.04 x 10^-5 erg/cm2. The 1-sec peak photon flux measured from
T+157.54 sec in the 15-150 keV band is 7.3 +- 0.4 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/906654/BA/


GRB_name: GRB190604A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24753
SUBJECT: GRB 190604A: AstroSat CZTI detection
DATE:    19/06/05 15:59:32 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma, D. Bhattacharya, T. Khanam and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190604A, which was also detected by Fermi GBM (GCN #24739), BALROG localization (Biltzinger B. et al., GCN #24740) and Global MASTER-Net (Lipunov V. et al., GCN #24741).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 10:42:41.5 UT. The measured peak count rate associated with the burst is 874 cts/s above the background in the combined data of four quadrants, with a total of 5755 cts. The local mean background count rate was 508 cts/s. Using cumulative rates, we measure a T90 of 13.55 s. In preliminary analysis, we find that 460 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190604B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24754
SUBJECT: GRB 190604B: Kitab observatory optical upper limit
DATE:    19/06/05 19:24:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Novichonok (KIAM), A. Pozanenko (IKI), E. Mazaeva 
(IKI), A. Volnova (IKI), I. Molotov (KIAM), Sh. Ehgamberdiev (UBAI) 
report on behalf of larger IKI GRB FuN collaboration:

We observed the field of the Swift GRB 190604B (Page et al., GCN  24742) 
  with RC-36 0.36-m telescope of Kitab Observatory starting on June 04 
(UT) 22:26:32 in  Clear filter.    We do not find any optical source 
within  enhanced Swift-XRT position (Evans  et al., GCN  24746). The 
non-detection is consistent with BOOTES-3 results (Hu et al., GCN  24750).

Preliminary photometry of the field is following.

Date       UT start   t-T0       Filter Exp.   OT  Err.   UL(3sigma)
                       (mid, days)        (s)

2019-06-04 22:26:32   0.32068    CR     21*60  n/d  n/d   18.6

The photometry is based on the nearby USNO-B1 (R2) stars.


GRB_name: GRB190605A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24755
SUBJECT: GRB 190605A: Fermi GBM Final Real-time Localization
DATE:    19/06/05 23:34:09 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 23:22:27 UT on 5 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190605A (trigger 581469752.117826 / 190605974).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 337.2, Dec = 4.8 (J2000 degrees, equivalent to J2000 22h 28m, 4d 47'), with a statistical uncertainty of 6.8 degrees.

The angle from the Fermi LAT boresight is 85.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190605974/quicklook/glg_skymap_all_bn190605974.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190605974/quicklook/glg_healpix_all_bn190605974.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190605974/quicklook/glg_lc_medres34_bn190605974.gif


GRB_name: GRB190604A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24758
SUBJECT: GRB 190604A: Insight-HXMT/HE detection
DATE:    19/06/06 10:14:36 GMT
FROM:    QiBin Yi at IHEP, HXMT  <yiqb@ihep.ac.cn>

Q. B. Yi, S. Xiao, Q. Luo, C. Cai, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:

At 2019-06-04T10:42:38.00 (T0), Insight-HXMT/HE detected 
GRB 190604A (trigger ID: HEB190604446) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #24739). 

The Insight-HXMT/HE light curve mainly consists of multiple
pulses with a duration (T90) of 6.37 s measured from T0+0.34 s. 
The 1-ms peak rate, measured from T0+2.82 s, is 1963 cnts/sec. 
The total counts from this burst is 6908 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190604446_lc.jpg

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24759
SUBJECT: Fermi trigger No 581478912 / GRB 190606A: AGILE/MCAL observations
DATE:    19/06/06 10:15:56 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), F. Verrecchia (SSDC, and INAF/OAR), N. Parmiggiani
(INAF/OAS-Bologna), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A.
Argan, M. Cardillo, C. Casentini, Y. Evangelista, G. Piano (INAF/IAPS), F.
Lucarelli, C. Pittori (SSDC, and INAF/OAR), A. Bulgarelli, V. Fioretti, F.
Fuschino (INAF/OAS-Bologna), M. Marisaldi (INAF/OAS-Bologna, and Bergen
University), M. Pilia, A. Trois (INAF/OA-Cagliari), I. Donnarumma (ASI), F.
Longo (Univ. Trieste and INFN Trieste), A. Giuliani (INAF/IASF-Mi), report
on behalf of the AGILE Team:

The AGILE Mini-CALorimeter (MCAL) detected the short burst GRB190606.08
(Fermi trigger No 581478912) at T0 = 2019-06-06 01:55:07.80 +/- 0.01 s
(UTC).

The event lasted about 0.22 s and released a total number of ~660 counts in
the detector (in the 0.4-100 MeV energy range), above an average background
rate of 660 counts / s.

The light curve shows a single sharp peak and can be found at
http://www.agilescienceapp.it/notices/GRB_062876_486870907.795776.png.

The time-integrated spectrum of the burst in 0.22 s can be fitted in the
energy range [0.4-100 MeV] with a single power law with ph.ind = 2.32
-0.12/+0.14, resulting in a reduced chi-square of 1.62 (86 d.o.f.). The
burst fluence in the same energy range and time interval is 1.71e-6
erg/cm^2 (90% confidence level).

The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive in the
energy range 0.4-100 MeV. Additional analysis of AGILE data is in progress.


GRB_name: GRB190605B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24760
SUBJECT: GRB 190605B: Insight-HXMT/HE detection
DATE:    19/06/06 10:22:20 GMT
FROM:    QiBin Yi at IHEP, HXMT  <yiqb@ihep.ac.cn>

Q. B. Yi, S. Xiao, Q. Luo, C. Cai, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:

At 2019-06-05T02:39:08.00 (T0), Insight-HXMT/HE detected 
GRB 190605B (trigger ID: HEB190605110) in a routine search of the data, 
which was also triggered by INTEGRAL/SPI-ACS.

The Insight-HXMT/HE light curve mainly consists of multiple
pulses with a duration (T90) of 14.69 s measured from T0+0.78 s. 
The 1-ms peak rate, measured from T0+2.57 s, is 2204 cnts/sec. 
The total counts from this burst is 12835 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190605110_lc.jpg

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190606A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24761
SUBJECT: GRB 190606A: Fermi-LAT detection
DATE:    19/06/06 15:06:23 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

E. Bissaldi (Politecnico & INFN Bari), M. Axelsson (KTH & Stockholm Univ.),
M. Arimoto (Kanazawa Univ.) and F. Longo (Univ & INFN Trieste)
report on behalf of the Fermi-LAT team:


"On June 6, 2019, Fermi-LAT detected high-energy emission
from GRB 190606A, which was also detected by Fermi-GBM
(trigger 581478912 / 190606080) and AGILE-MCAL
(Ursi et al., GCN #24759).

Due to the large angle with respect to the LAT boresight,
the positional error for this GRB is uncertain.
The best LAT on-ground location is found to be:

RA, Dec 76.54, -0.68 (degrees, J2000)

with an error radius of 3.0 deg (90% containment,
statistical error only).
This was 72 deg from the LAT boresight
at the time of the GBM trigger:
T0 = 01:55:07.78 UT.
  
The data from the Fermi-LAT show a significant increase
in the event rate after the GBM trigger that is spatially
correlated with the GBM emission with high significance.

The photon flux above 100 MeV in the time interval
T0 - T0+250 s after the GBM trigger is (4.3 +/- 1.9)E-05 ph/cm2/s.
The highest-energy photon in this interval is a 1.6 GeV event
observed at T0+154 s.
The estimated photon index above 100 MeV is 2.5 +/- 0.5.

The Fermi-LAT point of contact for this burst is
Elisabetta Bissaldi (elisabetta.bissaldi@ba.infn.it).


The Fermi-LAT is a pair conversion telescope designed
to cover the energy band from 20 MeV to greater than 300 GeV.
It is the product of an international collaboration between
NASA and DOE in the U.S. and many scientific
institutions across France, Italy, Japan and Sweden."


GRB_name: GRB190604B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24762
SUBJECT: GRB 190604B: VLT Afterglow Detection
DATE:    19/06/06 16:39:16 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

L. Izzo, D. A. Kann (both HETH/IAA-CSIC), D. B. Malesani (DTU Space), D. 
Hartmann (Clemson University), A. de Ugarte Postigo (HETH/IAA-CSIC, 
DARK/NBI), and N. R. Tanvir (Univ. Leicester) report on behalf of the 
Stargate Consortium:

We observed the field of GRB 190604B (Page et al., GCN 24742) with 
X-shooter mounted on the ESO VLT UT2 (Kueyen). Images were obtained in 
SDSS g'r'z', as well as a deeper 300 s r' exposure, centered at 05:24:16 
UT on June 05, 2019 (0.8483 days after the GRB trigger).

At the position of the UVOT afterglow (Breeveld et al., GCN 24747) and 
within the XRT error circle (Evans et al., GCN 24746), we detect a faint 
source only in the latter image.

Using a recent computation of the X-shooter acquisition camera 
zero-point value, the total number of counts, a seven arcsec radius 
aperture and the exposure time of 300 s, we derive a magnitude of r'(AB) 
= 23.27 +/- 0.09 mag.

Because of source faintness, no spectroscopy was attempted.


GRB_name: GRB190530A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24763
SUBJECT: GRB 190530A: Further OAJ/OSN photometry and analysis
DATE:    19/06/06 16:58:21 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC, 
DARK/NBI), L. Izzo, M. Blazek, C. C. Thoene, K. Bensch (all 
HETH/IAA-CSIC) report:

We checked the magnitude of our second-epoch OSN observation (Kann et 
al., GCN 24700) of the Fermi GBM/LAT GRB 190530A (Fermi GBM team, GCN 
24676; Longo et al., GCN 24679) and found a calculation error which 
resulted in an incorrect zero-point. Remeasuring the magnitude against 
four SDSS stars (once again transformed to Rc via the equations of 
Lupton 2005) we now derive Rc(AB) = 19.51 +/- 0.04 mag. This is in good 
agreement with the value obtained by Moskvitin & Uklein (GCN 24708). The 
magnitude of Belkin et al. (GCN 24698) is still overly bright compared 
to our new result, and the revised value from Vinko et al. (GCN 24751) 
is now significantly fainter.

We obtained 7 x 300 s images in SDSS r' with the 0.8m telescope of the 
Observatorio Astrofisico de Javalambre (Teruel, Spain). The first three 
images were taken too early in twilight and were discarded. The 
afterglow is clearly detected in the stack of the four last images, and 
we measure:

r'(AB) = 20.27 +/- 0.06 mag at 2.43735 days after the GRB.

This is in good agreement with an earlier value from Vinko et al. (GCN 
24751) combined with a steep decay.

Using the further photometry published since Kann et al. (GCN 24700) 
(Moskvitin et al., GCN 24708; Belkin et al., GCN 24712; Kumar et al., 
GCN 24729; Nandi et al., GCN 24745; Vinko et al., GCN 24751) we find:

- The steep decay between the observation of Watson et al. (GCN 24690) 
and Xin et al. (GCN 24697) remains, and is not significantly affected by 
our revised OSN measurement.
- There may be a small flare at 1.4 days (this GCN [OSN]; Moskvitin et 
al., GCN 24708).
- Starting at 2.2 days (Belkin et al., GCN 24712; Vinko et al., GCN 
24751; this GCN [OAJ]; Nandi et al., GCN 24745; Kumar et al., GCN 
24729), yet another steep decay sets in, for which we measure alpha = 
3.72 +/- 0.43. This value is perfectly in agreement with the one derived 
in Kann et al. (GCN 24700) at an earlier time, but now based on 
significantly more measurements.

Further follow-up is warranted, if possible.


GRB_name: GRB190606A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24764
SUBJECT: GRB 190606A: Fermi GBM detection
DATE:    19/06/06 18:05:00 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

O.J. Roberts (USRA/NASA-MSFC), S. Poolakkil (UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 01:55:07.76 UT on the 6th of June 2019, the Fermi Gamma-ray Burst 
Monitor (GBM) triggered and located GRB 190606A 
(trigger 581478912 / 190606080), which was also detected by AGILE 
(Ursi et al. 2019, GCN 24759) and the LAT (Bissaldi et al. 2019, GCN 24761).
The GBM on-ground location is consistent with the LAT position.

The angle from the Fermi LAT boresight is 72 degrees.

The GBM light curve shows a bright short spike with a duration (T90) of 
about 0.3 s (10-1000 keV). The time-averaged spectrum from T0+0 s to 
T0+0.3 s is best fit by a Band function with Epeak = 1779 +/- 185 keV, 
alpha = -0.95 +/- 0.02, and beta = -2.52 +/- 0.21

The event fluence (10-1000 keV) in this time interval is 
(4.88 +/- 0.08)E-06 erg/cm^2. The 64-msec peak photon flux measured
starting from T0+0.6 s in the 10-1000 keV band is 118 +/- 3 ph/s/cm^2."

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB190606A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24765
SUBJECT: IPN Triangulation of GRB 190606A (short)
DATE:    19/06/06 20:06:29 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin,
and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

and

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, report:

The short-duration, very bright GRB 190606A
(AGILE-MCAL detection: Ursi et al., GCN Circ. 24759;
Fermi-LAT detection: Bissaldi et al., GCN Circ. 24761;
Fermi-GBM detection: Roberts et al,. GCN Circ. 24764)
has been detected by Fermi (GBM; trigger 581478912), Konus-Wind,
INTEGRAL (SPI-ACS), and AGILE (MCAL), so far, at about 6904 s UT (01:55:04).

We have triangulated it to a Konus-GBM annulus centered at
RA(2000)=88.386 deg (05h 53m 33s)  Dec(2000)=+21.574 deg (+21d 34' 26"),
whose radius is 25.034 +/- 0.198 deg (3 sigma).

The LAT position reported by Bissaldi et al. (GCN Circ. 24761)
is consistent with the annulus. The annulus combined with
the LAT (90 % containment, statistical-only) error circle
gives the following error box:
--------------------------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ------------------------------------------------------------
  Center:
   76.561 (05h 06m 15s)   -0.638 ( -0d 38' 17")
  Corners:
   79.380 (05h 17m 31s)   -1.649 ( -1d 38' 57")
   79.227 (05h 16m 55s)   -2.015 ( -2d 00' 55")
   74.072 (04h 56m 17s)   +1.026 ( +1d 01' 35")
   73.869 (04h 55m 29s)   +0.686 ( +0d 41' 09")
  -------------------------------------------------------------
The error box area is 2.4 sq. deg (a factor of 10
smaller than that of the LAT error circle), and its maximum
dimension is 6 deg (the minimum one is 23.7 arcmin).
The Sun distance was ~22 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190606_T06903/IPN/

The time history and spectrum will be given in forthcoming
GCN Circulars.


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24766
SUBJECT: GRB 190114C: East Asia VLBI Network observations
DATE:    19/06/06 20:51:25 GMT
FROM:    Marcello Giroletti at INAF Euro VLBI  <marcello.giroletti@inaf.it>

M. Giroletti, M. Orienti (INAF-IRA), G. Ghirlanda, G. Ghisellini,
L. Nava, M. Ravasio, O. Salafia (INAF-OABrera), T. An (SHAO),
K. Hada (NAOJ), B. W. Sohn (KASI), G. Giovannini (Univ. Bologna),
Y. Zhang (UCAS)

We observed GRB 190114C (Gropp et al., GCN 23688) within the DDT project
a19mg01 using the East Asia VLBI Network (EAVN) at 22 GHz on three
epochs: 7, 16, and 33 days after the burst, respectively.  We report in
the table below the observing dates and times, with the resulting
3-sigma upper limits on the source flux density (assuming the source is
unresolved at the few milliarcsecond angular resolution of the instrument):

Date         Time (UT)     3-sigma u.l. (mJy)
2019-01-21   08:30-14:30   2.8
2019-01-30   08:00-14:00   1.8
2019-02-16   08:00-14:05   0.84

We acknowledge the EAVN Directors, the scheduler, and the staff at
the stations and at the KJCC for approving, executing, and correlating
these observations.


GRB_name: GRB190606A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24768
SUBJECT: GRB 190606A: Insight-HXMT/HE detection
DATE:    19/06/07 11:05:14 GMT
FROM:    QiBin Yi at IHEP, HXMT  <yiqb@ihep.ac.cn>

Q. B. Yi, S. Xiao, Q. Luo, C. Cai, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:

At 2019-06-06T01:55:07.00 (T0), Insight-HXMT/HE detected 
GRB 190606A (trigger ID: HEB190606079) in a routine search of the data, 
which was also triggered by Fermi/GBM (trigger #581478912) and
AGILE/MCAL (GCN #24759).  

The Insight-HXMT/HE light curve mainly consists of multiple
pulses with a duration (T90) of 0.12 s measured from T0+0.84 s. 
The 1-ms peak rate, measured from T0+0.89 s, is 49197 cnts/sec. 
The total counts from this burst is 2833 counts. 
Some part of the Insight-HXMT/HE light curve suffers data saturation 
due to the extreme brightness of this burst.
URL_LC: http://www.hxmt.org/images/GRB/HEB190606079_lc.jpg

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190608A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24769
SUBJECT: GRB 190608A: Fermi GBM Final Real-time Localization
DATE:    19/06/08 00:24:04 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 00:12:18 UT on 8 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190608A (trigger 581645543.394168 / 190608009).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 225.7, Dec = -31.4 (J2000 degrees, equivalent to J2000 15h 02m, -31d 23'), with a statistical uncertainty of 2.2 degrees.

The angle from the Fermi LAT boresight is 71.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190608009/quicklook/glg_skymap_all_bn190608009.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190608009/quicklook/glg_healpix_all_bn190608009.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190608009/quicklook/glg_lc_medres34_bn190608009.gif


GRB_name: GRB190605A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24771
SUBJECT: GRB 190605A: AstroSat CZTI detection
DATE:    19/06/08 06:19:35 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma, D. Bhattacharya, T. Khanam and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed a weak detection of a likely long GRB 190605A, which was also detected by Fermi GBM (GCN #24755) and Global MASTER-Net (Lipunov V., GCN #24756)

The source was detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 23:22:28.5 UT. The measured peak count rate associated with the burst is 189 cts/s above the background in the combined data of four quadrants, with a total of 482 cts. The local mean background count rate was 508 cts/s. Using cumulative rates, we measure a T90 of 4.46s.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190609A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24773
SUBJECT: GRB 190609A: Fermi GBM Final Real-time Localization
DATE:    19/06/09 07:45:52 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 07:34:05 UT on 9 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190609A (trigger 581758450.25943 / 190609315).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 165.8, Dec = -50.8 (J2000 degrees, equivalent to J2000 11h 03m, -50d 47'), with a statistical uncertainty of 1.9 degrees.

The angle from the Fermi LAT boresight is 30.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190609315/quicklook/glg_skymap_all_bn190609315.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190609315/quicklook/glg_healpix_all_bn190609315.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190609315/quicklook/glg_lc_medres34_bn190609315.gif


GRB_name: GRB190609A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24774
SUBJECT: GRB190609A: BALROG localization (Fermi Trigger 581758450 / GRB 190609315)
DATE:    19/06/09 08:06:38 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

 J. Burgess, B. Biltzinger, F. Kunzweiler, F. Berlato & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
581758450 at 07:34:05 on 09 June 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 177.6+/-6.9 deg
Decl.(2000.0) = -46.4+/-3.9 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190609315/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190609315/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190609315/json

                        


GRB_name: GRB190610A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24775
SUBJECT: GRB 190610A: Swift detection of a short burst
DATE:    19/06/10 11:51:39 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

P. A. Evans (U Leicester), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (PSU), M. J. Moss (GWU), D. M. Palmer (LANL),
B. Sbarufatti (PSU), M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report
on behalf of the Neil Gehrels Swift Observatory Team:

At 11:27:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190610A (trigger=907754).  Swift did not slew to
the burst location due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 46.289, -7.666 which is 
   RA(J2000) = 03h 05m 09s
   Dec(J2000) = -07d 39' 57"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 1 sec.  This is superimposed
on a rising background rate due to the approach of the SAA. 
The peak count rate was ~10,000 counts/sec (15-350 keV), 
at ~0 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 10:44 UT on 2019 June 14. There will thus be no XRT or
UVOT data for this trigger before this time. 

Burst Advocate for this burst is P. A. Evans (pae9 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190610B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24777
SUBJECT: GRB 190610B: Fermi GBM Final Real-time Localization
DATE:    19/06/10 18:11:12 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 17:59:49 UT on 10 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190610B (trigger 581882394.908204 / 190610750).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 327.4, Dec = 42.4 (J2000 degrees, equivalent to J2000 21h 49m, 42d 23'), with a statistical uncertainty of 1.2 degrees.

The angle from the Fermi LAT boresight is 19.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190610750/quicklook/glg_skymap_all_bn190610750.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190610750/quicklook/glg_healpix_all_bn190610750.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190610750/quicklook/glg_lc_medres34_bn190610750.gif


GRB_name: GRB190610B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24778
SUBJECT: GRB190610B: BALROG localization (Fermi Trigger 581882394 / GRB 190610750)
DATE:    19/06/10 18:23:18 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

 J. Burgess, B. Biltzinger, F. Kunzweiler, F. Berlato & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
581882394 at 17:59:49 on 10 June 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 327.4+/-1.7 deg
Decl.(2000.0) = 45.4+/-0.6 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190610750/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190610750/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190610750/json

[GCN OPS NOTE(10jun19): Per author's request, the GRB name in the Subject
was changed from "GRB 190610A" to "GRB 190610B".]


GRB_name: GRB190610C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24780
SUBJECT: GRB 190610C: Fermi GBM Final Real-time Localization
DATE:    19/06/10 20:11:24 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 20:00:23 UT on 10 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190610C (trigger 581889628.68482 / 190610834).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 314.8, Dec = -15.9 (J2000 degrees, equivalent to J2000 20h 59m, -15d 54'), with a statistical uncertainty of 11.2 degrees.

The angle from the Fermi LAT boresight is 95.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190610834/quicklook/glg_skymap_all_bn190610834.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190610834/quicklook/glg_healpix_all_bn190610834.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190610834/quicklook/glg_lc_medres34_bn190610834.gif


GRB_name: GRB190610A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24782
SUBJECT: GRB 190610A: Insight-HXMT/HE detection
DATE:    19/06/11 10:47:53 GMT
FROM:    Ce Cai at IHEP  <caice@ihep.ac.cn>

C. Cai, S. Xiao, Q. Luo, Q. B. Yi, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:

At 2019-06-10T11:27:45.00 (T0), Insight-HXMT/HE detected 
GRB 190610A (trigger ID: HEB190610477) in a routine search of the data, 
which was also triggered by Swift/BAT (GCN #24775). 

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 0.56 s measured from T0+0.96 s. 
The 1-ms peak rate, measured from T0+1.04 s, is 22407 cnts/sec. 
The total counts from this burst is 8510 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190610477_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190610A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24783
SUBJECT: GRB 190610A: Swift-BAT refined analysis
DATE:    19/06/11 14:09:44 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), P. A. Evans (U Leicester),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+35 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 190610A (trigger #907754)
(Evans et al., GCN Circ. 24775).  The BAT ground-calculated position is
RA, Dec = 46.244, -7.661 deg which is
   RA(J2000)  =  03h 04m 58.6s
   Dec(J2000) = -07d 39' 38.7"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a short spike that starts ~T+0.2, peaks
at ~T+0.3, and ends ~T+0.9. Due to the SAA, data beyond ~T+35 s are
unavailable.
T90 (15-350 keV) is 0.62 +- 0.11 sec (estimated error including
systematics).

The time-averaged spectrum from T+0.21 to T+0.89 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.32 +- 0.27.  The fluence in the 15-150 keV band is 4.1 +- 0.5 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T+0.05 sec in the 15-150 keV band
is 3.9 +- 0.5 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/907754/BA/


GRB_name: GRB190606A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24784
SUBJECT: Konus-Wind observation of GRB 190606A
DATE:    19/06/11 17:29:11 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The short-duration, very bright GRB 190606A
(AGILE-MCAL detection: Ursi et al., GCN Circ. 24759;
Fermi-LAT detection: Bissaldi et al., GCN Circ. 24761;
Fermi-GBM detection: Roberts et al., GCN Circ. 24764;
IPN triangulation: Kozlova et al., GCN 24765)
triggered Konus-Wind at T0=6903.8 s UT (01:55:03.800).

The burst light curve shows a single pulse
which starts at ~T0 and has a total duration of ~0.2 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.16(-0.18,+0.18)x10^-5 erg/cm2,
and a 16-ms peak flux, measured from T0+0.034 s,
of 1.45(-0.39,+0.35)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+0.192 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.13(-0.08,+0.09)
and Ep = 2373(-665,+939) keV (chi2 = 56/54 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.8
(chi2 = 55/53 dof).

The spectrum near the maximum count rate
(measured from T0 to T0+0.064 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
with  alpha = -1.19(-0.10,+0.12)
and Ep = 3194(-1324,+2736) keV (chi2 = 32/34 dof).
Fitting by a GRB (Band) model yields:
the low-energy photon index alpha = -0.88(-0.26,+0.45),
the high energy photon index beta = -1.67(-0.27,+0.15),
the peak energy Ep = 664(-388,+1038) keV
(chi2 = 26/33 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190606_T06903/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190611A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24785
SUBJECT: GRB 190611A: Swift detection of a burst
DATE:    19/06/11 18:02:03 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (SSDC), J.D. Gropp (PSU), N. J. Klingler (PSU),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), M. J. Moss (GWU),
D. M. Palmer (LANL), B. Sbarufatti (PSU), M. H. Siegel (PSU) and
A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 17:49:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190611A (trigger=907950).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 324.769, -56.082 which is 
   RA(J2000) = 21h 39m 05s
   Dec(J2000) = -56d 04' 54"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 10 sec.  The peak count rate
was ~900 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 17:50:55.4 UT, 113.5 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 324.72043, -56.07370 which
is equivalent to:
   RA(J2000)  = 21h 38m 52.90s
   Dec(J2000) = -56d 04' 25.3"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 102 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (3.25 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4.3
(+3.64/-3.06) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 116 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.04. 

Burst Advocate for this burst is V. D'Elia (delia AT ssdc.asi.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190611A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24786
SUBJECT: GRB 190611A: Enhanced Swift-XRT position
DATE:    19/06/11 20:43:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 772 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 190611A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 324.72268, -56.07426 which is equivalent
to:

RA (J2000): 21h 38m 53.44s
Dec (J2000): -56d 04' 27.3"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB190612A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24787
SUBJECT: GRB 190612A: Fermi GBM Final Real-time Localization
DATE:    19/06/12 04:08:23 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 03:57:24 UT on 12 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190612A (trigger 582004649.64834 / 190612165).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 223.9, Dec = 62.1 (J2000 degrees, equivalent to J2000 14h 55m, 62d 06'), with a statistical uncertainty of 9.3 degrees.

The angle from the Fermi LAT boresight is 120.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190612165/quicklook/glg_skymap_all_bn190612165.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190612165/quicklook/glg_healpix_all_bn190612165.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190612165/quicklook/glg_lc_medres34_bn190612165.gif


GRB_name: GRB190610B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24789
SUBJECT: GRB 190610B: AstroSat CZTI detection
DATE:    19/06/12 06:19:37 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma, D. Bhattacharya, T. Khanam and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190610B, which was also detected by Fermi GBM (GCN #24777), BALROG (Burgess J. et al., GCN # 24778) and Global MASTER-Net (Lipunov V. et al., GCN # 24779).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 18:00:05.5 UT. The measured peak count rate associated with the burst is 346 cts/s above the background in the combined data of four quadrants, with a total of 1899 cts. The local mean background count rate was 548 cts/s. Using cumulative rates, we measure a T90 of 13.5 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190611A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24790
SUBJECT: GRB 190611A, Swift-BAT refined analysis
DATE:    19/06/12 14:08:05 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), V. D'Elia (SSDC),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 190611A (trigger #907950)
(D'Elia et al., GCN Circ. 24785).  The BAT ground-calculated position is
RA, Dec = 324.689, -56.070 deg which is
   RA(J2000)  =  21h 38m 45.3s
   Dec(J2000) = -56d 04' 12.6"
with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 64%.

The mask-weighted light curve shows a single-peaked structure that starts
and peaks at ~T0, and ends at ~T+40 s. T90 (15-350 keV) is 41.8 +- 30.6 sec
(estimated error including systematics).

The time-averaged spectrum from T-0.9 to T+63.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.88 +- 0.54.  The fluence in the 15-150 keV band is 4.6 +- 1.6 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T+0.54 sec in the 15-150 keV band
is 0.9 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/907950/BA/


GRB_name: GRB190611A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24791
SUBJECT: GRB 190611A: Optical observations from VLT/FORS2 
DATE:    19/06/12 14:23:34 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

R. Sanchez-Ramirez (INAF-IAPS), L. Izzo (HETH/IAA-CSIC), 
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. B. Malesani 
(DTU Space), D. A. Kann (HETH/IAA-CSIC) report on behalf 
of the Stargate collaboration:

We observed the field of GRB 190611A (Dâ€™Elia et al. GCN 24785) 
with FORS2, mounted on UT1 (Antu) of ESO VLT (Paranal 
observatory). Two V-band images were obtained in search of the 
possible afterglow, at a mean epoch of 12 June 08:10:32 UT 
(14.36 hr after the burst). In the combined exposure of 180s, no 
new source was detected within the enhanced XRT error circle 
(Goad et al. GCN 24786) down to a 3-sigma limit of V(AB) = 24.0 
mag. Photometric calibration was performed with respect to field 
stars from the NOMAD catalogue.


GRB_name: GRB190611A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24792
SUBJECT: GRB 190611A: Swift/UVOT Upper Limits
DATE:    19/06/12 17:31:41 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

GRB 190611A: Swift/UVOT Upper Limits

K. K. Simpson (PSU) and V. D'Elia (SSDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190611A
118 s after the BAT trigger (D'Elia et al., GCN Circ. 24785).
No optical afterglow consistent with the XRT position (Goad et al., GCN
Circ. 24786)

RA (J2000): 21h 38m 53.44s
Dec (J2000): -56d 04' 27.3"

is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           118          268          147         >20.1
u_FC               276          525          246         >19.2
white              118          917          186         >20.0
u                  276          525          246         >19.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190611A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24793
SUBJECT: GRB 190611A: Swift-XRT refined Analysis
DATE:    19/06/12 18:03:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), E.
Ambrosi  (INAF-IASFPA) , A. D'Ai (INAF-IASFPA), A. Tohuvavohu (PSU) and
V. D'Elia report on behalf of the Swift-XRT team:

We have analysed 4.7 ks of XRT data for GRB 190611A (D'Elia et al. GCN
Circ. 24785), from 117 s to 22.2 ks after the  BAT trigger. The data
comprise 15 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Goad et al. (GCN Circ. 24786).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.93 (+0.09, -0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.48 (+0.24, -0.22). The
best-fitting absorption column is  8.5 (+8.2, -5.2) x 10^20 cm^-2,
consistent with the Galactic value of 3.2 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.5 x 10^-11 (4.9 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.5 (+8.2, -5.2) x 10^20 cm^-2
Galactic foreground: 3.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.48 (+0.24, -0.22)

If the light curve continues to decay with a power-law decay index of
0.93, the count rate at T+24 hours will be 2.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-13 (1.2 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00907950.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190611B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24794
SUBJECT: GRB 190611B: Fermi GBM detection
DATE:    19/06/12 18:39:54 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

C. Malacaria (NASA-MSFC/USRA) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 22:47:49.34 UT on the 11th of June 2019, 
the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 190611B (trigger 581986074 / 190611950).

The on-ground calculated location, using the GBM trigger
data, is RA =  88.9, DEC =  53.1 (J2000 degrees,
equivalent to 05 h 56 m, 53 d 07 '), with a statistical uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, 
with 90% of GRBs having a 3.7 deg error and a small tail suffering a 
larger than 10 deg systematic error 
[Connaughton et al. 2015, ApJS, 216, 32] ).

The angle from the Fermi LAT boresight 
at the GBM trigger time is 117.0 degrees.

The GBM light curve consists of two broad pulses
with a duration (T90) of about 100.6 s (50-300 keV).
The time-averaged spectrum from T0-0.0 s to T0+18.2 s is
best fit by a Band function with Epeak = 210.3 +/- 18.9  keV,
alpha = -1.00 +/- 0.04, and beta = -1.98 +/- 0.05

The event fluence (10-1000 keV) in this time interval is
(2.43 +/- 0.40)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+71.8 s in the 10-1000 keV band
is 32.4 +/- 0.6 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, 
please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"

[GCN OPS NOTE(16jun19), Per author's request, the "190611A"
in the first sentence was corrected to "190611B".]


GRB_name: GRB190613A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24798
SUBJECT: GRB 190613A: Swift detection of a burst with an optical counterpart
DATE:    19/06/13 04:18:46 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC),
J.D. Gropp (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), M. H. Siegel (PSU)
and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 04:07:18 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190613A (trigger=908288).  Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 182.559, +67.233 which is
   RA(J2000) = 12h 10m 14s
   Dec(J2000) = +67d 13' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The BAT light curve showed a single peak
structure with a duration of about 30 sec.  The peak count rate
was ~500 counts/sec (15-350 keV), at ~10 sec after the trigger.

The XRT began observing the field at 04:09:34.8 UT, 136.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 182.53286, 67.23489 which
is equivalent to:
   RA(J2000)  = 12h 10m 07.89s
   Dec(J2000) = +67d 14' 05.6"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 37 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. No
spectrum from the promptly downlinked event data is yet available to
determine the column density.

The initial flux in the 2.5 s image was 1.18e-09 erg cm^-2 s^-1 (0.2-10
keV).

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 144 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
  RA(J2000)  =  12:10:07.01 = 182.52919
  DEC(J2000) = +67:14:07.0  =  67.23528
with a 90%-confidence error radius of about 1.10 arc sec. This position is 9.9
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.28. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.02.

Burst Advocate for this burst is E. Ambrosi (elena.ambrosi AT inaf.it).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190613A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24799
SUBJECT: GRB 190613A: Fermi GBM Final Real-time Localization
DATE:    19/06/13 04:19:01 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 04:07:18 UT on 13 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190613A (trigger 582091643.234478 / 190613172).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 176.4, Dec = 64.8 (J2000 degrees, equivalent to J2000 11h 45m, 64d 47'), with a statistical uncertainty of 3.0 degrees.

The angle from the Fermi LAT boresight is 11.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613172/quicklook/glg_skymap_all_bn190613172.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613172/quicklook/glg_healpix_all_bn190613172.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613172/quicklook/glg_lc_medres34_bn190613172.gif


GRB_name: GRB190613A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24800
SUBJECT: GRB 190613A: BALROG localization (Fermi Trigger 582091643 / GRB 190613172)
DATE:    19/06/13 04:32:11 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

J. Burgess, B. Biltzinger, F. Kunzweiler, F. Berlato, & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
582091643 at 04:07:18 on 13 June 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 200.2+/-13.8 deg
Decl.(2000.0) = 66.4+/-3.8 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190613172/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190613172/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190613172/json

                        


GRB_name: GRB190613A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24801
SUBJECT: GRB 190613A: KAIT Optical Afterglow Confirmation
DATE:    19/06/13 05:02:42 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to the Swift GRB 190613A (Ambrosi et al.,
GCN 24798) starting at 734s after the burst. Observations were
performed with a sequence in the clear (roughly R), V, and I filters,
and the exposure time was 60 s per image. We detected a fading source
at the Swift/UVOT reported afterglow position (Ambrosi et al.,
GCN 24798) in all the filters. We estimate the clear band magnitude
to be ~18.2 at 764s after the burst and faded to ~19.0 at 1290s after the
burst.
Observation are on going, multi-band follow-ups are encouraged.

[GCN OPS NOTE(14jun19):  The typo in Swift's name was corrected.]


GRB_name: GRB190613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24803
SUBJECT: GRB 190613A: MASTER OT detection 
DATE:    19/06/13 07:48:54 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E.Gorbovskoy, V.Kornilov, N.Tiurina, A.Kuznetsov, I.Gorbunov, 
V.Vladimirov, P.Balanutsa, D.Vlasenko, D.Zimnukhov, F.Balakin,A. Chasovnikov,
V.Topolev, V.Senik, D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department),

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias),

D. Buckley (South African Astronomical Observatory),

R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University),

H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE, SJNU)

O. Gress, N.M. Budnev, O.Ershova, S.Yazev (Applied Physics Institute, Irkutsk State University),

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational State University),

A. Tlatov, D.Dormidontov, A.V. Parhomenko (Kislovodsk Solar  Station of the Pulkovo Observatory),

MASTER-IAC robotic telescope (MASTER Global Robotic Net:  Lipunov et al., 
2010, Advances in Astronomy,vol.2010, 30L  (http://observ.pereplet.ru)
located in Spain (IAC Teide Observatory) was pointed to 
the  GRB 190613A (Swift alert, Ambrosi et al. GCN 24798, Fermi 
localization GCN 24799, BALROG localization Burgess et al. GCN 24800)
38 sec after notice time (104 sec after trigger time)
at 2019-06-13 04:09:09 UT (Lipunov et al. GCN 24802).

On our first (20s exposure)  set MASTER auto-detection system
found 1 optical transient within Swift error-box (ra=182.558 dec=67.2325 r=0.05) 
brighter than 16.4.


  T-Tmid      Date      Time       Expt.        Ra                Dec           Mag
---------|---------------------|-------|-----------------|-----------------|-------
      114   2019-06-13 04:09:09      20   ( 12h 10m 07.08s , +67d 14m 06.5s)    15.96


this OT, discovered by Swift and also confirmed by KAIT(Ambrosi et al. GCN 24798, WeiKang Zheng et al. GCN 24801)

The 5-sigma upper limit has been about 16.4mag


GRB_name: GRB190609A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24804
SUBJECT: GRB 190609A: AstroSat CZTI detection
DATE:    19/06/13 09:39:49 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma, D. Bhattacharya, T. Khanam and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190609A, which was also detected by Fermi GBM (GCN #24773) and BALROG (Burgess J. et al., GCN #24774).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 07:34:44.5 UT. The measured peak count rate associated with the burst is 555 cts/s above the background in the combined data of four quadrants, with a total of 7392 cts. The local mean background count rate was 521 cts/s. Using cumulative rates, we measure a T90 of 40.1 s. In preliminary analysis, we find that 550 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190610A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24805
SUBJECT: GRB 190610A: CALET Gamma-Ray Burst Monitor detection
DATE:    19/06/13 10:21:46 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

T. Tamura (Kanagawa U),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita(AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu (Kanagawa U),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The short GRB 190610A (Swift-BAT trigger #907754: Evans et al., GCN
Circ. 24775, Palmer et al., GCN Circ. 24783; Insight-HXMT/HE detection:
Cai et al., GCN Circ. 24782) triggered the CALET Gamma-ray Burst Monitor
(CGBM) at 11:27:45.359 UTC on 10 June 2019. The burst signal was seen
by all CGBM detectors.

The burst light curve shows a single pulse which starts at T+0.58 sec,
peaks at T+0.83 sec and ends at T+1.41 sec. The T90 and T50 durations
measured by the SGM data are 0.61 +- 0.16 sec and 0.26 +- 0.05 sec
(40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1244201256/

The CALET data used in this analysis are provided by the Waseda CALET
Operation Center located at the Waseda University.


GRB_name: GRB190613B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24806
SUBJECT: GRB 190613B: Fermi GBM Final Real-time Localization
DATE:    19/06/13 10:58:04 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 10:47:00 UT on 13 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190613B (trigger 582115625.049376 / 190613449).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 305.4, Dec = -11.6 (J2000 degrees, equivalent to J2000 20h 21m, -11d 35'), with a statistical uncertainty of 3.2 degrees.

The angle from the Fermi LAT boresight is 60.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613449/quicklook/glg_skymap_all_bn190613449.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613449/quicklook/glg_healpix_all_bn190613449.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613449/quicklook/glg_lc_medres34_bn190613449.gif


GRB_name: GRB190613B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24807
SUBJECT: GRB 190613B: Swift detection of a burst with an optical counterpart
DATE:    19/06/13 10:58:54 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA), V. D'Elia (SSDC),
J.D. Gropp (PSU), N. J. Klingler (PSU), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 10:47:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190613B (trigger=908329).  Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 305.422, -4.664 which is
   RA(J2000) = 20h 21m 41s
   Dec(J2000) = -04d 39' 49" 
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 15 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~1 sec after the trigger.

The XRT began observing the field at 10:48:39.5 UT, 97.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 305.4294, -4.6461 which is equivalent to:
   RA(J2000)  = 20h 21m 43.06s
   Dec(J2000) = -04d 38' 46.0"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 69 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy.

The initial flux in the 2.5 s image was 4.90e-09 erg cm^-2 s^-1 (0.2-10
keV).

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 105 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  =  20:21:43.65 = 305.43189
  DEC(J2000) = -04:38:47.9  =  -4.64665
with a 90%-confidence error radius of about 0.62 arc sec. This position is 9.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.76 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.07.

Burst Advocate for this burst is A. D'Ai (antonino.dai AT inaf.it).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190613B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24808
SUBJECT: GRB 190613B: BALROG localization (Fermi Trigger 582115625 / GRB 190613449)
DATE:    19/06/13 11:13:48 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

J. Burgess, F. Kunzweiler, B. Biltzinger, F. Berlato,  & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
582115625 at 10:47:00 on 13 June 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 302.8+/-2.3 deg
Decl.(2000.0) = -8.2+/-2.7 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190613449/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190613449/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190613449/json

                        


GRB_name: GRB190613A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24809
SUBJECT: GRB 190613A: Enhanced Swift-XRT position
DATE:    19/06/13 11:26:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 3378 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 190613A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 182.52964, +67.23535 which is equivalent
to:

RA (J2000): 12h 10m 7.11s
Dec (J2000): +67d 14' 07.3"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB190613A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24810
SUBJECT: GRB 190613A: Swift-XRT refined Analysis
DATE:    19/06/13 12:51:45 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (ASDC), A. D'Ai
(INAF-IASFPA), A. Melandri (INAF-OAB), A. Tohuvavohu (PSU), S. J.
LaPorte (PSU) and  report on behalf of the Swift-XRT team: report on
behalf of the Swift-XRT team:

We have analysed 8.1 ks of XRT data for GRB 190613A, from 142 s to 18.3
ks after the  BAT trigger. The data comprise 127 s in Windowed Timing
(WT) mode with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Osborne et al. (GCN Circ.
24809).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=5.1 (+1.1, -0.9). At T+174 s  the decay
flattens to an alpha of -1.500000 (+0.905300, -0.000007). The light
curve breaks again at T+207 s to a decay with alpha=5.0 (+0.7, -0.6), 
and  again at T+372 s s to alpha=1.44 (+0.18, -0.15),  before a final
break at T+7345 s s after which the decay index is -1.5 (+0.0, -1.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.01 (+/-0.12). The
best-fitting absorption column is  5.1 (+2.8, -2.6) x 10^20 cm^-2, in
excess of the Galactic value of 1.5 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.75 (+0.22, -0.15)
and a best-fitting absorption column of 2.0 (+4.9, -0.5) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.7 x 10^-11 (3.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.0 (+4.9, -0.5) x 10^20 cm^-2
Galactic foreground: 1.5 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.75 (+0.22, -0.15)

If the light curve continues to decay with a power-law decay index of
-1.5, the count rate at T+24 hours will be 0.41 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.5 x
10^-11 (1.6 x 10^-11) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00908288.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190611B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24811
SUBJECT: IPN Triangulation of GRB 190611B
DATE:    19/06/13 14:03:15 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:

The long-duration GRB 190611B (Malacaria and Meegan, GCN Circ. 24794) 
was detected by Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS),
Mars-Odyssey (HEND), and Swift (BAT) at about 82069 s UT (22:47:49).

The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    84.968 (05h 39m 52s) +52.773 (+52d 46' 24")
  Corners:
    81.481 (05h 25m 55s) +50.833 (+50d 49' 57")
    88.130 (05h 52m 31s) +54.352 (+54d 21' 06")
    89.119 (05h 56m 29s) +54.477 (+54d 28' 38")
    82.284 (05h 29m 08s) +51.059 (+51d 03' 34")
  ---------------------------------------------
The error box area is about 1.15 sq. deg, and its maximum
dimension is 5.9 deg (the minimum one is 6.42 arcmin).
The Sun distance was about 30 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190611_T82065/IPN/

The Konus-Wind time history and spectrum will be given in a forthcoming
GCN Circular.


GRB_name: GRB190613B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24812
SUBJECT: GRB 190613B: Enhanced Swift-XRT position
DATE:    19/06/13 14:19:40 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2078 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 190613B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 305.43206, -4.64686 which is equivalent
to:

RA (J2000): 20h 21m 43.69s
Dec (J2000): -04d 38' 48.7"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB190611B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24813
SUBJECT: GRB 190611B: BALROG localization (Fermi Trigger 581986074 / GRB 190611950)
DATE:    19/06/13 14:34:27 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

 F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
581986074 at 22:47:49 on 11 June 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 85.2+/-1.1 deg
Decl.(2000.0) = 52.0+/-1.0 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190611950/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190611950/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190611950/json

                        


GRB_name: GRB190613B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24814
SUBJECT: GRB 190613B: Fermi GBM observation
DATE:    19/06/13 16:35:51 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

E. Bissaldi (Politecnico & INFN Bari), O.J. Roberts (USRA/NASA) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 10:47:00.05 UT on 13 June 2019, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 190613B (trigger 582115625 / 190613449),
which was also detected by the Swift/BAT (D'Ai et al. 2019, GCN 24807)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time using
the Swift-BAT position is 59 degrees.

The GBM light curve consists of single bright peak
with a duration (T90) of about 5 s (50-300 keV).
The time-averaged spectrum from T0-1 s to T0+4 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.96 +/- 0.05 and
the cutoff energy, parameterized as Epeak, is 334 +/- 35 keV.

The event fluence (10-1000 keV) in this time interval is
(4.4 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2 s in the 10-1000 keV band
is 7.5 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB190613A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24815
SUBJECT: GRB 190613A: Swift/UVOT Detection
DATE:    19/06/13 17:36:46 GMT
FROM:    Frank Marshall at Swift/UVOT  <marshall@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and E. Ambrosi (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190613A
145 s after the BAT trigger (Ambrosi et al., GCN Circ. 24798).
A source consistent with the enhanced XRT position
(Osborne et al. GCN Circ. 24809)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  12:10:07.01 = 182.52920 (deg.)
    Dec (J2000) = +67:14:07.0  =  67.23529 (deg.)
with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:
Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white              145          295          147         17.88 +/- 0.04
v                  634         1061           58         18.63 +/- 0.29
b                  560          753           39         18.93 +/- 0.21
u                  303          553          246         18.88 +/- 0.11
w1                 685        11118         1121        >20.1
m2                5323         6859          296        >20.8
w2                4913         6548          393        >21.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190613A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24816
SUBJECT: GRB 190613A: Fermi GBM detection
DATE:    19/06/13 17:38:42 GMT
FROM:    Suraj Poolakkil at UAH  <sp0076@uah.edu>

S. Poolakkil (UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 04:07:18.23 UT on 13 June 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190613A (trigger 582091643/ 190613172),
which was also detected by the Swift/BAT (Ambrosi et al. 2019, GCN 24798).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight
at the GBM trigger time is 9 degrees.

The GBM light curve shows a single peak
with a duration (T90) of about 18 s (50-300 keV).
The time-averaged spectrum from T0-1.0 s to T0+19.4 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is 0.06 +/- 0.18 and
the cutoff energy, parameterized as Epeak, is 108 +/- 5 keV.

The event fluence (10-1000 keV) in this time interval is
(3.092 +/- 0.129)E-06 erg/cm^2. The 1-sec peak photon flux
measured starting from T+11.9 s in the 10-1000 keV band
is 2.3 +/- 0.2 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB190613B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24817
SUBJECT: GRB 190613B: Swift/UVOT Detection
DATE:    19/06/13 17:39:39 GMT
FROM:    Frank Marshall at Swift/UVOT  <marshall@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190613B
106 s after the BAT trigger (D'Ai et al., GCN Circ. 24807).
A source consistent with the enhanced XRT position
(Beardmore et al. GCN Circ. 24812)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  20:21:43.66 = 305.43191 (deg.)
    Dec (J2000) = -04:38:48.0  =  -4.64666 (deg.)
with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white              106          256          147         17.84 +/- 0.04
v                  648          667           19        >18.0
b                  574          594           19        >18.7
u                  318          568          246         18.86 +/- 0.12
w1                 697          717           19        >18.6
m2                 672          692           19        >18.4
w2                 624          643           19        >18.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.07 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190613B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24818
SUBJECT: GRB 190613B: KAIT Optical Afterglow Confirmation
DATE:    19/06/13 18:48:19 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to the Swift GRB 190613B (D'Ai et al.
GCN 24807) starting at 2311s after the burst. Observations were
performed with a sequence in the clear (roughly R), V, and I filters,
and the exposure time was 20 s per image. We detected the optical
afterglow at the reported Swift/UVOT position (D'Ai et al., GCN 24798;
Marshall & D'Ai, GCN 24817) in clear band image. We estimate the
clear band magnitude to be ~19.3 at 2321s after the burst.

[GCN OPS NOTE(14jun19):  The typo in Swift's name was corrected.]


GRB_name: GRB190613A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24819
SUBJECT: GRB 190613A, Swift-BAT refined analysis
DATE:    19/06/13 19:46:50 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. Stamatikos (OSU), E. Ambrosi (INAF-IASFPA)
S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190613A (trigger #908288)
(Ambrosi et al., GCN Circ. 24798).  The BAT ground-calculated position is
RA, Dec = 182.552, 67.244 deg which is
   RA(J2000)  =  12h 10m 12.5s
   Dec(J2000) = +67d 14' 39.7"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 9%.

The mask-weighted light curve shows a weak pulse that starts at ~T0, peaks
at ~T+7 s, and ends at ~T+20 s. T90 (15-350 keV) is 17.6 +- 3.1 sec
(estimated error including systematics).

The time-averaged spectrum from T+0.6 to T+20.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.22 +- 0.26.  The fluence in the 15-150 keV band is 1.7 +- 0.3 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+6.88 sec in the 15-150 keV band
is 1.5 +- 0.7 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/908288/BA/

[GCN OPS NOTE(13jun19): Per author's request, in the 3rd line
"GCN Circ. 908288" was corrected to read "GCN Circ. 24798".


GRB_name: GRB190613B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24820
SUBJECT: GRB 190613B: Swift-BAT refined analysis
DATE:    19/06/13 19:48:02 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), A. D'Ai (INAF-IASFPA),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU),
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 190613B (trigger #908329)
(D'Ai et al., GCN Circ. 24807).  The BAT ground-calculated position is
RA, Dec = 305.434, -4.655 deg which is
   RA(J2000)  =  20h 21m 44.2s
   Dec(J2000) = -04d 39' 17.0"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 18%.

The mask-weighted light curve shows a main pulse structure that starts
at ~T-3 s, peaks at ~T0, and ends at ~T+2 s. In addition, there are
some weak emissions that lasts until ~T+175 s. T90 (15-350 keV)
is 160.84 +- 16.83 sec (estimated error including systematics).

The time-averaged spectrum from T-2.85 to T+175.42 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.84 +- 0.24.  The fluence in the 15-150 keV band is 2.3 +- 0.3 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+0.01 sec in the 15-150 keV band
is 5.7 +- 0.7 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/908329/BA/

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GRB_name: GRB190610A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24821
SUBJECT: GRB 190610A: Swift ToO observations
DATE:    19/06/13 20:26:46 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a ToO observation of the Swift/BAT GRB 190610A. 
Automated analysis of the XRT data will be presented online at
http://www.swift.ac.uk/ToO_GRBs/00020896

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the Swift/BAT event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190613A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24822
SUBJECT: GRB 190613A: FRAM-ORM afterglow detection
DATE:    19/06/13 20:37:13 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ),
Martin Masek, Petr Janecek, Sergey Karpov, Jakub Jurysek,
Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza
(Institute of Physics, Prague, CZ)

report:

The 25cm robotic telescope FRAM-ORM at La Palma (Spain)
reacted robotically to the alert of GRB190613A (Ambrosi et al,
GCNC 24798), starting with a series of 20 s unfiltered images
at 04:10:11 UT, i.e. 3 min post trigger.

We clearly detect the source reported by (Ambrosi et al, GCN
24798; Zheng & Filipenko, GCN 24801 and Lipunov et al, GCN
24803), decaying at a rate of alpha ~ 1.51. The brightnes of
the object was R = 18.2 +- 0.2 at an image centered at 04:25:15
UT, i.e. 18 min post burst.

[GCN OPS Note(15jun19): Per OPS, the extra "Subject:" was removed
from the Subject line.]


GRB_name: GRB190613B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24823
SUBJECT: GRB 190613B: Swift-XRT refined Analysis
DATE:    19/06/13 22:01:33 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U.
Leicester), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), A.
Tohuvavohu (PSU), S. J. LaPorte (PSU), J.A. Kennea (PSU) and A. D'Ai
report on behalf of the Swift-XRT team:

We have analysed 6.3 ks of XRT data for GRB 190613B (D'Ai et al. GCN
Circ. 24807), from 103 s to 19.3 ks after the  BAT trigger. The data
comprise 352 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN Circ. 24812).

The late-time light curve (from T0+5.3 ks) can be modelled with a
power-law decay with a decay index of alpha=0.52 (+/-0.11).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.93 (+/-0.05). The
best-fitting absorption column is  3.28 (+0.24, -0.23) x 10^21 cm^-2,
in excess of the Galactic value of 6.0 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.90 (+/-0.11) and a
best-fitting absorption column of 2.6 (+0.5, -0.4) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.8 x 10^-11 (5.2 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.6 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 6.0 x 10^20 cm^-2
Excess significance: 7.6 sigma
Photon index:      1.90 (+/-0.11)

If the light curve continues to decay with a power-law decay index of
0.52, the count rate at T+24 hours will be 0.091 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.5 x
10^-12 (4.8 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00908329.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190613B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24825
SUBJECT: GRB 190613B: Optical observations from NOT
DATE:    19/06/14 04:57:01 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D.B. Malesani 
(DTU Space), K.E. Heintz (U.Iceland), S. Moran (UTU, NOT) report 
on behalf of a larger collaboration:

We observed the field of GRB 190613B (Dâ€™Ai et al. GCN 24807, 
Burgess et al. GCN 24808, Beardmore et al. GCN 24812, Bissaldi et 
al. GCN 24814, Marshall et al. GCN 24817, Zheng & Filippenko 
GCN 24818, Ukwatta et al. GCN 24820, Page et al. GCN 24823) 
using STANCAM, mounted on the 2.5m Nordic Optical Telescope, at 
Roque de los Muchachos Observatory (La Palma, Spain). The 
observations consisted of 3x300s imaging in R-band and 5x200s in 
z-band. Observations started on 14 June at 2:50 UT (16.05 hr after 
the burst). The optical counterpart is well detected in both bands at 
an estimated R(Vega) = 21.8+/-0.2 mag, as compared to field stars 
from the Nomad catalogue.


GRB_name: GRB190613B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24826
SUBJECT: GRB 190613B: BOOTES-5/JGT early optical observations
DATE:    19/06/14 05:04:33 GMT
FROM:    Alberto J. Castro-Tirado at IAA-CSIC  <ajct@iaa.es>

Y.-D. Hu, X.-Y.Li, I. Carrasco, E. Fernandez-Garcia, A. Ayala and
A. J. Castro-Tirado (IAA-CSIC), D. Hiriart and W. H. Lee (UNAM),
S. Jeong and I. H. Park (SKKU) and M. D. Caballero-Garcia (ASU-CAS, CZ)
on behalf of a larger collaboration, report:

The 60cm BOOTES-5/JGT robotic telescope at Observatorio Astronomico
Nacional in San Pedro Martir (Mexico) automatically responded to the
Swift trigger of GRB 190613B (D'Ai et al., GCNC 24807). The first image
(1s exposure, clear-filter) was obtained at 10:48:04.16 UT (i.e. 62s
post-burst). We detect the optical afterglow at the position reported
by Swift (Beardmore et al. GCNC 24812, Marshall et al. GCNC 24817)
with R = 16.1. A sequence of images was obtained and the analysis is on
going. The magnitude is calibrated against the USNO-B1 catalog and is
not corrected for Galactic extinction in the direction of the GRB.

We thank the staff at Observatorio Astronomico Nacional in San Pedro
Martir for its excellent support.


GRB_name: GRB190611B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24827
SUBJECT: Konus-Wind observation of GRB 190611B
DATE:    19/06/14 12:22:39 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, A. Kozlova,
A.Lysenko,  D. Svinkin, A. Tsvetkova,  M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:

The long GRB 190611B
(Fermi GBM detection: Malacaria & Meegan, GCN 24794;
IPN triangulation: Hurley et al., GCN 24811)
triggered Konus-Wind (KW) at T0=82065.599 s UT (22:47:45.599).

The light curve of the burst shows two broad, multi-peaked pulses.
The total duration of the burst is ~130 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190611_T82065/

As observed by Konus-Wind, the burst had
a fluence of (9.2 Â± 1.0)x10^-5 erg/cm2 and
a 64-ms peak energy flux, measured from T0+17.344,
of (1.33 Â± 0.11)x10^-5 erg/cm2 (both in the 20 keV - 10 MeV
energy range).

The time-integrated spectrum (measured from T0 to T0+117.760 s)
is best fit in the 20 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.01 (-0.08,+0.08),
the high energy photon index beta = -2.74 (-0.88,+0.29),
the peak energy Ep = 250 (-21,+24) keV,
chi2 = 68/97 dof.

The spectrum near the peak count rate (measured from T0+67.840 s
to T0+77.568 s) is best fit in the 20 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.78 (-0.08,+0.09),
the high energy photon index beta = -2.20 (-0.13,+0.10),
the peak energy Ep = 307 (-29,+33) keV,
chi2 = 83/97 dof.

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB190610A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24828
SUBJECT: Konus-Wind observation of short/hard GRB 190610A
DATE:    19/06/14 14:06:17 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, A. Kozlova,
A.Lysenko,  D. Svinkin, A. Tsvetkova,  M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:

The short GRB 190610A
(Swift-BAT detection: Evans et al., GCN 24775;
Insight-HXMT/HE detection: Cai et al., GCN 24782)
triggered Konus-Wind (KW) at T0=41263.560 s UT (11:27:43.560).

The light curve of the burst shows a single, multi-peaked pulse
with a total duration of ~0.6 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190610_T41263/

As observed by Konus-Wind, the burst had
a fluence of (7.65 Â± 1.48)x10^-6 erg/cm^2 and
a 16-ms peak energy flux, measured from T0+0.080,
of (2.43 Â± 0.31)x10^-5 erg/cm^2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured from T0 to T0+0.256 s)
is well fitted in the 20 keV - 20 MeV range
by a cutoff power-law (CPL) function with the following model
parameters: the photon index alpha = -0.28(-0.26,+0.33),
and the peak energy Ep = 903(-181,+251) keV, chi2 = 53/47 dof.
Fitting this spectrum with the GRB (Band) function yields
nearly the same alpha and Ep, and an upper limit on beta of -2.3.

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB190613B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24829
SUBJECT: GRB 190613B: Insight-HXMT/HE detection
DATE:    19/06/14 14:23:15 GMT
FROM:    Qi Luo at IHEP  <luoqi@ihep.ac.cn>

Q. Luo, S. Xiao, C. Cai, Q. B. Yi, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:

At 2019-06-13T10:47:00.00 (T0), Insight-HXMT/HE detected 
GRB 190613B (trigger ID: HEB190613449) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #24806) and Swift/BAT 
(D'Ai et al. 2019, GCN #24807). 

The Insight-HXMT/HE light curve mainly consists of two 
pulses with a duration (T90) of 3.59 s measured from T0-0.56 s. 
The 1-ms peak rate, measured from T0+2.09 s, is 2847 cnts/sec. 
The total counts from this burst is 6013 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190613449_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190611B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24830
SUBJECT: GRB 190611B: CALET Gamma-Ray Burst Monitor detection
DATE:    19/06/14 14:25:24 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

N. Cannady (GSFC/UMBC),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long, bright GRB 190611B (Fermi GBM detection: Malacaria and Meegan,
GCN Circ. 24794; IPN Triangulation: Hurley et al., GCN Circ. 24811; BALROG
localization: Kunzweiler et al., GCN Circ. 24813) triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 22:47:46.257 UTC on 11 June 2019.
The burst signal was seen by all CGBM detectors.

The burst light curve shows two multi-peaked pulses: the first starts
at T+2.8 sec, peaks at T+4.9 sec and ends at T+16.9 sec, the second starts
at T+67.4 sec, peaks at T+75.4 sec and ends at T+118.8 sec. The T90 and
T50 durations measured by the SGM data are 100.9 +- 3.9 sec and
13.9 +- 1.1 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1244328454/

The CALET data used in this analysis are provided by the Waseda CALET
Operation Center located at the Waseda University.


GRB_name: GRB190613B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24831
SUBJECT: GRB 190613B: GROND Detection of the Optical/NIR Afterglow
DATE:    19/06/14 14:41:35 GMT
FROM:    Patricia Schady at Swift  <p.schady@bath.ac.uk>

P. Schady (Uni. Bath) and J. Bolmer (MPE Garching) report:


We observed the field of GRB 190613B (Fermi trigger 582115625.049376/190613449; GCN #24806, Swift trigger 908329; D'Ai et al., GCN #24807) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile).


Observations started at 09:18 UT on 14 June 2019, 22.4 hrs after the GRB trigger. They were performed at an average seeing of 1.4" and at an average airmass of 1.2.


We detect a single point source in our g'r'i'z'JH images consistent with the reported GRB optical and X-ray afterglow (Beardmore et al., GCN #24812, Marshall et al., GCN #24817). Based on a total 22 min exposure in g'r'i'z' and 22 min in JHK, we estimate the following preliminary magnitudes (all in Vega system):


g' = 22.79 +/- 0.05 mag
r' = 22.05 +/- 0.04 mag
i' = 21.56 +/- 0.05 mag
z' = 21.15 +/- 0.07 mag
J = 20.5 +/- 0.1 mag
H = 20.2 +/- 0.2 mag
K > 19.8 mag


Given magnitudes are calibrated against PanStarrs as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.06 mag in the direction of the burst (Schlafly & Finkbeiner 2011).

We thank the observer astronomer at the MPG 2.2m in La Silla for their help in obtaining these data.


GRB_name: GRB190613B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24832
SUBJECT: GRB 190613B: Optical observation from Asiago Schmidt
DATE:    19/06/14 15:13:45 GMT
FROM:    Sheng Yang at OAPD, INAF  <saberyoung@gmail.com>

S. Yang, L. Tomasella, E. Cappellaro (OAPD, INAF) and N. Khetan (GSSI, L'Aquila)

Using the 0.92m Asiago Schmidt telescope, we observed the field of GRB 190613B 11.954 h after the burst (Dâ€™Ai et al. GCN 24807)  in g, r and i.
We detected a source consistent with the optical and X-ray afterglow (Burgess et al. GCN 24808, Beardmore et al. GCN 24812, Bissaldi et al. GCN 24814, Marshall et al. GCN 24817, Zheng & Filippenko GCN 24818, Ukwatta et al. GCN 24820, Page et al. GCN 24823) in g band images while we could only set upper limits in the other bands.
The measured magnitude and 2.5-sigma upper limits are listed below:

Filter T_start   T_stop   JD_avg  Exp(s) Mag
g 2019-06-13T22:44:17 2019-06-13T23:02:00 58647.95239 180*5 21.40 +/- 0.30
r 2019-06-13T23:02:14 2019-06-13T23:20:00 58647.96488 180*5 > 20.1
i 2019-06-13T23:23:32 2019-06-13T23:34:38 58647.97735 180*5 > 20.4


GRB_name: GRB190610A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24833
SUBJECT: GRB 190610A: Swift-XRT observations
DATE:    19/06/14 15:34:31 GMT
FROM:    Aaron Tohuvavohu at PSU/Swift  <auc444@psu.edu>

A.P. Beardmore (U. Leicester), A. Melandri (INAF-OAB), P. D'Avanzo
(INAF-OAB), M.G. Bernardini (INAF-OAB), J.A. Kennea (PSU), B.
Sbarufatti (INAF-OAB/PSU), J.P. Osborne (U. Leicester) and P.A. Evans
(U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Swift/BAT-detected burst GRB 190610A (Palmer et al. GCN Circ. 24783),
collecting 5.0 ks of Photon Counting (PC) mode data between T0+292.3 ks
and T0+300.5 ks. 

One uncatalogued X-ray source has been detected consistent with being
within 187 arcsec of the Swift/BAT position, it is below the RASS limit
and shows no definitive signs of fading. Therefore, at the present time
we cannot confirm this as the afterglow. Details of this source are
given below:

Source 7:
  RA (J2000):  46.2216  =  03:04:53.17
  Dec (J2000): -7.6824  =  -07:40:56.7
  Error: 5.3 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (1.76 [+0.83, -0.64])e-3 ct s^-1  
  Distance: 111 arcsec from Swift/BAT position.
  Flux: (1.17 [+0.55, -0.42])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


We note that the position of this afterglow candidate is consistent
with the galaxy SDSS J030452.77-074055.3 (r=21.5 AB), which has unknown
redshift. 

Five uncatalogued sources were also detected too far from the GRB
position to be likely afterglow candidates.

The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
http://www.swift.ac.uk/ToO_GRBs/00020896.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190610A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24834
SUBJECT: GRB 190610A: Swift/UVOT Upper Limits
DATE:    19/06/14 17:08:39 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P.M. Kuin (UCL/MSSL) and P.A. Evans (Leicester U)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190610A
292282 s after the BAT trigger (Evans et al., GCN Circ. 24775).
No optical afterglow consistent with the BAT position or the XRT
candidate position (Beardmore et al., GCN Circ. No. 24833) has been
detected in the initial UVOT exposures.  Preliminary 3-sigma upper
limits using the UVOT photometric system (Breeveld et al. 2011,
AIP Conf. Proc. 1358, 373) for the initial exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

v               292282       300459         4890         >20.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.09 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24835
SUBJECT: GRB 190613A: SEDM Observations
DATE:    19/06/15 01:26:58 GMT
FROM:    Virginia Cunningham at U of MD  <vcunning@astro.umd.edu>

V. Cunningham (U of Maryland), J. D. Neill (Caltech), S. B. Cenko
(NASA GSFC), and R. Walters (Caltech) report on behalf of the
SEDM team:

We observed the optical counterpart to GRB 190613A (Ambrosi et al., GCN
24798) with the Spectral Energy Distribution Machine (SEDM) on the 60 inch
telescope at Palomar Observatory. The SEDM is a low resolution (R ~ 100)
integral field unit spectrometer with a multi-band (ugri) rainbow camera imager
(see Blagorodnova et al. 2018, PASP, 130, 035003, and Rigault et al. 2019,
astro-ph/1902.08526).

The SEDM began observing the optical counterpart at 04:18:22 UTC (8.75
minutes after the burst trigger time). We performed an 1800 s exposure over the
wavelength range 3800-9200 A. The continuum emission is well-fit by a power
law spectrum with index alpha = 0.56 (f_nu ~ nu^-alpha).  We detect an
absorption line at an observed wavelength of ~ 4597 A. We tentatively identify
this line as due to Lyman alpha at z = 2.78 - however due to the lack of
corroborating features we consider this redshift tentative currently.

[GCN OPS NOTE(07sep19): Per author's request, in the last paragraph,
the "alpha = 0.56" was changed to "alpha = 1.4".]


GRB_name: GRB190613B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24836
SUBJECT: GRB 190613B: SEDM Observations
DATE:    19/06/15 01:26:59 GMT
FROM:    Virginia Cunningham at U of MD  <vcunning@astro.umd.edu>

V. Cunningham (U of Maryland), J. D. Neill (Caltech), S. B. Cenko
(NASA GSFC), and R. Walters (Caltech) report on behalf of the
SEDM team:

We observed the optical counterpart to GRB 190613B (D'Ai et al. GCN 24807)
with the Spectral Energy Distribution Machine (SEDM) on the 60 inch
telescope at Palomar Observatory. The SEDM is a low resolution (R ~ 100)
integral field unit spectrometer with a multi-band (ugri) rainbow camera imager
(see Blagorodnova et al. 2018, PASP, 130, 035003, and Rigault et al. 2019,
astro-ph/1902.08526).

The SEDM began observing the optical counterpart at 11:00:28 UTC (11.79
minutes after the burst trigger time). We performed an 1800 s exposure over
the wavelength range 3800-9200 A.  We tentatively identify an absorption
feature at ~ 5385 A that is consistent with the Mg II 2796,2803 doublet at
z = 0.92. However, due to the relatively low significance of the feature and
the lack of corroborating lines, we cannot confirm this redshift currently.
The continuum emission is well-fit by a power law spectrum with index alpha = 1.8
(f_nu ~ nu^-alpha).

[GCN OPS NOTE(07sep19): Per author's request, In the last sentence,
the "alpha = 0.09" was changed to "alpha = 1.8".]


GRB_name: GRB190613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24838
SUBJECT: GRB 190613A: Kitab and AbAO optical upper limit
DATE:    19/06/15 09:38:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Novichonok (KIAM), A. Zhornichenko (KIAM), R. Ya. 
Inasaridze (AbAO),  V.R. Ayvazian (AbAO), A. Pozanenko (IKI), E. Mazaeva 
(IKI), A. Volnova (IKI), I. Molotov (KIAM), Sh. Ehgamberdiev (UBAI) report 
on behalf of larger IKI GRB FuN collaboration:

We observed the field of the  GRB 190613A (Ambrosi et al., GCN  24798) 
with RC-36  telescope of Kitab Observatory  and AS-32 of Abastumani 
observatory . We do not detect the optical afterglow (Ambrosi et al., GCN 
24798; Zheng et al., GCN  24801;  Lipunov et al., GCN  24803).  Preliminary 
photometry of the field is following.

Date       UT start   t-T0       Filter Exp.   OT  Err.   UL(3sigma) 
Telescope
                       (mid, days)        (s)

2019-06-13 16:26:41  0.54575    CR     5500  n/d  n/d   20.6  RC-36
2019-06-13 21:33:40  0.73706      R      1800  n/d  n/d   21.0  AS-32


The photometry is based on the nearby USNO-B1 (R2) stars
USNO-B1.0_id  R2
1572-0165015 13.62
1572-0164999 14.91
1572-0164916 14.28

[GCN OPS NOTE(15jun19): Per OPS, the typo in the Subject-line
"1906013A" was changed to "190613A".]


GRB_name: GRB190615A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24839
SUBJECT: GRB 190615A: Fermi GBM Final Real-time Localization
DATE:    19/06/15 15:28:10 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 15:16:27 UT on 15 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190615A (trigger 582304592.372344 / 190615636).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 191.4, Dec = 49.4 (J2000 degrees, equivalent to J2000 12h 45m, 49d 23'), with a statistical uncertainty of 2.3 degrees.

The angle from the Fermi LAT boresight is 122.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190615636/quicklook/glg_skymap_all_bn190615636.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190615636/quicklook/glg_healpix_all_bn190615636.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190615636/quicklook/glg_lc_medres34_bn190615636.gif


GRB_name: GRB190613B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24841
SUBJECT: GRB 190613B: Kitab observatory optical upper limit
DATE:    19/06/16 14:10:05 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Novichonok (KIAM), A. Zhornichenko (KIAM),  A. Pozanenko 
(IKI), E. Mazaeva  (IKI), A. Volnova (IKI), I. Molotov (KIAM), Sh. 
Ehgamberdiev (UBAI)  report on behalf of larger GRB IKI FuN collaboration:

We observed the field of the  GRB 190613B    (D'Aiet al., GCN  24807) with 
RC-36 0.36-m telescope of Kitab Observatory starting on June 13  (UT) 
22:26:32 in  Clear filter.    We do not detect the optical afterglow 
(D'Aiet al., GCN  24807; Marshall al., GCN  24817; Zheng al., GCN  24818; 
Ugarte Postigo al., GCN  24825; Hu al., GCN  24826).
Preliminary photometry of the field is following.

Date       UT start   t-T0       Filter Exp.   OT  Err.   UL(3sigma)
                       (mid, days)        (s)

2019-06-13  20:55:3    0.43001     CR     3600  n/d  n/d   20.0

The photometry is based on the nearby USNO-B1  (R2) stars.

USNO-B1.0_id R2
0853-0556521 16.14
0853-0556781 16.31


GRB_name: GRB190615A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24842
SUBJECT: GRB 190615A: Insight-HXMT/HE detection
DATE:    19/06/17 05:36:47 GMT
FROM:    Qi Luo at IHEP  <luoqi@ihep.ac.cn>

Q. Luo, S. Xiao, C. Cai, Q. B. Yi, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:

At 2019-06-15T15:16:27.00 (T0), Insight-HXMT/HE detected 
GRB 190615A (trigger ID: HEB190615636) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #24839). 

The Insight-HXMT/HE light curve mainly consists of a single 
pulse with a duration (T90) of 16.33 s measured from T0-1.65 s. 
The 1-ms peak rate, measured from T0+7.80 s, is 606 cnts/sec. 
The total counts from this burst is 4626 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190615636_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190615B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24843
SUBJECT: GRB 190615B: Insight-HXMT/HE detection
DATE:    19/06/17 06:02:30 GMT
FROM:    Qi Luo at IHEP  <luoqi@ihep.ac.cn>

Q. Luo, S. Xiao, C. Cai, Q. B. Yi, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:

At 2019-06-15T14:42:22.00 (T0), Insight-HXMT/HE detected 
GRB 190615B (trigger ID: HEB190615612) in a routine search of the data, 
which was also triggered by INTEGRAL (trigger_num:8299) and KONUS-Wind. 

The Insight-HXMT/HE light curve mainly consists of two 
pulses with a duration (T90) of 23.69 s measured from T0+0.66 s. 
The 1-ms peak rate, measured from T0+0.74 s, is 1980 cnts/sec. 
The total counts from this burst is 4942 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190615612_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190613B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24844
SUBJECT: Konus-Wind observation of GRB 190613B
DATE:    19/06/17 18:30:10 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 190613B
(Swift-BAT detection: D'Ai et al., GCN Circ. 24807;
Fermi-GBM observation: Bissaldi et al., GCN Circ. 24814;
Insight-HXMT/HE detection: Luo et al., GCN Circ. 24829)
triggered Konus-Wind at T0=38825.774 s UT (10:47:05.774).

The burst light curve shows a single pulse
which starts at ~T0-2.6 s and has a total duration of ~4 s.
The emission is seen up to ~3 MeV.

As observed by Konus-Wind, the burst
had a fluence of 3.48(-0.79,+1.29)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.544 s,
of 2.65(-1.10,+1.54)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 4 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.93(-0.53,+0.83)
and Ep = 277(-107,+331) keV (chi2 = 82/72 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.8
(chi2 = 82/71 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190613_T38825/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190611B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24845
SUBJECT: GRB 190611B: AstroSat CZTI detection
DATE:    19/06/18 04:27:34 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma, D. Bhattacharya, T. Khanam and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190611B, which was also detected by Fermi GBM (Malacaria C. et al., GCN #24794), Global MASTER-Net (Lipunov V. et al., GCN #24795), IPN Triangulation (Hurley K. et al., GCN #24811), BALROG (Kunzweiler F. et al., GCN #24813), Konus-Wind (Frederiks D. et al., GCN #24827) and CALET (Cannady N. et al., GCN #24830).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 22:47:51.5 UT. Fermi/GBM lightcurve consists of two broad pulses. AstroSat could detect only first pulse of the burst, as during the second pulse the detector was in South Atlantic Anomaly (SAA). The measured peak count rate associated with the burst is 387 cts/s above the background in the combined data of four quadrants, with a total of 1251 cts. The local mean background count rate was 578 cts/s. Using cumulative rates, we measure a T90 of 7.35 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190613B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24846
SUBJECT: GRB 190613B: AstroSat CZTI detection
DATE:    19/06/18 05:55:40 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma, D. Bhattacharya, T. Khanam and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190613B, which was also detected by Fermi GBM (GCN #24806), Swift detection (D'Ai A. et al., GCN #24807), BALROG (Burgess J. et al., GCN #24808), Swift-XRT (Beardmore A.P. et al., GCN #24812), Swift-BAT (Ukwatta T.N. et al., GCN #24820), Insight-HXMT/HE (Luo Q. et al., GCN #24829) and Konus-Wind (Svinkin D. et al., GCN #24844).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 10:47:02.5 UT. The measured peak count rate associated with the burst is 439 cts/s above the background in the combined data of four quadrants, with a total of 1298 cts. The local mean background count rate was 654 cts/s. Using cumulative rates, we measure a T90 of 11.75 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190619A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24847
SUBJECT: GRB 190619A: Fermi GBM Final Real-time Localization
DATE:    19/06/19 00:37:50 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 00:26:01 UT on 19 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190619A (trigger 582596766.776714 / 190619018).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 349.3, Dec = 12.9 (J2000 degrees, equivalent to J2000 23h 17m, 12d 54'), with a statistical uncertainty of 2.0 degrees.

The angle from the Fermi LAT boresight is 13.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190619018/quicklook/glg_skymap_all_bn190619018.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190619018/quicklook/glg_healpix_all_bn190619018.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190619018/quicklook/glg_lc_medres34_bn190619018.gif


GRB_name: GRB190613B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24848
SUBJECT: GRB 190613B: JCMT SCUBA-2 sub-mm observations
DATE:    19/06/19 01:14:23 GMT
FROM:    Ian Smith at Rice U  <iansmith@rice.edu>

I.A. Smith (Rice U.), D.A. Perley (LJMU), and N.R. Tanvir 
(U. of Leicester) report:

We observed the location of GRB 190613B (D'Ai et al., GCN 
Circ. 24807) using the SCUBA-2 sub-millimeter continuum camera 
on the James Clerk Maxwell Telescope.  The observation started 
at 11:40 UT on 2019-06-13, corresponding to 53 minutes after 
the burst trigger.  Exposures totaling 1.0 hours were made in 
very good weather conditions.  No source was detected, with 
the RMS background noise being 1.8 mJy/beam at 850 microns and 
21.3 mJy/beam at 450 microns.

We thank Kevin Silva, Jan Wouterloot, Koji Sugitani, and the 
JCMT staff for the prompt support of these observations that 
were taken under project M19AP044.


GRB_name: GRB190613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24850
SUBJECT: GRB 190613A: SEDM Observations
DATE:    19/06/19 14:01:11 GMT
FROM:    Virginia Cunningham at U of MD  <vcunning@astro.umd.edu>

V. Cunningham (U of Maryland), J. D. Neill (Caltech), S. B. Cenko

(NASA GSFC), and R. Walters (Caltech) report on behalf of the

SEDM team:

We observed the optical counterpart to GRB 190613A (Ambrosi et al., GCN

24798) with the Spectral Energy Distribution Machine (SEDM) on the 60 inch

telescope at Palomar Observatory. The SEDM is a low resolution (R ~ 100)

integral field unit spectrometer with a multi-band (ugri) rainbow camera
imager

(see Blagorodnova et al. 2018, PASP, 130, 035003, and Rigault et al. 2019,

astro-ph/1902.08526).

The SEDM began observing the optical counterpart at 04:18:22 UTC (8.75

minutes after the burst trigger time). We performed an 1800 s exposure over
the

wavelength range 3800-9200 A. The continuum emission is well-fit by a power

law spectrum with index alpha = 0.56 (f_nu ~ nu^-alpha).  We detect an

absorption line at an observed wavelength of ~ 4597 A. We tentatively
identify

this line as due to Lyman alpha at z = 2.78 - however due to the lack of

corroborating features we consider this redshift tentative currently.


GRB_name: GRB190619B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24851
SUBJECT: GRB 190619B: Fermi GBM Final Real-time Localization
DATE:    19/06/19 14:27:35 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 14:16:25 UT on 19 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190619B (trigger 582646590.891184 / 190619595).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 291.1, Dec = 20.2 (J2000 degrees, equivalent to J2000 19h 24m, 20d 11'), with a statistical uncertainty of 1.8 degrees.

The angle from the Fermi LAT boresight is 93.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190619595/quicklook/glg_skymap_all_bn190619595.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190619595/quicklook/glg_healpix_all_bn190619595.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190619595/quicklook/glg_lc_medres34_bn190619595.gif


GRB_name: GRB190619B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24852
SUBJECT: GRB 190619B: BALROG localization (Fermi Trigger 582646590 / GRB 190619595)
DATE:    19/06/19 14:37:34 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

J. Burgess, B. Biltzinger, F. Kunzweiler, F. Berlato,  & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
582646590 at 14:16:25 on 19 June 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 293.4+/-1.6 deg
Decl.(2000.0) = 14.3+/-1.8 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190619595/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190619595/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190619595/json

                        


GRB_name: GRB190620A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24860
SUBJECT: GRB 190620A: Fermi GBM Final Real-time Localization
DATE:    19/06/20 12:21:50 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 12:10:10 UT on 20 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190620A (trigger 582725415.808842 / 190620507).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 162.1, Dec = 30.5 (J2000 degrees, equivalent to J2000 10h 48m, 30d 30'), with a statistical uncertainty of 1.2 degrees.

The angle from the Fermi LAT boresight is 59.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190620507/quicklook/glg_skymap_all_bn190620507.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190620507/quicklook/glg_healpix_all_bn190620507.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190620507/quicklook/glg_lc_medres34_bn190620507.gif


GRB_name: GRB190620A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24861
SUBJECT: GRB 190620A: BALROG localization (Fermi Trigger 582725415 / GRB 190620507)
DATE:    19/06/20 12:32:56 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

 J. Burgess, F. Kunzweiler, B. Biltzinger, F. Berlato, & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
582725415 at 12:10:10 on 20 June 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 161.2+/-0.7 deg
Decl.(2000.0) = 29.8+/-0.6 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190620507/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190620507/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190620507/json

                        


GRB_name: GRB190615B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24870
SUBJECT: GRB 190615B: AstroSat CZTI detection
DATE:    19/06/21 10:43:59 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190615B, which was also detected by Insight-HXMT/HE (Luo Q. et al., GCN #24843).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 14:42:23.5 UT. The measured peak count rate associated with the burst is 946 cts/s above the background in the combined data of four quadrants, with a total of 4318 cts. The local mean background count rate was 640 cts/s. Using cumulative rates, we measure a T90 of 27.9 s. 

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190622A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24872
SUBJECT: GRB 190622A: Fermi GBM Final Real-time Localization
DATE:    19/06/22 09:02:46 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 08:50:06 UT on 22 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190622A (trigger 582886211.27625 / 190622368).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 165.2, Dec = -53.6 (J2000 degrees, equivalent to J2000 11h 00m, -53d 36'), with a statistical uncertainty of 22.9 degrees.

The angle from the Fermi LAT boresight is 23.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190622368/quicklook/glg_skymap_all_bn190622368.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190622368/quicklook/glg_healpix_all_bn190622368.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190622368/quicklook/glg_lc_medres34_bn190622368.gif


GRB_name: GRB190622A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24873
SUBJECT: GRB 190622A: BALROG localization (Fermi Trigger 582886211 / GRB 190622368)
DATE:    19/06/22 09:27:03 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
582886211 at 08:50:06 on 22 June 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 146.4+/-3.8 deg
Decl.(2000.0) = -41.1+/-3.0 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190622368/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190622368/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190622368/json

                        


GRB_name: GRB190623A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24875
SUBJECT: GRB 190623A: Fermi GBM Final Real-time Localization
DATE:    19/06/23 11:14:55 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 11:03:27 UT on 23 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190623A (trigger 582980612.094866 / 190623461).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 335.5, Dec = -23.3 (J2000 degrees, equivalent to J2000 22h 22m, -23d 18'), with a statistical uncertainty of 4.1 degrees.

The angle from the Fermi LAT boresight is 91.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190623461/quicklook/glg_skymap_all_bn190623461.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190623461/quicklook/glg_healpix_all_bn190623461.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190623461/quicklook/glg_lc_medres34_bn190623461.gif


GRB_name: GRB190626A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24882
SUBJECT: GRB 190626A: Fermi GBM Final Real-time Localization
DATE:    19/06/26 06:18:03 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 06:06:21 UT on 26 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190626A (trigger 583221986.683772 / 190626254).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 145.7, Dec = -41.1 (J2000 degrees, equivalent to J2000 09h 42m, -41d 06'), with a statistical uncertainty of 6.2 degrees.

The angle from the Fermi LAT boresight is 107.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190626254/quicklook/glg_skymap_all_bn190626254.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190626254/quicklook/glg_healpix_all_bn190626254.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190626254/quicklook/glg_lc_medres34_bn190626254.gif


GRB_name: GRB190619B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24883
SUBJECT: GRB 190619B: AstroSat CZTI detection
DATE:    19/06/26 06:22:17 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma, D. Bhattacharya and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190619B, which was also detected by Fermi GBM (GCN #24851), BALROG (Burgess J. et la., GCN #24852) and Global MASTER-Net (Lipunov V. et al., GCN #24853).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with strongest peak at 14:16:44.5 UT. The measured peak count rate associated with the burst is 251 cts/s above the background in the combined data of four quadrants, with a total of 3318 cts. The local mean background count rate was 620 cts/s. Using cumulative rates, we measure a T90 of 38.6 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190626B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24884
SUBJECT: GRB 190626B: Fermi GBM Final Real-time Localization
DATE:    19/06/26 12:48:02 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 12:36:48 UT on 26 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190626B (trigger 583245413.943206 / 190626526).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 188.0, Dec = 38.8 (J2000 degrees, equivalent to J2000 12h 31m, 38d 47'), with a statistical uncertainty of 25.5 degrees.

The angle from the Fermi LAT boresight is 23.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190626526/quicklook/glg_skymap_all_bn190626526.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190626526/quicklook/glg_healpix_all_bn190626526.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190626526/quicklook/glg_lc_medres34_bn190626526.gif


GRB_name: GRB190627A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24888
SUBJECT: GRB 190627A: Swift detection of a burst
DATE:    19/06/27 11:48:34 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

E. Sonbas (Adiyaman Univ.), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU), J.D. Gropp (PSU),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC), K. L. Page (U Leicester),
M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 11:18:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190627A (trigger=911609).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 244.830, -5.292, which is 
   RA(J2000)  =  16h 19m 19s
   Dec(J2000) = -05d 17' 31"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a couple of peaks
with a total duration of about 10 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 11:20:20.8 UT, 109.8 seconds after
the BAT trigger. The initial XRT centroid was caused by a cosmic ray, and 
is therefore unrelated to the trigger. While no significant X-ray source 
was then detected in 20 s of promptly-downlinked data, there is a small 
number of X-ray photons at the same location as the tentative UVOT source. 

UVOT took a finding chart exposure of  29 seconds with the White filter
starting 114 seconds after the BAT trigger. The 2.7'x2.7' sub-image is
unavailable at this time. The list of sources generated on board shows a
possible new source at a location of:

  RA(J2000)  =  16:19:18.80 = 244.8283
  DEC(J2000) = -05:17:23.2  =  -5.2898

The list of sources is typically complete to about 18 mag. No correction
has been made for the expected extinction corresponding to E(B-V) of 0.18. 

Burst Advocate for this burst is E. Sonbas (edasonbas AT yahoo.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190627A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24889
SUBJECT: GRB 190627A: Swift/UVOT Detection 
DATE:    19/06/27 15:57:34 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M. H. Siegel (PSU) and E. Sonbas (Adiyaman Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190627A
115 s after the BAT trigger (Sonbas et al., GCN Circ. 24888).
An uncatalogued source consistent with the BAT position
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  16:19:18.69 = 244.82788 (deg.)
   Dec (J2000) = -05:17:20.8  =  -5.28912 (deg.)
with an estimated uncertainty of 0.46 arc sec. (radius, 90% confidence).

Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: 

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white              115          144           29         18.15 +/- 0.10

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.18 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190627A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24890
SUBJECT: GRB 190627A: Enhanced Swift-XRT position
DATE:    19/06/27 18:11:26 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2515 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 190627A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 244.82800, -5.28899 which is equivalent
to:

RA (J2000): 16h 19m 18.72s
Dec (J2000): -05d 17' 20.4"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24892
SUBJECT: GRB 190627A: NUTTelA-TAO optical observations
DATE:    19/06/27 20:42:40 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), M. Krugov (AFIF), P. Ðœinaev (IKI), I. Reva (AFIF), 
B. Grossan (ECL), E. Mazaeva  (IKI), A. Volnova (IKI) report on behalf 
of larger GRB IKI FuN collaboration:

We observed the field of the  GRB 190627A    (Sonbas  al., GCN  24888) 
with CDK700 telescope (NUTTelA-TAO project) of Assy-Turgen observatory 
starting on June 27  (UT) 17:01:00  in  R-filter.    We clearly detect 
the optical afterglow (Sonbas  al., GCN  24888; Siegel al., GCN  24889).
Preliminary photometry of the afterglow is following.

Date       UT start   t-T0       Filter Exp.   OT  Err.
                       (mid, days)        (s)

2019-06-27 17:19:20   0.25056     R     60  17.44 0.05
2019-06-27 19:10:35   0.32782     R     60  17.73 0.07


The photometry is based on the nearby USNO-B1  (R2) stars.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24893
SUBJECT: GRB 190627A: Montarrenti Observatory optical detection
DATE:    19/06/27 23:30:48 GMT
FROM:    Simone Leonini at Monarrenti Obs  <s.leonini@iol.it>

S. Leonini, M. Conti and P. Rosi (Montarrenti Observatory, Siena, Italy) report:

We observed the optical afterglow of GRB 190627A (Swift trigger 911609, E. Sonbas et al., GCN Circ. 24888) with the automatic 0.53m RC telescope + U47 detector at Montarrenti Observatory (Siena, Italy, IAU code C88).

The observations were started immediately after the sunset (approximately 9 hours post-burst) stacking 3 unfiltered CCD exposures of 30s for each run.

The OT was detected in all frames as follows:

2019 Jun 27.85897 UT (20:36:55 mid-time) R=18.0 +/-0.14
2019 Jun 27.92990 UT (22:19:03 mid-time) R=18.1 +/-0.13

Preliminary magnitudes were obtained using Astrometrica software using USNO-B1 catalogue for positions and photometry. An ensemble between 121 and 126 stars were used for the magnitude comparison. Measures are not corrected for galactic dust extinction.

The position of the GRB (within the error box given by Swift) is the following:

RA    (J2000) 16h 19m 18.70s +/-0.19
Decl. (J2000) -05Â° 17'  20.8"   +/-0.18

The message may be cited.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24894
SUBJECT: GRB190627A: VIRT Afterglow observation
DATE:    19/06/28 03:28:52 GMT
FROM:    Antonino Cucchiara at UVI  <antonino.cucchiara@uvi.edu>

D. Morris, S. Prentice, A. Cucchiara, (UVI), P. Gokool daas
(SFSU), N. Orange (Orangewave Inc.) report:

On June 28.02 UT we began observing the field of GRB 190627A
(Sombas et al, GCN 24888; Siegel et al, GCN 24889) with the
0.5m Virgin Island Robotic Telescope (VIRT) located
at the Etelman Observatory.
We performed a series of exposures in the R filter under
optimal weather conditions.

In a total coadded exposure of 510s we clearly identify the
optical afterglow reported by Siegel et al, (GCN 24889) and
Pozanenko  et al. (GCN 24892).

Our preliminary photometry, calibrated against 10 USNO-B1
stars are:

R= 18.38 +- 0.12

This magnitude has not been corrected for Galactic extinction.
The VIRT is still in its commissioning phase and further observations
are ongoing.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24895
SUBJECT: GRB 190627A: MASTER optical counterpart observation
DATE:    19/06/28 09:04:55 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, F.Balakin, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, 
A.Kuznetsov, F.Balakin, V.Vladimirov, D. Vlasenko, I.Gorbunov,D.Zimnukhov, V.Senik, D.Kuvshinov 
(Lomonosov Moscow State University, SAI, Physics Department),

R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA),

H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias)

D. Buckley (South African Astronomical Observatory),

O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API),

A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),

V. Yurkov, A. Gabovich, Yu. Sergienko (Blagoveschensk Educational State University)

MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)
located in South Africa (South African Astronomical Observatory)
started inspect of Swift GRB 190627A error-box (Sonbas  et al. GCN 24888, trigger 911609, 11:18:31UT, BAT 16h 19m 19.20s , - 5d 17m 31.20s, R=0.05)
  19594 sec after trigger time at 2019-06-27 16:45:05 UT, with upper limit up to  19.4 mag.

MASTER auto-detection system detected optical counterpart
with unfiltered m_OT~18.2 (W=0.2B+0.8R calibrated by USNO-B1 R2,B2)
(OT was discovered by Swift GCN 24888, and also publishied in GCN 24889, GCN 24892, GCN 24893, GCN24894)

Observations started at twilight after sunset.
Observations began at alt. = 30 deg., the sun  altitude  was -12.8 deg.
The galactic latitude b = -60 deg., longitude l = 98 deg.

The observation and reduction will continue.
The message may be cited.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24896
SUBJECT: GRB 190627A: GMG observation
DATE:    19/06/28 10:45:28 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, C.-J. Wang and J.-M. Bai report:


We observed the field of GRB 190627A (Sonbas et al. GCN Circ. 24888) with the 2.4-meter optical telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatories. The observation began at UT 13:49:34, 27, June, 2019, about 2.5 hours after the trigger. We clearly detected the afterglow (Sonbas et al. GCN Circ. 24888; Siegel et al. GCN Circ 24889). We obtained the preliminary magnitude of R~16.9. We compared our result to those from other reports (e.g., Pozanenko et al. GCN Circ 24892, Leonini et al. GCN Circ 24893, Morris et al. GCN Circ. 24894, and Lipunov et al. GCN Circ. 24895). It seems that there was a brightening phase during about 3 hours after the trigger. We encourage other groups for the further investigation.


GRB_name: GRB190628A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24897
SUBJECT: GRB 190628A: Fermi GBM Final Real-time Localization
DATE:    19/06/28 12:42:23 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 12:30:55 UT on 28 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190628A (trigger 583417860.320222 / 190628521).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 144.1, Dec = -77.1 (J2000 degrees, equivalent to J2000 09h 36m, -77d 05'), with a statistical uncertainty of 6.4 degrees.

The angle from the Fermi LAT boresight is 120.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190628521/quicklook/glg_skymap_all_bn190628521.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190628521/quicklook/glg_healpix_all_bn190628521.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190628521/quicklook/glg_lc_medres34_bn190628521.gif


GRB_name: GRB190610A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24898
SUBJECT: GRB 190610A: Further Swift-XRT observations
DATE:    19/06/28 14:21:27 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:

Swift-XRT has carried out further observations of GRB 190610A (Palmer et 
al. GCN Circ. 24783, Beardmore et al., GCN Circ. 24883), in order to 
ascertain whether the faint source in the BAT error circle ("Source 7") 
is fading. Marginal evidence of fading has been detected.

In our later-epoch observations, the source is not detected at the 
3-sigma level. The 3-sigma upper limit is 1.27 x 10^-3 ct/sec, or a 
1-sigma confidence interval count-rate is 3.2 (+5.6, -1.7) x 10^-4 
ct/sec (all rates are 0.3-10 keV). The original detection had a count 
rate of 1.76 (+0.83, -0.64) x 10^-3 ct/sec.

Thus the source appears to be fading, but only at the 2.1-sigma level.

Given the low significance of the fading, the faintness of the source, 
and the fact that low-level variability is not uncommon among X-ray 
sources, we cannot say with confidence that this is definitely the 
afterglow of GRB 190610A, however it remains a tantalising possibility.
Due to the faint nature of the object, no further XRT observations are 
planned.

The details of the source can be viewed, and the light curve rebinned, 
at: http://www.swift.ac.uk/ToO_GRBs/00020896/Source7.php

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190627A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24899
SUBJECT: GRB 190627A: Swift-BAT refined analysis (short-soft burst)
DATE:    19/06/28 15:01:57 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

S. D. Barthelmy (GSFC),  J. R. Cummings (CPI), H. A. Krimm (NSF),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), E. Sonbas (Adiyaman Univ.),  M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190627A (trigger #911609)
(Sonbas, et al., GCN Circ. 24888).  The BAT ground-calculated position is
RA, Dec = 244.843, -5.302 deg which is 
  RA(J2000)  =  16h 19m 22.3s 
  Dec(J2000) = -05d 18' 08.6" 
with an uncertainty of 2.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 73%.

The mask-weighted light curve shows a single peak, visible only in the softest
energy channels, with a duration of about four seconds.  The burst location
went out of the BAT field soon after T+400 sec due to a spacecraft slew.
T90 (15-350 keV) is 1.60 +- 0.28 sec (estimated error including systematics).

The time-averaged spectrum from T+0.04 to T+1.78 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.38 +- 0.38.  The fluence in the 15-150 keV band is 9.9 +- 2.2 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T+0.78 sec in the 15-150 keV band
is 1.1 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

Although GRB 190627A has a brief duration, it is not clear that it is a short GRB.  
The duration and relative softness of the spectrum place it intermediate between 
most short and long bursts detected by BAT.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/911609/BA/


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24900
SUBJECT: GRB 190627A: NUTTelA-TAO optical counterpart observations
DATE:    19/06/28 17:31:25 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Volnova (IKI), M. Krugov (AFIF),  I. Reva (AFIF), 
P. Minaev (IKI), B. Grossan (ECL), E. Mazaeva  (IKI)  report on behalf 
of larger GRB IKI FuN collaboration:

We observed the the optical afterglow (e.g. Sonbas  al., GCN  24888; 
Siegel al., GCN  24889) with CDK700 telescope (NUTTelA-TAO project) of 
Assy-Turgen observatory starting on June 28  (UT) 15:30:37  in R-filter. 
    We clearly detect the optical afterglow (Sonbas  al., GCN  24888; 
Siegel al., GCN  24889).
Preliminary photometry of the afterglow is following.

Date       UT start   t-T0       Filter Exp.   OT   Err.
                       (mid, days)        (s)

2019-06-28 15:30:37   1.18332     R     20*60  19.6 0.16

The photometry is based on the nearby USNO-B1  (R2) stars.

We encourage  spectroscopic observations to determine redshift and 
nature of the burst.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24901
SUBJECT: GRB 190627A: Optical imaging and spectroscopy from Calar Alto
DATE:    19/06/28 18:44:11 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC, 
DARK/NBI), L. Izzo, M. Blazek, C. C. Thoene (all HETH/IAA-CSIC), A. 
Guijarro, and S. Pedraz (both CAHA) report:

We observed the afterglow of the short-soft GRB 190627A (Sonbas et al. 
GCN 24888, Siegel et al. GCN 24889, Evans et al. GCN 24890, Pozanenko et 
al. GCN 24892, Leonini et al. GCN 24893, Morris et al. GCN 24894, 
Lipunov et al. GCN 24895, Mao et al. GCN 24896, Barthelmy et al. GCN 
24899) with CAFOS at the 2.2 m telescope of the Calar Alto Observatory, 
in Almeria (Spain). We obtained imaging in g', r', i' and z' bands, as 
well as a low resolution spectrum. Observations were obtained in 
inclement weather conditions (2".5 seeing and low transparency because 
of Calima).

The imaging consisted of 5 x 60 s exposures each in the z' and i' bands, 
and 1 x 300 s each in r' and g' band. The optical counterpart is well 
detected in each of the individual images. At a mean epoch 21:54:42 UT 
(10.603 hr after the burst,) the object had a magnitude of r'(AB) = 
18.33 +/- 0.04 mag as compared to field stars from the PanSTARRS 
catalog.

The spectrum was obtained at a mean time of 11.675 hrs after trigger and 
consisted of an exposure of 3 x 1800 s. We used the B-200 grism that 
covers the range between 3500 and 8800 AA with a resolving power of R ~ 
400. The spectrum shows a clear continuum across the complete range, 
with an average signal-to-noise ratio per dispersion element of 5.5. 
However, we are not able to match any of the marginal absorption 
features with a particular redshift. We have made the reduced spectrum 
publicly available through GRBSpec [1].

Further observations are planned.

[1] http://GRBSpec.iaa.es


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24902
SUBJECT: GRB 190627A: NIR imaging from Liverpool Telescope
DATE:    19/06/28 18:46:13 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

M. Blazek, L. Izzo, D. A. Kann (all HETH/IAA-CSIC), A. de Ugarte Postigo 
(HETH/IAA-CSIC, DARK/NBI), and C. C. Thoene (HETH/IAA-CSIC) report:

We observed the afterglow of the short-soft GRB 190627A (Sonbas et al. 
GCN 24888, Siegel et al. GCN 24889, Evans et al. GCN 24890, Pozanenko et 
al. GCN 24892, Leonini et al. GCN 24893, Morris et al. GCN 24894, 
Lipunov et al. GCN 24895, Mao et al. GCN 24896, Barthelmy et al. GCN 
24899, Kann et al., GCN 24901) with IO-I on the 2 m Liverpool Telescope, 
at the Roque de los Muchachos Observatory, in La Palma (Spain).

The observation consisted of 4 visits of 10 x 60 s in the H band, with 
good detections at all epochs. In the first epoch, obtained at a mean 
epoch 11.6492 hr after the burst, the object is detected at a magnitude 
of H(AB) = 17.04 +/- 0.10 mag. The photometry was performed with respect 
to 2MASS field stars.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24903
SUBJECT: GRB 190627A: Optical imaging by D50 from Ondrejov
DATE:    19/06/28 21:19:49 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Martin Jelinek and Jan Strobl (ASU CAS Ondrejov, CZ)
report:

We observed GRB 190627A (Sonbas et al. GCNC 24888) with the 50 cm robotic
telescope (D50) of Ondrejov observatory in the Czech Republic, obtaining a
series of 120s images starting at 20:35UT, i.e. 33.3h post trigger.

We can detect the optical afterglow (Siegel & Sonbas, GCNC 24889; Leonini
et al., GCNC 24893 and others), providing the preliminary magnitude R=19.8,
in a good agreement with extrapolation of the power-law decay slope we
observed the last night.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24904
SUBJECT: GRB 190627A: NOT optical observations
DATE:    19/06/28 22:08:37 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Daniele B. Malesani (DTU Space), Jyri J. Lehtinen (MPS), Teemu Willamo 
(Univ. Helsinki), Zipei Zhu (NAO/CAS), Dong Xu (NAO/CAS), report on 
behalf of a larger collaboration:

We observed the bright optical counterpart (Siegel & Sonbas, GCN 24889) 
of GRB 190627A (Sonbas et al., GCN 24888) using the Nordic Optical 
Telescope (NOT) equipped with the StanCam imager, using the Bessel R and 
I filters. Observations were conducted starting on Jun 28.886 UT (1.415 
days after the trigger).

The optical counterpart is clearly detected in our images in both 
filters. We measure a preliminary magnitude r = 20.2 +- 0.1 AB 
(calibrated against the Pan-STARRS catalog).


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24905
SUBJECT: GRB 190627A: GMG observation at the second epoch
DATE:    19/06/29 07:55:06 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, C.-J. Wang and J.-M. Bai report:


We observed the field of GRB 190627A (Sonbas et al. GCN Circ. 24888) with the 2.4-meter optical telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatories. We performed the second epoch observation at UT 17:40:32, 28, June, 2019, about 1.3 days after the trigger. We obtained the preliminary magnitude of R~20.0. Our result seems to be consistent to those from other photometric observations at the same epoch (e.g., Pozanenko et al. GCN Circ 24900; Jelinek & Strobl GCN Circ 24903; Malesani et al. GCN Circ 24904).


GRB_name: GRB190627A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24906
SUBJECT: GRB 190627A: Swift-XRT refined Analysis
DATE:    19/06/29 13:55:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi 
(INAF-IASFPA) , J.A. Kennea (PSU), B. Sbarufatti (PSU), D.N. Burrows
(PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester) and E.
Sonbas (Adiyaman Univ.) report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 190627A (Sonbas et al. GCN
Circ. 24888), from 121 s to 119.5 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Evans et al. (GCN Circ. 24890).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.12 (+0.15, -0.19), followed by a break at T+22.1 ks to
an alpha of 1.48 (+0.17, -0.16).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.96 (+0.16, -0.09). The
best-fitting absorption column is  consistent with the Galactic value
of 1.8 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.6 x 10^-11 (4.7 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.8 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 1.8 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.96 (+0.16, -0.09)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00911609.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24907
SUBJECT: GRB 190627A : Xinglong 2.16m optical observation
DATE:    19/06/29 16:06:41 GMT
FROM:    Liping Xin at NAOC, SVOM  <xlp@nao.cas.cn>

L. P. Xin,  J. J. Ren, X. H, Han, G. W. Li,  R. S. Zhang,   J. Wang,  
J. Y. Wei,   Y. G. Yang, E. W. Liang,  X. G. Wang,   H. L. Li, 
X. M. Lu,  L. Huang,    H. B. Cai,   Y. L. Qiu,  Y. Xu, 
Y.  J. Xiao,  Y. T. Zheng,  C. Wu,   J. S. Deng,   D. W. Xu,  
D. Turpin,  W. L. Dong, P. P. Zhang report:

We observed  GRB 190627A  (Sonbas et al., GCN 24888 ) using the  
Xinglong-2.16m equipped with  the BFOSC camera. Observations 
were carried out from 13:46:06 to 14:06:29 UT on 2019-06-29,  
5*300sec R band images were obtained.

The optical afterglow (Siegel & Sonbas, GCN 24889, 
Lipunov et al., GCN Circ 24895; Morris et al., GCN Circ 24894; 
Leonini et al., GCN Circ 24893; Pozaneko et al., GCN Circ 24892; 
Pozanenko et al. GCN Circ 24900;  Kann et al., GCN Circ 24901; 
Blazek et al., GCN Circ 24902;  Jelinek & Strobl GCN Circ 24903; 
Malesani et al. GCN Circ 24904,  Mao et al., GCN Circ 24896,  24905) 
was marginal detected in our stacked image with a magnitude of 
R=20.5+/-0.2 mag at the mid time of about 2.1 days after the burst. 
The photometry is calibrated with nearby USNO B1.0 stars


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24911
SUBJECT: GRB 190627A: Koshka Zeiss-1000 optical counterpart observations
DATE:    19/06/30 03:16:01 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), A. Novichonok (KIAM), S. Belkin (IKI),  A. 
Zhornichenko (KIAM), A. Pozanenko (IKI), E. Mazaeva (IKI),  I. Molotov 
(KIAM)  report on behalf of larger GRB IKI FuN collaboration:

We observed the the optical afterglow of GRB 190627A (e.g. Sonbas  al., 
GCN  24888; Siegel al., GCN  24889) with Zeiss-1000 1-m telescope of 
Koshka Observatory on June, 27 and June, 28  in  R-filter.   We clearly 
detect the  afterglow in both epoch. Preliminary photometry of the 
afterglow is following.

Date       UT start   t-T0       Filter Exp.   OT   Err.   UL
                      (mid, days)        (s)

2019-06-27 18:53:57   0.31732    R     180  17.70  0.08  19.9
2019-06-27 19:42:20   0.35092    R     180  17.80  0.07  20.3
2019-06-28 19:22:50   1.36775    R    5400  19.75  0.08  21.5

The photometry is based on the same USNO-B1.0 (R2) stars used in GCNs 
24892 and 24900.


GRB_name: GRB190630A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24912
SUBJECT: GRB 190630A: Fermi GBM Final Real-time Localization
DATE:    19/06/30 06:21:40 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 06:09:58 UT on 30 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190630A (trigger 583567803.319036 / 190630257).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 307.0, Dec = -1.3 (J2000 degrees, equivalent to J2000 20h 27m, -1d 18'), with a statistical uncertainty of 7.7 degrees.

The angle from the Fermi LAT boresight is 48.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190630257/quicklook/glg_skymap_all_bn190630257.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190630257/quicklook/glg_healpix_all_bn190630257.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190630257/quicklook/glg_lc_medres34_bn190630257.gif


GRB_name: GRB190630B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24913
SUBJECT: Swift Trigger 912102:  possible GRB 190630B
DATE:    19/06/30 06:24:47 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

H. A. Krimm (NSF), N. J. Klingler (PSU), K. L. Page (U Leicester) and
A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 06:02:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located possible GRB 190630B (trigger=912102).  Swift slewed immediately to the location. 
The BAT on-board calculated location is 
RA, Dec 223.669, +41.521 which is 
   RA(J2000) = 14h 54m 41s
   Dec(J2000) = +41d 31' 16"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 5 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~0 sec after the trigger. 
This increase in flux occurred during a rise in background due to
entry to the SAA, so it is not immediately clear from the BAT data 
alone that this is indeed a burst rather than a noise event. 

The XRT began observing the field at 06:03:10.7 UT, 62.1 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT took a finding chart exposure of  66 seconds with the White filter
starting 65 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.01. 

Due to the high background in the BAT and the lack of immediate
counterpart detection in the XRT, the Swift team will not be able to
confirm or deny whether this event is a GRB without further data. 

Burst Advocate for this burst is H. A. Krimm (hkrimm AT nsf.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24916
SUBJECT: GRB 190627A: VLT/FORS2 spectroscopic redshift
DATE:    19/06/30 10:01:00 GMT
FROM:    Jure Japelj at API,U of Amsterdam  <japelj.jure@gmail.com>

J. Japelj (Uni. Amsterdam), D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo
(HETH/IAA-CSIC, DARK/NBI), L. Izzo (HETH/IAA-CSIC), J. P. U. Fynbo (DAWN/NBI
and DAWN/DTU), D. B. Malesani (DTU Space), V. D'Elia (SSDC), N. R. Tanvir
(Univ. Leicester), S. D. Vergani (CNRS -GEPI/Observatorie de Paris), G.
Pugliese,
L. Kaper (Uni. Amsterdam) report on behalf of the Stargate collaboration:

We observed the optical counterpart (Siegel et al., GCN 24889; Pozanenko
et al., GCN 24892) of GRB 190627A (Sonbas et al., GCN 24888) with the ESO
VLT UT1 equipped with the FORS2 spectrograph. We obtained a 30 min spectrum
with the 600RI (512 - 845 nm) and a 30 min spectrum with the 600z (737-1070
nm)
grism. Observations started at 01:12:41 UT on June 30 (i.e., 2.57 days
after the
GRB detection).

In the spectrum, the continuum is clearly detected. We detect three MgII
absorption systems at redshifts z = 1.942, 1.774 and 1.681. The redshift
z = 1.942 and 1.681 absorption systems also exhibit FeII lines. We conclude
that z = 1.942 is the likely redshift of GRB 190627A.

We acknowledge the ESO observing staff at Paranal, especially Karleyne Silva
and Juan Carlos Munoz.


GRB_name: GRB190630B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24918
SUBJECT: GRB 190630B, Swift-BAT refined analysis
DATE:    19/06/30 16:01:10 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

J. R. Cummings (CPI), S. D. Barthelmy (GSFC),  H. A. Krimm (NSF),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), F. Marshall (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-240 to T+50 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190630B (trigger #912102)
(Krimm, et al., GCN Circ. 24913).  The BAT ground-calculated position is
RA, Dec = 223.729, 41.528 deg which is 
  RA(J2000)  =  14h 54m 55.0s 
  Dec(J2000) = +41d 31' 42.4" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a single, weak pulse with a FRED-like
shape, starting from T-3 sec, peaking at T+1 sec and fading to background by
T+6 sec.  We note that data is available until approximately T+250 sec.  However,
after T+50 sec, the background cannot be properly subtracted due to high 
background levels arising from Swiftâ€™s entry into the SAA.  Therefore we only
use data prior to T+50 sec for analysis.  The raw light curve shows no sign of any
burst activity after the initial pulse.  T90 (15-350 keV) is 5.6 +- 0.9 sec 
(estimated error including systematics).

The time-averaged spectrum from T-1.7 to T+4.7 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.36 +- 0.24.  The fluence in the 15-150 keV band is 2.8 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.19 sec in the 15-150 keV band
is 1.1 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

In the initial circular for GRB 190630B (Krimm, et al., GCN Circ. 24913), this event
was reported as a possible burst.   After the more complete analysis carried out here,
we conclude that Swift trigger 912102 is indeed a GRB.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/912102/BA/


GRB_name: GRB190630B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24919
SUBJECT: GRB 190630B: Swift-XRT refined Analysis
DATE:    19/06/30 17:37:06 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester), P.A. Evans (U. Leicester) and F.E. Marshall
(NASA/GSFC) report on behalf of the Swift-XRT team:

We have analysed 2.4 ks of XRT data for GRB 190630B, from 47 s to 28.2
ks after the  BAT trigger. The data comprise 8 s in Windowed Timing
(WT) mode (taken while Swift was slewing), with the remainder in Photon
Counting (PC) mode. Using 307 s of PC mode data and 1 UVOT image, we
find an enhanced XRT position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
223.70024, +41.52614 which is equivalent to:

RA (J2000): 14h 54m 48.06s
Dec(J2000): +41d 31' 34.1"

with an uncertainty of 3.1 arcsec (radius, 90% confidence).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.32 (+0.08, -0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.0 (+1.1, -0.4). The
best-fitting absorption column is  consistent with the Galactic value
of 1.4 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.0 x 10^-11 (3.3 x 10^-11) erg cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      1 (+/-20) x 10^20 cm^-2
Galactic foreground: 1.4 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      3.0 (+1.1, -0.4)

If the light curve continues to decay with a power-law decay index of
1.32, the count rate at T+24 hours will be 6.5 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.0 x
10^-14 (2.1 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00912102.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190630C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24927
SUBJECT: GRB 190630C: Swift detection of a burst
DATE:    19/07/01 00:05:00 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

T. N. Ukwatta (LANL), J.D. Gropp (PSU), H. A. Krimm (NSF),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL) and A. Tohuvavohu (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 23:52:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190630C (trigger=912239).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 293.908, -32.751 which is 
   RA(J2000) = 19h 35m 38s
   Dec(J2000) = -32d 45' 03"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 120 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 23:55:28.8 UT, 149.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 293.87874,
-32.74273 which is equivalent to:
   RA(J2000)  = 19h 35m 30.90s
   Dec(J2000) = -32d 44' 33.8"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 93 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 1.02e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 157 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.11. 

This source lies within the current (Sector 13) field-of-view of TESS camera 1. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190631A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24929
SUBJECT: Swift GRB190631. Global MASTER-Net observations report 
DATE:    19/07/01 00:55:20 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D.Kuvshinov 
(Lomonosov Moscow State University, SAI, Physics Department),

R. Podesta, C.Lopez, F. Podesta, C.Francile 
(Observatorio Astronomico Felix Aguilar OAFA),

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

R. Rebolo, M. Serra 
(The Instituto de Astrofisica de Canarias)

D. Buckley 
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev, O.Ershova 
(Irkutsk State University, API),

A. Tlatov, D. Dormidontov 
(Kislovodsk Solar Station of the Pulkovo Observatory),

V. Yurkov, A. Gabovich, Yu. Sergienko 
(Blagoveschensk Educational State University)




MASTER-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB190631. (trigger No 912239, 19h 35m 37.92s , -32d 45m 03.60s, R=0.05) errorbox  50 sec after trigger time at 2019-06-30 23:53:49 UT, with upper limit up to  17.8 mag. Observations started at twilight.  The observations began at zenit distance = 78 deg. The sun  altitude  is -16.8 deg. 

MASTER-OAFA robotic telescope  located in Argentina (OAFA observatory of San Juan National University) was pointed to the Swift GRB190631. errorbox  56 sec after trigger time at 2019-06-30 23:53:55 UT, with upper limit up to  17.6 mag. The observations began at zenit distance = 71 deg. The sun  altitude  is -27.2 deg. 

MASTER-IAC robotic telescope  located in Spain (IAC Teide Observatory) was pointed to the Swift GRB190631. errorbox  83 sec after trigger time at 2019-06-30 23:54:22 UT, with upper limit up to  18.8 mag. The observations began at zenit distance = 68 deg. The sun  altitude  is -36.0 deg. 

The galactic latitude b = -60 deg., longitude l = 98 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1061706

We obtain a following upper limits.  

Tmid-T0  |          Site       |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________

      55 |      MASTER-Tavrida |   C |    10 | 16.5 |        
      61 |         MASTER-OAFA |   C |    10 | 16.5 |        
      94 |          MASTER-IAC |  P| |    20 | 17.5 |        
      94 |          MASTER-IAC |  P- |    20 | 17.2 |        
      94 |      MASTER-Tavrida |   C |    20 | 17.2 |        
     117 |         MASTER-OAFA |   C |    20 | 17.0 |        
     143 |      MASTER-Tavrida |   C |    30 | 17.4 |        
     150 |          MASTER-IAC |  P| |    30 | 17.8 |        
     150 |          MASTER-IAC |  P- |    30 | 17.5 |        
     184 |         MASTER-OAFA |   C |    30 | 17.2 |        
     202 |      MASTER-Tavrida |   C |    40 | 17.6 |        
     204 |          MASTER-IAC |  P- |    40 | 17.6 |        
     204 |          MASTER-IAC |  P| |    40 | 18.1 |        
     267 |         MASTER-OAFA |   C |    50 | 17.5 |        
     269 |          MASTER-IAC |  P| |    50 | 18.3 |        
     269 |          MASTER-IAC |  P- |    50 | 17.9 |        
     271 |      MASTER-Tavrida |   C |    50 | 17.8 |        
     343 |          MASTER-IAC |  P| |    60 | 18.5 |        
     343 |          MASTER-IAC |  P- |    60 | 18.1 |        
     368 |         MASTER-OAFA |   C |    70 | 17.6 |        
     434 |          MASTER-IAC |  P- |    80 | 18.3 |        
     435 |          MASTER-IAC |  P| |    80 | 18.7 |        
     544 |          MASTER-IAC |  P- |   100 | 18.5 |        
     544 |          MASTER-IAC |  P| |   100 | 18.8 |        
Filter C is a clear (unfiltred) band. 


The observation and reduction will continue. 
The message may be cited.


GRB_name: GRB190630C
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24930
SUBJECT: GRB 190630C: Enhanced Swift-XRT position
DATE:    19/07/01 03:12:27 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 195 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 190630C, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 293.88034, -32.74405 which is equivalent
to:

RA (J2000): 19h 35m 31.28s
Dec (J2000): -32d 44' 38.6"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB190630B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24931
SUBJECT: GRB 190630B: KAIT Optical Afterglow Confirmation
DATE:    19/07/01 05:41:45 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to the Swift GRB 190630B (Krimm et al.,
GCN 24913; Cummings et al. GCN 24918) starting at 310s after the burst.
Observations were performed with a sequence in the clear (roughly R),
V, and I filters, and the exposure time was 60 s per image. Further
analysis on our reported afterglow candidate (Zheng & Filippenko, GCN
24914) shows that the candidate position is within the enhanced XRT
error circle (Page et al., GCN 24919), and its brightness faded more than
2 magnitude during our ~2 hours observing range. We therefore confirm
this is the optical afterglow of GRB 190630B. A preliminary KAIT clear
band light curve is available at:
http://w.astro.berkeley.edu/~zwk/grb/GRB190630B/GRB190630B_kait.jpg


GRB_name: GRB190701A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24934
SUBJECT: GRB 190701A: Swift detection of a burst
DATE:    19/07/01 09:58:42 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

T. N. Ukwatta (LANL), A. P. Beardmore (U Leicester),
N. J. Klingler (PSU), H. A. Krimm (NSF), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester) and A. Tohuvavohu (PSU) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 09:45:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190701A (trigger=912310).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 28.063, +58.906 which is 
   RA(J2000) = 01h 52m 15s
   Dec(J2000) = +58d 54' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 100 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~37 sec after the trigger. 

The XRT began observing the field at 09:47:41.9 UT, 141.1 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 28.08019, 58.91005 which
is equivalent to:
   RA(J2000)  = 01h 52m 19.25s
   Dec(J2000) = +58d 54' 36.2"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 35 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 6.36
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 144 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the large, but uncertain, extinction expected. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190701A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24935
SUBJECT: GRB 190701A: Prompt enhanced Swift-XRT position
DATE:    19/07/01 10:25:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:

Using  promptly downlinked XRT event data for GRB 190701A, we find an
enhanced XRT position of the afterglow: RA, Dec: 28.0815, 58.9095 which
is equivalent to:
   RA (J2000)  = 01 52 19.56
   Dec (J2000) = +58 54 34.3
with an uncertainty of 2.1 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/912310.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190701B
Detection_method: IBAS
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24936
SUBJECT: GRB 190701B: a long GRB detected by IBAS
DATE:    19/07/01 11:18:25 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

D.Gotz (CEA, Saclay), S.Mereghetti (INAF, IASF-Milano), C.Ferrigno,
E.Bozzo, V.Savchenko (ISDC, Versoix), L.Ducci (IAAT, Germany and ISDC,
Versoix) and J.Borkowski (CAMK, Torun) report:

a gamma ray burst lasting about 23 s has been detected by IBAS in the
IBIS/ISGRI data at 10:04:58  UT of July 1st, 2019.

The refined coordinates (J2000) are:

R.A.= 350.4091 deg
DEC.= +64.3457 deg
with an uncertainty of  1.1 arcmin (90% c.l.).

The burst had a peak flux of 0.1  photons/cm2/s (20-200 keV, 1-s integration  time) 
and a fluence in the same energy range of about 5.e-8 erg/cm2.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB190701A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24937
SUBJECT: GRB 190701A: MAXI/GSC detection
DATE:    19/07/01 11:55:46 GMT
FROM:    Motoko Serino at RIKEN/MAXI  <motoko@crab.riken.jp>

K. Setoguchi (Kyoto U.), H. Negoro, M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.), 
S. Nakahira, T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, M. Serino, S. Sugita, H. Nishida, A. Yoshida (AGU), 
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.), 
M. Shidatsu (Ehime U.),
N. Kawai, M. Sugizaki, M. Oeda, K. Shiraishi (Tokyo Tech), 
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, M. Tominaga (JAXA), 
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, T. Yoshitake (Kyoto U.), 
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), 
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.), 
T. Kawamuro (NAOJ), 
K. Yamaoka (Nagoya U.),
Y. Kawakubo (LSU)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient 
source at 09:46:42 UT on July 1, 2019.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (27.548 deg, 58.852 deg) = (01 50 11, +58 51 06) (J2000)
with a 90% C.L. statistical error of 0.16 deg and an additional systematic uncertainty 
of 0.1 deg (90% containment radius).
Without assumptions on the source constancy, we obtain a rectangular error box
for the transient source with the following corners: 
(25.762, 59.105) deg = (01 43 02, +59 06 17) (J2000)
(25.721, 58.781) deg = (01 42 53, +58 46 51) (J2000)
(29.166, 58.620) deg = (01 56 39, +58 37 11) (J2000)
(29.239, 58.942) deg = (01 56 57, +58 56 31) (J2000).
This position is consistent with that of GRB 190701A detected 
by Swift (Ukwatta et al., GCN 24934, Evans et al., GCN 24935).

The X-ray flux averaged over the scan was 416 +- 39 mCrab
(4.0-10.0keV, 1 sigma error).

There was no significant excess flux in the previous transit at UT 08:14 
and in the next transit at 11:19 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB190630C
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24939
SUBJECT: GRB 190630C: AstroSat CZTI detection
DATE:    19/07/01 13:59:57 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

V. Sharma, R. Gaikwad, D. Bhattacharya and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190630C, which was also detected by Swift (Ukwatta T. N. et al., GCN # 24927) and Swift-XRT (Goad M. R. et al., GCN # 24930).

The source was clearly detected in the 40-200 keV energy range. The light curve shows single pulse of emission with strongest peak at 23:53:01 UT. The measured peak count rate associated with the burst is 153 cts/s above the background in the combined data of four quadrants, with a total of 1301 cts. The local mean background count rate was 571 cts/s. Using cumulative rates, we measure a T90 of 21.3 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190701A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24940
SUBJECT: GRB 190701A: Enhanced Swift-XRT position
DATE:    19/07/01 14:48:42 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 890 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 190701A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 28.08140, +58.90943 which is equivalent
to:

RA (J2000): 01h 52m 19.54s
Dec (J2000): +58d 54' 33.9"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB190630C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24941
SUBJECT: GRB 190630C: Swift-BAT refined analysis
DATE:    19/07/01 14:58:51 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

H. A. Krimm (NSF), S. D. Barthelmy (GSFC),  J. R. Cummings (CPI),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190630C (trigger #912239)
(Ukwatta, et al., GCN Circ. 24927).  The BAT ground-calculated position is
RA, Dec = 293.890, -32.759 deg which is 
  RA(J2000)  =  19h 35m 33.6s 
  Dec(J2000) = -32d 45' 32.5" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 57%.

The mask-weighted light curve shows a single FRED-shaped burst, beginning 
at ~T-5 sec, peaking at T+0 sec, and declining to background by ~T+40 sec.
A spacecraft slew took the burst position out of the BAT field of view just before
T+500 sec. T90 (15-350 keV) is 38.4 +- 9.3 sec (estimated error including systematics).

The time-averaged spectrum from T-1.92 to T+50.23 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.96 +- 0.11.  The fluence in the 15-150 keV band is 2.3 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.12 sec in the 15-150 keV band
is 2.0 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/912239/BA/


GRB_name: GRB190630B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24943
SUBJECT: GRB 190630B: Swift/UVOT Upper Limits 
DATE:    19/07/01 17:59:50 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

GRB 190630B: Swift/UVOT Upper Limits

K. K. Simpson (PSU) and F. E. Marshall (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190630B
65 s after the BAT trigger (Krimm et al., GCN Circ. 24913).   
No optical afterglow consistent with the optical position
(Zheng and Filippenko GCN Circ. 24914)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system 
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:

Filter         T_start(s)   T_stop(s)    Exp(s)      Mag

white            65         131          65       >20.5
b             57357       57675         308      >20.69
uvm2          39177       40077         885      >20.36
u             46044       46193         145      >19.89
v             55313       55640         317      >18.87
uvw1          40084       40453         363      >20.02
uvw2          49543       49700         155      >19.09


The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190630C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24944
SUBJECT: GRB 190630C: KAIT Optical Upper Limit
DATE:    19/07/01 18:00:13 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 190630C (Ukwatta et al.,
GCN 24927) starting at ~0.379 days after the burst. Observations
were performed in the clear (roughly R) filters, a total of 31
images were obtained and the exposure time was 60 s per image.
We do not detect any optical afterglow candidate within the Enhanced
XRT position error circle (Goad et al., GCN 24930), neither in single
image, nor in the co-add images. We estimate our limiting magnitude
of our co-added image is ~19.0 mag calibrated to the APASS catalog.


GRB_name: GRB190630C
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24945
SUBJECT: GRB 190630C: Swift/UVOT Upper Limits
DATE:    19/07/01 19:32:37 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

GRB 190630C: Swift/UVOT Upper Limits

K. K. Simpson (PSU) and T. N. Ukwatta (LANL)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190630C
136 s after the BAT trigger (Ukwatta et al., GCN Circ. 24927).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 24930)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           157          307          147         >20.5
white              157          307          147         >20.5
v                  136          412           32         >18.1
w2                 367          387           19         >20.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.11 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190701A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24946
SUBJECT: GRB 190701A: COATLI Optical Observations
DATE:    19/07/01 19:51:59 GMT
FROM:    Rosa Leticia Becerra Godinez at Inst. de Astronoma,UNAM  <rbecerra@astro.unam.mx>

Rosa L. Becerra (UNAM), Alan M. Watson (UNAM),  Nat Butler (ASU),
Diego GonzÃ¡lez (UNAM),Alexander Kutyrev (GSFC), William H. Lee (UNAM),
Margarita Pereyra (UNAM), and Eleonora Troja (GSFC) report:

We observed the field of GRB 190701A (Ukwatta et al., GCN Circ.
24934) with the COATLI 50-cm telescope and interim imager at the
Observatorio AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir
(http://coatli.astroscu.unam.mx) from 2019-07-01 09:47:03 to 10:05:06
(from 25.6 seconds after the alert or 103 seconds to 0.33 hours after
the trigger), obtaining a total of 490 seconds of exposure in the w filter.

Comparing to the USNO and Pan-STARRS1 catalogs, we do not detect any new
sources brighter than w = 20.99 (3-sigma limiting mag) in the XRT error
region
(Osborne et al., GCN Circ. 24940).

Our w magnitudes are calibrated against the Pan-STARRS1 catalog, are on
an approximate AB system, and are not corrected for Galactic extinction
in the direction of the GRB.

We thank the COATLI technical team and the staff of the Observatorio
AstronÃ³mico Nacional.


GRB_name: GRB190630C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24947
SUBJECT: GRB 190630C: ISON-Castelgrande optical upper limit
DATE:    19/07/01 20:07:58 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), S. Schmalz (KIAM), A. Pozanenko (IKI), A. Volnova 
(IKI),  E. Mazaeva  (IKI),  I. Molotov (KIAM) report on behalf of larger 
GRB IKI FuN collaboration:

We observed the field of GRB 190630C (Ukwatta et al., GCN 24927) with 
ORI-22 (22 cm) telescope of ISON-Castelgrande observatory in Clear 
filter starting on July 01  (UT) 00:03:42.  We do not detect any object 
within enhanced Swift-XRT position (Goad et al., GCN 24930). Preliminary 
photometry of the field is following

Date       UT start t-T0    Filter Exp.   OT    Err. UL
                     (mid, days) (s)

2019-07-01 00:03:42 0.02584  CR    53*60  n/d   n/d 18.8

The photometry is  based on nearby USNO-B1.0 (R2) stars.


GRB_name: GRB190630B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24949
SUBJECT: GRB 190630B: Tien Shan and Koshka Zeiss-1000 optical upper limits
DATE:    19/07/01 21:13:42 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Kusakin (FAPHI), I. Reva (FAPHI), A. Novichonok 
(KIAM), A. Pozanenko (IKI), E. Mazaeva (IKI),  A. Volnova (IKI), I. 
Molotov (KIAM) report on behalf of larger GRB IKI FuN collaboration:

We observed the field of GRB 190630B (Krimm, et al., GCN 24913)   with 
Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting 
on June, 30 (UT) 18:40:21  and  Koshka Observatory starting on June, 30 
(UT) 20:38:42 in  R-filter. We do not detect the afterglow (Zheng, et 
al., GCN  24914; Zheng, et al., GCN  24931). Preliminary photometry of 
the field is following

Date       UT start t-T0    Filter Exp.  OT    Err. UL   Observatory
                     (mid, days)    (s)

2019-06-30 18:40:21 0.55999 R      6720  n/d   n/d  22.3 TSHAO
2019-06-30 20:38:42 0.63060 R      3780  n/d   n/d  21.9 Koshka

The photometry is based on several nearby USNO-B1.0 stars.
USNO-B1.0_id R2
1315-0255078 18.06
1314-0253302 17.18
1314-0253267 15.88


GRB_name: GRB190701A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24954
SUBJECT: GRB190701A: No candidates/counterpart in optical follow-up from GROWTH-India Telescope
DATE:    19/07/01 22:13:43 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

H. Kumar, V. Karambelkar, K. Deshmukh, G. Waratkar, V. Bhalerao (IITB), G.
C. Anupama, T. Stanzin (IIA) report on behalf of the GROWTH collaboration:

We observed GRB190701A reported by T. N. Ukwatta et al, (GCN 24934) with
0.7m GROWTH-India telescope. The field was observed in g, r and i filters.
We didnâ€™t detect any new source within an uncertainty region of 1.9
arcseconds (radius, 90% containment) around RA(J2000) = 01h 52m 19.54s,
Dec(J2000) = +58d 54' 33.9" (J.P. Osborne et al, GCN 24940).

We obtained the following upper limits:

------------------------------------------------------------------

 JD(Start)| Exposure(sec) | Filter | lim_Mag |

------------------------------------------------------------------

 2458666.351 | 600 | g | 19.18|

 2458666.373 | 600 | r | 20.57|

 2458666.382 | 600 | i | 19.52|

------------------------------------------------------------------


The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government
of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).


GRB_name: GRB190701A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24955
SUBJECT: GRB 190701A: Swift/UVOT Upper Limits
DATE:    19/07/01 22:18:53 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M. H. Siegel (PSU) and T. N. Ukwatta (LANL)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190701A
145 s after the BAT trigger (Ukwatta et al., GCN Circ. 24934).
No optical afterglow consistent with the enhanced XRT position
(Osborne et al. GCN Circ. 24940)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           145          295          147         >20.3
u_FC               303          553          246         >19.8
white              145         6776          727         >21.2
v                  629        11104          409         >19.3
b                  559         6570          432         >20.6
u                  303         6365          659         >20.6
w1                 677         6160          432         >19.9
m2                 652         5955          432         >19.3
w2                 610        10926         1158         >20.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.59 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190630C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24958
SUBJECT: GRB 190630C: Swift-XRT refined Analysis
DATE:    19/07/02 00:05:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , V. D'Elia
(ASDC), B. Sbarufatti (PSU), D.N. Burrows (PSU), J. D. Gropp (PSU),
J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore
(U. Leicester) and T.N. Ukwatta report on behalf of the Swift-XRT team:

We have analysed 5.7 ks of XRT data for GRB 190630C (Ukwatta et al. GCN
Circ. 24927), from 155 s to 57.3 ks after the  BAT trigger. The data
comprise 56 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Goad et al. (GCN Circ. 24930).

The light curve can be modelled with an initial power-law decay with an
index of alpha=4.3 (+0.7, -0.5), followed by a break at T+310 s to an
alpha of 1.06 (+0.12, -0.23).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.09 (+0.33, -0.29). The
best-fitting absorption column is  2.7 (+/-0.7) x 10^21 cm^-2, in
excess of the Galactic value of 1.1 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.2 (+/-0.3) and a
best-fitting absorption column of 2.0 (+1.0, -0.9) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.2 x 10^-11 (4.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.0 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^21 cm^-2
Excess significance: 1.7 sigma
Photon index:      2.2 (+/-0.3)

If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 3.0 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.7 x
10^-14 (1.4 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00912239.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190701A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24961
SUBJECT: GRB 190701A: Swift-XRT refined Analysis
DATE:    19/07/02 02:35:59 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

E. Ambrosi  (INAF-IASFPA) , V. D'Elia (ASDC), D.N. Burrows (PSU), J. D.
Gropp (PSU), A. Tohuvavohu (PSU), K.L. Page (U. Leicester), A.P.
Beardmore (U. Leicester), P.A. Evans (U. Leicester), A. D'Ai
(INAF-IASFPA) and T.N. Ukwatta report on behalf of the Swift-XRT team:

We have analysed 8.4 ks of XRT data for GRB 190701A (Ukwatta et al. GCN
Circ. 24934), from 144 s to 34.9 ks after the  BAT trigger. The data
comprise 10 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Osborne et al. (GCN Circ. 24935).

The light curve can be modelled with an initial power-law decay with an
index of alpha=8.0 (+0.0, -0.9), followed by a break at T+239 s to an
alpha of 0.40 (+0.08, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.81 (+0.23, -0.12). The
best-fitting absorption column is  consistent with the Galactic value
of 6.4 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.7 x 10^-11 (7.1 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.4 (+/-1.0) x 10^21 cm^-2
Galactic foreground: 6.4 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.81 (+0.23, -0.12)

If the light curve continues to decay with a power-law decay index of
0.40, the count rate at T+24 hours will be 0.018 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.5 x
10^-13 (1.3 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00912310.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190630A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24965
SUBJECT: IPN triangulation of GRB 190630A (short)
DATE:    19/07/02 12:01:33 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova and K. Hurley, on behalf of the IPN,

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

S. Xiao, C. K. Li, X. B. Li, Y. Huang, and S. L. Xiong
on behalf of the Insight-HXMT GRB team,
report:

The short-duration GRB 190630A was detected
by Fermi (GBM trigger 583567803), INTEGRAL (SPI-ACS),
and Insight (HXMT/HE) at about 22198 s UT (06:09:58).

We have triangulated this GRB to a GBM-INTEGRAL annulus centered at
RA(2000)=32.604 deg (02h 10m 25s)  Dec(2000)=-47.005 deg (-47d 00' 16"),
whose radius is 73.654 +/- 2.609 deg (3 sigma).

The annulus is partially consistent with the 90% localization
probability region of GW compact binary merger candidate
event S190630ag (The LIGO Scientific Collaboration and the Virgo
Collaboration GCN Circ. 24922).

This annulus may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190630_T22198/IPN/


GRB_name: GRB190628B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24972
SUBJECT: GRB 190628B - AstroSat CZTI detection
DATE:    19/07/03 12:04:21 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

A. Marathe (NITK, IITB), Y. Sharma (IITB), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190628B, in the 40-200 keV energy range. The light curve shows two pulses of emission with strongest peak at 04:23:39 UT. The measured peak count rate associated with the burst is 212 cts/s above the background in the combined data of quadrants B, C and D. with a total of 600 cts. Data from quadrant A were excluded from analysis due to noisy pixels. The local mean background count rate was 437 cts/s. Using cumulative rates, we measure a T90 of 12 s.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190701A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24973
SUBJECT: GRB 190701A, Swift-BAT refined analysis 
DATE:    19/07/03 14:11:50 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),  J. R. Cummings (CPI),
H. A. Krimm (NSF), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190701A (trigger #912310)
(Ukwatta, et al., GCN Circ. 24934).  The BAT ground-calculated position is
RA, Dec = 28.131, 58.899 deg which is 
  RA(J2000)  =  01h 52m 31.5s 
  Dec(J2000) = +58d 53' 56.9" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 52%.

The mask-weighted light curve shows a multi-peaked structure.  The main period
of emission includes three broad peaks between roughly T+0 sec and T+100 sec,
peaking about T+38 sec.  T90 (15-350 keV) is 52.4 +- 4.0 sec (estimated error
including systematics).

The time-averaged spectrum from T+35.0 to T+90.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.91 +- 0.27.  The fluence in the 15-150 keV band is 8.7 +- 1.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+37.92 sec in the 15-150 keV band
is 1.2 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/912310/BA/


GRB_name: GRB190530A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24978
SUBJECT: GRB 190530A: Observation of the afterglow by NOEMA
DATE:    19/07/04 15:22:54 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), M. Bremer (IRAM), 
S. Schulze (Weizmann), C. C. Thoene, D. A. Kann, L. Izzo, M. Blazek, 
K. Bensch (all HETH/IAA-CSIC), D. A. Perley (LJMU), S. Martin (ALMA), 
I. de Gregorio-Monsalvo (ESO), M. Michalowski (AOI-AMU), 
R. Sanchez-Ramirez (INAF-IAPS), D. B. Malesani (DTU Space) report:

We observed the field of the bright GRB 190530A (Fermi team GCN 
24676) with NOEMA, at wavelengths between 76 and 150 GHz in 4 
epochs, ranging between 31 May 2019, at 14:29 UT (1.17 days after the 
burst) and 15 June 2019, at 20:54 UT (16.44 days after the burst). The 
afterglow (discovered in the optical by Lipunov et al. GCN 24680) was 
detected on the first epoch with a flux density of 1.0 mJy at 92 GHz. At 
this time the peak frequency was located close to this observed frequency.

In the subsequent epochs the peak frequency of the synchrotron spectrum 
was bluewards of the 76 GHz frequency band and the source declined 
steadily in flux density until it was no longer detected in our latest 
observation, which had an r.m.s of 0.066 mJy at the 92 GHz band.


GRB_name: GRB190701B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24979
SUBJECT: Konus-Wind observation of GRB 190701B
DATE:    19/07/04 16:20:23 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 190701B (IBAS detection: Gotz et al., GCN 24936)
triggered Konus-Wind at T0=36303.292 s UT (10:05:03.292).

The burst light curve shows a multi-peaked structure
which starts at ~T0-3.3 s and has a total duration of ~13 s.
The emission is seen up to ~1.3 MeV.

As observed by Konus-Wind, the burst
had a fluence of 3.51(-0.46,+0.70)x10^-6 erg/cm2,
and a 64-ms peak energy flux, measured from T0-0.072 s,
of 1.39(-0.63,+0.68)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 1.3 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.43(-0.33,+0.41),
and Ep = 112(-30,+64) keV (chi2 = 48/60 dof).
Fitting by the GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index:
beta < -2.17 (chi2 = 48/59 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190701_T36303/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24986
SUBJECT: GRB 190627A: Discovery Channel Telescope late time observations
DATE:    19/07/05 16:02:47 GMT
FROM:    Simone Dichiara at UMCP/NASA/GSFC  <dichiara@umd.edu>

S.Dichiara (UMD, NASA-GSFC), P. Gatkine (UMD), J.M. Durbak (UMD),
E. Troja (UMD, NASA-GSFC), S.B. Cenko (NASA-GSFC), A. Kutyrev (UMD,
NASA-GSFC), S. Veilleux (UMD), report on behalf of a larger
collaboration:

We observed at the optical counterpart of GRB 190106A (Sonbas et al.,
GCN 24888) using the Large Monolithic Imager (LMI) on the 4.3m Discovery
Channel Telescope (DCT) at Happy Jack, AZ. Observations started on July
 05, 07:46:14 UT (about 7.85 days after the Swift trigger) with SDSS r
and i filters.
We detected the optical counterpart (Siegel & Sonbas, GCN 24889)
measuring the following AB magnitudes:

Start Time           Exposure    Filter    Magnitude
(days from trigger)     (s)
-------------------------------------------------------
7.85               4x300          r'    23.36 +- 0.11
7.87               4x300          i'    23.17 +- 0.11
-------------------------------------------------------

Magnitudes are calibrated against Pan-STARRS catalog.

We thank the staff of the Discovery Channel Telescope in particular
Casey Kyte, Ishara Nisley for assistance with these observations.


GRB_name: GRB190706A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24992
SUBJECT: GRB 190706A: MAXI/GSC detection
DATE:    19/07/06 10:53:40 GMT
FROM:    Kazuki Shiraishi at Tokyo Institute of Technology  <shiraishi@hp.phys.titech.ac.jp>

K. Shiraishi (Tokyo Tech), H. Negoro, M. Nakajima, W. Maruyama, M. Aoki, K.
Kobayashi (Nihon U.),
S. Nakahira, T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, M. Serino, S. Sugita, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
M. Shidatsu (Ehime U.),
N. Kawai, M. Sugizaki, M. Oeda (Tokyo Tech),
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, M.
Tominaga (JAXA),
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake
(Kyoto U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.),
T. Kawamuro (NAOJ),
K. Yamaoka (Nagoya U.),
Y. Kawakubo (LSU)

report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered an uncatalogued X-ray transient
source at 03:26:23 UT on July 6, 2019.

Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (26.605 deg, -43.248 deg) = (01 46 25, -43 14 52) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.39 deg and 0.36 deg, respectively.
The roll angle of the long axis from the north direction is 51.0 deg
counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90% containment
radius).
The X-ray flux averaged over the scan was 53 +- 16 mCrab
(4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (26.800, -41.863) deg = (01 47 11, -41 51 46) (J2000)
(R.A., Dec) = (25.798, -41.961) deg = (01 43 11, -41 57 39) (J2000)
(R.A., Dec) = (26.264, -44.604) deg = (01 45 03, -44 36 14) (J2000)
(R.A., Dec) = (27.310, -44.502) deg = (01 49 14, -44 30 07) (J2000)

There was no significant excess flux in the previous transit at UT 01:53
and in the next transit at 04:59 UT with an upper limit of 20 mCrab for
each.


GRB_name: GRB190706B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24993
SUBJECT: GRB 190706B: Swift detection of a burst
DATE:    19/07/06 12:53:10 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Tohuvavohu (PSU), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), B. Sbarufatti (PSU)
and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 12:40:50 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190706B (trigger=913302).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 107.449, -29.584, which is 
   RA(J2000)  =  07h 09m 48s
   Dec(J2000) = -29d 35' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a few peaks
with a total duration of about 25 sec.  The peak count rate
was ~1100 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 12:42:24.4 UT, 94.4 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 107.46161, -29.55341 which is
equivalent to:
   RA(J2000)  = 07h 09m 50.79s
   Dec(J2000) = -29d 33' 12.3"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 116 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.40
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 100 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.15. 

Burst Advocate for this burst is A. Tohuvavohu (aaronb AT swift.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190706B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24994
SUBJECT: GRB 190706B: Prompt enhanced Swift-XRT position
DATE:    19/07/06 13:23:56 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:

Using  promptly downlinked XRT event data for GRB 190706B, we find an
enhanced XRT position of the afterglow: RA, Dec: 107.4616, -29.5525
which is equivalent to:
   RA (J2000)  = 07 09 50.78
   Dec (J2000) = -29 33 09.1
with an uncertainty of 2.0 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/913302.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190706B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24995
SUBJECT: GRB 190706B: Enhanced Swift-XRT position
DATE:    19/07/06 15:30:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1466 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 190706B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 107.46211, -29.55293 which is equivalent
to:

RA (J2000): 07h 09m 50.91s
Dec (J2000): -29d 33' 10.5"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB190706B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  24999
SUBJECT: GRB 190706B: Swift-XRT refined Analysis
DATE:    19/07/06 23:11:12 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), J. D. Gropp (PSU), J.A. Kennea (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester),
A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB) and A. Tohuvavohu report
on behalf of the Swift-XRT team:

We have analysed 8.5 ks of XRT data for GRB 190706B (Tohuvavohu et al.
GCN Circ. 24993), from 98 s to 29.4 ks after the  BAT trigger. The data
comprise 26 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Beardmore et al. (GCN Circ. 24994).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.80 (+0.08, -0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.94 (+0.23, -0.22). The
best-fitting absorption column is  3.1 (+1.0, -0.7) x 10^21 cm^-2,
consistent with the Galactic value of 2.4 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.9 x 10^-11 (5.5 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+1.0, -0.7) x 10^21 cm^-2
Galactic foreground: 2.4 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.94 (+0.23, -0.22)

If the light curve continues to decay with a power-law decay index of
0.80, the count rate at T+24 hours will be 5.0 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-13 (2.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00913302.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190706B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25003
SUBJECT: GRB 190706B: Swift-BAT refined analysis
DATE:    19/07/07 02:03:38 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU),
A. Tohuvavohu (PSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 190706B (trigger #913302)
(Tohuvavohu et al., GCN Circ. 24993).  The BAT ground-calculated position is
RA, Dec = 107.443, -29.575 deg which is
   RA(J2000)  =  07h 09m 46.4s
   Dec(J2000) = -29d 34' 30.7"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 69%.

The mask-weighted light curve shows a multi-peaked structure that starts
at ~T0 and ends at ~T+30 s. The highest peak occurs at ~T+1 s.
T90 (15-350 keV) is 25.16 +- 6.35 sec (estimated error including
systematics).

The time-averaged spectrum from T-0.25 to T+27.48 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.90 +- 0.23.  The fluence in the 15-150 keV band is 5.8 +- 0.9 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T+0.10 sec in the 15-150 keV band
is 1.4 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/913302/BA/


GRB_name: GRB190707A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25005
SUBJECT: GRB 190707A: Fermi GBM Final Real-time Localization
DATE:    19/07/07 07:01:55 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 06:50:05 UT on 7 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190707A (trigger 584175010.12659 / 190707285).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 152.9, Dec = -31.0 (J2000 degrees, equivalent to J2000 10h 11m, -31d 00'), with a statistical uncertainty of 2.0 degrees.

The angle from the Fermi LAT boresight is 62.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190707285/quicklook/glg_skymap_all_bn190707285.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190707285/quicklook/glg_healpix_all_bn190707285.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190707285/quicklook/glg_lc_medres34_bn190707285.gif


GRB_name: GRB190707A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25006
SUBJECT: GRB 190707A: BALROG localization (Fermi Trigger 584175010 / GRB 190707285)
DATE:    19/07/07 07:12:39 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

J. Burgess, B. Biltzinger, F. Kunzweiler, F. Berlato & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
584175010 at 06:50:05 on 07 July 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 153.3+/-1.7 deg
Decl.(2000.0) = -36.3+/-2.7 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190707285/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190707285/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190707285/json

                        


GRB_name: GRB190707B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25008
SUBJECT: GRB 190707B: Fermi GBM Final Real-time Localization
DATE:    19/07/07 07:34:07 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 07:23:01 UT on 7 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190707B (trigger 584176986.215968 / 190707308).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 184.3, Dec = -9.5 (J2000 degrees, equivalent to J2000 12h 17m, -9d 30'), with a statistical uncertainty of 4.9 degrees.

The angle from the Fermi LAT boresight is 72.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190707308/quicklook/glg_skymap_all_bn190707308.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190707308/quicklook/glg_healpix_all_bn190707308.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190707308/quicklook/glg_lc_medres34_bn190707308.gif


GRB_name: GRB190706B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25023
SUBJECT: GRB 190706B: Swift/UVOT Detection
DATE:    19/07/07 19:29:34 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and A. Tohuvavohu (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190706B
100 s after the BAT trigger (Tohuvavohu et al., GCN Circ. 24993).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 24995) is detected in the initial UVOT
exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white_FC           100          250          147         20.35 +/- 0.27
u_FC               312          562          246        >19.86
white              100         5778          519         >20.9
v                  642        17542          561         >19.9
b                  568         5644          292         >20.6
u                  312        13071          647         >19.9
w1                 691        11551         1204         >20.0
m2                 666         7285          490         >19.6
w2                 618        17284         1199         >20.5


The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.15 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190704A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25024
SUBJECT: IPN triangulation of GRB 190704A (short)
DATE:    19/07/07 20:59:48 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,

The short-duration GRB 190704A has been detected by Konus-Wind,
INTEGRAL (SPI-ACS trigger 8323) and Swift (BAT), so far,
at about 22353 s UT (06:12:33).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Corners:
   329.352 (21h 57m 25s) +48.888 (+48d 53' 15")
   328.224 (21h 52m 54s) +47.140 (+47d 08' 24")
   240.886 (16h 03m 33s)  -1.156 ( -1d 09' 23")
   242.721 (16h 10m 53s)  -1.662 ( -1d 39' 42")
  ---------------------------------------------
The error box area is 175 sq. deg, and its maximum
dimension is 88.2 deg (the minimum one is 57.1 arcmin).
The Sun distance was greater than ~100 deg.

This box may be improved.

Fermi-GBM was enabled at the time of the GRB according to
glg_poshist_all_190704_v00.fit, so the non-detection by GBM
implies that the burst was Earth-Occulted for Fermi.

This burst is spatially and temporally inconsistent with IceCube-190704A 
(The IceCube Collaboration, GCN Circ. 24981) and Baksan Neutrino 
Observatory Alerts on 2019-07-03 (Lipunov et al., GCN Circ. 24976
and 24980).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190704_T22351/IPN

The time history and spectrum will be given in forthcoming
GCN Circulars.


GRB_name: GRB190708A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25030
SUBJECT: GRB 190708A: Fermi GBM Final Real-time Localization
DATE:    19/07/08 08:56:44 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 08:45:11 UT on 8 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190708A (trigger 584268316.798502 / 190708365).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 209.9, Dec = -1.3 (J2000 degrees, equivalent to J2000 13h 59m, -1d 18'), with a statistical uncertainty of 7.2 degrees.

The angle from the Fermi LAT boresight is 74.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190708365/quicklook/glg_skymap_all_bn190708365.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190708365/quicklook/glg_healpix_all_bn190708365.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190708365/quicklook/glg_lc_medres34_bn190708365.gif


GRB_name: GRB190704A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25032
SUBJECT: Konus-Wind observation of GRB 190704A
DATE:    19/07/08 13:14:30 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:

The short-duration, hard-spectrum
(IPN triangulation: Svinkin et al., GCN 25024)
triggered Konus-Wind at T0=22355.497 s UT (06:12:35.497).

The burst light curve shows a pulse with a duration of ~1.5 s
followed by a weaker pulse at ~T0+3.0.
The emission is seen up to ~16 MeV.

As observed by Konus-Wind, the burst
had a fluence of 3.56(-1.26,+3.48)x10^-6 erg/cm2,
and a 64-ms peak energy flux, measured from T0-0.310 s,
of 5.03(-2.48,+6.16)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 16 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.72(-0.41,+0.63),
and Ep = 861(-420,+2298) keV (chi2 = 21/20 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190704_T22355/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190706C
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25035
SUBJECT: IPN triangulation of GRB 190706C (long/very bright)
DATE:    19/07/08 19:18:06 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team, report:

The long-duration, very bright GRB 190706C
has been detected by INTEGRAL (SPI-ACS trigger 8325),
CALET (GBM trigger 1246455687), Konus-Wind, and Swift (BAT),
so far, at about 49348 s UT (13:42:28).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   351.671 (23h 26m 41s) +24.754 (+24d 45' 15")
  Corners:
   352.463 (23h 29m 51s) +23.689 (+23d 41' 22")
   352.742 (23h 30m 58s) +23.905 (+23d 54' 20")
   350.850 (23h 23m 24s) +25.803 (+25d 48' 11")
   350.570 (23h 22m 17s) +25.583 (+25d 35' 00")
  ---------------------------------------------
The error box area is about 3079 sq. arcmin, and its maximum
dimension is 2.59 deg (the minimum one is 20.0 arcmin).
The Sun distance was about 100 deg.

This box may be improved.

This burst is spatially and temporally inconsistent with
LIGO/Virgo S190706ai (LVC GCN Circ. 24998) and
LIGO/Virgo S190707q (LVC GCN Circ. 25012).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190706_T49348/IPN

The time history and spectrum will be given in forthcoming
GCN Circulars.


GRB_name: GRB190706D
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25036
SUBJECT: IPN triangulation of GRB 190706D (short)
DATE:    19/07/08 19:23:17 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team, report:

The short-duration GRB 190706D has been detected by
INTEGRAL (SPI-ACS trigger 8326), Konus-Wind,
and Swift (BAT), so far, at about 61381 s UT (17:03:01).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   324.618 (21h 38m 28s)  +9.901 ( +9d 54' 02")
  Corners:
   329.663 (21h 58m 39s)  +2.806 ( +2d 48' 22")
   334.060 (22h 16m 14s)  +7.015 ( +7d 00' 54")
   317.812 (21h 11m 15s) +15.409 (+15d 24' 34")
   312.109 (20h 48m 26s)  +9.995 ( +9d 59' 42")
  ---------------------------------------------
The error box area is about 113 sq. deg, and its maximum
dimension is 21.9 deg (the minimum one is 6 deg).
The Sun distance was about 130 deg.

This box may be improved.

The main fraction of the box was Earth occulted for Fermi.

This burst is spatially and temporally inconsistent with
LIGO/Virgo S190706ai (LVC GCN Circ. 24998) and
LIGO/Virgo S190707q (LVC GCN Circ. 25012).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190706_T61390/IPN

The time history and spectrum will be given in forthcoming
GCN Circulars.


GRB_name: GRB190708B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25037
SUBJECT: GRB 190708B: MAXI/GSC detection
DATE:    19/07/08 21:35:14 GMT
FROM:    Motoko Serino at RIKEN/MAXI  <motoko@crab.riken.jp>

Y. Kawakubo (LSU), M. Nakajima (Nihon U.), M. Serino (AGU),
H. Negoro, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.),
S. Nakahira, T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, S. Sugita, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
M. Shidatsu (Ehime U.),
N. Kawai, M. Sugizaki, M. Oeda, K. Shiraishi (Tokyo Tech),
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, M. Tominaga (JAXA),
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.),
T. Kawamuro (NAOJ),
K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at 19:49:58 UT .
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (326.571 deg, 7.711 deg) = (21 46 17, +07 42 39) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.22 deg and 0.19 deg, respectively.
The roll angle of long axis from the north direction is 125.0 deg counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 394 +- 60 mCrab
(4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (325.953, 7.630) deg = (21 43 48, +07 37 47) (J2000)
(R.A., Dec) = (326.121, 7.246) deg = (21 44 29, +07 14 45) (J2000)
(R.A., Dec) = (327.396, 7.791) deg = (21 49 35, +07 47 27) (J2000)
(R.A., Dec) = (327.229, 8.175) deg = (21 48 54, +08 10 30) (J2000)
There was no significant excess flux in the previous transit at UT 19:29
and in the next transit at 21:02 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB190706C
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25038
SUBJECT: GRB 190706C: CALET Gamma-Ray Burst Monitor detection
DATE:    19/07/09 10:01:00 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

T. Sakamoto, A. Yoshida, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The bright GRB 190706C (IPN triangulation: Svinkin et al., GCN
Circ. 25035) triggered the CALET Gamma-ray Burst Monitor (CGBM)
at 13:42:22.560 UTC on 6 July 2019.
The burst signal was seen by all CGBM detectors.

The burst light curve shows a single multi-peaked emission episode which
starts at T+3.5 sec, peaks at T+6.6 sec and ends at T+10.4 sec. The T90
and T50 durations measured by the SGM data are 3.9 +- 0.8 sec and
2.2 +- 0.1 sec (40-1000 keV), respectively.

Despite the burst high intensity there is almost no emission above ~1 MeV.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1246455687/

The CALET data used in this analysis are provided by the Waseda CALET
Operation Center located at the Waseda University.


GRB_name: GRB190708B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25040
SUBJECT: GRB 190708B: Tiled Swift observations
DATE:    19/07/09 12:21:11 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
MAXI GRB 190708B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00080

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the MAXI event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190708B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25041
SUBJECT: GRB 190708B: Tiled Swift observations
DATE:    19/07/09 12:31:46 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
MAXI GRB 190708B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00080

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the MAXI event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190706C
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25042
SUBJECT: Konus-Wind observation of GRB 190706C
DATE:    19/07/09 12:39:03 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration, very bright GRB 190706C
(IPN triangulation: Svinkin et al., GCN 25035;
CALET Gamma-Ray Burst Monitor detection: Sakamoto et al., GCN 25038)
triggered Konus-Wind at T0=49348.84 s UT (13:42:28.840).

The burst light curve shows a multi-peaked structure
with a total duration of ~6.5 s.
The emission is seen up to ~2 MeV.

As observed by Konus-Wind, the burst
had a fluence of 2.52(-0.17,+0.20)x10^-5 erg/cm2,
and a 64-ms peak energy flux, measured from T0+2.640 s,
of 1.80(-0.19,+0.19)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+3.072 s)
is best fit in the 20 keV - 2 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.56(-0.09,+0.10),
the high energy photon index beta = -3.09(-0.70,+0.35),
the peak energy Ep = 281(-20,+19) keV,
chi2 = 34/56 dof.

The spectrum near the peak count rate
(measured from T0+2.048 to T0+3.072 s)
is best fit in the 20 keV - 3 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.39(-0.12,+0.13),
and Ep = 288(-19,+22) keV (chi2 = 53/51 dof).
Fitting by the GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index:
beta < -2.86 (chi2 = 52/50 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190706_T49348/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190708B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25043
SUBJECT: Konus-Wind observation of GRB 190708B
DATE:    19/07/09 15:08:44 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lysenko,
and T. Cline on behalf of the Konus-Wind team, report:

A long GRB was detected by Konus-Wind (KW) in the
waiting mode on July 8, 2019 at ~71160 s UT (19:46:00),
~240 s before the MAXI trigger (GRB 190708B;
Kawakubo et al., GCN 25037).

The burst light curve shows a single pulse
with a duration of ~ 20 s. Taking into account the
proximity of this burst to the MAXI/GSC trigger and
the consistency of the KW ecliptic latitude response with
the position of GRB 190708B we suggest that KW observed
the main part of GRB 190708B.

As observed by KW, the burst had a fluence of
3.44(-0.33,+1.35)x10^-6 erg/cm2 and a 2.944-s peak flux,
measured from ~T0(MAXI)-236.3 s, of 2.54(-0.73,+1.21)x10^-7 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

Modeling the KW 3-channel time-integrated spectrum
(from ~T0(MAXI)-242.2 s to ~T0(MAXI)-221.6 s)
by a simple power-law model yields the power law
index of -2.01(-0.08,+0.16), chi2 = 3.3/1 dof.

Modeling this spectrum by a power law with exponential cutoff model
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with the photon index alpha fixed to -1, yields
Ep = 91.6 (-15.7,+28.7) keV, chi2 = 0.12/1 dof.

The KW light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB190708B

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.


GRB_name: GRB190706D
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25047
SUBJECT: Konus-Wind observation of GRB 190706D
DATE:    19/07/10 12:32:13 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:

The short-duration GRB 190706D
(IPN triangulation: Svinkin et al., GCN 25036)
triggered Konus-Wind at T0=61390.044 s UT (17:03:10.044).

The burst light curve shows a a single pulse
which starts at ~T0-0.3 s and has a total duration of ~0.5 s.
The emission is seen up to ~3 MeV.

As observed by Konus-Wind, the burst
had a fluence of 7.44 (-1.10,+1.24)x10^-7 erg/cm2,
and a 64-ms peak energy flux, measured from T0+0.082 s,
of 2.37 (-0.35,+0.40)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

Since the bulk of the burst emission was detected before
the trigger, the spectral analysis was performed using
the KW 3-channel light curve data.

Modeling the KW 3-channel time-integrated spectrum
(from T0-0.294 s to T0+0.172 s)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -0.71 (-0.30,+0.36), and Ep = 246 (-51,+70) keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190706_T61390/

All the quoted errors are at the 68% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190708B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25053
SUBJECT: GRB 190708B: Swift-XRT observations
DATE:    19/07/11 06:46:42 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

A. Tohuvavohu (PSU), J.A. Kennea (PSU), B. Sbarufatti (PSU), J.P.
Osborne (U. Leicester), K.L. Page (U. Leicester), A. D'Ai
(INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB) and P.A.
Evans (U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the MAXI-detected
burst GRB 190708B (Kawakubo et al. GCN Circ. 25037) in a series of
observations tiled on the sky. The total exposure time is 3.9 ks,
distributed over 7 tiles; the maximum exposure at a single sky location
was 1.2 ks. The data were collected between T0+58.5 ks and T0+69.2 ks,
and are entirely in Photon Counting (PC) mode. 

One uncatalogued X-ray source has been detected, it is below the RASS
limit and shows no definitive signs of fading. Therefore, at the
present time we cannot confirm this as the afterglow. Details of this
source are given below:

Source 1:
  RA (J2000):  326.4868  =  21:45:56.83
  Dec (J2000): +7.8821  =  +07:52:55.5
  Error: 7.7 arcsec (radius, 90% conf.)
  Count-rate: 0.0151 [+0.0054, -0.0044] ct s^-1   
  Distance: 685 arcsec from MAXI position.
  Flux: (2.13 [+0.77, -0.62])e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)

A catalogued source was also detected.

The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00080.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190712A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25055
SUBJECT: GRB 190712A: Fermi GBM Final Real-time Localization
DATE:    19/07/12 02:28:32 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 02:16:41 UT on 12 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190712A (trigger 584590606.72695 / 190712095).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 288.4, Dec = 56.2 (J2000 degrees, equivalent to J2000 19h 13m, 56d 12'), with a statistical uncertainty of 7.6 degrees.

The angle from the Fermi LAT boresight is 66.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190712095/quicklook/glg_skymap_all_bn190712095.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190712095/quicklook/glg_healpix_all_bn190712095.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190712095/quicklook/glg_lc_medres34_bn190712095.gif


GRB_name: GRB190706C
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25060
SUBJECT: GRB 190706C: Insight-HXMT/HE detection
DATE:    19/07/12 13:55:37 GMT
FROM:    YaoGuang Zheng at IHEP  <zhengyg@ihep.ac.cn>

Y. G. Zheng, C. Cai, Q. Luo, S. Xiao, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-07-06T13:42:25.95 (T0), Insight-HXMT/HE detected 
GRB 190706C (trigger ID: HEB190706571) in a routine search of the data, 
which was also triggered by INTEGRAL/SPI-ACS (trigger #8325),
CALET/CGBM (GCN #25038) and Konus-Wind (GCN #25042).

The Insight-HXMT/HE light curve mainly consists of a multiple  
pulses with a duration (T90) of 2.88 s measured from T0+0.13 s. 
The 1-ms peak rate, measured from T0+2.76 s, is 25839 cnts/sec. 
The total counts from this burst is 32484 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190706571_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190706D
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25061
SUBJECT: GRB 190706D: Insight-HXMT/HE detection
DATE:    19/07/12 14:08:53 GMT
FROM:    YaoGuang Zheng at IHEP  <zhengyg@ihep.ac.cn>

Y. G. Zheng, C. Cai, Q. Luo, S. Xiao, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-07-06T17:03:05.40 (T0), Insight-HXMT/HE detected 
GRB 190706D (trigger ID: HEB190706710) in a routine search of the dataï¼Œ
which was also triggered by INTEGRAL/SPI-ACS (trigger #8326) 
and Konus-Wind (GCN #25047).

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 0.28 s measured from T0-0.10 s. 
The 1-ms peak rate, measured from T0-0.07 s, is 2551 cnts/sec. 
The total counts from this burst is 633 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190706710_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190714A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25068
SUBJECT: GRB 190714A: MAXI/GSC detection
DATE:    19/07/14 14:05:03 GMT
FROM:    Motoko Serino at RIKEN/MAXI  <motoko@crab.riken.jp>

M. Serino (AGU), H. Negoro (Nihon U.), 
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.),
S. Nakahira, T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, S. Sugita, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
M. Shidatsu (Ehime U.),
N. Kawai, M. Sugizaki, M. Oeda, K. Shiraishi (Tokyo Tech),
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, M. Tominaga (JAXA),
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.),
Y. Kawakubo (LSU),
T. Kawamuro (NAOJ),
K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at 13:20:27 UT.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (246.579 deg, 14.917 deg) = (16 26 18, +14 55 01) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.24 deg and 0.21 deg, respectively.
The roll angle of long axis from the north direction is 12.0 deg counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 230 +- 41 mCrab
(4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (247.817, 15.678) deg = (16 31 16, +15 40 40) (J2000)
(R.A., Dec) = (247.520, 15.992) deg = (16 30 04, +15 59 31) (J2000)
(R.A., Dec) = (245.586, 14.273) deg = (16 22 20, +14 16 22) (J2000)
(R.A., Dec) = (245.884, 13.962) deg = (16 23 32, +13 57 43) (J2000)
There was no significant excess flux in the previous transit at UT 11:48
with an upper limit of 20 mCrab for each.


GRB_name: GRB190714A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25069
SUBJECT: GRB 190714A: Tiled Swift observations
DATE:    19/07/14 15:43:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
MAXI GRB 190714A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00081

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the MAXI event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190714B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25070
SUBJECT: GRB 190714B: Fermi GBM Final Real-time Localization
DATE:    19/07/14 22:18:39 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

The Fermi GBM team reports the detection of a likely long GRB.

At 13:44:39 UT on 14 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 190714B (trigger 584804684.038996 / 190714573).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 71.2, Dec = -6.1 with a statistical uncertainty of 2.0 degrees.

The angle from the Fermi LAT boresight is 106.7 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190714573/quicklook/glg_skymap_all_bn190714573.png

The HEALPix FITS file, including the estimated localization systematic, can
be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190714573/quicklook/glg_healpix_all_bn190714573.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190714573/quicklook/glg_lc_medres34_bn190714573.gif


GRB_name: GRB190708B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25073
SUBJECT: GRB 190708B: confirmation of the X-ray afterglow
DATE:    19/07/15 19:19:43 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

B. Sbarufatti (PSU) reports on behalf of the Swift/XRT team:

Swift has performed further observations of the field of the
MAXI/GSC-detected burst GRB 190708B (Kawabuko et al., GCN 25037). 
An additional 3.4 ks of data were collected between 5.96 days  and 6.11 days after the MAXI trigger.
Source 1, initially reported by Tohuvavohu et al. (GCN 25053) as the likely X-ray counterpart, has faded to a level of 2.9E-3 counts/s (1.3E-13 ergs/cm^2/s). 
Source 1 is  therefore confirmed as the X-ray afterglow of GRB 190708B.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190714A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25076
SUBJECT: GRB 190714A: an X-ray flare from 2E 1624.6+1504/UCAC4 525-061488 
DATE:    19/07/16 15:40:08 GMT
FROM:    Hitoshi Negoro at Nihon U  <negoro.hitoshi@nihon-u.ac.jp>

H. Negoro (Nihon U.), W. Iwakiri, T. Sato (Chuo U.), J. Kennea (PSU), K. Page (U. Leicester),
M. Serino (AGU), T. Mihara (RIKEN), Y. Tsuboi (Chuo U.),
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.), 
S. Nakahira, T. Tamagawa, M. Matsuoka (RIKEN), 
T. Sakamoto, S. Sugita, H. Nishida, A. Yoshida (AGU), 
R. Sasaki, H. Kawai (Chuo U.), M. Shidatsu (Ehime U.),
N. Kawai, M. Sugizaki, M. Oeda, K. Shiraishi (Tokyo Tech), 
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N.Isobe, R. Shimomukai, M. Tominaga (JAXA), 
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.), 
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), 
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.), 
T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU)
report on behalf of the MAXI team:

Swift-XRT performed 7 tiled followup observations for GRB 190714A (Serino et al. GCN 25068;
Evans GCN 25069) on July 14th, 2019 (from T0 +7.9 ks to T0 +9.3 ks).
We conclude that GRB 190714A is not a GRB, but very likely to be an X-ray flare from 
the M (or dMe) star 2E 1624.6+1504/UCAC4 525-061488 (for detail, see Negoro et al. ATel #12944). 


GRB_name: GRB190716A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25078
SUBJECT: GRB 190716A: Fermi GBM Final Real-time Localization
DATE:    19/07/16 22:11:43 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 22:00:08 UT on 16 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190716A (trigger 585007213.119332 / 190716917).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 345.6, Dec = -0.8 (J2000 degrees, equivalent to J2000 23h 02m, 0d 48'), with a statistical uncertainty of 6.4 degrees.

The angle from the Fermi LAT boresight is 74.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190716917/quicklook/glg_skymap_all_bn190716917.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190716917/quicklook/glg_healpix_all_bn190716917.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190716917/quicklook/glg_lc_medres34_bn190716917.gif


GRB_name: GRB190716A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25079
SUBJECT: GRB 190716A: BALROG localization (Fermi Trigger 585007213 / GRB 190716917)
DATE:    19/07/16 22:29:05 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
585007213 at 22:00:08 on 16 July 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 337.9+/-1.5 deg
Decl.(2000.0) = -0.1+/-1.8 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190716917/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190716917/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190716917/json

                        


GRB_name: GRB190613B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25081
SUBJECT: GRB 190613B: FRAM-Auger afterglow detection
DATE:    19/07/17 11:48:38 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ),
Martin Masek, Petr Janecek, Sergey Karpov, Jakub Jurysek,
Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza
(Institute of Physics, Prague, CZ)

report:

The 30cm robotic telescope FRAM-Auger in MalargÃ¼e
(Argentina) reacted robotically to the Swift/BAT and
Fermi/GBM alert of GRB190613B (D'Ai et al., GCNC 24807;
Bissaldi et al., GCNC 24814), starting with a series of
20s unfiltered images at 10:47:33.45 UT, i.e. 31.4s
post trigger.

We detect the source reported by Marshall et al. (GCN
24817), Zheng & Filipenko (GCN 24818), Hu et al. (GCNC
24826), de Ugarte Postigo (GCNC 24825) and other teams
at a 5 x 20s combined image taken between 79s and 202s
after the initial trigger. The brightness of the object
was r'(AB) = 15.6 +- 0.2, as calibrated against APASS
Catalogue.


GRB_name: GRB190718A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25082
SUBJECT: GRB 190718A: Swift detection of a burst
DATE:    19/07/18 04:51:09 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (SSDC), E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA),
N. J. Klingler (PSU), D. M. Palmer (LANL) and A. Tohuvavohu (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 04:41:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190718A (trigger=915091).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 336.531, -41.221 which is 
   RA(J2000) = 22h 26m 07s
   Dec(J2000) = -41d 13' 13"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 20 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 04:42:21.5 UT, 66.4 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 336.57614, -41.20264 which is
equivalent to:
   RA(J2000)  = 22h 26m 18.27s
   Dec(J2000) = -41d 12' 09.5"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 138 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.24 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4.3
(+2.81/-2.43) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 69 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.01. 

Burst Advocate for this burst is V. D'Elia (delia AT ssdc.asi.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190718A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25084
SUBJECT: GRB 190718A: Enhanced Swift-XRT position
DATE:    19/07/18 11:41:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1160 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 190718A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 336.57610, -41.20446 which is equivalent
to:

RA (J2000): 22h 26m 18.26s
Dec (J2000): -41d 12' 16.1"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB190718A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25085
SUBJECT: GRB 190718A: FRAM-Auger optical limit
DATE:    19/07/18 12:52:21 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ),
Martin Masek, Petr Janecek, Sergey Karpov, Jakub Jurysek,
Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza
(Institute of Physics, Prague, CZ)

report:

The 30cm robotic telescope FRAM-Auger in Malargue
(Argentina) reacted robotically to the Swift/BAT alert
of GRB190718A (D'Elia et al., GCNC 25082), starting
with a series of 20s unfiltered images at 04:45:11 UT,
i.e. 236s post trigger.

We do not detect any new source at or around the
reported X-ray errorbox reported by Evans et al. (GCN
25084) at single frames or a combined 20 x 20s image
taken between 236s and 1123s after the initial trigger.
The combined exposure  has a limiting magnitude r'(AB)
= 18.0, as calibrated against the APASS Catalogue.


GRB_name: GRB190718A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25089
SUBJECT: GRB 190718A: Swift/UVOT Upper Limits
DATE:    19/07/18 16:18:19 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (U.Warwick) and V. D'Elia (SSDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190718A
70 s after the BAT trigger (D'Elia et al., GCN Circ. 25082).
No optical afterglow consistent with the XRT position
(Evans et al., GCN Circ. 25084) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC            70          219          147         >20.9
u_FC               282          532          246         >20.0
white               70         1184          353         >21.0
v                  612         1061           78         >18.3
b                  538         1159           58         >19.1
u                  282         4874          307         >20.0
w1                 661         4847          235         >19.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190718A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25093
SUBJECT: GRB 190718A: Swift-XRT refined Analysis
DATE:    19/07/18 18:29:45 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B. Sbarufatti (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), P. D'Avanzo (INAF-OAB), M.G.
Bernardini (INAF-OAB), E. Ambrosi  (INAF-IASFPA) , D.N. Burrows (PSU),
J. D. Gropp (PSU) and V. D'Elia report on behalf of the Swift-XRT team:

We have analysed 6.4 ks of XRT data for GRB 190718A (D'Elia et al. GCN
Circ. 25082), from 70 s to 41.2 ks after the  BAT trigger. The data
comprise 349 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN Circ. 25084).

The late-time light curve (from T0+4.6 ks) can be modelled with a
power-law decay with a decay index of alpha=1.03 (+0.18, -0.17).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.64 (+0.15, -0.14). The
best-fitting absorption column is  7.0 (+4.2, -3.8) x 10^20 cm^-2, in
excess of the Galactic value of 1.2 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.0 x 10^-11 (4.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.0 (+4.2, -3.8) x 10^20 cm^-2
Galactic foreground: 1.2 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index:      1.64 (+0.15, -0.14)

If the light curve continues to decay with a power-law decay index of
1.03, the count rate at T+24 hours will be 0.011 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.5 x
10^-13 (5.0 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00915091.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190718A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25097
SUBJECT: GRB 190718A: Swift-BAT refined analysis
DATE:    19/07/19 01:24:16 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), V. D'Elia (SSDC),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 190718A (trigger #915091)
(D'Elia et al., GCN Circ. 25082).  The BAT ground-calculated position is
RA, Dec = 336.605, -41.184 deg which is
   RA(J2000)  =  22h 26m 25.2s
   Dec(J2000) = -41d 11' 02.7"
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a main multi-peaked structure
that starts at ~ T0 and ends at ~T+17 s. In addition, there is a weak
pulse at ~T+700 s, which is at the same time as the large flare seen
by the XRT. T90 (15-350 keV) is 720.0 +- 35.8 sec (estimated error
including systematics).

The time-averaged spectrum from T+0.1 to T+17.1 sec (i.e., the duration
of the main emission) is best fit by a simple power-law model.  The power
law
index of the time-averaged spectrum is 1.38 +- 0.26.  The fluence in the
15-150 keV band is 3.6 +- 0.6 x 10^-7 erg/cm2. The spectral analysis for
the total burst duration from ~T0 to ~T+720 s does not produce reasonable
fits due to the large quiescent period from ~T+17 s to ~T+700 s.
The 1-sec peak photon flux measured from T+0.08 sec in the 15-150 keV band
is 1.0 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/915091/BA/


GRB_name: GRB190719A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25098
SUBJECT: GRB 190719A: Fermi GBM Final Real-time Localization
DATE:    19/07/19 02:54:00 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 02:42:21 UT on 19 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190719A (trigger 585196946.536694 / 190719113).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 123.9, Dec = -30.8 (J2000 degrees, equivalent to J2000 08h 15m, -30d 48'), with a statistical uncertainty of 5.2 degrees.

The angle from the Fermi LAT boresight is 61.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190719113/quicklook/glg_skymap_all_bn190719113.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190719113/quicklook/glg_healpix_all_bn190719113.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190719113/quicklook/glg_lc_medres34_bn190719113.gif


GRB_name: GRB190719B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25101
SUBJECT: GRB 190719B: a long GRB detected by INTEGRAL
DATE:    19/07/19 07:14:03 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro.mereghetti@inaf.it>

S.Mereghetti (INAF, IASF-Milano), D.Gotz (CEA, Saclay),  C.Ferrigno,
E.Bozzo, V.Savchenko (ISDC, Versoix), L.Ducci (IAAT, Germany and ISDC,
Versoix), and J.Borkowski (CAMK, Torun) report:

a gamma ray burst lasting about 40 s has been detected by the off-line IBAS
analysis in the  IBIS/ISGRI data at 03:14  UT of 2019 July 19.
No alerts have been  distributed because the real-time IBAS program were
 not running at the time of the burst.

The burst refined coordinates (J2000) are:

R.A.= 344.518 deg
DEC.=  59.858 deg

with an uncertainty of  2.5   arcmin (90% c.l.).

The burst had a peak flux of  0.1    counts/cm2/s (20-200 keV, 1-s
integration
time) and a fluence in the same energy range of about 4e-7  erg/cmq.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB190719C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25104
SUBJECT: GRB 190719C: Fermi GBM Final Real-time Localization
DATE:    19/07/19 15:09:44 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 14:58:34 UT on 19 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190719C (trigger 585241119.558452 / 190719624).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 244.5, Dec = 4.9 (J2000 degrees, equivalent to J2000 16h 18m, 4d 54'), with a statistical uncertainty of 4.6 degrees.

The angle from the Fermi LAT boresight is 92.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190719624/quicklook/glg_skymap_all_bn190719624.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190719624/quicklook/glg_healpix_all_bn190719624.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190719624/quicklook/glg_lc_medres34_bn190719624.gif


GRB_name: GRB190719C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25106
SUBJECT: GRB 190719C: Swift detection of a burst
DATE:    19/07/19 15:22:37 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC),
J.D. Gropp (PSU), N. J. Klingler (PSU), H. A. Krimm (NSF),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), B. Sbarufatti (PSU) and A. Tohuvavohu (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 14:58:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190719C (trigger=915381).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 240.210, +12.977 which is 
   RA(J2000) = 16h 00m 50s
   Dec(J2000) = +12d 58' 39"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a total duration of about 100 sec.  The peak count rate
was ~6000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 14:59:35.3 UT, 60.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 240.20700,
12.99995 which is equivalent to:
   RA(J2000)  = 16h 00m 49.68s
   Dec(J2000) = +12d 59' 59.8"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 83 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (4.69 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.9
(+3.40/-2.88) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 0.1 s image was 1.69e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 71 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.04. 

The Fermi GBM team announced the detection of GRB 190719C (GCN Circ
25104).  Given the temporal coincidence, it is likely that this is the
same burst. 

Burst Advocate for this burst is E. Ambrosi (elena.ambrosi AT inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190719C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25110
SUBJECT: GRB 190719C: NOT candidate optical afterglow and host
DATE:    19/07/19 23:23:34 GMT
FROM:    Kasper Elm Heintz at Univ. of Iceland and DAWN/NBI  <keh14@hi.is>

Daniele B. Malesani (DTU Space), Kasper E. Heintz (Univ. Iceland), Daniel A. Perley (LJMU), Bo Milvang-Jensen (DAWN/NBI), Shane Moran (NOT and Univ. Turku) report on behalf of a larger collaboration:

We observed the field of the Fermi and Swift GRB 190719C (Fermi GBM Team, GCN 25104; Ambrosi et al., GCN 25106) using the Nordic Optical Telescope equipped with the ALFOSC camera. A set of 3 exposures by 300 s each was secured in the r band.

At the edge of the currently available XRT error circle (3.6" error radius), a single object is detected at approximate coordinates (J2000):

RA = 16:00:49.59
Dec = +13:00:04.3

This object is clearly extended, and we measure r = 22.01 +- 0.05 AB using a wide aperture, calibrated against nearby Pan-STARRS objects.

We notice that the object is also detected in the Pan-STARRS r-band image, for which we measure a slightly fainter magnitude r = 22.50 +- 0.16 AB. Visual comparison of the NOT and Pan-STARRS images indicated a shift in the centroid between the two epochs, with excess light in the NOT images to the West of the archival object.

We thus suggest that we are seeing a faint afterglow superimposed on its host galaxy. Further imaging at later epochs is required to carry out image subtraction and provide accurate position and magnitude for the afterglow.

New observations with the NOT will be requested as soon as the telescope is available.


GRB_name: GRB190720A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25123
SUBJECT: GRB 190720A: Fermi GBM Final Real-time Localization
DATE:    19/07/20 14:54:07 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 14:42:09 UT on 20 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190720A (trigger 585326534.78377 / 190720613).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 202.7, Dec = 41.8 (J2000 degrees, equivalent to J2000 13h 30m, 41d 47'), with a statistical uncertainty of 1.2 degrees.

The angle from the Fermi LAT boresight is 59.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190720613/quicklook/glg_skymap_all_bn190720613.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190720613/quicklook/glg_healpix_all_bn190720613.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190720613/quicklook/glg_lc_medres34_bn190720613.gif


GRB_name: GRB190720A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25124
SUBJECT: GRB 190720A: BALROG localization (Fermi Trigger 585326534 / GRB 190720613)
DATE:    19/07/20 15:17:17 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
585326534 at 14:42:09 on 20 July 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 203.4+/-0.6 deg
Decl.(2000.0) = 42.7+/-0.5 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190720613/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190720613/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190720613/json

                        


GRB_name: GRB190719C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25125
SUBJECT: GRB 190719C: Swift-XRT refined Analysis
DATE:    19/07/20 15:22:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne
(U. Leicester), M.G. Bernardini (INAF-OAB), M. Capalbi (INAF-IASFPA),
D.N. Burrows (PSU), J. D. Gropp (PSU), A. Tohuvavohu (PSU) and E.
Ambrosi report on behalf of the Swift-XRT team:

We have analysed 2.4 ks of XRT data for GRB 190719C (Ambrosi et al. GCN
Circ. 25106), from 64 s to 52.0 ks after the  BAT trigger. The data
comprise 353 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The refined XRT position is RA, Dec =
240.2069, +13.0000 which is equivalent to:

RA (J2000): 16 00 49.65
Dec(J2000): +13 00 00.0

with an uncertainty of 3.6 arcsec (radius, 90% confidence). a rise,
withpower-law index .

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.42 (+0.04, -0.03). The
best-fitting absorption column is  2.26 (+0.19, -0.18) x 10^21 cm^-2,
in excess of the Galactic value of 4.7 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.54 (+0.29, -0.25)
and a best-fitting absorption column of 9.0 (+9.8, -4.3) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.5 x 10^-11 (5.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.0 (+9.8, -4.3) x 10^20 cm^-2
Galactic foreground: 4.7 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.54 (+0.29, -0.25)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00915381.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190719C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25126
SUBJECT: GRB 190719C: Swift-XRT light-curve fit
DATE:    19/07/20 15:41:49 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

GCN Circ. 25125 was missing the details of the fit to the XRT light-curve.
The correct information is as follows:

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.11 (+/-0.05), followed by a break at T+387 s to an
alpha of 3.7 (+1.0, -0.4). A second break occurs at T+967 s to an alpha of
0.33 (+0.06, -0.09).

If the light curve continues to decay with a power-law decay index of
0.33, the count rate at T+24 hours will be 0.14 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.3 x
10^-12 (7.0 x 10^-12) erg cm^-2 s^-1.

We apologise for the omission of these numbers in the earlier circular.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190719C
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25128
SUBJECT: GRB 190719C: Swift/UVOT Upper Limits
DATE:    19/07/20 16:32:27 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and E. Ambrosi (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190719C
71 s after the BAT trigger (Ambrosi et al., GCN Circ. 25106).
No optical afterglow consistent with the XRT position is detected in the
initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC            71          221          147         >20.6
u_FC               283          533          246         >20.6
white               71          756          186         >20.8
v                  613          807           39         >18.7
b                  538          732           39         >19.9
u                  283          706          265         >20.5
w1                 662          856           39         >19.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).

The upper limits are consistent with the faint candidate
afterglow reported by Malesani et al. (GCN Circ. 25110).


GRB_name: GRB190719C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25129
SUBJECT: GRB 190719C: Swift-BAT refined analysis
DATE:    19/07/20 17:47:52 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. Sakamoto (AGU), E. Ambrosi (INAF-IASFPA),
S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+962 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 190719C (trigger #915381)
(Ambrosi et al., GCN Circ. 25106).  The BAT ground-calculated position is
RA, Dec = 240.208, 13.005 deg which is
   RA(J2000)  =  16h 00m 49.8s
   Dec(J2000) = +13d 00' 18.4"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a multi-peaked structure that starts
at ~T0 and ends at ~T+200 s. The main peak occurs at ~T0. T90 (15-350 keV)
is 185.7 +- 9.7 sec (estimated error including systematics).

The time-averaged spectrum from T-0.09 to T+201.96 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.64 +- 0.09.  The fluence in the 15-150 keV band is 5.1 +- 0.3 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+0.27 sec in the 15-150 keV band
is 5.5 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/915381/BA/


GRB_name: GRB190719C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25130
SUBJECT: GRB 190719C: Fermi GBM detection
DATE:    19/07/20 20:29:46 GMT
FROM:    Suraj Poolakkil at UAH  <sp0076@uah.edu>

S. Poolakkil (UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

At 14:58:34.56 UT on 19 July 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190719C (trigger 585241119/ 190719624),
which was also detected by the Swift/BAT (Ambrosi et al. 2019, GCN 25106).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight
at the GBM trigger time is 86 degrees.

The GBM lightcurve shows an initial bright short spike followed
by longer duration emission containing multiple peaks.
with a duration (T90) of about 175 s (50-300 keV).
The time-averaged spectrum from T0-2.0 s to T0+3.0 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.87 +/- 0.18 and
the cutoff energy, parameterized as Epeak, is 81 +/- 9 keV.

The event fluence (10-1000 keV) in this time interval is
(1.155 +/- 0.082)E-06 erg/cm^2. The 1-sec peak photon flux
measured starting from T+0.19 s in the 10-1000 keV band
is 8.3 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB190720A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25131
SUBJECT: GRB 190720A: Fermi GBM detection
DATE:    19/07/20 23:13:48 GMT
FROM:    C. Michelle Hui at MSFC/Fermi-GBM  <cmhui.astro@gmail.com>

C. M. Hui (NASA-MSFC) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

At 14:42:09.78 UT on 20 July 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190720A (trigger 585326534/190720613).

The on-ground calculated location, using the GBM trigger
data, is RA = 202.72 , DEC = +41.78  (J2000 degrees,
equivalent to 13h 30m, +41d 42.0'), with an uncertainty
of 1.16 degrees (radius, 1-sigma containment, statistical only;
there is additionally a systematic error which we have characterized
as a core-plus-tail model, with 90% of GRBs having a 3.7 deg error
and a small tail suffering a larger than 10 deg systematic error
[Connaughton et al. 2015, ApJS, 216, 32] ).
The angle from the Fermi LAT boresight is 59.00  degrees.

The GBM light curve shows/consists of single peak
with a duration (T90) of about 6.1s (50-300 keV).
The time-averaged spectrum from T0-0.0s to T0+8.8s is
adequately fit by a Band function with Epeak = 182 +/- 6 keV,
alpha = -0.89 +/- 0.02, and beta = -2.21 +/- 0.04.

The event fluence (10-1000 keV) in this time interval is
(2.74 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.5s in the 10-1000 keV band is 48.2 +/- 0.5 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html
<https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html>
For Fermi GBM data and info,
please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/


GRB_name: GRB190720B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25132
SUBJECT: GRB 190720B: Fermi GBM Final Real-time Localization
DATE:    19/07/20 23:20:09 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 23:08:38 UT on 20 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190720B (trigger 585356923.763906 / 190720964).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 138.9, Dec = -55.6 (J2000 degrees, equivalent to J2000 09h 15m, -55d 36'), with a statistical uncertainty of 2.4 degrees.

The angle from the Fermi LAT boresight is 54.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190720964/quicklook/glg_skymap_all_bn190720964.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190720964/quicklook/glg_healpix_all_bn190720964.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190720964/quicklook/glg_lc_medres34_bn190720964.gif


GRB_name: GRB190720B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25137
SUBJECT: GRB 190720B: Insight-HXMT/HE detection
DATE:    19/07/21 14:32:36 GMT
FROM:    Qi Luo at IHEP  <luoqi@ihep.ac.cn>

Q. Luo, C. Cai, S. Xiao, Q. B. Yi, Y. G. Zheng, Y. Huang, 
C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-07-20T23:08:39.50 (T0), Insight-HXMT/HE detected 
GRB 190720B (trigger ID: HEB190720964) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #25132). 

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 8.59 s measured from T0-1.01 s. 
The 1-ms peak rate, measured from T0-0.14 s, is 873 cnts/sec. 
The total counts from this burst is 3465 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190720964_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190720A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25139
SUBJECT: IPN triangulation of GRB 190720A
DATE:    19/07/22 22:53:38 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:

The long-duration GRB 190720A
(Fermi-GBM detection: Fermi GBM Team, GCN Circ. 25123,
Hui and Meegan, GCN Circ. 25131;
BALROG localization: Kunzweiler et al., GCN Circ. 25124)
was detected by Fermi (GBM trigger 585326534), Konus-Wind,
INTEGRAL (SPI-ACS), and Mars-Odyssey (HEND)
at about 52930 s UT (14:42:10).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   205.406 (13h 41m 37s) +41.340 (+41d 20' 25")
  Corners:
   205.272 (13h 41m 05s) +50.612 (+50d 36' 42")
   205.533 (13h 42m 08s) +49.639 (+49d 38' 19")
   204.561 (13h 38m 15s) +31.484 (+31d 29' 04")
   204.550 (13h 38m 12s) +32.598 (+32d 35' 54")
  ---------------------------------------------
The error box area is about 2.4 sq. deg, and its maximum
dimension is 19.1 deg (the minimum one is 7.8 arcmin).
The Sun distance was about 71 deg.

This box may be improved.

This burst is spatially and temporally inconsistent with
LIGO/Virgo S190720a (LVC GCN Circ. 25115).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190720_T52927/IPN

The Konus-Wind time history and spectrum will be given in a forthcoming
GCN Circular.


GRB_name: GRB190723A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25140
SUBJECT: GRB 190723A: Fermi GBM Final Real-time Localization
DATE:    19/07/23 07:36:11 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 07:24:17 UT on 23 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190723A (trigger 585559462.869138 / 190723309).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 289.5, Dec = 25.2 (J2000 degrees, equivalent to J2000 19h 18m, 25d 11'), with a statistical uncertainty of 10.5 degrees.

The angle from the Fermi LAT boresight is 70.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190723309/quicklook/glg_skymap_all_bn190723309.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190723309/quicklook/glg_healpix_all_bn190723309.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190723309/quicklook/glg_lc_medres34_bn190723309.gif


GRB_name: GRB190724A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25142
SUBJECT: GRB 190724A: Fermi GBM Final Real-time Localization
DATE:    19/07/24 00:55:40 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 00:43:56 UT on 24 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190724A (trigger 585621841.792286 / 190724031).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 170.4, Dec = 15.2 (J2000 degrees, equivalent to J2000 11h 21m, 15d 11'), with a statistical uncertainty of 13.6 degrees.

The angle from the Fermi LAT boresight is 36.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190724031/quicklook/glg_skymap_all_bn190724031.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190724031/quicklook/glg_healpix_all_bn190724031.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190724031/quicklook/glg_lc_medres34_bn190724031.gif


GRB_name: GRB190719C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25144
SUBJECT: GRB 190719C: optical afterglow confirmation
DATE:    19/07/24 08:31:42 GMT
FROM:    Kasper Elm Heintz at Univ. of Iceland and DAWN/NBI  <keh14@hi.is>

Kasper E. Heintz (Univ. Iceland), Daniele B. Malesani (DTU Space), Daniel A. Perley (LJMU), Shane Moran (NOT and Univ. Turku), report on behalf of a larger collaboration:

We observed again the field of GRB 190719C (Ambrosi et al., GCN 25106; Poolakkil & Meegan, GCN 25130) using the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. A coadded exposure of 3000 s was collected in the SDSS r filter, starting on July 21.125 UT (1.501 days after the GRB).

The source first noticed in our previous observation (Malesani et al., GCN 25110) visually faded and is no longer clearly detected. This was quantitatively confirmed by carrying out image subtraction between the two epochs. A clear residual is visible at coordinates (J2000):

RA = 16:00:49.58
Dec = 13:00:04.5

This is approximately 0.7" west of the object visible in the archival Pan-STARRS images.

Photometry of the transient computed on the subtraction image (calibrated against nearby stars from the Pan-STARRS catalog) yields r = 23.03 +- 0.12 AB at epoch July 19.88 UT (Malesani et al., GCN 25110). We caution that the actual brightness would be higher if significant residual light were present in our second epoch of observation (this would be ~20% for a t^-1 decay).

The consistency with the X-ray afterglow position (Beardmore et al., GCN 25125) and the optical fading confirm that the source above is the afterglow of GRB 190719C. The close angular proximity with the object seen in the Pan-STARRS images suggests it to be the GRB host galaxy.


GRB_name: GRB190724A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25146
SUBJECT: IPN triangulation of GRB 190724A (short)
DATE:    19/07/24 19:53:13 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova and K. Hurley, on behalf of the IPN,

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

and

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
report:

The short-duration GRB 190724A has been detected
by Fermi (GBM trigger 585621841) and INTEGRAL (SPI-ACS), so far,
at about 2637 s UT (00:43:57).

We have triangulated this GRB to a GBM-INTEGRAL annulus centered at
RA(2000)=206.373 deg (13h 45m 29s)  Dec(2000)=+50.590 deg (+50d 35' 22"),
whose radius is 51.149 +/- 3.567 deg (3 sigma).

This annulus is consistent with, but reduces the area of, the Fermi GBM
localization (The Fermi GBM team, GCN Circ. 25142)

This annulus may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190724_T02636/IPN/


GRB_name: GRB190720A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25148
SUBJECT: GRB 190720A: CALET Gamma-Ray Burst Monitor detection
DATE:    19/07/25 05:57:30 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

Y. Kawakubo (LSU),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long bright GRB 190720A (Fermi GBM detection: Hui and Meegan,
GCN Circ. 25131; BALROG localization: Kunzweiler et al., GCN Circ. 25124;
IPN triangulation: Hurley et al., GCN Circ. 25139) triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 14:42:10.000 UTC on 20 July 2019.
The burst signal was seen by all CGBM detectors.
No real-time CGBM GCN notice was distributed about this trigger because
the real-time communication from the ISS was off (loss of signal).

The burst light curve shows a single multi-peaked pulse which starts
at T-0.2 sec, peaks at 2.4 sec and ends at T+14.0 sec. The T90 and T50
durations measured by the SGM data are 5.9 +- 1.0 sec and 2.1 +- 0.2 sec
(40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1247668851/

The CALET data used in this analysis are provided by the Waseda CALET
Operation Center located at the Waseda University.


GRB_name: GRB190723A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25149
SUBJECT: GRB 190723A: Insight-HXMT/HE detection
DATE:    19/07/25 07:13:38 GMT
FROM:    Ce Cai at IHEP  <caice@ihep.ac.cn>

C. Cai, Q. Luo, S. Xiao, Q. B. Yi, Y. G. Zheng, Y. Huang, 
C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-07-23T07:24:17.87 (T0), Insight-HXMT/HE detected 
GRB 190723A (trigger ID: HEB190723308) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #25140). 

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 3.23 s measured from T0-1.55 s. 
The 1-ms peak rate, measured from T0-1.66 s, is 818 cnts/sec. 
The total counts from this burst is 1433 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190723308_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190724A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25150
SUBJECT: GRB 190724A: Insight-HXMT/HE detection
DATE:    19/07/25 09:46:18 GMT
FROM:    Ce Cai at IHEP  <caice@ihep.ac.cn>

C. Cai, Q. Luo, S. Xiao, Q. B. Yi, Y. G. Zheng, Y. Huang, 
C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-07-24T00:43:56.750 (T0), Insight-HXMT/HE detected 
GRB 190724A (trigger ID: HEB190724030) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #25142). 

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 0.06 s measured from T0+0.01 s. 
The 1-ms peak rate, measured from T0+0.02 s, is 10765 cnts/sec. 
The total counts from this burst is 634 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190724030_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB190726A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25154
SUBJECT: GRB 190726A: Fermi GBM Final Real-time Localization
DATE:    19/07/26 15:36:44 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 15:24:53 UT on 26 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190726A (trigger 585847498.610468 / 190726642).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 310.3, Dec = 34.3 (J2000 degrees, equivalent to J2000 20h 41m, 34d 17'), with a statistical uncertainty of 1.2 degrees.

The angle from the Fermi LAT boresight is 72.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190726642/quicklook/glg_skymap_all_bn190726642.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190726642/quicklook/glg_healpix_all_bn190726642.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190726642/quicklook/glg_lc_medres34_bn190726642.gif


GRB_name: GRB190726A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25155
SUBJECT: GRB 190726A: BALROG localization (Fermi Trigger 585847498 / GRB 190726642)
DATE:    19/07/26 15:59:52 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
585847498 at 15:24:53 on 26 July 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 310.8+/-0.9 deg
Decl.(2000.0) = 34.9+/-1.2 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190726642/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190726642/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190726642/json

                        


GRB_name: GRB190726B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25157
SUBJECT: GRB 190726B: Fermi GBM Final Real-time Localization
DATE:    19/07/26 20:25:31 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 20:14:30 UT on 26 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190726B (trigger 585864875.561318 / 190726843).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 342.7, Dec = -56.0 (J2000 degrees, equivalent to J2000 22h 50m, -56d 00'), with a statistical uncertainty of 2.4 degrees.

The angle from the Fermi LAT boresight is 67.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190726843/quicklook/glg_skymap_all_bn190726843.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190726843/quicklook/glg_healpix_all_bn190726843.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190726843/quicklook/glg_lc_medres34_bn190726843.gif


GRB_name: GRB190726B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25158
SUBJECT: GRB 190726B: BALROG localization (Fermi Trigger 585864875 / GRB 190726843)
DATE:    19/07/26 20:35:57 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

F. Kunzweiler, B. Biltzinger,  F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
585864875 at 20:14:30 on 26 July 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 328.2+/-5.5 deg
Decl.(2000.0) = -48.3+/-1.9 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190726843/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190726843/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190726843/json


GRB_name: GRB190726B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25159
SUBJECT: GRB 190726B: BALROG localization (Fermi Trigger 585864875 / GRB 190726843)
DATE:    19/07/26 20:35:57 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

F. Kunzweiler, B. Biltzinger,  F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
585864875 at 20:14:30 on 26 July 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 328.2+/-5.5 deg
Decl.(2000.0) = -48.3+/-1.9 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190726843/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190726843/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190726843/json

                        


GRB_name: GRB190727A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25173
SUBJECT: GRB 190727A: Fermi GBM Final Real-time Localization
DATE:    19/07/27 16:13:30 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 16:01:52 UT on 27 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190727A (trigger 585936117.276574 / 190727668).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 224.5, Dec = 19.4 (J2000 degrees, equivalent to J2000 14h 58m, 19d 23'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 20.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190727668/quicklook/glg_skymap_all_bn190727668.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190727668/quicklook/glg_healpix_all_bn190727668.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190727668/quicklook/glg_lc_medres34_bn190727668.gif


GRB_name: GRB190727A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25175
SUBJECT: GRB 190727A: BALROG localization (Fermi Trigger 585936117 / GRB 190727668)
DATE:    19/07/27 16:23:03 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
585936117 at 16:01:52 on 27 July 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 232.3+/-2.0 deg
Decl.(2000.0) = 20.9+/-2.1 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190727668/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190727668/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190727668/json

                        


GRB_name: GRB190727B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25176
SUBJECT: GRB 190727B: Swift detection of a burst
DATE:    19/07/27 20:28:15 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Y. Lien (GSFC/UMBC), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), J. A. Kennea (PSU), N. J. Klingler (PSU),
A. Melandri (INAF-OAB), M. J. Moss (GWU), K. L. Page (U Leicester),
D. M. Palmer (LANL) and A. Tohuvavohu (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 20:18:17 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190727B (trigger=916733).  Swift could not slew to the location
due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 126.481, -13.268 which is 
   RA(J2000) = 08h 25m 55s
   Dec(J2000) = -13d 16' 03"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 50 sec.  The peak count rate
was ~20,000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 16:42 UT on 2019 September 12. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is A. Y. Lien (amy.y.lien AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB190727B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25177
SUBJECT: GRB 190727B: Fermi GBM Final Real-time Localization
DATE:    19/07/27 20:29:22 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 20:17:56 UT on 27 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190727B (trigger 585951481.447196 / 190727846).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 130.6, Dec = -15.7 (J2000 degrees, equivalent to J2000 08h 42m, -15d 41'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 44.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190727846/quicklook/glg_skymap_all_bn190727846.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190727846/quicklook/glg_healpix_all_bn190727846.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190727846/quicklook/glg_lc_medres34_bn190727846.gif


GRB_name: GRB190727B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25178
SUBJECT: GRB 190727B: BALROG localization (Fermi Trigger 585951481 / GRB 190727846)
DATE:    19/07/27 22:03:51 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
585951481 at 20:17:56 on 27 July 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 128.2+/-0.3 deg
Decl.(2000.0) = -12.2+/-0.5 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190727846/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190727846/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190727846/json

                        


GRB_name: GRB190727B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25180
SUBJECT: GRB 190727B: Fermi GBM observations
DATE:    19/07/28 04:43:17 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

P. Veres and C. Meegan (both UAH) report on behalf of the Fermi GBM Team:

At 20:17:56.45 UT on 27 July 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190727B (trigger 585951481/190727846), which was
also detected by the Swift/BAT (Lien et al., GCN 25176). The GBM on-ground
location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 46 degrees.

The GBM light curve consists of multiple overlapping pulses with a duration
(T90) of about 35 s (50-300 keV). The time-averaged spectrum from T0 to
T0+44 s is adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.26 +/- 0.01 and the cutoff
energy, parameterized as Epeak, is 621 +/- 26 keV.

The event fluence (10-1000 keV) in this time interval is (7.02 +/-
0.05)E-05 erg/cm^2. The 1-second peak photon flux measured starting from
T0+21.8 s in the 10-1000 keV band is 43.0 +/- 0.4 ph/s/cm^2.

The spectral analysis results presented above are preliminary; final
results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM
data and information, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/


GRB_name: GRB190728A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25181
SUBJECT: GRB 190728A: Fermi GBM Final Real-time Localization
DATE:    19/07/28 06:41:31 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 06:30:36 UT on 28 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190728A (trigger 585988241.852436 / 190728271).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 356.7, Dec = 5.4 (J2000 degrees, equivalent to J2000 23h 46m, 5d 24'), with a statistical uncertainty of 5.7 degrees.

The angle from the Fermi LAT boresight is 85.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190728271/quicklook/glg_skymap_all_bn190728271.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190728271/quicklook/glg_healpix_all_bn190728271.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190728271/quicklook/glg_lc_medres34_bn190728271.gif


GRB_name: GRB190727B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25186
SUBJECT: GRB 190727B: Fermi-LAT detection
DATE:    19/07/28 08:23:56 GMT
FROM:    Makoto Arimoto at Tokyo Inst of Tech  <arimoto@hp.phys.titech.ac.jp>

M. Kovacevic (INFN Perugia), D. Tak (Univ. of Maryland & NASA/GSFC),
F. Longo (University and INFN, Trieste),
M. Arimoto (Kanazawa Univ.), and M. Axelsson (KTH and Stockholm Univ.)
report on behalf of the Fermi-LAT team:

On July 27, 2019, Fermi-LAT detected high-energy emission from
GRB 190727B, which was also detected by Fermi-GBM (Veres et al., GCN
25180) and Swift-BAT (Lien et al., GCN 25176).

The best LAT on-ground location is found to be

RA, Dec 126.19, -13.34 (degrees, J2000)

with an error radius of 0.28 deg (90% containment, statistical error only).
This was 46 deg from the LAT boresight at the time of the GBM trigger:

T0 =  20:17:56.45 UT.

The data from the Fermi-LAT show a significant increase
in the event rate after the GBM trigger that is spatially correlated with the
GBM emission with high significance.
The photon flux above 100 MeV in the time interval 0-1500 s after the
GBM trigger is (3.15 +/- 1.25)E-6 ph/cm2/s.
The highest-energy photon in this interval is a 2.2 GeV event observed
at T0 + 345 s.
The estimated photon index above 100 MeV is -2.3 +/- 0.4.

The Fermi-LAT point of contact for this burst is Milos Kovacevic
(milos.kovacevic@pg.infn.it).

The Fermi-LAT is a pair conversion telescope designed to cover
the energy band from 20 MeV to greater than 300 GeV.
It is the product of an international collaboration between
NASA and DOE in the U.S. and many scientific institutions
across France, Italy, Japan and Sweden.


GRB_name: GRB190728A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25205
SUBJECT: IPN triangulation of GRB 190728A (short)
DATE:    19/07/28 19:27:50 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin and K. Hurley, on behalf of the IPN,

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

and

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
report:

The short-duration GRB 190728A (The Fermi GBM team, GCN Circ. 25181)
has been detected by Fermi (GBM trigger 585988241) and
INTEGRAL (SPI-ACS), so far, at about 23437 s UT (06:30:37).

We have triangulated this GRB to a GBM-INTEGRAL annulus centered at
RA(2000)=82.621 deg (05h 30m 29s) Dec(2000)=-46.530 deg (-46d 31' 49"), 
whose radius is 86.613 +/- 1.356 deg (3 sigma).

The IPN localization is consistent with, but reduces the area of, the 
Fermi GBM one.

This localization may be improved.

This burst is spatially and temporally (occurred ~14 min before) 
inconsistent with LIGO/Virgo S190728q.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190728_T23436/IPN/


GRB_name: GRB190727B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25211
SUBJECT: GRB 190727B: Swift-BAT refined analysis
DATE:    19/07/28 23:21:40 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 190727B (trigger #916733)
(Lien et al., GCN Circ. 25176).  The BAT ground-calculated position is
RA, Dec = 126.500, -13.272 deg which is
   RA(J2000)  =  08h 25m 59.9s
   Dec(J2000) = -13d 16' 18.9"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 70%.

The mask-weighted light curve shows a structure with multiple bright pulses
that starts at ~T-20 s and ends at ~T+45 s. The brightest peak occurs at
~T+2 s. T90 (15-350 keV) is 40.14 +- 1.40 sec (estimated error including
systematics).

The time-averaged spectrum from T-21.30 to T+44.47 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.41 +- 0.03.  The fluence in the 15-150 keV band is 1.8 +- 0.03 x 10^-5
erg/cm2.
The 1-sec peak photon flux measured from T+1.13 sec in the 15-150 keV band
is 20.9 +- 0.7 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/916733/BA/


GRB_name: GRB190727B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25218
SUBJECT: Konus-Wind observation of GRB 190727B
DATE:    19/07/29 16:14:05 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 190727B
(Swift-BAT detection: Lien et al., GCN Circ. 25176;
Fermi-GBM observations: Veres and Meegan, GCN Circ. 25180;
Fermi-LAT detection: Kovacevic et al., GCN Circ. 25186)
triggered Konus-Wind at T0=73072.783 s UT (20:17:52.783).

The burst light curve shows a multi-peaked structure
which starts at ~T0-3.8 s and has a total duration of ~62 s.
The emission is seen up to ~6 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190727_T73072/

As observed by Konus-Wind, the burst
had a fluence of 9.92(-1.04,+1.04)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+21.040 s,
of 1.82(-0.34,+0.33)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+44.800 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.11(-0.07,+0.07),
the high energy photon index beta = -2.27(-0.29,+0.16),
the peak energy Ep = 402(-49,+64) keV
(chi2 = 106/97 dof).

The spectrum near the maximum count rate
(measured from T0+16.640 to T0+21.504 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.07(-0.08,+0.09),
the high energy photon index beta = -2.38(-0.85,+0.24),
the peak energy Ep = 566(-98,+136) keV
(chi2 = 94/97 dof).

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190731A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25240
SUBJECT: GRB 190731A: Fermi GBM Final Real-time Localization
DATE:    19/07/31 22:49:31 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 22:38:20 UT on 31 Jul 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190731A (trigger 586305505.368608 / 190731943).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 342.8, Dec = -73.9 (J2000 degrees, equivalent to J2000 22h 51m, -73d 54'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 43.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190731943/quicklook/glg_skymap_all_bn190731943.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190731943/quicklook/glg_healpix_all_bn190731943.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190731943/quicklook/glg_lc_medres34_bn190731943.gif


GRB_name: GRB190731A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25244
SUBJECT: GRB190731A: Fermi-LAT detection
DATE:    19/08/01 06:50:53 GMT
FROM:    Masanori Ohno at Hiroshima University  <ohno@astro.hiroshima-u.ac.jp>

M. Ohno (Hiroshima Univ.), F. Longo (University and INFN, Trieste),
M. Arimoto (Kanazawa Univ.), M.  Axelsson (KTH and Stockholm Univ.), and F.
Dirirsa (Univ. of Johannesburg)
report on behalf of the Fermi-LAT team:

On July, 31, 2019 Fermi-LAT detected high-energy emission from GRB 190731A,
which was also detected by Fermi-GBM (Fermi GBM Team, GCN 25240).

The best LAT on-ground location is found to be

RA, Dec = 339.94, -76.62 (J2000)

with an error radius of 0.28 deg (90 % containment, statistical error only).
This was 40 deg from the LAT boresight at the time of the GBM trigger:

T0 =  22:38:20 UT.

 The data from the Fermi-LAT show a significant increase
in the event rate after the GBM trigger that is spatially correlated with
the
GBM emission with high significance.
The photon flux above 100 MeV in the time interval 0-800 s after the
GBM trigger is (1.91 +/- 0.65)E-5 ph/cm2/s.
The highest-energy photon in this interval is a 3.8 GeV event observed
at T0 + 234 s.
The estimated photon index above 100 MeV is -2.17 +/- 0.26.

The Fermi-LAT point of contact for this burst is Masanori Ohno
(ohno@astro.hiroshima-u.ac.jp).

 A Swift ToO has been approved for this burst.


The Fermi-LAT is a pair conversion telescope designed to cover
the energy band from 20 MeV to greater than 300 GeV.
It is the product of an international collaboration between
NASA and DOE in the U.S. and many scientific institutions
across France, Italy, Japan and Sweden.


GRB_name: GRB190731A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25245
SUBJECT: GRB 190731A: Swift ToO observations
DATE:    19/08/01 07:08:16 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a ToO observation of the Fermi/LAT GRB 190731A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00020914

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the Fermi/LAT event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190731A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25246
SUBJECT: GRB 190731A: CALET Gamma-Ray Burst Monitor detection
DATE:    19/08/01 10:06:20 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

Y. Asaoka (Waseda U),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long bright GRB 190731A (Fermi GBM Final Real-time Localization: Fermi
GBM Team, GCN Circ. 25240; Fermi-LAT detection: Ohno et al., GCN Circ.
25244) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 22:38:18.315
UTC on 31 July 2019. The burst signal was seen by all CGBM detectors.

The burst light curve shows a single multi-peaked emission episode which
starts at T+3.1 sec, peaks at T+4.4 sec and ends at T+26.0 sec. The T90
and T50 durations measured by the SGM data are 14.6 +- 1.8 sec and
5.0 +- 0.5 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1248647800/

The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.


GRB_name: GRB190726B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25247
SUBJECT: GRB 190726B: AstroSat CZTI detection
DATE:    19/08/01 11:12:22 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190726B, which was also detected by Fermi GBM (GCN #25157), BALROG localization (Kunzweiler F. et al., GCN #25158) and Global MASTER-Net (Lipunov V. et al., GCN #25161).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with strongest peak at 20:14:54.0 UT. The measured peak count rate associated with the burst is 253 cts/s above the background in the combined data of four quadrants, with a total of 11142 cts. The local mean background count rate was 508 cts/s. Using cumulative rates, we measure a T90 of 209.0 s. In preliminary analysis, we find that 478 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190731A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25248
SUBJECT: GRB 190731A: Fermi GBM detection
DATE:    19/08/01 13:55:41 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

 O.J. Roberts (USRA) and C. Meegan (UAH) report on behalf 
of the Fermi GBM Team:

"At 22:38:20.37 UT on 31 July 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190731A (trigger 586305505 / 190731943), which 
was also detected by the LAT (Ohno et al., GCN 25244). 
The GBM on-ground location is consistent with the LAT position.

The initial angle from the Fermi LAT boresight to
the best location is 40 degrees.

The GBM light curve consists of several bright peaks
with a duration (T90) of 15.9 +/- 0.4 s (50-300 keV).
The time-averaged spectrum from T0+1.6 s to T0+17.9 s is
best fit by a Band function with Epeak = 456 +/- 9,
alpha index = -0.74 +/- 0.01 and beta index = -2.40 +/- 0.05.

The event fluence (10-1000 keV) in this time interval is
(8.57 +/- 0.05)E-05 erg/cm^2. The 1s peak photon flux measured
starting from T0+1.9 s in the 10-1000 keV band
is 55.5 +/- 0.4 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html 

For Fermi GBM data and info, 
please visit the official Fermi GBM Support Page: 
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB190731A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25250
SUBJECT: IPN Triangulation of GRB 190731A
DATE:    19/08/01 20:42:05 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin,
and T. Cline on behalf of the Konus-Wind team,

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,

and

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:

The long-duration, bright GRB 190731A
(Fermi LAT detection: Ohno et al., GCN 25244;
CALET GBM detection: Asaoka et al., GCN 25246;
Fermi GBM detection: Roberts & Meegan, GCN 25248)
has been detected by FERMI (GBM trigger 586305505), INTEGRAL (SPI-ACS),
Mars-Odyssey (HEND), Konus-Wind, CALET (GBM), and Swift (BAT),
so far, at about 81500 s UT (22:38:20).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a GBM-HEND annulus centered at
RA(2000)=321.552 deg (21h 26m 13s)  Dec(2000)=-16.302 deg (-16d 18' 08"),
whose radius is 61.012 +/- 0.062 deg (3 sigma).

The LAT position reported by Ohno et al. (GCN Circ. 25244)
is consistent with the annulus. The annulus combined with
the LAT (90 % containment, statistical-only) error circle
gives the following error box:
--------------------------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ------------------------------------------------------------
  Center:
   339.864 (22h 39m 27s) -76.572 (-76d 34' 19")
  Corners:
   338.734 (22h 34m 56s) -76.599 (-76d 35' 57")
   338.813 (22h 35m 15s) -76.724 (-76d 43' 27")
   341.083 (22h 44m 20s) -76.530 (-76d 31' 50")
   340.796 (22h 43m 11s) -76.424 (-76d 25' 25")
  -------------------------------------------------------------
The error box area is 244 sq. arcmin (a factor of 4
smaller than that of the LAT error circle), and its maximum
dimension is 33.6 arcmin (the minimum one is 7.4 arcmin).
The Sun distance was ~121 deg.

Both Swift XRT sourses found so far (www.swift.ac.uk/ToO_GRBs/00020914/)
are consistent with the box.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190731_T81500/IPN/

The Konus-Wind time history and spectrum will be given in a forthcoming
GCN Circular.


GRB_name: GRB190731A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25251
SUBJECT: GRB 190731A: Swift-XRT afterglow detection
DATE:    19/08/01 21:24:27 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

J.P. Osborne (U. Leicester), E. Ambrosi  (INAF-IASFPA) , M. Capalbi
(INAF-IASFPA), M. Perri (ASDC), J. D. Gropp (PSU), A. Tohuvavohu (PSU),
J.A. Kennea (PSU), K.L. Page (U. Leicester) and P.A. Evans (U.
Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 190731A (Ohno et al. GCN Circ. 25244),
collecting 5.0 ks of Photon Counting (PC) mode data between T0+33.4 ks
and T0+62.9 ks. 

Eleven uncatalogued X-ray sources are detected, of which one ("Source
1") is fading with 3-sigma significance, and is therefore likely the
GRB afterglow. Using 1953 s of PC mode data and 4 UVOT images, we find
an enhanced XRT position (using the XRT-UVOT alignment and matching
UVOT field sources to the USNO-B1 catalogue): RA, Dec = 339.72015,
-76.57744 which is equivalent to:

RA (J2000): 22h 38m 52.84s
Dec(J2000): -76d 34' 38.8"

with an uncertainty of 2.2 arcsec (radius, 90% confidence). This
position is 4.0 arcmin from the Fermi/LAT position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.3 (+0.6, -0.7).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.5 (+/-0.5). The
best-fitting absorption column is  5.9 (+2.8, -2.2) x 10^21 cm^-2, in
excess of the Galactic value of 9.8 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.3 x 10^-11 (7.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.9 (+2.8, -2.2) x 10^21 cm^-2
Galactic foreground: 9.8 x 10^20 cm^-2
Excess significance: 3.6 sigma
Photon index:      2.5 (+/-0.5)

If the light curve continues to decay with a power-law decay index of
1.3, the count rate at T+24 hours will be 0.015 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.9 x
10^-13 (1.2 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis of the likely afterglow
are at https://www.swift.ac.uk/ToO_GRBs/00020914/Source1.php.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00020914.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190719C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25252
SUBJECT: GRB 190719C: VLT/X-shooter spectroscopic redshift of the host galaxy
DATE:    19/08/01 22:01:30 GMT
FROM:    Andrea Rossi at INAF  <andrea.rossi@inaf.it>

A. Rossi (INAF-OAS), K. E. Heintz (Univ. Iceland), J. P. U. Fynbo 
(DAWN/NBI), D. B. Malesani (DTU Space), A. de Ugarte Postigo 
(HETH/IAA-CSIC, DARK/NBI), S. D. Vergani (Obs. Paris/GEPI and CNRS), D. 
A. Kann, C. C. Thoene, L. Izzo (HETH/IAA-CSIC), S. Campana (INAF-OAB), 
G. Pugliese, L. Kaper (Univ. Amsterdam), C. Kouveliotou (GWU), and N. R. 
Tanvir (Univ. Leicester) report on behalf of the Stargate collaboration:

We observed the location of the candidate host galaxy (Malesani et al., 
GCN 25110; Heintz et al., GCN 25144) of GRB 190719C (Ambrosi et al., GCN 
25106; Poolakkil & Meegan, GCN 25130) using the ESO VLT UT2 (Kueyen) 
equipped with the X-shooter spectrograph. Our spectra cover the 
wavelength range 3000-21000 AA, and consist of 4 exposures by 600 s 
each. Our observations started on 2019 August 01 at 00:48:20 UT, ~13.4 
days after the GRB detection. The slit was centred on the nucleus of the 
nearby object visible in the Pan-STARRS archival images, and was 
oriented in order to include the afterglow position.

While only weak continuum is visible, several clear emission lines are 
detected in the near-infrared arm. We identify the [O ii] 3727/3729 
doublet, Hbeta, [O iii] 4959, and [O iii] 5007, at a common redshift z = 
2.469.

No clear emission (lines nor continuum) is detected at the location of 
the afterglow, so we have no direct measurement of the GRB redshift. The 
random association probability with the Pan-STARRS object is however 
rather small (~3*10^-3), suggesting a physical connection. We also note 
that the Pan-STARRS galaxy is exceptionally luminous, with an absolute 
magnitude M = -22.9 AB (computed at 1800 AA rest frame). The measured 
offset would correspond to 6.6 kpc in projection - a rather large value 
but not surprising for such a bright host. In conclusion, we propose z = 
2.469 as the redshift of GRB 190719C.

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Gaspare Lo Curto, Marcela Espinoza, Boris 
Haeussler, Aleksandra Solarz, and Steffen Mieske.


GRB_name: GRB190720B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25254
SUBJECT: GRB 190720B: AstroSat CZTI detection
DATE:    19/08/02 11:25:01 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190720B, which was also detected by Fermi GBM (GCN #25132) and Insight-HXMT/HE (Luo Q. et. al., GCN #25137).

The source was clearly detected in the 40-200 keV energy range. The light curve shows single pulse of emission with strongest peak at 23:08:40.0 UT. The measured peak count rate associated with the burst is 116 cts/s above the background in the combined data of four quadrants, with a total of 493 cts. The local mean background count rate was 507 cts/s. Using cumulative rates, we measure a T90 of 8.5 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190731A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25256
SUBJECT: GRB 190731A: no OT detected by MASTER 
DATE:    19/08/02 13:04:26 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy (MASTER,Lomonosov MSU), D.Svinkin (Konus-Wind,Ioffe institute)
V. Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, V. Vladimirov,D. Vlasenko, I.Gorbunov,D.Zimnukhov,
V. Senik, A.Chasovnikov,  A.Pozdnyakov, D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department),
R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias IAC),
R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA),
H. Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
D. Buckley (South African Astronomical Observatory SAAO),
O. Gress, N.M. Budnev, O.Ershova (Irkutsk State University, API),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko (Blagoveschensk Educational State University)

MASTER Global Robotic Net ( http://observ.pereplet.ru, Lipunov et al., 2010,Advances in Astronomy, vol. 2010, 30L)
observed GRB 190731A (Fermi team GCN 25240) in alert (Lipunov et al. GCN 25243) and inspect modes.

MASTER-VWF (very wide field) cameras (D=82 mm, F/1.2, FOV=2x384 sq. degree)  located in MASTER-SAAO robotic telescope
was pointed to the GRB 190731A by Fermi GBM (trigger 586305505) localization.
The first images obtain 21 seconds after notice and 45 second after trigger time at 2019-07-31 22:39:05.

Due to the MASTER-VWFC  field of view both  Fermi/LAT(Ohno et al., GCN 25244) and Swift/XRT (Evans et al. 25245,
Osborne et al., GCN 25251,and also detected by CALET Asaoka et al. GCN25246 and triangulated by IPN Hurley et al. GCN25250)
position are covered by these images.

We do not see any optical transients at Swift XRT position with upper limit 12.5m (MASTER-VWFC).

MASTER-SAAO robotic telescope was pointed to the GRB 190731A LAT localization (Fermi LAT team GCN 25244) 
errorbox  65745 sec after trigger time at 2019-08-01 16:54:08 UT, with upper limit up to  21.4 mag (MASTER-II).
Observations started at twilight.
The observations began at zenit distance = 65 deg, the sun  altitude  is -11.3 deg.
During this observations we also not find any optical transient connected with GRB.

Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1093251

We obtain a following upper limits.

Tmid-T0  |      Date Time      |          Site       |             Coord (J2000)          |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
    65835 | 2019-08-01 16:54:08 |         MASTER-SAAO | ( 22h 42m 57.83s , -76d 43m 34.01s) |   C |   180 | 18.3 |
    66194 | 2019-08-01 17:00:06 |         MASTER-SAAO | ( 22h 38m 17.07s , -76d 43m 24.10s) |   C |   180 | 19.4 |
    66344 | 2019-08-01 17:00:06 |         MASTER-SAAO | ( 22h 38m 17.12s , -76d 43m 24.11s) |   C |   480 | 19.1 |  Coadd
    68464 | 2019-08-01 17:38:56 |         MASTER-SAAO | ( 22h 17m 50.68s , -76d  4m 50.21s) |   C |    60 | 19.3 |
    68844 | 2019-08-01 17:45:16 |         MASTER-SAAO | ( 22h 17m 51.60s , -76d  4m 41.03s) |   C |    60 | 19.3 |
    69225 | 2019-08-01 17:51:37 |         MASTER-SAAO | ( 22h 51m 04.79s , -76d  5m 15.39s) |   C |    60 | 19.1 |
    69789 | 2019-08-01 18:01:01 |         MASTER-SAAO | ( 22h 51m 07.30s , -76d  5m 25.37s) |   C |    60 | 19.4 |
    73540 | 2019-08-01 19:03:32 |         MASTER-SAAO | ( 22h 44m 49.14s , -78d  4m 44.09s) |   C |    60 | 19.4 |
    73976 | 2019-08-01 19:10:48 |         MASTER-SAAO | ( 22h 44m 50.07s , -78d  4m 35.94s) |   C |    60 | 19.4 |
    83563 | 2019-08-01 21:49:36 |         MASTER-SAAO | ( 22h 39m 03.78s , -76d 38m 29.08s) |   C |   180 | 19.8 |
    83743 | 2019-08-01 21:49:36 |         MASTER-SAAO | ( 22h 39m 03.83s , -76d 38m 29.08s) |   C |   540 | 21.0 |  Coadd
    83775 | 2019-08-01 21:53:07 |         MASTER-SAAO | ( 22h 39m 07.18s , -76d 38m 13.34s) |   C |   180 | 20.3 |
    83986 | 2019-08-01 21:56:39 |         MASTER-SAAO | ( 22h 39m 07.84s , -76d 38m 16.00s) |   C |   180 | 20.3 |
    84616 | 2019-08-01 21:56:39 |         MASTER-SAAO | ( 22h 39m 07.85s , -76d 38m 16.00s) |   C |  1440 | 21.0 |  Coadd
    84197 | 2019-08-01 22:00:10 |         MASTER-SAAO | ( 22h 39m 09.53s , -76d 38m 36.09s) |   C |   180 | 20.3 |
    84377 | 2019-08-01 22:00:10 |         MASTER-SAAO | ( 22h 39m 09.55s , -76d 38m 36.11s) |   C |   540 | 21.4 |  Coadd
    84469 | 2019-08-01 22:04:42 |         MASTER-SAAO | ( 22h 39m 13.22s , -76d 38m 16.65s) |   C |   180 | 20.3 |
    84680 | 2019-08-01 22:08:13 |         MASTER-SAAO | ( 22h 39m 13.30s , -76d 38m 16.35s) |   C |   180 | 20.5 |
    84892 | 2019-08-01 22:11:45 |         MASTER-SAAO | ( 22h 39m 14.79s , -76d 38m 35.89s) |   C |   180 | 20.4 |
    85072 | 2019-08-01 22:11:45 |         MASTER-SAAO | ( 22h 39m 14.79s , -76d 38m 35.91s) |   C |   540 | 21.0 |  Coadd
    85106 | 2019-08-01 22:15:19 |         MASTER-SAAO | ( 22h 39m 17.57s , -76d 38m 35.58s) |   C |   180 | 20.5 |
    85317 | 2019-08-01 22:18:49 |         MASTER-SAAO | ( 22h 39m 18.81s , -76d 38m 15.77s) |   C |   180 | 20.4 |
    85528 | 2019-08-01 22:22:20 |         MASTER-SAAO | ( 22h 39m 18.99s , -76d 38m 15.51s) |   C |   180 | 20.4 |
Filter C is a clear (unfiltred) band.

This GRB was also detected by CALET (Asaoka et al. GCN25246), triangulated by IPN (Hurley et al. GCN25250)

The observation and reduction will continue.


GRB_name: GRB190731A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25257
SUBJECT: GRB 190731A: Swift/UVOT Upper Limits
DATE:    19/08/02 13:47:54 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (U.Warwick) and S. Dichiara (UMCP/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190731A
33372 s after the LAT trigger (Ohno et al., GCN Circ. 25244).
No optical afterglow consistent with the XRT position
(Osborne et al., GCN Circ. 25251) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

v                39548        40152          590         >20.0
b                45350        45715          355         >20.7
w2               33372        33977          596         >20.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.13 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190731A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25258
SUBJECT: GRB 190731A: AstroSat CZTI detection
DATE:    19/08/03 04:09:06 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma, D. Bhattacharya and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190731A, which was also detected by Fermi GBM (GCN #25240), Global MASTER-Net (Lipunov V. et al., GCN #25242), Fermi-LAT (Ohno M. et al., GCN #25244), Swift ToO (Evans P. A. et al., GCN #25245), CALET Gamma-Ray Burst Monitor detection (Asaoka Y. et al., GCN #25246), IPN Triangulation (Hurley K. et al., GCN #25250) and Swift-XRT (Osborne J.P. et al., GCN #25251).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 22:38:24.0 UT. The measured peak count rate associated with the burst is 2165 cts/s above the background in the combined data of four quadrants, with a total of 18049 cts. The local mean background count rate was 520 cts/s. Using cumulative rates, we measure a T90 of 20 s. In preliminary analysis, we find that 1455 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190804A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25259
SUBJECT: GRB 190804A: Fermi GBM Final Real-time Localization
DATE:    19/08/04 01:35:19 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 01:23:27 UT on 4 Aug 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190804A (trigger 586574612.354622 / 190804058).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 108.0, Dec = -64.9 (J2000 degrees, equivalent to J2000 07h 12m, -64d 54'), with a statistical uncertainty of 12.0 degrees.

The angle from the Fermi LAT boresight is 117.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190804058/quicklook/glg_skymap_all_bn190804058.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190804058/quicklook/glg_healpix_all_bn190804058.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190804058/quicklook/glg_lc_medres34_bn190804058.gif


GRB_name: GRB190804B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25262
SUBJECT: GRB 190804B: MAXI/GSC detection
DATE:    19/08/04 12:00:58 GMT
FROM:    Hitoshi Negoro at Nihon U  <negoro.hitoshi@nihon-u.ac.jp>

T. Sato (Chuo U.), H. Negoro, M. Nakajima, W. Maruyama, M. Aoki, 
K. Kobayashi (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), 
T. Sakamoto, M. Serino, S. Sugita, H. Nishida, A. Yoshida (AGU), 
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai (Chuo U.),  M. Shidatsu (Ehime U.),
N. Kawai, M. Sugizaki, M. Oeda, K. Shiraishi (Tokyo Tech), S. Nakahira, Y. Sugawara, 
S. Ueno, H. Tomida, M. Ishikawa, N.Isobe, R. Shimomukai, M. Tominaga (JAXA), 
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.), 
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), 
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.), 
T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered on an uncatalogued X-ray transient source at 
07:58:15 UT on  2019 August 04.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (239.895 deg, -44.773 deg) = (15 59 34, -44 46 22) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.29 deg and 0.24 deg, respectively. 
The roll angle of the long axis from the north direction is 39.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 118 +- 21 mCrab
(4.0-10.0keV, 1 sigma error).

Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (240.071, -43.705) deg = (16 00 17, -43 42 17) (J2000)
(R.A., Dec) = (239.431, -43.730) deg = (15 57 43, -43 43 47) (J2000)
(R.A., Dec) = (239.594, -45.994) deg = (15 58 22, -45 59 38) (J2000)
(R.A., Dec) = (240.259, -45.968) deg = (16 01 02, -45 58 04) (J2000)
There was no significant excess flux in the previous transit at 06:25 UT, 
and in the next transit at 09:30 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB190804B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25263
SUBJECT: GRB 190804B: Tiled Swift observations
DATE:    19/08/04 18:18:21 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
MAXI GRB 190804B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00082

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the MAXI event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190804C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25264
SUBJECT: GRB 190804C: Fermi GBM Final Real-time Localization
DATE:    19/08/04 19:11:39 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 19:00:37 UT on 4 Aug 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190804C (trigger 586638042.518414 / 190804792).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 97.8, Dec = 42.3 (J2000 degrees, equivalent to J2000 06h 31m, 42d 17'), with a statistical uncertainty of 4.4 degrees.

The angle from the Fermi LAT boresight is 98.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190804792/quicklook/glg_skymap_all_bn190804792.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190804792/quicklook/glg_healpix_all_bn190804792.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190804792/quicklook/glg_lc_medres34_bn190804792.gif


GRB_name: GRB190804C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25265
SUBJECT: GRB 190804C: BALROG localization (Fermi Trigger 586638042 / GRB 190804792)
DATE:    19/08/04 19:22:56 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
586638042 at 19:00:37 on 04 Aug. 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 86.4+/-4.1 deg
Decl.(2000.0) = 46.0+/-2.1 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190804792/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190804792/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190804792/json

                        


GRB_name: GRB190805A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25269
SUBJECT: GRB 190805A: Fermi GBM Final Real-time Localization
DATE:    19/08/05 02:44:39 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 02:32:30 UT on 5 Aug 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190805A (trigger 586665155.450396 / 190805106).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 167.6, Dec = -23.8 (J2000 degrees, equivalent to J2000 11h 10m, -23d 48'), with a statistical uncertainty of 3.2 degrees.

The angle from the Fermi LAT boresight is 121.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190805106/quicklook/glg_skymap_all_bn190805106.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190805106/quicklook/glg_healpix_all_bn190805106.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190805106/quicklook/glg_lc_medres34_bn190805106.gif


GRB_name: GRB190805B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25270
SUBJECT: GRB 190805B: Fermi GBM Final Real-time Localization
DATE:    19/08/05 04:56:51 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 04:46:00 UT on 5 Aug 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190805B (trigger 586673165.970428 / 190805199).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 209.8, Dec = 19.5 (J2000 degrees, equivalent to J2000 13h 59m, 19d 30'), with a statistical uncertainty of 2.6 degrees.

The angle from the Fermi LAT boresight is 46.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190805199/quicklook/glg_skymap_all_bn190805199.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190805199/quicklook/glg_healpix_all_bn190805199.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190805199/quicklook/glg_lc_medres34_bn190805199.gif


GRB_name: GRB190805B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25271
SUBJECT: GRB 190805B: MAXI/GSC detection
DATE:    19/08/05 05:32:21 GMT
FROM:    Hitoshi Negoro at Nihon U  <negoro@cygnus.phys.cst.nihon-u.ac.jp>

T. Sato (Chuo U.), H. Negoro, M. Nakajima, W. Maruyama, M. Aoki, 
K. Kobayashi (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), 
T. Sakamoto, M. Serino, S. Sugita, H. Nishida, A. Yoshida (AGU), 
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai (Chuo U.),  M. Shidatsu (Ehime U.),
N. Kawai, M. Sugizaki, M. Oeda, K. Shiraishi (Tokyo Tech), S. Nakahira, Y. Sugawara, 
S. Ueno, H. Tomida, M. Ishikawa, N.Isobe, R. Shimomukai, M. Tominaga (JAXA), 
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.), 
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), 
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.), 
T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered on an uncatalogued X-ray transient source 
at 04:49:12 UT on 2019 August 05.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (211.853 deg, 19.766 deg) = (14 07 24, +19 45 57) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.30 deg and 0.29 deg, respectively. 
The roll angle of the long axis from the north direction is 170.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 109 +- 18 mCrab
(4.0-10.0keV, 1 sigma error).

Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (210.974, 20.151) deg = (14 03 53, +20 09 03) (J2000) 
(R.A., Dec) = (210.941, 19.551) deg = (14 03 45, +19 33 03) (J2000) 
(R.A., Dec) = (212.931, 19.442) deg = (14 11 43, +19 26 31) (J2000) 
(R.A., Dec) = (212.971, 20.042) deg = (14 11 53, +20 02 31) (J2000) 
There was no significant excess flux in the previous transit at 03:16 UT
with an upper limit of 20 mCrab.

This burst is likely the same one that Fermi detected about 3 min earlier
(Trigger number 586673165).


GRB_name: GRB190805B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25272
SUBJECT: GRB 190805B: BALROG localization (Fermi Trigger 586673165 / GRB 190805199)
DATE:    19/08/05 07:50:20 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
586673165 at 04:46:00 on 05 Aug. 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 207.8+/-2.2 deg
Decl.(2000.0) = 19.4+/-2.0 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190805199/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190805199/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190805199/json

                        


GRB_name: GRB190804B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25273
SUBJECT: GRB 190804B: Swift-XRT observations
DATE:    19/08/05 08:58:34 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

J.P. Osborne (U. Leicester), M. Capalbi (INAF-IASFPA), M. Perri (ASDC),
V. D'Elia (ASDC), A. Tohuvavohu (PSU), J.A. Kennea (PSU), B. Sbarufatti
(PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester) and P.A.
Evans (U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the MAXI-detected
burst GRB 190804B (Sato et al. GCN Circ. 25262) in a series of
observations tiled on the sky. The total exposure time is 1.3 ks,
distributed over 7 tiles; the maximum exposure at a single sky location
was 395 s. The data were collected between T0+37.2 ks and T0+38.6 ks,
and are entirely in Photon Counting (PC) mode. 

Two uncatalogued X-ray sources have been detected, however none of them
is above the RASS limit or shows definitive signs of fading. Therefore,
at the present time we cannot identify which, if any, is the afterglow.
Details of these sources are given below:

Source 1:
  RA (J2000):  239.7568  =  15:59:1.62
  Dec (J2000): -44.6361  =  -44:38:09.8
  Error: 4.1 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: 0.031 [+0.014, -0.011] ct s^-1   
  Distance: 606 arcsec from MAXI position.
  Flux: (1.38 [+0.60, -0.46])e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 2:
  RA (J2000):  240.0251  =  16:00:6.02
  Dec (J2000): -44.7816  =  -44:46:53.9
  Error: 3.9 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: 0.113 [+0.038, -0.031] ct s^-1   
  Distance: 333 arcsec from MAXI position.
  Flux: (5.1 [+1.7, -1.4])e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)

The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00082.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190731A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25274
SUBJECT: Konus-Wind observation of GRB 190731A
DATE:    19/08/05 15:36:05 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration, hard-spectrum, very bright GRB 190731A
(Fermi-LAT detection: Ohno et al., GCN 25244;
CALET Gamma-Ray Burst Monitor detection: Asaoka  et al., GCN 25246;
Fermi GBM detection: Roberts & Meegan, GCN 25248;
IPN Triangulation: Hurley et al., GCN 25250;
AstroSat CZTI detection: Ghumatkar et al., GCN 25258)
triggered Konus-Wind at T0=81504.082 s UT (22:38:24.082).

The burst light curve shows a multi-peaked structure
which starts at ~T0-1.5 s and has a total duration of~22.0 s.
The emission is seen up to ~5 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.32(-0.08,+0.08)x10^-4 erg/cm2,
and a 64-ms peak energy flux, measured from T0+0.944 s,
of 3.89(-0.46,+0.46)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+23.808 s)
is best fit in the 20 keV - 5 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.69(-0.05,+0.06),
the high energy photon index beta = -2.30(-0.13,+0.11),
the peak energy Ep = 406(-30,+30) keV,
chi2 = 121/98 dof.

The spectrum near the peak count rate
(measured from T0+0.256 to T0+1.536 s)
is best fit in the 20 keV - 20 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.63(-0.07,+0.08),
the high energy photon index beta = -2.69(-0.50,+0.29),
the peak energy Ep = 875(-118,+120) keV,
chi2 = 107/69 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190731_T81504/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190805B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25275
SUBJECT: GRB 190805B: Tiled Swift observations
DATE:    19/08/05 18:09:15 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
MAXI GRB 190805B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00083

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the MAXI event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190805B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25277
SUBJECT: GRB 190805B: Fermi GBM detection
DATE:    19/08/05 21:16:24 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

R. Hamburg (UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 04:46:00.97 UT on 05 August 2019, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 190805B (trigger 586673165 / 190805199),
which was also detected by the MAXI/GSC (Sato et al. 2019, GCN 25271).
The Fermi GBM Final Real-time Localization (GCN 25270) is consistent with
the MAXI position.

The angle from the Fermi LAT boresight at the GBM trigger time is 46
degrees.

The GBM light curve shows a spiky, multi-peaked structure with a
duration (T90) of about 22 s (50-300 keV). The time-averaged
spectrum from T0-4.6 s to T0+ 25.1 s is best fit by a power law function
with an exponential high-energy cutoff. The power law index
is -1.07 +/- 0.05 and the cutoff energy, parameterized as Epeak,
is 389 +/- 51 keV.

The event fluence (10-1000 keV) in this time interval is
(1.03 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+16 s in the 10-1000 keV band
is 7.6 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB190805B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25279
SUBJECT: GRB 190805B: Swift-XRT observations
DATE:    19/08/06 05:24:47 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

M. Perri (ASDC), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A. Kennea
(PSU), B. Sbarufatti (PSU), D.N. Burrows (PSU), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester) and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the MAXI-detected
burst GRB 190805B (Sato et al. GCN Circ. 25271) in a series of
observations tiled on the sky. The total exposure time is 1.3 ks,
distributed over 7 tiles; the maximum exposure at a single sky location
was 391 s. The data were collected between T0+47.6 ks and T0+49.0 ks,
and are entirely in Photon Counting (PC) mode. 

No X-ray sources have been detected. The 3-sigma upper limit in the
field (not including the regions where the tiles overlap) ranges from
~0.03 to ~0.11 ct s^-1, corresponding to a 0.3-10 keV observed flux of
1.2e-12 to 4.4e-12 erg cm^-2 s^-1 (assuming a typical GRB spectrum).

The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00083.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190806A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25280
SUBJECT: GRB 190806A: Fermi GBM Final Real-time Localization
DATE:    19/08/06 16:23:39 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 16:12:33 UT on 6 Aug 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190806A (trigger 586800758.324292 / 190806675).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 121.1, Dec = -75.4 (J2000 degrees, equivalent to J2000 08h 04m, -75d 24'), with a statistical uncertainty of 4.3 degrees.

The angle from the Fermi LAT boresight is 32.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190806675/quicklook/glg_skymap_all_bn190806675.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190806675/quicklook/glg_healpix_all_bn190806675.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190806675/quicklook/glg_lc_medres34_bn190806675.gif


GRB_name: GRB190805B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25285
SUBJECT: Konus-Wind observation of GRB 190805B
DATE:    19/08/08 05:42:10 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 190805B
(MAXI/GSC detection: Sato et al., GCN Circ. 25271;
Fermi/GBM detection: Hamburg & Meegan, GCN Circ. 25277)
triggered Konus-Wind at T0=17159.354 s UT (04:45:59.354).

The burst light curve shows a multipeaked structure
which starts at ~T0-6.1 s and has a total duration of ~27.9 s.
The emission is seen up to ~6 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.46(-0.16,+0.24)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+14.832 s,
of 4.76(-1.60,+8.56)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+24.832 s)
is best fit in the 20 keV - 6 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.07(-0.23,+0.26)
and Ep = 315(-73,+148) keV (chi2 = 66/79 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.0
(chi2 = 65/78 dof).

The spectrum near the maximum count rate
(measured from T0+8.448 to T0+16.640 s)
is best fit in the 20 keV - 6 MeV range
by a power law with exponential cutoff model
with  alpha = -1.28(-0.44,+0.55)
and Ep = 281(-118,-281) keV (chi2 = 45/78 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.7
(chi2 = 44/77 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190805_T17159/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190804B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25286
SUBJECT: GRB 190804B: Swift-XRT afterglow detection
DATE:    19/08/08 08:43:25 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

J.P. Osborne (U. Leicester), M. Capalbi (INAF-IASFPA), M. Perri (ASDC),
V. D'Elia (ASDC), A. Tohuvavohu (PSU), J.A. Kennea (PSU), B. Sbarufatti
(PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester) and P.A.
Evans (U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has conducted further observations of the field of the
MAXI-detected burst GRB 190804B (Sato et al. GCN Circ. 25262). The
observations now extend from T0+37.2 ks to T0+273.4 ks. 

Of the sources reported by Osborne et al. (GCN Circ. 25273), "Source 2"
has faded from 1.1e-01 count/s to 1.1e-03 count/s between observations
and is believed to be the afterglow.  The position of this source
(astrometrically enhanced by using the XRT-UVOT alignment and matching
UVOT field sources to the USNO-B1 catalogue) is RA, Dec=240.0251,
-44.7816 which is equivalent to:

RA (J2000): 16:00:6.02
Dec(J2000): -44:46:53.9

with an uncertainty of 3.8 arcsec (radius, 90% confidence). Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and
Evans et al. (2009, MNRAS, 397, 177). This position is 5.6 arcmin from
the MAXI position.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020916.
The results of the full analysis of the tiled XRT observations are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00082.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190805B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25287
SUBJECT: GRB 190805B: AstroSat CZTI detection
DATE:    19/08/08 11:27:52 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma and D. Bhattacharya and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190805B, which was also detected by Fermi GBM Final Real-time Localization (GCN #25270), MAXI/GSC detection (Sato T. et al., GCN #25271), BALROG localization (Biltzinger B. et al., GCN #25272), Tiled Swift observations (Evans P. A. et al., GCN #25275), Fermi GBM detection (Hamburg R. et al., GCN #25277), Swift-XRT (Perri M. et al., GCN #25279) and Konus-Wind (Kozlova A. et al., GCN #25285).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 04:46:05.0 UT. The measured peak count rate associated with the burst is 323 cts/s above the background in the combined data of four quadrants, with a total of 4289 cts. The local mean background count rate was 588 cts/s. Using cumulative rates, we measure a T90 of 24 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190804A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25289
SUBJECT: GRB 190804A: AstroSat CZTI detection
DATE:    19/08/08 12:06:02 GMT
FROM:    Prachee Ghumatkar at IUCAA/AstroSat  <prachee@iucaa.in>

P. Ghumatkar, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of GRB 190804A, which was also detected by Fermi GBM (GCN #25259) and Global MASTER-Net (Lipunov V. et al., GCN #25260).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 01:23:28.0 UT. The measured peak count rate associated with the burst is 149 cts/s above the background in the combined data of four quadrants, with a total of 298 cts. The local mean background count rate was 535 cts/s. Using cumulative rates, we measure a T90 of 2 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB190808A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  25290
SUBJECT: GRB 190808A: Fermi GBM Final Real-time Localization
DATE:    19/08/08 12:06:43 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 11:56:27 UT on 8 Aug 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190808A (trigger 586958192.790556 / 190808498).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 282.2, Dec = -31.8 (J2000 degrees, equivalent to J2000 18h 48m, -31d 48'), with a statistical uncertainty of 16.1 degrees.

The angle from the Fermi LAT boresight is 88.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190808498/quicklook/glg_skymap_all_bn190808498.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190808498/quicklook/glg_healpix_all_bn190808498.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190808498/quicklook/glg_lc_medres34_bn190808498.gif


