| Summary table |
|---|
| Variable |
Value |
Source |
| T0 |
2:23:00 UTC |
GCN_circulars,Swift Det |
| ra |
251.9788° |
Swift |
| decl |
71.8271° |
Swift |
| pos_error |
2.85e-04° |
Swift |
| T90 |
7.0 s |
Swift |
| T90_start |
2:23:00 UTC |
Swift |
| fluence |
8.20e-07 erg/cm² |
Swift |
| redshift |
3.1550 |
IPN |
| T100 |
7.0 s |
|
| GBM_located |
False |
|
| mjd |
55271.09930555556 |
GCN_circulars,Swift Det |
| IPN table |
|---|
| GRB_name |
GRB100316A |
| ra |
252.0333° |
| decl |
71.8333° |
| pos_error |
5.00e-02° |
| redshift |
3.1550 |
| Swift table |
|---|
| GRB_name |
GRB100316A |
| t_trigger |
2:23:00 UTC |
| ra |
251.9788° |
| decl |
71.8271° |
| pos_error |
2.85e-04° |
| T90 |
7.0 s |
| fluence |
8.20e-07 erg/cm² |
| GCN 10484 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10484 |
| Detection_method |
Swift Det |
| t_trigger |
2:23:00 UTC |
| ra |
252.0320° |
| decl |
71.8250° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10484
SUBJECT: GRB 100316A: Swift detection of a burst
DATE: 10/03/16 02:35:00 GMT
FROM: Wayne Baumgartner at GSFC
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
C. B. Markwardt (CRESST/GSFC/UMD), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC), E. Troja (NASA/GSFC/ORAU),
T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the
Swift Team:
At 02:23:00 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100316A trigger=416076). The BAT on-board calculated location is
RA, Dec 252.032, +71.825 which is
RA(J2000) = 16h 48m 08s
Dec(J2000) = +71d 49' 31"
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 10 sec. The peak count rate
was ~2000 counts/sec (15-350 keV), at ~2 sec after the trigger.
Due to an observing constraint, Swift will not slew until
T0+51.8 minutes. There will be no XRT or UVOT data until
this time.
Burst Advocate for this burst is W. H. Baumgartner (wayne AT milkyway.gsfc.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/too.html.)
|
| GCN 10485 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10485 |
| Detection_method |
Swift-XRT Other |
| ra |
251.9789° |
| decl |
71.8265° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10485
SUBJECT: GRB 100316A: Swift-XRT detection
DATE: 10/03/16 04:12:35 GMT
FROM: Andy Beardmore at U Leicester
A.P. Beardmore, K.L. Page and O. Littlejohns (U. Leicester) report
on behalf on the Swift-XRT team:
Using 2.4ks of promptly downlinked data starting at 51.8 minutes after
the trigger we find an uncatalogued X-ray
source located at RA, Dec = 251.9789, 71.8265
which is equivalent to:
RA (J2000) = 16 47 54.94
DEC (J2000) = +71 49 35.3
with an uncertainty of 4.53 arcsec (radius, 90% containment).
It is not possible to tell whether the source is fading
with the limited data available so far.
|
| GCN 10486 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10486 |
| Detection_method |
Swift-UVOT Det |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10486
SUBJECT: GRB 100316A: Swift/UVOT Observations
DATE: 10/03/16 04:16:17 GMT
FROM: Mike Siegel at PSU/Swift MOC
M. H. Siegel (PSU) and W. H. Baumgartner (GSFC/UMBC) report on behalf
of the
Swift/UVOT team:
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 3200 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 (Beardmore et al., GCN Circ. 10485). 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 0.03.
|
| GCN 10487 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10487 |
| Detection_method |
Optical |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10487
SUBJECT: GRB 100316 optical candidate from 1.23m CAHA telescope
DATE: 10/03/16 04:22:03 GMT
FROM: Javier Gorosabel at IAA-CSIC
J. Gorosabel (IAA-CSIC), V. Peris (U. Valencia), P. Kubanek (IAA-CSIC,
U. Valencia), report on behalf of a larger collaboration:
"We have carried out R-band observations of the GRB100316 BAT error
box (Baumgartner et al., GCN 10484) with the 1.23m telescope of Calar
Alto. The observations started on March 16.1075 UT (11.7 min after the
GRB). We detect an object with a rough magnitude of R~20.5 coincident
with the XRT (GCN 10485) position and very likely not present on the
DSS. Further observations are encouraged to determine the
possible fading behaviour of this source. We propose that object as
the potential optical afterglow of GRB100316."
[GCN OPS NOTE(16mar10): Per author's request, the "Feb 16.1075" was changed
to "March 16.1075".]
|
| GCN 10488 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10488 |
| Detection_method |
Optical |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10488
SUBJECT: GRB 100316 optical candidate from 1.23m CAHA telescope
DATE: 10/03/16 05:16:37 GMT
FROM: Javier Gorosabel at IAA-CSIC
J. Gorosabel (IAA-CSIC), V. Peris (U. Valencia), P. Kubanek (IAA-CSIC,
U. Valencia), report on behalf of a larger collaboration:
"We have carried out R-band observations of the GRB100316 BAT error
box (Baumgartner et al., GCN 10484) with the 1.23m telescope of Calar
Alto. The observations started on Feb 16.1075 UT (11.7 min after the
GRB). We detect an object with a rough magnitude of R~20.5 coincident
with the XRT (GCN 10485) position and very likely not present on the
DSS. Further observations are encouraged to determine the
possible fading behaviour of this source. We propose that object as
the potential optical afterglow of GRB100316."
|
| GCN 10490 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10490 |
| Detection_method |
Swift-XRT Det |
| ra |
251.9815° |
| decl |
71.8278° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10490
SUBJECT: GRB 100316A: Enhanced Swift-XRT position
DATE: 10/03/16 08:21:20 GMT
FROM: Phil Evans at U of Leicester
P.A. Evans reports on behalf of the Swift-XRT team
Using 1129 s of XRT Photon Counting mode data and 2 UVOT
images, 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 = 251.98150, 71.82780 which is equivalent to:
RA (J2000): 16 47 55.56
Dec (J2000): +71 49 40.0
with an uncertainty of 2.9 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 is an official product of the Swift-XRT team.
|
| GCN 10499 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10499 |
| Detection_method |
Swift-UVOT Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10499
SUBJECT: GRB100316A: Swift/UVOT Upper Limits
DATE: 10/03/16 14:30:44 GMT
FROM: Samantha Oates at MSSL
S. R. Oates (MSSL-UCL) and W. H. Baumgartner (GSFC/UMBC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of
GRB 100316A 3201s after the BAT trigger (Baumgartner et al., GCN Circ.
10484).
We do not detect any source at the enhanced Swift XRT position
(Evans et al. GCN Circ. 10490) and at the location of the candidate
source detected
by the CAHA telescope (Gorosabel et al. GCN Circ. 10487).
The 3-sigma upper limits for the finding chart exposures (FC)
and summed images are:
Filter T_start T_stop Exp(s) Mag (3-sigma upper limit)
-------------------------------------------------------------
white (FC) 3201 3350 147 > 21.08
white 3770 5408 393 > 21.32
v 4182 16726 1210 > 20.48
b 3565 5203 393 > 20.79
u 3359 11527 1110 > 20.66
uvw1 4593 10786 1082 > 21.11
uvm2 4387 17306 1648 > 21.11
uvw2 3977 15812 1279 > 21.28
-------------------------------------------------------------
The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight of E_(B-V) = 0.03 mag.
All photometry is on the UVOT photometric system described in Poole et
al. (2008, MNRAS, 383, 627).
|
| GCN 10501 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10501 |
| Detection_method |
Swift-BAT Det |
| ra |
251.9530° |
| decl |
71.8190° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10501
SUBJECT: GRB 100316A: Swift-BAT refined analysis
DATE: 10/03/16 16:03:52 GMT
FROM: Scott Barthelmy at NASA/GSFC
W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 100316A (trigger #416076)
(Baumgartner, et al., GCN Circ. 10484). The BAT ground-calculated position is
RA, Dec = 251.953, 71.819 deg which is
RA(J2000) = 16h 47m 48.8s
Dec(J2000) = +71d 49' 09.5"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 16%.
The mask-weighted light curve shows a FRED-like pulse starting at ~T-1 sec,
peaking at ~t+2 sec, and ending at ~T+20 sec. T90 (15-350 keV) is
7.0 +- 0.9 sec (estimated error including systematics).
The time-averaged spectrum from T-1.2 to T+6.7 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.46 +- 0.18. The fluence in the 15-150 keV band is 8.2 +- 0.9 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.94 sec in the 15-150 keV band
is 2.3 +- 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/416076/BA/
|
| GCN 10503 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10503 |
| Detection_method |
Swift-XRT Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10503
SUBJECT: GRB 100316A: Swift-XRT refined analysis
DATE: 10/03/16 17:21:12 GMT
FROM: Andy Beardmore at U Leicester
A. P. Beardmore (U. Leicester) and W. H. Baumgartner (GSFC/UMBC) report
on behalf of the Swift-XRT team:
Due to an Earth-limb constraint, Swift performed a delayed slew to GRB
100316A (Baumgartner et al. GCN Circ. 10484), with XRT observations
starting 3.2 ks after the BAT trigger. The enhanced XRT position for this
burst was given by Evans (GCN. Circ 10490).
The X-ray light curve, obtained from 7.5 ks of Photon Counting (PC)
mode data spanning 3.2 ks to 17.3 ks after the trigger, can be
modelled by a power-law decay, with a decay slope of 1.3 +/- 0.3.
An X-ray spectrum formed from the same data can be modelled by an
absorbed power-law, with a photon index of 2.3 +0.3 -0.5 and absorbing
column density of (1.5 +1.2 -1.1) x 10^21 cm^-2, which is in excess of
the Galactic value of 4.4 x 10^20 cm^-2 (Kalberla et al. 2005) in the
direction of the source. The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum is 3.4 x 10^-11 (5.3
x 10^-11) erg cm^-2 count^-1.
If the light curve continues to decay at the same rate, the count rate
at T+24 hours will be 1.2 x 10^-3 count s^-1, corresponding to an
observed (unabsorbed) 0.3-10 keV flux of 4.0 x 10^-14 (6.3 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/00416076.
This circular is an official product of the Swift-XRT team.
|
| GCN 10504 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10504 |
| Detection_method |
Optical |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10504
SUBJECT: GRB 100316A: TAROT Calern observatory optical observations
DATE: 10/03/16 18:09:07 GMT
FROM: Bruce Gendre at ASDC
Gendre B. (ASDC), Klotz A. (CESR-OMP),
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:
We imaged the field of GRB 100316A detected by SWIFT
(trigger 416076, GCN 10484, Baumgartner et al. ) with the TAROT robotic
telescope (D=25cm)
located at the Calern observatory, France.
The observations started 1323s after the GRB trigger
(1299s after the notice). The elevation of the field increased from
58 degrees above horizon and weather conditions were good.
We obtained 16 image with clear filter and 8 images with R filter
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT within the exposures. Co-adding the images taken
with clear filter, we can set a limiting magnitude of:
R > 20.0 between t0+1323s to t0+3327s
at the position of the candidate reported by Gorosabel et al. (GCN 10487)
and Beardmore et al. (GCN 10485).
Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.
N.B. Galactic coordinates are lon=103.8139 lat=+35.1341
and the galactic extinction in R band is 0.1 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.
This message may be cited.
|
| GCN 10521 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10521 |
| Detection_method |
Optical |
| ra |
252.0268° |
| decl |
71.8376° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10521
SUBJECT: GRB 100316A: optical observations in CrAO
DATE: 10/03/18 01:23:18 GMT
FROM: Alexei Pozanenko at IKI, Moscow
V. Rumyantsev (CrAO), A. Pozanenko (IKI) report on behalf of larger GRB
follow-up collaboration:
We observed the field of the Swift GRB 100316A (Baumgartner et al. GCN
10484) with Shajn telescope of CrAO starting (UT) March 16 19:15 under
descending weather conditions and mean seeing of 2 arcsec. No object is
detected in enhanced XRT error circle (Evans, GCN 10490).
The upper limit of point like object in a stacked image based on USNO-B1.0
star 1618-0120609 (J2000) RA= 16:48:06.44 Dec= +71:50:15.2 (assuming
R2=15.25) is following:
T0+ Filter, Exposure, mag.
(mid, d) (s)
0.7061 R 8x60 > 21.6
The non-detection is strongly support the object of R~20.5 reported in GCN
10487 (Gorosabel et al) is the optical afterglow of GRB100316A.
|
| GCN 10565 table |
|---|
| GRB_name |
GRB100316A |
| GCN_number |
10565 |
| Detection_method |
Swift-BAT Det |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10565
SUBJECT: GRB 100316A: R-band limit
DATE: 10/04/02 12:51:11 GMT
FROM: Myungshin Im at Seoul Nat U
Jang, M., Im, M. (SNU), and Y. Urata (NCU) report on behalf of
the EAFON collaboration:
We observed GRB100316A in R-band starting at 2010 March16, 08:09:17UT,
or 20.78 ks after the BAT triggered (Baumgartner et al, GCN 10484),
using the 1.0m telescope at Mt.Lemmon in Arizona, U.S. operated
by Korea Astronomy Space Science Institute.
No afterglow candidate was detected from a stacked image of eight 300s-frames.
within the error circle of the enhanced XRT position (Evans et al.,GCN 10490).
We estimate the 3-sigma limiting magnitude of the afterglow to be
R ~ 22.0 +/- 0.2 at the midpoint time of the stacked image (~T0+21.98 ks)
by calibrating it against sixteen USNO-B1 stars near the GRB, using their
R2 magnitudes without correcting for the Galactic extinction.
Our limit indicates fading of the optical afterglow candidate reported by
Gorosabel et al. (GCN 10488) shortly after.
We thank the LOAO operator, I. Baek for her help with the observation
|