| Summary table |
|---|
| Variable |
Value |
Source |
| GRB_name_Fermi |
GRB130206817 |
|
| T0 |
19:36:27.892 UTC |
Fermi_GBM |
| ra |
140.3767° |
Swift |
| decl |
-58.1936° |
Swift |
| pos_error |
5.95e-04° |
Swift |
| T90 |
91.585 s |
Fermi_GBM |
| T90_error |
12.332 s |
Fermi_GBM |
| T90_start |
19:36:27.892 UTC |
Fermi_GBM |
| fluence |
2.57e-06 erg/cm² |
Fermi_GBM |
| fluence_error |
7.05e-08 erg/cm² |
Fermi_GBM |
| T100 |
128.108 s |
|
| GBM_located |
False |
|
| mjd |
56329.81698949074 |
Fermi_GBM |
| Fermi GBM table |
|---|
| GRB_name_Fermi |
GRB130206817 |
| trigger_name |
bn130206817 |
| ra |
140.3750° |
| decl |
-58.1600° |
| pos_error |
7.65e+00° |
| datum |
2013-02-06 |
| t_trigger |
19:36:30.452 UTC |
| T90 |
91.585 s |
| T90_error |
12.332 s |
| T90_start |
19:36:27.892 UTC |
| fluence |
2.57e-06 erg/cm² |
| fluence_error |
7.05e-08 erg/cm² |
| flux_1024 |
2.14e+00 erg/cm²/s |
| flux_1024_error |
2.41e-01 erg/cm²/s |
| flux_1024_time |
1.79e+00 erg/cm²/s |
| flux_64 |
5.72e+00 erg/cm²/s |
| flux_64_error |
1.66e+00 erg/cm²/s |
| IPN table |
|---|
| GRB_name |
GRB130206A |
| ra |
140.3750° |
| decl |
-58.1667° |
| pos_error |
5.00e-02° |
| Swift table |
|---|
| GRB_name |
GRB130206A |
| t_trigger |
19:36:28 UTC |
| ra |
140.3767° |
| decl |
-58.1936° |
| pos_error |
5.95e-04° |
| T90 |
128.0 s |
| fluence |
2.00e-06 erg/cm² |
| Fermi LAT table |
|---|
| GRB_name_Fermi |
GRB130206817 |
| GRB_name |
GRB130206A |
| MET |
381872193.0 |
| datum |
2013-02-06 |
| t_trigger |
19:36:30 UTC |
| ra |
140.3767° |
| decl |
-58.1936° |
| pos_error |
1.56e-03° |
| GCN 14181 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14181 |
| Detection_method |
Swift Det |
| t_trigger |
19:36:28 UTC |
| ra |
140.3750° |
| decl |
-58.1600° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14181
SUBJECT: GRB 130206A: Swift detection of a burst
DATE: 13/02/06 19:43:58 GMT
FROM: Jamie A. Kennea at PSU/Swift-XRT
M. De Pasquale (UCL-MSSL), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), S. R. Oates (UCL-MSSL),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC) and V. N. Yershov (UCL-MSSL) report on
behalf of the Swift Team:
At 19:36:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130206A (trigger=547918).
The BAT on-board calculated location is
RA, Dec 140.375, -58.160 which is
RA(J2000) = 09h 21m 30s
Dec(J2000) = -58d 09' 36"
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 50 sec. The peak count rate
was ~2500 counts/sec (15-350 keV), at ~4 sec after the trigger.
Due to an observing constraint, Swift will not slew until T0+48.5
minutes. There will be no XRT or UVOT data until this time.
Burst Advocate for this burst is M. De Pasquale (mdp AT mssl.ucl.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/too.html.)
|
| GCN 14183 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14183 |
| Detection_method |
Swift-XRT Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14183
SUBJECT: GRB 130206A: Swift-XRT observations
DATE: 13/02/06 21:22:04 GMT
FROM: Phil Evans at U of Leicester
J.P. Osborne (U. Leicester), D.N. Burrows (PSU), J.A. Kennea (PSU), G.
Cusumano (INAF-IASF PA), M. Perri (ASDC) and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team:
The XRT began observing the field of GRB 130206A at 20:27:46.2 UT,
3077.7 seconds after the BAT trigger. No source was detected in 1.9 ks
of promptly downlinked data. We are waiting for the full dataset to
detect and localise the XRT counterpart.
|
| GCN 14184 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14184 |
| Detection_method |
Swift-UVOT Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14184
SUBJECT: Swift GRB 130206A - analysis of Swift/UVOT initial data.
DATE: 13/02/06 22:32:32 GMT
FROM: Patricia Schady at MPE/Swift
M. De Pasquale (MSSL-UCL) on behalf of the Swift/UVOT team reports:
UVOT took a finding chart exposure of 150 seconds with the White
filter starting 3080 seconds after the BAT trigger. No credible
candidates have been identified in the initial data products. The
8'x8' region for the list of sources generated on-board covers about
86% of the BAT error circle. The list of sources is typically complete
to about 18 mag.
The GRB occurred in a crowded field only 5.8 deg from the Galactic Plane.
No correction has been made for the expected extinction corresponding to
E(B-V) of 0.49.
|
| GCN 14185 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14185 |
| Detection_method |
Optical |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14185
SUBJECT: GRB 130206A: Zadko observatory - Gingin optical observations
DATE: 13/02/06 22:44:26 GMT
FROM: Alain Klotz at IRAP-CNRS-OMP
A. Klotz (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. Coward (UWA),
B. Gendre (IRAP-CNRS-OMP), M. Boer, K. Siellez, H. Dereli ,
O. Bardho (UNS-CNRS-OCA), A. Williams (PO-UWA), R. Martin (PO-UWA)
report:
We imaged the field of GRB 130206A detected by SWIFT
(trigger 547918) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.
The observations started 106s after the GRB trigger
(73s after the notice). The elevation of the field
decreased from 48 degrees above horizon and weather
conditions were good.
The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT in the BAT error box with a
limiting magnitude of:
t0+106s to t0+166s : R > 16.5
The second image is 30.0s exposure in tracking mode:
t0+187s to t0+217s : R > 18.3
We co-added a series of images in tracking mode:
t0+187s to t0+482s : R > 20.1
The analysis was made by substraction with images
acquired one hour later.
Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.
N.B. Galactic coordinates are lon=278.0587 lat=-5.8228
and the corresponding galactic absorption in R band
should be about 1.1 mag (Schlegel et al. 1998).
This message may be cited.
|
| GCN 14186 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14186 |
| Detection_method |
Swift-BAT Det |
| ra |
140.3870° |
| decl |
-58.1930° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14186
SUBJECT: GRB 130206A, Swift-BAT refined analysis
DATE: 13/02/07 13:51:11 GMT
FROM: Hans Krimm at NASA-GSFC
M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), M. De Pasquale (UCL-MSSL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D.
M. Palmer (LANL), T. Sakamoto (AGU), J. Tueller (GSFC),
T. N. Ukwatta (MSU) (i.e. the Swift-BAT team):
Using the data set from T-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130206A (trigger #547918)
(De Pasquale, et al., GCN Circ. 14181). The BAT ground-calculated position is
RA, Dec = 140.387, -58.193 deg which is
RA(J2000) = 09h 21m 32.9s
Dec(J2000) = -58d 11' 35.6"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 52%.
The mask-weighted light curve shows two clusters of peaks. The first runs from
approximately T-10 sec to T+15 sec and the second from T+20 sec to T+60 sec,
though the count rate does not return to baseline between the two clusters.
Each of these clusters consists of multiple sub-peaks. There is also some
low-level emission extending out to T+150 sec. T90 (15-350 keV) is
128.0 +- 50.6 sec (estimated error including systematics).
The time-averaged spectrum from -12.78 to 147.21 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.56 +- 0.17. The fluence in the 15-150 keV band is 2.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+42.72 sec in the 15-150 keV band is
0.3 +- 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/547918/BA/
|
| GCN 14188 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14188 |
| Detection_method |
Swift-XRT Other |
| ra |
140.3767° |
| decl |
-58.1936° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14188
SUBJECT: GRB 130206A: XRT and UVOT follow-up observations.
DATE: 13/02/07 20:22:53 GMT
FROM: MSSL Swift/UVOT team at MSSL/Swift
Andy Beardmore (Univ. Leicester), A. Breeveld (MSSL-UCL) and M. De
Pasquale (MSSL-UCL) on behalf of the Swift team, report:
The Swift-XRT began observing the field of GRB130206A (De Pasquale et al.,
GCN Circ. 14181) in photon counting mode at 2013-02-06 20:28 UT, 3090 s
after the trigger. In 10.3 ks of data we find a faint source at RA, Dec =
140.37670, -58.19362 which is equivalent to
RA (J2000) = 09h 21m 30.41s
Dec (J2000) = -58d 11' 37.0"
with an uncertainty of 5.6 arcseconds (radius, 90% confidence). The
source is located 20 arcseconds from the BAT refined position
(Stamatikos et al, GCN Circ, 14186), within the BAT error circle.
The source is detected at a count rate of 0.0017 ± 0.0006 count/s. We
cannot tell if it is fading at this time.
The Swift/UVOT began settled observations of the field of GRB130206A
3081 s after the BAT trigger.
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 3081 3231 147 >21.4
white 3081 16409 2114 >23.1
v 4062 22199 1319 >20.3
b 3445 15497 1278 >22.3
u 3239 28222 634 >21.2
w1 4473 27971 1082 >21.0
m2 4268 27065 1312 >20.7
w2 3857 32412 2546 >21.3
The magnitudes in the table are not corrected for the strong Galactic
extinction due to the reddening of E(B-V) = 0.48 in the direction of the
burst (Schlegel et al. 1998).
|
| GCN 14189 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14189 |
| Detection_method |
Fermi GBM Det |
| t_trigger |
19:36:30.450 UTC |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14189
SUBJECT: GRB 130206A: Fermi GBM observation
DATE: 13/02/07 22:21:38 GMT
FROM: Adam Goldstein at Fermi-GBM/UAH
A. Goldstein (UAH) reports on behalf of the Fermi GBM Team:
At 19:36:30.45 UT on 06 February 2013, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 130206A
(trigger 381872193 /130206817) which was also detected by
the Swift/BAT (De Pasquale et al. 2013, GCN 14181). The GBM
on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 19 degrees.
The GBM light curve consists of three overlapping pulses
with a duration (T90) of about 91 s (50-300 keV). The
time-averaged spectrum from T0=-1.5 s to T0+85.6 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.1 +/- 0.2 and
the cutoff energy, parameterized as Epeak, is 132.6 +/- 34.0 keV.
The event fluence (10-1000 keV) in this time interval is
(3.3 +/- 0.4)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.8 s in the 10-1000 keV band is
2.1 +/- 0.2 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog.
|
| GCN 14190 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14190 |
| Detection_method |
Fermi LAT Det |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14190
SUBJECT: GRB 130206A: Fermi LAT Observations
DATE: 13/02/07 23:11:00 GMT
FROM: Judith Racusin at GSFC
J. L. Racusin (NASA/GSFC), G. Vianello (Stanford), N. Omodei (Stanford), and D. Kocevski (NASA/GSFC), report on behalf of the Fermi-LAT team:
The Fermi Large Area Telescope (LAT) observed GRB 130206A, detected by Fermi-GBM (Goldstein et al., GCN 14189) and Swift-BAT (De Pasquale et al., GCN 14181).
The burst location was within the LAT field of view at an angle of ~19.4 degrees to the LAT boresight, and had a zenith angle of 69 degrees. No significant excess is seen using standard analysis procedures. The burst exited the nominal LAT field of view roughly ~600 s after the GBM trigger.
We estimate the 95% confidence upper limits in the energy range of 100 MeV - 10 GeV, assuming spectral index of -2.1, over the time interval 0-40 s:
F(100MeV-10GeV) < 3.7e-05 (ph/cm^2/s)
<1.5e-02 (MeV/cm^2/s)
<2.4e-08 (erg/cm^2/s)
Using the non-standard LAT Low Energy (LLE) data selection, >60 counts above background were observed in a single FRED like pulse, peaking ~15 s after the GBM trigger. This corresponds to a significance of 2.9 sigma without taking into account trial factors, and therefore does not constitute a clear detection. On the other hand, the putative signal shows good correlation with the low-energy (GBM) light curve. Such faint signal is constituted by low energy gamma-rays, below 75 MeV, and therefore has insufficient spatial resolution to provide a reliable LAT localization. Indeed, no events were observed above 75 MeV using the standard analysis classes.
The Fermi LAT point of contact for this burst is Judith Racusin (judith.racusin@nasa.gov).
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.
|
| GCN 14191 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14191 |
| Detection_method |
GROND |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14191
SUBJECT: GRB 130206A: GROND Observations
DATE: 13/02/08 19:20:31 GMT
FROM: Ana Nicuesa at TLS Tautenburg
F. Knust (MPE Garching), A. Nicuesa Guelbenzu (TLS Tautenburg)
and J. Greiner (MPE Garching) report on behalf of the GROND team:
We observed the field of GRB 130206A (Swift trigger 547918; De Pasquale
et al.,GCN 14181) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2m MPG/ESO telescope at La Silla
Observatory (Chile).
The first observations started at 01:10 UT on 07 Feb 2013, 6.5 hrs after
the GRB trigger, and a second epoch was taken at 7:47 UT on 8 Feb 2013.
These observations were performed at an average seeing of 1.4/1.0 arcsec
and at an average airmass of 1.3/1.4.
We detect three sources within the 5.6 arcsec Swift-XRT error circle
(Beardmore et al., GCN 14188), at positions:
Source 1
RA (2000.0) = 09h 21m 30.45s
Decl. (2000.0) = -58d 11' 34.7"
Source 2
RA (2000.0) = 09h 21m 30.10s
Decl. (2000.0) = -58d 11' 36.5"
Source 3
RA (2000.0) = 09h 21m 30.14s
Decl. (2000.0) = -58d 11' 41.2"
with an uncertainty of 0.5" in each coordinate.
For the aforementioned three sources, the preliminary photometry does
not show any variability. Image subtraction between the two epochs
has revealed no residuals either.
Based on exposures of 42 min in g'r'i'z' and 54 min in JHK,
we do not detect the afterglow within the 5.6" XRT error circle
to the following 3-sigma upper limits (AB system):
g' > 24.7,
r' > 24.6,
i' > 23.8,
z' > 23.8,
J > 21.6,
H > 21.2 and
K > 20.6
The given limits are derived based on calibrating the images against GROND
zeropoints and 2MASS field stars and are not corrected for the Galactic
foreground extinction corresponding to a reddening of E_(B-V)= 0.5 in the
direction of the burst (Schlegel et al. 1998).
|
| GCN 14203 table |
|---|
| GRB_name |
GRB130206A |
| GCN_number |
14203 |
| Detection_method |
Swift Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 14203
SUBJECT: Swift GRB130206A: late XRT observations.
DATE: 13/02/14 21:58:20 GMT
FROM: MSSL Swift/UVOT team at MSSL/Swift
M. De Pasquale (MSSL-UCL), A. Beardmore (Univ. Leicester) report, on behalf
of the Swift team:
The X-ray source described in GCN circ. 14188 (Beardmore et al. 2013) is not
detected anymore in XRT observations performed between 33 and 550 ks after
the trigger, for a total of 35.2 ks of integration time. The 3 sigma upper limit is
0.00089 count/s, appreciably lower than the count rate observed in previous
observations.
Because of the fading behaviour of this source, we conclude it was likely
the X-ray afterglow of GRB130206A.
We also note that successive analysis of late data has reduced the error circle
radius of the source to 4.6'' (90% confidence level).
|