GRB 101011A
GCN Circular 11331
Subject
GRB 101011A: Swift detection of a burst
Date
2010-10-11T17:11:43Z (15 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@milkyway.gsfc.nasa.gov>
J. K. Cannizzo (NASA/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), M. M. Chester (PSU), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
V. Mangano (INAF-IASFPA), K. L. Page (U Leicester),
D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC),
A. Rowlinson (U Leicester), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC) and E. Troja (NASA/GSFC/ORAU) report on
behalf of the Swift Team:
At 16:58:35 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101011A (trigger=436094). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 48.298, -65.986, which is
RA(J2000) = 03h 13m 12s
Dec(J2000) = -65d 59' 08"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows about 5 peaks
with a duration of about 50 sec. The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 16:59:53.5 UT, 78.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 48.29427,
-65.98212 which is equivalent to:
RA(J2000) = 03h 13m 10.62s
Dec(J2000) = -65d 58' 55.6"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 14 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 (3.27 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 4.4
(+3.08/-2.53) x 10^21 cm^-2 (90% confidence).
The initial flux in the 2.5 s image was 6.35e-10 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White
filter starting 84 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 0.03.
Burst Advocate for this burst is J. K. Cannizzo (cannizzo 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 Circular 11332
Subject
GRB 101011A: Swift-BAT refined analysis
Date
2010-10-11T20:22:32Z (15 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. K. Cannizzo (NASA/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+302 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 101011A (trigger #436094)
(Cannizzo, et al., GCN Circ. 11331). The BAT ground-calculated position is
RA, Dec = 48.274, -65.990 deg, which is
RA(J2000) = 03h 13m 05.7s
Dec(J2000) = -65d 59' 23.2"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 87%.
The mask-weighted light curve shows an initial FRED-like pulse starting
at ~T-0.3 sec, peaking at ~T+0.6 sec, then followed by several other weaker
peaks lasting out to ~T+90 sec. T90 (15-350 keV) is 71.5 +- 18.3 sec
(estimated error including systematics).
The time-averaged spectrum from T-0.4 to T+84.2 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.24 +- 0.14. The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.22 sec in the 15-150 keV band
is 1.3 +- 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/436094/BA/
GCN Circular 11333
Subject
GRB 101011A: Enhanced Swift-XRT position
Date
2010-10-11T20:46:49Z (15 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.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 1274 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 101011A, 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 = 48.29486, -65.98182 which is equivalent
to:
RA (J2000): 03h 13m 10.77s
Dec (J2000): -65d 58' 54.5"
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.
GCN Circular 11334
Subject
GRB 101011A: Swift/UVOT Observations of a Possible Optical Afterglow
Date
2010-10-11T23:16:27Z (15 years ago)
From
Stephen Holland at USRA/NASA/GSFC/SSC <Stephen.T.Holland@nasa.gov>
S. T. Holland (CRESST/GSFC/USRA) and M. De Pasquale (UCL-MSSL)
report on the behalf of the Swift UVOT team:
The Swift/UVOT observed the field of GRB 101011A starting 66 s
after the BAT trigger (Cannizzo, et al., 2010, GCN Circ. 11331).
Settled observations started at 85 s. We detect an optical source
that may be fading and is not present in the USNO-B1.0 catalogue,
2MASS point source catalogue, or the DSS. The preliminary UVOT
position is:
RA (J2000) = 03:13:10.47 = 48.29363 (deg)
Dec (J2000) = -65:58:54.7 = -65.98186 (deg)
with an estimated uncertainty of 1.14 arcsec (radius, 90% confidence,
statistical + systematic). This is 1.84 arcsec west of the
UVOT-enhanced XRT position (Evans, et al., 2010, GCN Circ. 11333).
Preliminary white magnitudes and 3-sigma upper limits for
the source are:
Filter T_start T_stop Exp(s) Mag Err
-----------------------------------------------------------
white (fc) 85 235 147 21.38 0.34
white 876 1025 147 >21.7
-----------------------------------------------------------
The quoted magnitudes and upper limits have not been corrected
for the expected Galactic extinction along the line of sight
corresponding to a reddening of E_{B-V} = 0.03 mag (Schlegel, et al.,
1998, ApJS, 500, 525). All photometry is on the UVOT photometry
system described in Poole et al. (2008, MNRAS, 383, 627).
GCN Circular 11335
Subject
GRB 101011A: XRT Refined Analysis
Date
2010-10-11T23:26:10Z (15 years ago)
From
Antonia Rowlinson at U.of Leicester <bar7@star.le.ac.uk>
A. Rowlinson (U. Leicester) and J. K. Cannizzo (NASA/UMBC) report on
behalf of the Swift-XRT team:
We have analysed 3.9 ks of XRT data for GRB 101011A (Cannizzo et al. GCN
Circ. 11331), from 66 s to 7.2 ks after the BAT trigger. The data
comprise 86 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et al.
(GCN. Circ 11333).
The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=0.8 (+0.5, -1.7). At T+116 s the decay
steepens to an alpha of 2.49 (+0.18, -0.19) before breaking again at
T+656 s to a final decay with index alpha=1.13 (+0.28, -0.25).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.41 (+0.20, -0.19). The
best-fitting absorption column is 7.6 (+6.0, -4.3) x 10^20 cm^-2,
consistent with the Galactic value of 3.3 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.94 (+0.26, -0.30)
and a best-fitting absorption column of 1.5 (+/-0.8) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 4.2 x 10^-11 (5.7 x 10^-11) erg cm^-2
count^-1.
If the light curve continues to decay with a power-law decay index of
1.13, the count rate at T+24 hours will be 4.2 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.8 x
10^-14 (2.4 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/00436094.
This circular is an official product of the Swift-XRT team.
GCN Circular 11336
Subject
GRB 101011A: Zadko observatory - Gingin optical observations
Date
2010-10-12T09:07:35Z (15 years ago)
From
Bruce Gendre at ASDC <bruce.gendre@asdc.asi.it>
M. Laas-Bourez(UWA/ICRAR), D. Coward(UWA), D. Blair (UWA),
B. Gendre (ASDC/OAR), M. Boer (OHP-CNRS), A. Klotz (CESR-UPS-CNRS), P.
Thierry (CESR-UPS-CNRS) report:
We imaged the field of GRB 101011A detected by SWIFT
(trigger 436094) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.
The observations started 3932.8s after the GRB trigger
(3910s after the notice). The elevation of the field increased from
55 degrees above horizon and weather conditions
were good with a high level of humidity.
30 images have been maded with a duration of 180.0s each
(see the description in Klotz et al., 2006, A&A 451, L39).
At the position of the XRT afterglow (Evans et al., GCN 11333), we do
not detect any source with a limiting magnitude of g> 19.5
on the single images.
We co-added a series of exposures between t0+3932.8s to t0+9869.4s
We do not detect any afterglow, with a limiting magnitude of g> 21.5
Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.
N.B. Galactic coordinates are lon=283.3069 lat=-45.3657
This message may be cited.
GCN Circular 11337
Subject
GRB 101011A, GROND upper limits
Date
2010-10-12T13:43:38Z (15 years ago)
From
Sylvio Klose at TLS Tautenburg <klose@tls-tautenburg.de>
M. Nardini, T. Kruehler (both MPE Garching), S. Klose, A. Rossi (both TLS
Tautenburg), and J. Greiner (MPE Garching) report on behalf of the GROND
team:
We observed the field of GRB 101011A (Swift trigger #436094; Cannizzo et
al. 2010, GCN #11331; Markwardt et al. 2010, GCN #11332) simultaneously in
g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the
2.2 m MPI/ESO telescope on LaSilla. Observations started at 00:10 UT,
October 12, i.e. seven hours after the burst once the field became visible
over La Silla.
In stacked images with a mid-time of 1:06 UT (seeing 2.2 arcsec; mean
airmass 1.8) we do not detect any source at the position of the faint
optical transient seen by UVOT (Holland et al. 2010, GCN #11334) down to
the following limits (3 sigma, AB system):
g' > 24.4,
r' > 23.7,
i' > 22.7,
z' > 22.5,
J > 22.1,
H > 21.5.
These upper limits have been calibrated based on USNO and 2MASS stars.
GCN Circular 11338
Subject
GRB 101011A: Swift/UVOT observations
Date
2010-10-12T14:08:49Z (15 years ago)
From
Massimiliano de Pasquale at MSSL-UCL <mdp@mssl.ucl.ac.uk>
M. De Pasquale (MSSL-UCL) and J. Cannizzo (GSFC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 101011A
85s after the BAT trigger (Cannizzo et al., GCN Circ. 11331).
Summing up white band exposures up to 1374s after the trigger, including
the finding chart, we find a strong indication (2.9 sigma level) of an
uncatalogued source at
���������� RA = 03h 13m 10.77s, Dec = -65d 58m 54.0s (J2000)
���������� RA = 48.29487, Dec = -65.98167 (J2000)
with an error of 1.1 arcseconds. This refined position is within 0.5
arcseconds from the XRT refined position (Evans et al., GCN Circ. 11333)
and supersedes the previous onegiven in Holland et al. (GCN Circ. 11334).
In the individual and summed UVOT exposures in other filters, no optical
afterglow is detected.� Preliminary 3-sigma upper limits using the UVOT
photometric system (Poole et al. 2008, MNRAS, 383, 627) for the first
finding chart (FC) exposure and subsequent exposures are:
Filter�������� T_start(s)�� T_stop(s)����Exp(s)����Mag
white(FC)���������� 85��������� 235������147 >21.3
white���������������85������� 1374������373���21.7 � 0 0.4
white�������������4311���� �� 6627������393 >22
v������������������627�� � ��18725�����1375 >20.8
b������������������533����� 41918�����1055 >21.4
u������������������297����� 41737�����2865 >22.0
uw1��������������� 577������ 47696�����2595 >21.7
um2��������������� 652����� 46017�����2996 >21.7
uw2��������������� 603������ 17812����� 376 >21.5
The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 11343
Subject
GRB 101011A: BOOTES-3 Upper Limit
Date
2010-10-16T10:14:45Z (15 years ago)
From
Juan Carlos Tello at IAA-CSIC <jtello@iaa.es>
J.C. Tello, M. Jelinek, A.J. Castro-Tirado, J. Gorosabel (IAA-CSIC,
Granada), A, de Ugarte Postigo (DARK/NBI), W. Allen (Vintage Lane Obs.),
Ph. Yock and Kuan-Yu Lin (Auckland Univ.), report on behalf of a larger
collaboration:
"We have carried out observations of the Swift GRB 101011A (Cannizzo et
al. GCNC 11331) on Oct 12.4751 - 12.6972 UT (~23.76 hr after the onset of
the burst, mean observing time) with the 0.6m Yock-Allen robotic telescope
(BOOTES-3) located in Blenheim, New Zealand.
We do not detect any optical source within the Swift-XRT refined error
circle (Evans et al. GCNC 11333).
The 3 sigma limiting magnitude of the co-added unfiltered image
(Texp=165x60s) is R ~ 19.0, using USNO-B1.0 as photometric reference.
GCN Circular 11344
Subject
GRB 101011A: Fermi GBM detection
Date
2010-10-16T23:51:41Z (15 years ago)
From
Michael Burgess at UAH <james.burgess@uah.edu>
Michael Burgess (UAH)
reports on behalf of the Fermi GBM Team:
"At 16:58:36.53 UT on 11 October 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101011A (trigger 308509118 /101011707) which
was
also detected by the SWIFT-BAT (Cannizzo et al. 2010, GCN 11331)
The GBM on-ground location is consistent with the Swift position.
This burst was also independently detected by INTEGRAL SPI-ACS.
The angle from the Fermi LAT boresight is 144 degrees.
The GBM light curve consists of a several moderately bright
peaks with a duration (T90) of about 35.01 s (8-1000 keV).
The time-averaged spectrum from T0-0.768 s to T0+35.78 s is
best fit by a power law function with an exponential
high energy cutoff. The power law index is -.49 +/- .25 and
the cutoff energy, parameterized as Epeak, is 296.6 +/- 49.4 keV
The event fluence (8-1000 keV) in this time interval is
(5.24 +/- .39)E-6 erg/cm^2. The .256-sec peak photon flux measured
starting from T0+25.15 s in the 8-1000 keV band
is 5.16 +/- 1.6 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
________________________________
J. Michael Burgess
University of Alabama - Huntsville
National Space Science and Technology Center
james.m.burgess@nasa.gov
256.792.8423
ICQ: 573311449
________________________________
J. Michael Burgess
jmichaelburgess@gmail.com
256.792.8423
GCN Circular 11362
Subject
GRB 101011A: miniTAO/ANIR NIR upper limits
Date
2010-10-23T01:17:30Z (15 years ago)
From
Takeo Minezaki at U.of Tokyo/Astro <minezaki@mtk.ioa.s.u-tokyo.ac.jp>
M. Konishi, T. Morokuma, S. Koshida, N. Matsunaga,
T. Minezaki, and Y. Yoshii (University of Tokyo)
report on behalf of the TAO project team:
We observerd GRB 101011A (Cannizzo et al., GCN 11331) with
the near-infrared camera ANIR mounted on the miniTAO 1.0m
telescope at the University of Tokyo Atacama Observatory
on the summit of Co. Chajnantor (5640m altitude) in
the northern Chile.
The Ks-band observation started from 2010-10-13 06:20 UT
(38hours after the burst), and total exposure time was
1620sec. No object was detected within the enhanced XRT
error circle (Evans et al., GCNC 11333).
The three sigma upper limit is listed below, where the flux
calibration was carried out using 2MASS stars within the FoV.
Band Mid-UT AB-Mag
----------------------------
Ks 06:35:02 >19.7
----------------------------