GRB 100513A
GCN Circular 10820
Subject
GRB 100513A: CrAO optical observations
Date
2010-06-01T20:26:58Z (16 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
V. Rumyantsev (CrAO), A. Pozanenko (IKI) report on behalf of larger GRB
follow-up collaboration:
We observed the field of the Swift GRB 100513A (Baumgartner et al. GCN
10746)
with Shajn telescope of CrAO in R-filter between May, 13 (UT) 18:43 --
20:38, and in I-filter on May, 14 (UT) 19:47 -- 20:57 and on May, 16 (UT)
18:28 -- 20:20.
The afterglow (Morgan et al. GCN 10747) is clearly detected on May, 13,14
and not detected on May 16. The afterglow coordinates are (J2000) RA = 11 18
26.85 Dec = +03 37 40.3 with uncertainty of 0.3 arcsec.
The photometry of stacked images based on USNO-B1.0 star 0936-0206849
(RA(J2000) = 11:18:37.91 Dec(J2000)= +03:37:43.1) assuming R=18.59
I=17.88 is following:
T0+ Filter, Exposure, mag. Upper Limit
(mid, d) (s)
0.7313 R 104x60 23.03 +/- 0.12 24.3
1.7573 I 64x60 21.59 +/- 0.07 23.6
3.7202 I 91x60 >23.5 23.5
The combined images can be found at http://grb.rssi.ru/GRB100513A/
Using above photometry combined with reported earlier (R = 21.39 at 2.46
hours, GCN 10750; J-filter photometry in GCNs 10747, 10749; i'=21.3 at 9.89
hours, GCN 10757) one can suggest taht power law index of decay light curve
in J, R and I- bandpass is compatible and equal to ~0.7 in the first day.
The break of power law can be assumed in I-band between first and third days
with power law decay index > 2.
GCN Circular 10774
Subject
GRB 100513A: MITSuME Akeno Optical Observation
Date
2010-05-18T13:50:13Z (16 years ago)
From
Yoichi Yatsu at Tokyo Tech. <yatsu@hp.phys.titech.ac.jp>
Y.Yatsu, H. Nakajima, T. Enomoto, K. Kawakami,
K. Tokoyoda, Shimokawabe, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:
We observed the field of GRB100513A (Baumgartner et al. GCNC 10746)
with the three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50 cm optical telescope at Akeno, Japan.
The observation started at 2010-05-13 11:07:42 UT.
On the combined images, we could not find the optical counterpart
in the XRT error circle (GCN 10746) in the three bands.
The 3-sigma upper limits based on the GSC2.3 catalog are listed below:
Start(UT) -- END(UT) Total EXP[sec] g' Rc Ic
----------------------------------------------------------------
11:07:42.1 -- 11:32:45.1 540.0 >18.9 >18.8 >18.3
14:23:16.8 -- 14:50:38.0 960.0 >17.8 >18.0 >17.4
14:50:46.5 -- 15:36:25.0 2220.0 > 19.1 > 19.0 > 18.4
----------------------------------------------------------------
GCN Circular 10768
Subject
GRB 100513A: EVLA radio observation
Date
2010-05-16T22:59:55Z (16 years ago)
From
Poonam Chandra at Royal Mil. College Canada <Poonam.Chandra@rmc.ca>
Poonam Chandra (RMC) and Dale A=2E Frail (NRAO) report on behalf of a
larger collaboration:
We observed GRB 100513A (Baumgartner et al. GCN 10746) with the
Expanded Very Large Array (EVLA) on May 14.02 UT at a center frequency
of 8.46 GHz. We do not detect any radio source anywhere within the
refined XRT error circle (Evans et al., GCN 10751) to a 3-sigma limit
of 60 uJy. The peak flux at the PAIRITEL afterglow position (Morgan et al.,
GCN 10747) is -43+/-20 uJy.
The EVLA is still undergoing active commissioning and we caution that
these results should be considered preliminary=2E The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities=2C Inc.
GCN Circular 10757
Subject
GRB 100513A: Faulkes Telescope South observations
Date
2010-05-13T16:15:41Z (16 years ago)
From
Cristiano Guidorzi at Ferrara U,Italy <guidorzi@fe.infn.it>
C. Guidorzi (U. Ferrara) & A. Gomboc (U. Ljubljana)
report on behalf of a large collaboration:
On 2010 May 13 at 11:44:17 UT the 2-m Faulkes Telescope
South began observing the Swift GRB 100513A (Baumgartner
et al., GCN Circ. 10746) using the i' filter,
corresponding to 9.6 hr after the burst trigger time.
We clearly detect the NIR afterglow (Morgan et al.
GCN Circ. 10747, 10749) with the following magnitude:
Mid time from Total Exp Filter Magnitude
trigger (hr) (s)
-------------------------------------------------
9.89 6x300 i' 21.3 +- 0.2
-------------------------------------------------
Magnitude has been calibrated from nearby SDSS stars.
GCN Circular 10756
Subject
GRB 100513A: Swift/UVOT upper limits
Date
2010-05-13T16:01:19Z (16 years ago)
From
Erik Hoversten at Swift/Penn State <hoversten@astro.psu.edu>
E. A. Hoversten (PSU) 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
100513A 130s after the BAT trigger (Baumgartner et al., GCN 10746).
We do not detect any source at the enhanced Swift XRT position
(Evans et al., GCN 10751) nor at the position of the PAIRITEL NIR
detection (Morgan et al., GCN 10747). UVOT magnitude 3-sigma
upper limits are reported in the following table:
Filter T_start T_stop Exp(s) Mag (3-sigma upper limit)
-------------------------------------------------------------
white 130 1707 411 > 21.29
v 618 1757 136 > 19.02
b 544 1683 116 > 19.89
u 289 1658 343 > 20.22
uvw1 667 1462 97 > 19.33
uvm2 5000 5200 196 > 19.59
uvw2 6026 6226 196 > 20.03
The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight of E_(B-V) = 0.05 mag
(Schlegel et al. 1998). All photometry is on the UVOT photometric
system described in Poole et al. (2008, MNRAS, 383, 627).
GCN Circular 10755
Subject
GRB 100513A, RIMOTS optical upper limits
Date
2010-05-13T15:06:18Z (16 years ago)
From
Kazuhiro Noda at Miyazaki U <kaz1206@astro.miyazaki-u.ac.jp>
K.Noda, N.Ohmori, A.Daikyuji, Y.Nisioka, M.Yamauchi
(University of Miyazaki)
We have observed the field covering the error circle of
GRB GRB100513A (Swift trigger 421814, GCN 10746(Baumgartner et al.),
GCN 10746(Morgan et al.), GCN 10751(Evans et al.))
with the unfiltered CCD camera on the 30-cm telescope
at University of Miyazaki.
The observation was started 12:52:15 UT, about 10.7 hr
after the Swift trigger time.
We have compared our data of 30 sec exposures
with the USNO-A2.0 catalog,
There is no new source at the reported position.
(GCN 10746(Baumgartner et al.), GCN 10746(Morgan et al.), GCN 10751(Evans et al.))
the upper limits are as follows:
--------------------------------------------------------------
Start(UT) End(UT) Num. of frames Limit (mag.)
--------------------------------------------------------------
12:52:15 12:52:45 1 14.05
12:52:15 13:51:11 42 16.78
---------------------------------------------------------------
GCN Circular 10754
Subject
GRB 100513A: Swift XRT refined analysis
Date
2010-05-13T14:32:45Z (16 years ago)
From
Vanessa Mangano at INAF-IASFPA <vanessa@ifc.inaf.it>
V. Mangano (INAF IASF Pa), B. Sbarufatti (INAF IASF Pa, INAF OAB)
report on behalf the Swift XRT team:
We have analysed the first four orbits of XRT data of GRB 100513A
(Baumgartner et al. in GCN Circ. 10746),
consisting of 154 s exposure in Windowed Timing mode
(from T+130 s to T+284 s) and 9 ks exposure in Photon Counting
mode (from T+285 s to T+19 ks).
The UVOT-enhanced XRT position was given by Evans et al.
in GCN Circ. 10751.
After an initial flaring activity the light curve can be modelled
with a power-law decay with an index of alpha=3.3 +/- 0.15
followed by a break at 714 +/- 40 s to an alpha=0.78 +/- 0.04.
A spectrum formed from the WT[PC] mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.0+/-0.2 [2.3+/-0.2].
The best-fitting absorption column at the estimated redshift z=4.8
(Cenko et al. in GCN Circ. 10752) is 1.9 +/- 1.1 x 10^22 cm^-2,
in excess of the Galactic value of 4.2 x 10^20 cm^-2 (Kalberla et al.
2005).
Uncertainties are given at 90% c.l.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from these spectra is 3.4 x 10^-11 (4.3 x 10^-11) erg cm^-2
count^-1.
If the light curve continues to decay with a power-law decay index of
0.78, the count rate at T+24 hours will be 0.004 count s^-1, corresponding
to an observed (unabsorbed) 0.3-10 keV flux of 1.4 x 10^-13 (1.7 x 10^-13)
erg cm^2-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00421814.
This circular is an official product of the Swift-XRT team.
GCN Circular 10753
Subject
GRB 100513A: Swift-BAT refined analysis
Date
2010-05-13T11:16:24Z (16 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
T. N. Ukwatta (GWU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
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)
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 100513A (trigger #421814)
(Baumgartner, et al., GCN Circ. 10746). The BAT ground-calculated position is
RA, Dec = 169.606, 3.617 deg, which is
RA(J2000) = 11h 18m 25.5s
Dec(J2000) = +03d 37' 00.4"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 90%.
The mask-weighted light curve shows multiple overlapping peaks starting
at ~T-40 sec, peaking around T_zero, and ending at ~T+60 sec with a weak
tail extending out to around T+180 sec. T90 (15-350 keV) is 84 +- 21 sec
(estimated error including systematics).
The time-averaged spectrum from T-64.1 to T+44.6 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.62 +- 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+1.09 sec in the 15-150 keV band
is 0.6 +- 0.1 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/421814/BA/
GCN Circular 10752
Subject
GRB 100513A: Gemini/GMOS Spectroscopic Redshift
Date
2010-05-13T07:39:53Z (16 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. B. Cenko, D. A. Perley, A. N. Morgan, C. R. Klein, J. S. Bloom, N. R.
Butler, and B. E. Cobb (UC Berkeley) report on behalf of a larger
collaboration:
We have obtained an optical spectrum of the afterglow (Morgan et al., GCN
10747) of GRB 100513A (Baumgartner et al., GCN 10746) with the Gemini
Multi-Object Spectrograph mounted on the 8 m Gemini North
telescope. Observations began at 6:13 UT on 13 May (~ 4.1 hours after the
GRB) and cover the wavelength range from 6000-10000 A.
The spectrum exhibits a strong break at approximately 7000 A which we
associate with a damped Ly-alpha system at z ~ 4.8. We identify a series
of narrow absorption features redward of Ly-alpha, including O I 1302, Si
II 1304, C II 1334, C II* 1335, Si IV 1393, 1402, Si II 1526, and C IV
1548, 1550 all at a common redshift of z = 4.772. The presence of C II*,
along with Ly-alpha forest continuum emission blueward of 7000 A, strongly
suggest this is the redshift of the GRB host galaxy.
The presence of the Ly-alpha break at 7000 A further explains the
relatively faint R-band afterglow observed by Perley et al (GCN 10750;
also Updike et al., GCN 10748).
We wish to thank the entire Gemini staff, in particular Richard McDermid,
for the prompt execution of these observations.
GCN Circular 10751
Subject
GRB 100513A: Enhanced Swift-XRT position
Date
2010-05-13T07:12:23Z (16 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 3728 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 100513A, 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 = 169.61169, +3.62774 which is equivalent
to:
RA (J2000): 11h 18m 26.81s
Dec (J2000): +03d 37' 39.9"
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.
GCN Circular 10750
Subject
GRB 100513A: Lick observations and R-band dropout
Date
2010-05-13T07:03:07Z (16 years ago)
From
Daniel Perley at U.C. Berkeley <dperley@astro.berkeley.edu>
D. A. Perley, C. R. Klein, and A. N. Morgan (UC Berkeley) report:
We began observing the location of the afterglow of GRB 100513A
(Baumgartner et al., GCN 10746) at 04:06 UT using the Nickel 40-inch
telescope at Lick Observatory. A total of fourteen 300-second images
were acquired in the R-band under clear sky conditions.
A co-add of the first 9 images (midpoint 04:35 UT) reveals a faint point
source at the position reported by Morgan et al (GCN 10747). The source
is near the detection limit of the co-add and is not detected in
individual images.
Photometry of the object relative to three nearby SDSS stars (converted
to Rc via the Lupton transformation equation) gives the following magnitude:
R = 21.39 +/- 0.25 (t_mid = 2.46 hours)
We note that this is significantly fainter than expected from the
preliminary JHK magnitudes of Morgan et al (GCN 10749). The IR spectral
index is relatively flat (beta~0.5), suggesting little host extinction.
Assuming no extinction in addition to the Galactic value, a direct
power-law extrapolation of the JHK data to R-band over-predicts the
observed flux by >2 magnitudes, strongly suggesting an R-band dropout
and likely redshift of 4.6 < z < 6.0. We note also that the X-ray
column is consistent with no absorption beyond Galactic (Baumgartner et
al.), consistent with a high-redshift origin.
We encourage I/z/Y-band follow-up to better constrain the redshift and
dust extinction. Spectroscopic observations are planned.
GCN Circular 10749
Subject
GRB 100513A: PAIRITEL continued observations and confirmation of fading
Date
2010-05-13T06:36:33Z (16 years ago)
From
Adam Morgan at U.C. Berkeley <qmorgan@gmail.com>
A. N. Morgan, D. A. Perley, C. R. Klein, and J. S. Bloom (UC Berkeley) report:
We continued to observe the location of GRB 100513A (Baumgartner et al.,
GCN 10746) with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona.
The candidate afterglow (Morgan et al., GCN 10747) is detected in all
three filters (J, H, and Ks) in the first epoch. The source fades
between epochs, confirming that this is indeed the afterglow of GRB
100513A.
The preliminary photometry yields:
post burst
t_mid (hr) exp.(s) filt mag m_err
0.99 1030 J 17.8 0.1
0.99 1030 H 17.2 0.1
0.99 1030 Ks 16.4 0.2
1.68 1685 J 18.0 0.1
1.68 1685 H 17.6 0.1
2.72 2855 J 18.4 0.2
All magnitudes are given in the Vega system, calibrated to 2MASS. No
correction for Galactic extinction has been made to the above reported
values.
[GCN OPS NOTE(13may10): Per author's request, the Palmer reference
was change to the Baumgartner reference.]
GCN Circular 10748
Subject
GRB 100513A: SARA-N Upper Limit
Date
2010-05-13T05:26:18Z (16 years ago)
From
Adria C. Updike at Clemson U <aupdike@clemson.edu>
Adria C. Updike, Dieter H. Hartmann (Clemson University) and Tomomi Otani
(FIT) report:
We observed the field of GRB 100513A (Baumgartner et al., GCN 10746)
beginning 1 hour and 55 minutes after the burst with the SARA-North 0.9m
telescope located at KPNO. We do not detect the afterglow candidate
(Morgan et al., 10747) in 4 minutes of stacked exposures in each of the R
and I bands to a limiting magnitude of 19.5 in R and 19 in I (as compared
to the USNO B1.0 catalog).
GCN Circular 10747
Subject
GRB 100513A: PAIRITEL NIR afterglow candidate
Date
2010-05-13T03:48:19Z (16 years ago)
From
Adam Morgan at U.C. Berkeley <qmorgan@gmail.com>
A. N. Morgan, D. A. Perley, C. R. Klein, and J. S. Bloom (UC Berkeley) report:
We observed the location of GRB 100513A (Baumgartner et al., GCN 10746)
with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations
began at 2010-05-13 03:03:07 UT, ~0.77 hours after the Swift Trigger,
after sunset. In mosaics (effective exposure time of 0.92 hours)
taken simultaneously in the J, H, and Ks filters, we detect a NIR
source within the XRT error circle at a location:
11:18:26.8, +03:37:40 (J2000)
The preliminary photometry yields:
post burst
t_mid (hr) exp.(s) filt mag m_err
0.93 772 J 17.7 0.1
All magnitudes are given in the Vega system, calibrated to 2MASS. No
correction for Galactic extinction has been made to the above reported
values.
[GCN OPS NOTE(13may10): Per author's request, the Palmer reference
was change to the Baumgartner reference.]
GCN Circular 10746
Subject
GRB 100513A: Swift detection of a burst
Date
2010-05-13T02:23:42Z (16 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
H. A. Krimm (CRESST/GSFC/USRA), R. Margutti (INAF-OAB),
C. B. Markwardt (CRESST/GSFC/UMD), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the
Swift Team:
At 02:07:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100513A (trigger=421814). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 169.580, +3.605 which is
RA(J2000) = 11h 18m 19s
Dec(J2000) = +03d 36' 19"
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 50 sec. The peak count rate
was ~1000 counts/sec (15-350 keV), at ~5 sec after the trigger.
The XRT began observing the field at 02:09:15.5 UT, 126.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued,
fading X-ray source with an enhanced position: RA, Dec 169.6119, 3.6272 which
is equivalent to:
RA(J2000) = 11h 18m 26.86s
Dec(J2000) = +03d 37' 38.1"
with an uncertainty of 2.5 arcseconds (radius, 90% containment). This
location is 139 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
4.19e+20 cm^-2 (Kalberla et al. 2005).
UVOT took a finding chart exposure of 150 seconds with the White
filter starting 130 seconds after the BAT trigger. No credible
afterglow candidate has been found in the initial data products. The
XRT position is outside of the 2.7'x2.7' sub-image. 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 0.05.
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.)