GRB 100514A
GCN Circular 10819
Subject
GRB 100514A: CrAO optical observations
Date
2010-06-01T20:19:58Z (15 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 re-observed the field of the Swift GRB 100514A (Markwardt et al. GCN
10759) with Shajn telescope of CrAO in filter I between (UT) May, 16 23:21
and May, 17 00:54. We do not detect the afterglow of GRB 100514A (Marshall
et al, GCN 10766; Rumyantsev et al, GCN 10767).
The upper limit based on USNO-B1.0 star 1191-0563318 (J2000) RA=
21:55:19.80 Dec= +29:10:10.0 (assuming I=18.09) is following:
T0+ Filter, Exposure, mag.
(mid, d) (s)
2.2182 I 64x60 >22.9
The combined images can be found http://grb.rssi.ru/GRB100514A/
GCN Circular 10767
Subject
GRB 100514A: optical afterglow confirmation
Date
2010-05-16T21:42:21Z (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 100514A (Markwardt et al. GCN 10759)
with Shajn telescope of CrAO between (UT) May 15 00:04:38 and 15T01:10:33
under good weather conditions and mean seeing of 2 arcsec. Inside the
enhanced XRT error circle (Goad et al. GCN 10762) we detect the object with
coordinates
RA(J2000): 21 55 17.46
Dec(J2000): +29 09 36.13
with uncertainties of 0.3" in each coordinates.
The photometry of the object based on USNO-B1.0 star 1191-0563318 (J2000)
RA= 21:55:19.80 Dec= +29:10:10.0 (assuming R2=19.25) is following:
T0+ Filter, Exposure, mag.
(mid, d) (s)
0.2390 R 57x60 23.2 +/- 0.2
The afterglow candidate reported by Marshall and Markwardt (GCN 10766) is
fading by ~2 mag. within 5.7 hours, and hence we confirm the afterglow.
GCN Circular 10766
Subject
GRB 100514A: Swift/UVOT Observations
Date
2010-05-15T16:12:01Z (16 years ago)
From
Frank Marshall at GSFC <marshall@milkyway.gsfc.nasa.gov>
F.E. Marshall (NASA/GSFC) and C.B. Markwardt (CRESST/GSFC/UMD)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 100514A
110 s after the BAT trigger (Markwardt et al., GCN Circ. 10759).
There is a marginal (2.6-sigma) detection of a possible optical
afterglow at the enhanced XRT position
(M.R. Goad et al., GCN Circ. 10762) in the first white finding chart.
There is no detection in any of the other initial UVOT exposures.
Preliminary results (3-sigma upper limits or values with 1-sigma uncertainties)
using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the finding chart (FC)
exposures and summed subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 110 260 147 21.1 +/- 0.3
u_FC 268 518 246 >20.2
white 549 7708 516 >21.0
v 600 6843 529 >20.0
b 524 7666 529 >20.5
u 268 7459 775 >20.5
w1 650 7254 529 >21.0
m2 624 7048 529 >20.2
w2 574 6639 352 >19.9
The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.10 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 10765
Subject
GRB 100514A: YNAO-GMG observations
Date
2010-05-15T15:04:17Z (16 years ago)
From
Jirong Mao at INAF-OAB <jirong.mao@brera.inaf.it>
J. Mao (YNAO & INAF-OAB) and J. Bai (YNAO) report on behalf of the GMG group:
Starting from 19h 49m 49s UT, after about 1 hour of the GRB trigger, we observed the field of GRB 100514A (Markwardt et al. GCN 10759) with one 2.4-m telescope located at Gao-Mei-Gu (GMG). We did not find any optical afterglows in a series of R-band images. The magnitude limit(relative to USNO-B1) is about 20.6.
This message might be cited.
GCN Circular 10764
Subject
GRB 100514A: Swift XRT refined analysis
Date
2010-05-15T09:49:49Z (16 years ago)
From
Giulia Stratta at ASDC <giulia.stratta@gmail.com>
G. Stratta (ASDC), V. D'Elia (ASDC) and C. B. Markwardt (CRESST/GSFC/UMD)
report on behalf of the Swift-XRT team:
We have analysed 24.9 ks of XRT data for GRB 100514A (Markwardt et al. GCN
Circ. 10759), from 91 s to 25.0 ks after the BAT trigger. The data comprise
82 s in Windowed Timing (WT) mode (the first 9 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 Goad et al. (GCN. Circ 10762).
The light curve can be modelled with a broken power-law decay with decay
indices of alpha_1 = 5.15 +/- 0.15, alpha_2 = 0.55 +/- 0.20 and a break
at t = 560+/-60 sec after the trigger.
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.96 (+0.18, -0.17). The
best-fitting absorption column is 2.9 (+/-0.3) x 10^21 cm^-2, in excess of
the Galactic value of 7.7 x 10^20 cm^-2 (Kalberla et al. 2005). The counts
to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum is 2.1 x 10^-11 (2.0 x 10^-10) erg cm^-2 count^-1. The spectrum
softens in the PC mode data to a photon spectral index of 2.74 (+0.46,
-0.44) with a best-fitting column of 5.4 (+6.5, -2.9) x 10^20 cm^-2 in
excess
of the Galactic value. The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum is now 2.9 x 10^-11 (5.5 x
10^-11) erg cm^-2 count^-1.
Uncertainties are given at 90% confidence level.
If the light curve continues to decay with a power-law decay index of 0.55,
the count rate at T+24 hours will be 1.8 x 10^-3 count s^-1, corresponding
to an observed (unabsorbed) 0.3-10 keV flux of 5.2 x 10^-14 (9.9 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/00421962.
This circular is an official product of the Swift-XRT team.
GCN Circular 10763
Subject
GRB 100514A: MASTER-Net optical observations
Date
2010-05-15T07:20:45Z (16 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V.Krushinski, I.Zalozhnih, T.Kopytova, A.Popov
Ural State University, Kourovka
E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, A.Sankovich
Sternberg Astronomical Institute, Moscow State University
K.Ivanov, S.Yazev, N.M.Budnev, E.Konstantinov, V.Lenok, O.Gres,
O.Chuvalaev
Irkutsk State University
V.Yurkov, Yu.Sergienko, D.Varda, A.Garusina Blagoveschensk Educational State
University, Blagoveschensk
A. Tlatov, A.V. Parkhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located at Kourovka Observatory (Ural) was responted to the
GRB 100514A (Swift Bat alert, Markwardt et al, GCN CIRC 10759) 25 sec
after Notice time and 71 s after the GRB time.
There is no OT on the first 20-s exposition time unfiltered images inside
Swift XRT error box (Goad et al., GCN CIRC 10762)
brighter 17.0.
The message may be cited.
mailto: lipunov@sai.msu.ru
GCN Circular 10762
Subject
GRB 100514A: Enhanced Swift-XRT position
Date
2010-05-15T03:19:02Z (16 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.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 1720 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 100514A, 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 = 328.82257, +29.16001 which is equivalent
to:
RA (J2000): 21h 55m 17.42s
Dec (J2000): +29d 09' 36.0"
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 10761
Subject
GRB 100514A: Swift-BAT refined analysis
Date
2010-05-15T01:48:18Z (16 years ago)
From
Craig Markwardt at NASA/GSFC/UMD <craigm@milkyway.gsfc.nasa.gov>
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), 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 100514A (trigger
#421962) (Markwardt, et al., GCN Circ. 10759). The BAT ground-calculated
position is RA, Dec = 328.757, 29.175 deg, which is
RA(J2000) = 21h 55m 01.7s
Dec(J2000) = +29d 10' 29.8"
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 76%.
The mask-weighted light curve shows FRED-like peak starting at ~T-2 sec,
peaking at ~T+7 sec, and ending at ~T+38 sec. T90 (15-350 keV) is 26.2
+- 8.2 sec (estimated error including systematics).
The time-averaged spectrum from T+0.3 to T+30.8 sec is best fit by a
simple power-law model. The power law index of the time-averaged
spectrum is 1.97 +- 0.25. The fluence in the 15-150 keV band is 4.0 +-
0.7 x 10-7 erg/cm2. The 1-sec peak photon flux measured from T+6.23 sec
in the 15-150 keV band is 0.6 +- 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/421962/BA/
GCN Circular 10760
Subject
GRB 100514A: Faulkes Telescope South observations
Date
2010-05-14T21:58:05Z (16 years ago)
From
Carole Mundell at ARI, JMU,Liverpool <cgm@astro.livjm.ac.uk>
C.G. Mundell, R.J. Smith (Liverpool JMU), C. Guidorzi (U. Ferrara), A. Gomboc
(U. Ljubljana) report on behalf of a large collaboration:
"On 2010 May 14 at 18:57:31.55 UT the 2-m Faulkes Telescope South began
observing Swift GRB 100514A (Markwardt et al., GCN Circ. 10759) at
3.55 min after the GRB trigger time.
No optical afterglow is detected in R or i'-band filters to the following
limits (relative to the USNO-B1) derived from co-added images:
Mid time from Filter Limiting Magnitude
trigger (min)
------------------------------------------------
34.36 R > 20.3
38.55 i' > 19.5
------------------------------------------------
We note that our limits seem to support a relatively high z for this burst,
rather than a nearby extinguished afterglow, consistent with the lack of
additional column density in the X-ray spectrum. Further followup observations
are encouraged."
GCN Circular 10759
Subject
GRB 100514A: Swift detection of a burst
Date
2010-05-14T19:05:55Z (16 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
C. B. Markwardt (CRESST/GSFC/UMD), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
S. Campana (INAF-OAB), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), C. Guidorzi (U Ferrara),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
W.B Landsman (GSFC), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
M. Perri (ASDC), T. Sakamoto (NASA/UMBC), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC), M. A. Stark (PSU),
R. L. C. Starling (U Leicester), G. Stratta (ASDC),
T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the
Swift Team:
At 18:53:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100514A (trigger=421962). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 328.821, +29.170 which is
RA(J2000) = 21h 55m 17s
Dec(J2000) = +29d 10' 13"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows a few overlapping peaks
with a duration of about 30 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 18:55:39.5 UT, 101.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright, fading
uncatalogued X-ray source located at RA, Dec 328.82244, 29.15989 which
is equivalent to:
RA(J2000) = 21h 55m 17.39s
Dec(J2000) = +29d 09' 35.6"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 36 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
7.74e+20 cm^-2 (Kalberla et al. 2005).
The initial flux in the 2.5 s image was 4.16e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 110 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
0.10.
Burst Advocate for this burst is C. B. Markwardt (Craig.Markwardt 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/too.html.)