GRB 100814A
GCN Circular 11153
Subject
GRB 100814A: Maidanak optical observations
Date
2010-08-27T20:30:05Z (15 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (SAI MSU), A. Pozanenko (IKI), O. Vozyakova (SAI MSU), B.
Satovski (Astrotel), M. Im (Seoul National Univ), M. Ibrahimov (MAO) report
on behalf of larger GRB follow-up collaboration:
We observed the field of the Swift GRB 100814A (Beardmore et al. GCN 11087)
with AZT-22 telescope of Maidanak observatory. Several images in R were
obtained starting on Aug. 14 (UT) 22:56:44. We clearly the afterglow
(Schaefer et al. GCN 11086; Beardmore et al. GCN 11087). The photometry of
stacked image against USNO-B1.0 field stars is following
t-T0, Filter, Exposure, OT, Upper limit (3 sigma)
(mid, d) (s)
0.81185 R 30*60 18.75+/-0.01 23.4
the photometry error is statistical only.
GCN Circular 11134
Subject
GRB 100814A: Suzaku WAM observation of the prompt emission
Date
2010-08-23T01:12:09Z (15 years ago)
From
Yusuke Nishioka at Miyazaki U. <yusuke613@astro.miyazaki-u.ac.jp>
Y. Nishioka, N. Ohmori, A. Daikyuji, M. Yamauchi (Univ. of Miyazaki),
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.),
N. Vasquez (Tokyo Tech.) K. Yamaoka (Aoyama Gakuin U.), S. Sugita
(Nagoya U.),
Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), Y. Urata, P. Tsai (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo),
S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report:
The long GRB 100814A (Swift/BAT trigger #431605 ; Krimm et al., GCN 11094;
Fermi/GBM trigger #303450610 ; von Kienlin et al., GCN 11099) triggered
the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range
of 50 keV - 5 MeV at 03:50:08.51 UT (=T0).
The observed light curve shows a multi-peaked structure starting at
T0-1.5s, ending
at T0+19.5s, followed by a weaker emission seen up to T0+150.5s with a
duration
(T90) of about 110 seconds. The fluence in 100 - 1000 keV was
7.14(+1.03/-1.37) x 10^-6 erg/cm^2. The 1-s peak flux measured from
T0+0.5s was
2.00(-0.48,+0.40) photons/cm^2/s in the same energy range.
Preliminary result shows that the time-averaged spectrum from T0-1.5s to
T0+150.5s is well fitted by a single power-law with a photon index
of 3.18(+1.03/-0.7) (chi^2/d.o.f = 13.32/15).
All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.
The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html
--
------------------------------------
$B5\:jBg3X(B $B9)3X8&5f2J(B $B1~MQJ*M}3X@l96(B
$B=$;N2]Dx(B $B#2G/(B
$B@>2,!!M42p(B
yusuke613@astro.miyazaki-u.ac.jp
------------------------------------
GCN Circular 11133
Subject
GRB 100814A: ISON-NM optical observations
Date
2010-08-22T07:30:05Z (15 years ago)
From
Leonid Elenin at ISON <l.elenin@gmail.com>
L. Elenin, I. Molotov (ISON), A. Volnova (SAI MSU), A. Pozanenko (IKI)
report on behalf of larger
GRB follow-up collaboration:
We continue observation of the Swift GRB 100814A (Beardmore et al. GCN
11087) with 0.45-m telescope of ISON-NM observatory on Aug. 20 (UT)
08:42:06 - 09:33:14 and Aug. 21 (UT) 09:45:22 - 11:04:41.
The afterglow (Schaefer et al. GCN 11086; Beardmore et al. GCN 11087) is
well detected on stacked images for both epochs. Preliminary photometry of
unfiltered image against USNO-B1.0 star 0720-0016107, assuming R=19.73 is
following:
T-T0, filter, exposure, OT
(day)
6.2205 W 300x10 21.66 +/- 0.23
7.2734 W 300x15 22.50 +/- 0.30
The photometry errors are statistical only.
The images of GRB100814A is available at:
http://spaceobs.org/images/GRB1000814A-3epoch.jpg
GCN Circular 11131
Subject
EVLA radio afterglow detection of GRB 100814A
Date
2010-08-19T23:45:19Z (15 years ago)
From
Poonam Chandra at Royal Mil. College Canada <Poonam.Chandra@rmc.ca>
Poonam Chandra (RMC), Dale A. Frail (NRAO) and S. Bradley Cenko (Berkeley)
report on behalf of a larger collaboration:
"We observed the localization of GRB 100814A (Beardmore et al. GCN
11087) with the Expanded Very Large Array (EVLA) on August 18.38 UT at a
C band wide receiver (receiver frequency range 4-8 GHz). We detect the radio
afterglow of the GRB at the Swift-XRT position (Beardmore et al. GCN
11092) at 4.5 and 7.9 GHz frequencies. The flux densities at
4.5 and 7.9 GHz bands are 198+/-29 uJy and 453+/-23 uJy, respectively.
The EVLA is still undergoing active commissioning and we caution that
these results should be considered preliminary. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc."
GCN Circular 11129
Subject
GRB 100814A: optical observations
Date
2010-08-18T17:23:27Z (15 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
L. Elenin, I. Molotov (ISON), A. Pozanenko (IKI) report on behalf of larger
GRB follow-up collaboration:
We observed the field of the Swift GRB 100814A (Beardmore et al. GCN 11087)
with 0.45-m telescope �f ISON-NM observatory on Aug. 17 (UT) 10:07:17 -
10:48:07.
The afterglow (Schaefer et al. GCN 11086; Beardmore et al. GCN 11087) is
well detected. Preliminary photometry of unfiltered image against USNO-B1.0
field stars (R) is following
T-T0, filter, exposure, OT
(day)
3.2689 W 300x7 19.79 +/- 0.05
the photometry error is statistical only.
GCN Circular 11122
Subject
GRB 100814A : Liverpool Telescope Observations
Date
2010-08-17T10:52:58Z (15 years ago)
From
Zach Cano at ARI/John Moores Liverpool <zec@astro.livjm.ac.uk>
Z. Cano (Liverpool JMU), C. Guidorzi (U.Ferrara) report on behalf of a
larger collaboration:
We observed the optical afterglow of GRB 100814A (Schaefer et al., GCN
11086; Beardmore et al., GCN 11087) with the 2m Liverpool Telescope,
starting at 22:16:09 UT on the 16th of August 2010, in filters r and i.
We clearly detect the afterglow in both filters with the following
magnitudes:
======================================
Filter T-To (days) Mag
--------------------------------------
R 2.96 19.75 +/- 0.02
I 2.93 18.32 +/- 0.04
======================================
The photometric calibration is performed against USNO-B1 objects
0720-0016107 (R2=19.58) and 0719-0016667 (I=17.27). Our detection is
consistent with the values reported by Malesani et al. (GCN 11121).
Observations are ongoing.
GCN Circular 11121
Subject
GRB 100814A: NOT optical observations
Date
2010-08-17T09:33:24Z (15 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani, J.P.U. Fynbo (DARK/NBI), D. Xu (Weizmann Inst.), P.
Jakobsson (Univ. Iceland), L. Buchhave, T. Hansen (NBI), report on behalf of a
larger collaboration:
We observed the optical afterglow of GRB 100814A (Schaefer et al., GCN
11086; Beardmore et al., GCN 11087) with the NOT equipped with ALFOSC.
Observations were carried out in the R band, with a mean time August
17.13 UT (2.97 days after the burst).
The optical afterglow is well detected, with R=19.5 compared to several
USNO stars in the field. The error is about 0.3 mag, completely due to
the scatter in the calibration stars.
[GCN OPS NOTE(17aug10): Per author's request, TH was added to the author list.]
GCN Circular 11119
Subject
Konus-Wind observation of GRB 100814A
Date
2010-08-17T08:48:16Z (15 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:
The long GRB 100814A (Swift-BAT trigger=431605;
Beardmore et al., GCN 11087; Krimm et al., GCN 11094)
triggered Konus-Wind at T0=13811.288s UT (03:50:11.288)
The burst light curve consists of several pulses
with a total duration of ~150 s.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB100814_T13811/
As observed by Konus-Wind the burst
had a fluence of (1.2 +/- 0.2)x10-5 erg/cm2,
and a 256-ms peak flux measured from T0+1.024s
of (0.75 +/- 0.25)x10-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).
The time-integrated spectrum of the burst
(from T0 to T0+155.904 s) is best fit
in the 20 keV - 2 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.4(-0.3, +0.4),
and Ep = 128(-17, +23) keV (chi2 = 59/58 dof).
The spectrum at the maximum count rate
(measured from T0 to T0+8.848 s) is best fit
in the 20 keV - 2 MeV range by a power law
with exponential cutoff model, for which
alpha = 0.55 +/- 0.30,
and Ep = 147(-10, +12) keV (chi2 = 55/58 dof).
All the quoted results are preliminary.
All the quoted errors are at the 90% confidence level.
GCN Circular 11118
Subject
GRB 100814A : Lulin optical observation
Date
2010-08-17T08:03:26Z (15 years ago)
From
Yuji Urata at Nat. Central U. <urata@astro.ncu.edu.tw>
Y. Urata (NCU) and K.Y Huang (ASIAA)
on behalf of EAFON report;
"We observed the GRB 100814A optical afterglow (Beardmore et al. GCN
11087) using Lulin One-meter Telescope (LOT) with g', r', i' and
z'-band filters. The observation started at 2010 August 16 19:09 about
2.65 days after the trigger. All of images show the optical afterglow
clearly. The brightness of the afterglow calibrated against USNO-B1
stars in the field is R~19.2.
The afterglow decays only ~0.5 magnitude from our previous observation
at August 14 (0.7 days after the burst). This interesting feature is
also notified by Pasquale (# 11107).
Further observation is scheduled."
GCN Circular 11107
Subject
GRB100814A - interesting UVOT lightcurve.
Date
2010-08-16T15:52:03Z (15 years ago)
From
Massimiliano de Pasquale at MSSL-UCL <mdp@mssl.ucl.ac.uk>
M. De Pasquale, C. J. Saxton, and S. R. Oates (MSSL/UCL) report, on
behalf of the Swift/UVOT team:
Swift GRB 100814A (Beardmore et al. GCN circ 11087) shows an interesting
optical/UV lightcurve, with a flux rise detected by UVOT between
approximately 10,000 and 100,000 seconds after the trigger. At about 40
hours after the trigger, the afterglow was still of magnitude ~ 19 in
the u and v filters.
Ground based observatories are encouraged to follow up this event.
GCN Circular 11100
Subject
Swift/UVOT observations of GRB100814A - title correction to GCN 11097
Date
2010-08-15T17:31:14Z (15 years ago)
From
Massimiliano de Pasquale at MSSL-UCL <mdp@mssl.ucl.ac.uk>
M. De Pasquale (MSSL/UCL) and C. J. Saxton (MSSL/UCL) on behalf of the
Swift/UVOT team report:
In the title of the GCN circular 11097 we mention "GRB100814B."
It should have been "GRB100814A". Apologies for the mistake.
GCN Circular 11099
Subject
GRB 100814A: Fermi GBM observation
Date
2010-08-15T12:23:54Z (15 years ago)
From
Andreas von Kienlin at MPE <azk@mpe.mpg.de>
A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team:
"At 03:50:08.81 UT on 14 August 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 100814A (trigger 303450610 / 100814160),
which was also detected by the Swift-BAT (Beardmore et al. 2008, GCN 11087)
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 87.2 degrees.
The GBM light curve consists of several pulses
with a duration (T90) of about 149 +/- 1 s (50-300 keV).
The time-averaged spectrum from T0+0.003 s to T0+157.57 s is
best fit by a Band function with Epeak = 106.4 +13.9/-12.6 keV,
alpha = -0.64 +0.14/-0.12, and beta = -2.02 +0.09/-0.12
(Castor C-STAT 807 for 484 d.o.f.).
The event fluence (10-1000 keV) in this time interval is
(1.98 +/- 0.06)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+6.784 s in the 10-1000 keV band
is 4.5 +/- 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 Circular 11098
Subject
GRB 100814A: Submm observations from APEX
Date
2010-08-15T12:02:52Z (15 years ago)
From
Antonio Deugarte at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (INAF-OAB, DARK/NBI), C. de Breuck,
A.J. Castro-Tirado (IAA-CSIC), G. Siringo, F.M. Montenegro-Montes,
M. Martinez (APEX), A. Hacar (OAN), T. Stanke, A. Lundgren,
M. Dumke (ESO) report on behalf of a larger
collaboration:
"We have observed the field of GRB 100418A (Beardmore et al.
GCNC 11087) using LABOCA/APEX at Chajnantor (Chile) in the
345 GHz band. Observations began on 15th August at 05:39 UT
(25.8 hours after the burst onset). In a preliminary analysis
we do not detect any new source at the position of the afterglow
(Schaefer et al. GCNC 11086, De Pasquale et al. GCNC 11095)
down to a 3-sigma limit of 5.4 mJy. The formal flux density at
the position of the afterglow is 4.6+/-1.8 mJy."
GCN Circular 11097
Subject
Swift/UVOT Observations of GRB100814A - a clearer table.
Date
2010-08-15T09:33:27Z (15 years ago)
From
Massimiliano de Pasquale at MSSL-UCL <mdp@mssl.ucl.ac.uk>
M. De Pasquale (MSSL-UCL) and C.J. Saxton (MSSL-UCL)
report on the behalf of the Swift UVOT team:
In the GCN circ 11095 (Swift/UVOT observations of
GRB100814A) the table containing the information
on epochs and magnitudes could not be read well because
of a formatting problem. In the following, we rewrite
the table with a clearer look.
We apologize for any inconvenience it might have caused.
Filter T_start T_stop Exp(s) Mag Err
----------------------------------------------------------
u (fc) 153 403 246 16.80 0.06
v 458 627 39 17.91 0.32
b 408 721 53 21.22 0.20
u 153 701 285 16.84 0.06
uvw1 507 676 39 17.33 0.20
uvm2 483 651 39 17.86 0.31
uvw2 434 602 39 >18.52 3-sigma UL
white 3858 4211 344 18.63 0.07
----------------------------------------------------------
[GCN OPS NOTE(15aug10): Per author's request, the "B"
in the Subject line was changed to "A".]
GCN Circular 11096
Subject
GRB 100814A: Swift-XRT refined analysis
Date
2010-08-14T20:34:14Z (15 years ago)
From
Andy Beardmore at U Leicester <apb@star.le.ac.uk>
A. P. Beardmore (U Leicester) and C. J. Saxton (MSSL-UCL) report on
behalf of the Swift-XRT team:
We have analysed 6.0 ks of XRT data for GRB 100814A (Beardmore et
al. GCN Circ. 11087), from 76 s to 28.6 ks after the BAT trigger. The
data comprise 721 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
Beardmore et al. (GCN. Circ 11092).
The X-ray light curve initially rises by a factor of ~2 in count rate,
reaching a broad peak at approximately T+160 s after the trigger, on top
of which are superimposed three small flares at T+146, 176 and 220 s,
respectively. At T+295 s the light curve falls with a steep decay of
alpha=5.7 (+0.4, -0.3), then breaks to a shallow decay at T+517 s, after
which it decays with an index of 0.47 (+0.03, -0.04).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.68 (+0.04, -0.03). The
best-fitting absorption column is 5.0 (+/-0.8) x 10^20 cm^-2, in
excess of the Galactic value of 1.8 x 10^20 cm^-2 (Kalberla et
al. 2005). The PC mode spectrum has a photon index of 1.90 (+0.11,
-0.10) and a best-fitting absorption column of 3.1 (+2.2, -1.4) x
10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum is 3.8 x 10^-11 (4.2 x
10^-11) erg cm^-2 count^-1.
If the light curve continues to decay with a power-law decay index
of 0.47, the count rate at T+24 hours will be 0.18 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of
7.0 x 10^-12 (7.7 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00431605.
This circular is an official product of the Swift-XRT team.
GCN Circular 11095
Subject
Swift/UVOT observations of GRB100814A
Date
2010-08-14T15:26:23Z (15 years ago)
From
Patricia Schady at MPE/Swift <msslba@googlemail.com>
M. De Pasquale (MSSL-UCL) and C.J. Saxton (MSSL-UCL)
report on the behalf of the Swift UVOT team:
��The Swift/UVOT began settled observations of the field of
GRB 100814A 153 s after the BAT trigger ��(Beardmore et
al. 2010, GCN Circ. 11087) with a finding chart in the u
filter. We detect the optical afterglow in all filters except
uvw2. The refined UVOT position is
��RA ��(J2000) = 01h 29m 53.61s = 22.47338
��Dec (J2000) = -17d 59m 43.6s = -17.99545
with an estimated uncertainty of 0.6 arcsec (radius, 90% confidence,
statistical + systematic). This is about 1.5 arcsec north of the
UVOT-enhanced XRT position (Beardmore et al. 2010, GCN Circ.
11092).
��Preliminary magnitudes, and 3-sigma upper limits for detecting a
source in the finding charts and in co-added images are
Filter �� �� ��T_start �� T_stop �� ��Exp(s) �� �� ��Mag �� Err
---------------------------------------------------------------------
�� ��u (fc) �� �� ��153 �� �� ��403 �� �� �� 246 �� �� 16.80 0.06
�� ��v �� �� �� �� �� 458 �� ���� 627 �� �� �� ��39 �� �� ��17.91 0.32
�� ��b �� �� �� �� �� 408 �� ���� 721 �� �� �� ��53 �� �� ��21.22 0.20
�� ��u �� �� �� �� �� 153 �� ���� 701 �� �� ��285 �� �� ��16.84 0.06
��uvw1 �� �� �� ��507 �� �� ��676 �� �� �� ��39 �� �� �� 17.33 0.20
��uvm2 �� �� �� 483 �� �� 651 �� �� �� 39 �� �� ��17.86 0.31
��uvw2 �� �� �� ��434 �� �� 602 �� �� �� 39 �� ��>18.52 ��3-sigma UL
��white �� �� ��3858 �� �� 4211 �� �� �� 344 �� �� ��18.63 0.07
-----------------------------------------------------------
��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} = 0.02 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 11094
Subject
GRB 100814A, Swift-BAT refined analysis
Date
2010-08-14T13:16:56Z (15 years ago)
From
Takanori Sakamoto at NASA/GSFC <takanori.sakamoto-1@nasa.gov>
H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 100814A (trigger #431605)
(Beardmore, et al., GCN Circ. 11087). The BAT ground-calculated position is
RA, Dec = 22.479, -17.990 deg which is
RA(J2000) = 01h 29m 55.0s
Dec(J2000) = -17d 59' 25.7"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 90%.
The mask-weighted light curve shows three FRED-like spikes starting around
T-4 sec, T+60 sec and T+140 sec. Those spikes peak around T+5 sec, T+70 sec
and T+145 sec. The low level emission is visible up to T+235 sec.
T90 (15-350 keV) is 174.5 +- 9.4 sec (estimated error including systematics).
The time-averaged spectrum from T-3 to T+235 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.47 +- 0.04. The fluence in the 15-150 keV band is 9.0 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T-0.06 sec in the 15-150 keV band
is 2.5 +- 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/431605/BA/
GCN Circular 11093
Subject
GRB 100814A: CQUEAN r- and i-band Observation
Date
2010-08-14T12:59:28Z (15 years ago)
From
Myungshin Im at Seoul Nat U <mim@astro.snu.ac.kr>
Myungshin Im, Won-Kee Park (CEOU/Seoul National Univ),
Soojong Pak, Hyeongju Jeong, Eunbin Kim, and Jinyoung Kim
(Kyunghee University)
We observed GRB 100814A (Beardmore et al. GCN 11087) with the SDSS
r- and i-filters during the commissioning run of CQUEAN (the Camera for
QUasars in the Early uNiverse) on the 2.1m telescope at the McDonald
Observatory. The observation started at 2010 August 14, 08:57:54 UT,
about 5 hours after the BAT trigger.
A series of 180 secs exposures were taken, and we confirm the afterglow
at the location reported by Schaefer et al. (GCN 11086) and Gorosabel et
al.(GCN 11090). A preliminary photometry from a single frame with the
mid-point time of 09:00:24 UT is r ~ 19.10 +- 0.03 AB mag (subject to
systematic error in the zero point determination), consistent with the
value reported by Filgas et al. (GCN 11091). The photometric calibration
is based on a standard star observation on the same night (BD+17 4708).
We thank the staffs of the McDonalnd Observatory, Peter S. Odoms and
John Kuehne for their assistance of the CQUEAN commissioning run.
GCN Circular 11092
Subject
GRB 100814A: Enhanced Swift-XRT position
Date
2010-08-14T12:17:34Z (15 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.
Using 5031 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 100814A, 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 = 22.47308, -17.99503 which is equivalent
to:
RA (J2000): 01h 29m 53.54s
Dec (J2000): -17d 59' 42.1"
with an uncertainty of 1.5 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 11091
Subject
GRB 100814A: GROND Detection of the Optical/NIR Afterglow
Date
2010-08-14T11:20:51Z (15 years ago)
From
Patricia Schady at MPE/Swift <pschady@mpe.mpg.de>
R. Filgas, P. Schady and J. Greiner (MPE Garching) report on behalf of
the GROND team:
We observed the field of GRB 100814A (Swift trigger 431605; Beardmore
et al., GCN #11087) 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 at
La Silla Observatory (Chile).
Observations started at 03:57 UT, 7 minutes after the GRB trigger at
03:50 UT, and are continuing. They were performed at an average seeing
of 1.2" and at an average airmass of 2.
We detect a single point source in all GROND optical (g'r'i'z') and
NIR bands (JHK) at a position consistent with the coordinates provided
by Schaefer et al. (GCN #11086) and Gronwall et al. (GCN #11088), and
consistent with the spectroscopic redshift of z=1.44 (O'Meara et al.
GCN #11089).
The afterglow decays as a power law with a best-fit index of alpha ~
0.5, decaying from r' = 18.0 +/- 0.1 at T+25 minutes down to r' = 19.5
+/- 0.1 (all in AB system) by the end of our observations, at T+6
hours. Analysis is on going.
Given magnitudes are calibrated against USNO zeropoints and are not
corrected for the expected Galactic foreground extinction
corresponding to a reddening of E(B-V)=0.02 in the direction of the
burst (Schlegel et al. 1998).
GCN Circular 11090
Subject
GRB 100814A: IAC80 R-band observations
Date
2010-08-14T05:52:08Z (15 years ago)
From
Javier Gorosabel at IAA-CSIC <jgu@iaa.es>
J. Gorosabel (IAA-CSIC), S. Rodriguez LLano (IAC), A.J. Castro-Tirado
(IAA-CSIC), report on behalf of a larger collaboration:
"Following the detection of GRB 100814A by Swift (Beardmore et
al. GCNC 11087) we have acquired a series of R-band images with the
0.82-m IAC80 telescope at Observatory of Teide, Tenerife, Spain.
The first exposure started on Aug 14.1788 UT (~27.3 minutes post
burst). The optical afterglow (Schaefer et al. GCNC 11086; Gronwall
et al. GCN 11088) is detected with a preliminary magnitude of R~18.7,
assuming a magnitude of R=16.87 for the USNO-B1.0 star placed at
RA(J2000)=01:29:43.606, DEC(J2000)=-18:00:38.61."
GCN Circular 11089
Subject
GRB100814A: Magellan Echellette Observations
Date
2010-08-14T05:09:50Z (15 years ago)
From
Hsiao-Wen Chen at U Chicago <hchen@oddjob.uchicago.edu>
John O'Meara (Saint Michael's College), Hsiao-Wen Chen (UChicago), Jason
X. Prochaska (UC Santa Cruz) report on behalf of a larger collaboration:
"We observed the afterglow of GRB100814A reported by Schaefer et al. (GCN
11086) and confirmed by Gronwall et al. (GCN 11088) using the MagE
echellette spectrograph on the Magellan Clay Telescope. The observations
started at UT 04:46 on August 14, 2010, ~ one hour after the inital
trigger. We obtained a 900s exposure. Our preliminary reduction shows
that the afterglow spectrum displays absorption transitions due to AlIII,
FeII, and MgII at redshift z=1.44, which we tentatively identify as the
host redsdhift of the GRB.
Further analysis is underway.
This message may be cited."
GCN Circular 11088
Subject
GRB 100814A: Swift UVOT observations of the optical afterglow
Date
2010-08-14T04:49:29Z (15 years ago)
From
Caryl Gronwall at PSU/Swift-UVOT <caryl@astro.psu.edu>
C. Gronwall (PSU) and C. J. Saxton (MSSL) report on behalf of the
Swift/UVOT team:
In response to GRB 100814A (Swift/BAT trigger 431605) at 03:50:11 UT,
UVOT took a finding chart exposure of 250 seconds with the U filter
starting
153 seconds after the BAT trigger. There is a candidate afterglow in the
rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 01:29:53.54 = 22.47309
DEC(J2000) = -17:59:43.5 = -17.99541
with a 90%-confidence error radius of about 0.75 arc sec. This
position is 4.7
arc sec. from the center of the XRT error circle. This position
supersedes
the position given in (Beardmore et al., GCN Circ. 11087) and is
consistent
with the optical afterglow position from ROTSE (Schaefer et al., GCN
Circ. 11086).
The estimated magnitude is 16.76 with a 1-sigma error of about 0.14.
No correction
has been made for the expected extinction corresponding to E(B-V) of
0.02.
GCN Circular 11087
Subject
GRB 100814A: Swift detection of a burst with an optical afterglow
Date
2010-08-14T04:22:40Z (15 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
A. P. Beardmore (U Leicester), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), N. P. M. Kuin (UCL-MSSL),
O. M. Littlejohns (U Leicester), C. B. Markwardt (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
C. J. Saxton (UCL-MSSL), R. L. C. Starling (U Leicester),
E. Troja (NASA/GSFC/ORAU) and T. N. Ukwatta (GSFC/GWU) report on
behalf of the Swift Team:
At 03:50:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100814A (trigger=431605). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 22.481, -17.986 which is
RA(J2000) = 01h 29m 55s
Dec(J2000) = -17d 59' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed three separate
peaks over a total interval of at least 150 sec. The peak count rate
was ~6000 counts/sec (15-350 keV), at ~6 sec after the trigger.
The XRT began observing the field at 03:51:38.6 UT, 87.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 22.47220,
-17.99643 which is equivalent to:
RA(J2000) = 01h 29m 53.33s
Dec(J2000) = -17d 59' 47.1"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 48 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
1.75e+20 cm^-2 (Kalberla et al. 2005).
The initial flux in the 2.5 s image was 6.18e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 250 seconds with the U filter
starting 153 seconds after the BAT trigger. A bright optical afterglow
candidate was found at RA=22.4749, dec=-17.9932 which is
RA = 01h 29m 53.98s
Dec=-17d 59m 35.5s
(J2000). The estimated magnitude is U=16.8 .
Burst Advocate for this burst is C. J. Saxton (cjs2 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 Circular 11086
Subject
GRB 100814A: ROTSE-III Detection of Optical Counterpart
Date
2010-08-14T04:14:34Z (15 years ago)
From
Brad Schaefer at LSU <schaefer@grb.phys.lsu.edu>
B. E. Schaefer (Louisiana State), E.S. Rykoff (UCSB), W. Rujopakarn
(Steward), S. B. Pandey (U Mich), W. Zheng (U Mich), report on behalf of
the ROTSE collaboration:
ROTSE-IIIc, located at the H.E.S.S. site at Mt. Gamsberg, Namibia,
responded to GRB 100814A (Swift trigger 431605). The first image was at
03:55:01.1 UT, 289.8 s after the burst (4.1 s after the GCN notice time).
The unfiltered images are calibrated relative to USNO A2.0. We detect a
new object, not visible in the DSS (second epoch), nor in our first set of
observations with coordinates:
01:29:53.67 -17:59:41.58 (J2000), with positional uncertainty
of 1" or better
start UT mag mlim(of image)
----------------------------------
03:55:11.3 17.4 8.0
A jpeg image is available at
http://www.rotse.net/images/gsq431605_3c011-020_key.jpg Note that the
object marked 29 is the candidate in question.
Continuing observations are in progress.