GRB 061110A
GCN Circular 5794
Subject
GRB061110A - Optical Non-detection
Date
2006-11-10T12:17:30Z (19 years ago)
From
Brian Schmidt at RSAA, ANU (MSSSO) <brian@mso.anu.edu.au>
Brian Schmidt and Gordon Garradd (ANU) report on behalf of a larger
collaboration
"We have observed the field of GRB061110A with the Uppsala Schmidt
Telescope at Siding Spring Observatory. An Image taken at 11:59 UT shows
no object at the XRT position brighter than R=19th magnitude."
GCN Circular 5802
Subject
GRB 061110A, Swift-BAT refined analysis
Date
2006-11-10T23:16:30Z (19 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
J. Cummings (GSFC/UMBC), L. Barbier (GSFC), S. D. Barthelmy (GSFC),
A. D. Falcone (PSU), E. Fenimore (LANL), N. Gehrels (GSFC),
D. Hullinger (BYU-Idaho), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/ORAU),
G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC)
on behalf of the Swift-BAT team:
Using the data set from T-240 to T+726 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 061110A (trigger #238108)
(Falcone, et al., GCN Circ. 5795). The BAT ground-calculated position
is RA,Dec = 336.284, -2.252 deg {22h 25m 8.1s, -2d 15' 6.0"} (J2000)
+- 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%.
The mask-weighted lightcurve shows a FRED-like peak starting at ~T-15 sec,
peaking at ~T+5 sec, and extending out to ~T+80 sec. T90 (15-350 keV)
is 41 +- 2 sec (estimated error including systematics). The spectral lag
is 2.75 sec +0.55-0.48 sec (between the 15-25 to 50-100 keV bands).
The time-averaged spectrum from T-8.8 to T+38.5 is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.67 +- 0.12. The fluence in the 15-150 keV band is 1.1 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+9.74 sec in the 15-150 keV
band is 0.5 +- 0.1 ph/cm2/sec. All the quoted errors are at the 90%
confidence level.
GCN Circular 5806
Subject
GRB 061110A: Swift XRT refined analysis
Date
2006-11-11T00:05:23Z (19 years ago)
From
Loredana Vetere at PSU <vetere@astro.psu.edu>
L. Vetere, D. Morris, C. Pagani, J. Racusin, A. Falcone, D. N. Burrows (PSU)
report on behalf of the Swift XRT team:
We have analysed the first 3 orbits of XRT data for GRB 061110A.
A 560s photon counting mode image provides a refined XRT position:
RA(J2000) = 22 25 09.9
Dec(J2000) = -02 15 30.7
with an uncertainty of 3.7 arcsec (90% containment). This position is 2.2
arcsec away from the previous XRT position (Falcone et al. GCN 5795), 1.66
arcsec away from the optical afterglow detection by Chen et al. (GCN 5797)
and 1.5 arcsec away from its later confirmation by Zhai et al. (GCN 5798).
The X-ray light curve in PC mode shows a rapid decay with a slope of -2.36
+/-0.22 in all the 1st orbit. While the 2nd and 3rd orbits show flattening.
A power-law fit to the WT spectrum gives a photon index of 3.1 +/- 0.2 and a
column density of (1.6 +/- 0.2)e21 cm^-2. We note that the galactic hydrogen
column density in the direction of the burst is 4.94e20 cm^-2. The 0.2-10.0 keV
observed mean flux during WT observation is 1.1-09 ergs cm^-2 s^-1, which
corresponds to an unabsorbed flux of ergs 3.4e-09cm^-2 s^-1.
We are waiting for new data to make a prediction of the count rate. Note that
the new event, GRB 061110B (GCN 5800), is 1hr away in RA and it is currently
taking all the time from this observation.
This circular is an official product of the Swift XRT Team.
GCN Circular 5812
Subject
GRB 061110A - VLT tentative redshift
Date
2006-11-11T13:54:33Z (19 years ago)
From
Christina Thoene at Niels Bohr Institute,DARK Cosmo Ctr <cthoene@astro.ku.dk>
Christina C. Thoene, Johan P.U. Fynbo (DARK-NBI), Pall Jakobsson (Univ. of
Hertfordshire), Paul M. Vreeswijk (ESO) and Jens Hjorth (DARK-NBI) report
on behalf of a larger collaboration:
We obtained a series of 3x1800s spectra of the OT of GRB 061110A
(GCNs 5797, 5798, 5799) on November 11, 02:50UT (15h after the burst),
using FORS1/VLT and grism 300V. At the time of the observations, the OT
had a magnitude of about R=22 using photometric zeropoints from the ESO
webpages.
Based on the detection of weak emission lines at 6551 AA and 8803 AA which
we interpret as [OII] 3727 and [OIII] 5007 from the host galaxy, we
determine a tentative redshift of z=0.757 for GRB 061110A. The continuum
extends down to the blue end of the spectrum at 3600 AA which places an
additional limit of z<2 on the redshift of this burst.
We thank the staff at VLT for performing the observations.
GCN Circular 5813
Subject
Swift/UVOT Upper Limits for GRB061110a
Date
2006-11-11T20:07:07Z (19 years ago)
From
Patricia Schady at MSSL/Swift <ps@mssl.ucl.ac.uk>
P. Schady (UCL-MSSL), A.D. Falcone (PSU) report on behalf of the
Swift/UVOT team:
The Swift/UVOT began observing the field of GRB 061110a at 11:48:32 on
2006-11-10 UT, 71s after the BAT trigger (Falcone et al., GCN 5795). No new
source was detected within the XRT error circle (Vetere et al., GCN 5806) or at
the afterglow position reported by Zhai et al. (GCN 5798) in coadded images in
any filter down to the following 3-sigma magnitude upper limits:
Filter T_mid (s) Exp. (s) 3-sigma UL
------------------------------------------------
V 3952 2579 20.42
B 4016 442 20.55
U 3888 452 20.28
UVW1 3792 452 19.72
UVM2 6192 1273 20.55
UVW2 4128 452 20.31
------------------------------------------------
T_mid is the mid time of the coadded exposure with respect to the BAT trigger.
These upper limits are not corrected for Galactic extinction E(B-V) = 0.09.
GCN Circular 5815
Subject
Swift TOO observations of GRB061110A
Date
2006-11-11T20:38:25Z (19 years ago)
From
Abe Falcone at PSU/Swift <afalcone@astro.psu.edu>
A. Falcone (Penn State) and N. Gehrels (GSFC) report on behalf of Swift
Team:
On 2006 Nov 11 at 19:45:11 UT, Swift began target of opportunity
observations of GRB 061110A to resume monitoring the afterglow during
the weekend. Follow-up observations with other instruments are encouraged.
GCN Circular 5817
Subject
GRB 061110A: refined R-band analysis
Date
2006-11-12T16:07:43Z (19 years ago)
From
Christina Thoene at Niels Bohr Institute,DARK Cosmo Ctr <cthoene@astro.ku.dk>
Christina C. Thoene and Johan P. U. Fynbo (DARK Cosmology Centre) report:
We further analysed our R-band data of the afterglow of GRB 061110A taken
with ALFOSC/NOT (GCN 5799) and FORS1/VLT (GCN 5812).
Crosscalibration of the two observation sets with a nearby star
(RA=22:25:07.76, Dec=-02:15:00.52) and zeropoints from the ESO webpages
gives revised magnitudes of R=23.3 at 8h after the burst (NOT) and
R=23.9 at 14h (VLT), where we assume R=22.1 for the magnitude of
the star. The offset to the magnitudes reported earlier are due to old
ALFOSC zeropoints and refined reduction.
Together with the magnitude reported in GCN 5798, we find that a single
powerlaw decay with a slope of alpha=0.83 +- 0.08 fits the data well. A
plot of the lightcurve can be found at
www.astro.ku.dk/~cthoene/GRBs
GCN Circular 5818
Subject
GRB061110A: Correction to GCN5817
Date
2006-11-12T19:45:13Z (19 years ago)
From
Johan U. Fynbo at U.Copenhagen <jfynbo@astro.ku.dk>
Johan P. U. Fynbo (DARK) report:
Unfortunately I made an error in the gain-correction in the photometry
reported in GCN #5817. Here are the correct numbers for the revised
photometry. In the NOT images taken about 8 hr after the GRB) we measure
R=22.5. In the VLT image taken about 14 hr after the GRB we measure
R=23.1. Here we assume R=21.3 for the star at RA(2000) = 22:25:07.760,
Dec(2000) = -02:15:00.52. I apologize for the confusion.
GCN Circular 6759
Subject
GRB 061110A: redshift confirmed
Date
2007-08-13T17:22:18Z (18 years ago)
From
Daniele Malesani at Niels Bohr Inst,Dark Cosmology Center <malesani@astro.ku.dk>
J.P.U. Fynbo, C.C. Thoene, D. Malesani, J. Hjorth, P.M. Vreeswijk
(DARK), and P. Jakobsson (Univ. Hertfordshire) report on behalf of a
larger collaboration:
We inspected in detail our VLT spectra (Thoene et al., GCN 5812) of the
afterglow of GRB 061110A (Falcone et al., GCN 5795; Chen et al., GCN 5797).
Further to the lines reported in GCN 5812 (6552 and 8803 A), interpreted
as [OII] and [OIII] 5007 at z=0.758, we also detect emission at 8547 A,
which corresponds to Hbeta at the same redshift. We thus consider the
redshift to be secure.