GRB 060602A
GCN Circular 5201
Subject
GRB060602A: Bootes-IR observations
Date
2006-06-03T01:25:24Z (19 years ago)
From
Petr Kubanek at AIO <petr@lascaux.asu.cas.cz>
Stanislav V�tek, Martin Jelinek, Alberto J. Castro-Tirado (IAA CSIC
Granada, Spain), Petr Kub�nek (ASU AV CR Ondrejov & ISDC, Versoix)
on behalf of the BOOTES collaboration report:
Bootes-IR telescope, located at IAA Observatory de Sierra Nevada,
observed position of GRB 060602A (S. Barthelmy GCN 5196), starting 13.7
sec post GCN notice (61.6 sec post GRB).
At images obtained at considerable airmass, we do not detect any new
object down to R~15 mag.
Futher analysis is in progress.
This message may be cited.
GCN Circular 5203
Subject
GRB060602A: optical observations(/transient?)
Date
2006-06-03T02:31:33Z (19 years ago)
From
Brian Lindgren Jensen at U.of Copenhagen <brian_j@astro.ku.dk>
Brian L. Jensen, Jens Hjorth, Johan Fynbo (Dark Cosmology Centre, NBI),
Jyri N�r�nen (University of Helsinki) report:
"We have observed the field of GRB060602A (Schady et al., GCN 5196) in
the R-band with the NOT+ALFOSC (La Palma), starting at June 2.908 (15
min. after the burst). All R:6x300s cover the full 3' radius BAT error
circle. Visual comparison to the SDSS (Cool et al., GCN 5197), does not
reveal any new bright sources in the field.
However, a faint source, not readily apparent on SDSS (r-band), is
observed at:
RA = 09:58:16.73
Dec = +00:18:12.7
- located 1.2' from the centre of the BAT error-circle.
A preliminary calibration to SDSS photometry of the field (Cool et al.,
GCN 5197) yields a magnitude for the source of R~22.5+-0.3. Further
observations are needed in order to determine whether the source is
transient.
A finding chart is available at:
http://www.astro.ku.dk/~brian_j/grb/grb060602.897/ "
GCN Circular 5206
Subject
GRB 060602A: Swift-BAT Refined Analysis
Date
2006-06-03T18:39:05Z (19 years ago)
From
Hans Krimm at NASA-GSFC <krimm@milkyway.gsfc.nasa.gov>
T. Sakamoto (GSFC/ORAU), L. Barbier (GSFC), S. Barthelmy (GSFC),
J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC),
D. Hullinger (BYU-Idaho), M. Koss (GSFC/UMD), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC),
G. Sato (GSFC/JSPS/USRA), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC),
on behalf of the Swift-BAT team:
Using the data set from T-119.7 to T+182.3 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 060602A
(trigger #213180) (Schady, et al., GCN 5196). The BAT
ground-calculated position
is (RA,Dec) = 149.576, 0.322 deg {9h 58m 18.3s, 0d 19' 20.7"} (J2000)
+- 1.6 arcmin, (radius, sys+stat, 90% containment). The partial
coding was 43%.
The light curve shows a single broad triangular shaped peak lasting from
~T+0 to ~T+70 sec. The burst is most prominent in the 50-100 keV band and
shows clear evidence of hard to soft spectral evolution.
T90 (15-350 keV) is 60 +- 10 sec (estimated error including systematics).
The time-averaged spectrum from T-0.7 to T+67.0 is best fit by
a simple power-law model. The power law index of the time-averaged
spectrum is 1.14 +- 0.16. The fluence in the 15-150 keV band is
1.6 +- 0.1 x 10^-06 erg/cm2. The 1-sec peak photon flux measured
from T+7.74 sec in the 15-150 keV band is 0.1 +- 0.3 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.
GCN Circular 5211
Subject
GRB 060602A: Swift-BAT Refined Analysis: Correction
Date
2006-06-04T02:13:48Z (19 years ago)
From
Takanori Sakamoto at NASA/GSFC <takanori@milkyway.gsfc.nasa.gov>
T. Sakamoto (GSFC/ORAU) on behalf of the Swift-BAT team:
There is an error in the 1-s peak photon flux reported in
Sakamoto et al. (GCN Circular 5206). Due to hard and weak
nature of the burst, only the 90% upper limit of 0.5 ph/cm2/s
is possible to constrain from a power-law fit.
We apologize for this mistake. We thank Kazutaka Yamaoka for
pointing it out.
GCN Circular 5245
Subject
GRB060602A: Swift/UVOT upper limits
Date
2006-06-08T12:41:19Z (19 years ago)
From
Alexander Blustin at MSSL-UCL <ajb@mssl.ucl.ac.uk>
A. J. Blustin (UCL-MSSL) and P. Schady (UCL-MSSL) report on behalf
of the Swift/UVOT team:
Due to a moon constraint, Swift/UVOT did not begin observing the
field of GRB060602A until 15:55:25 on 2006-06-04, 1.766 days after
the BAT trigger (Schady et al., GCN 5196). We observe no optical/UV
afterglow candidate within the refined BAT error circle (Sakamoto
et al. 5206) or at the position of the afterglow candidate reported
by the NOT team (Jensen et al., GCN 5203). 3-sigma magnitude upper
limits, in coadded images, at the position of the NOT afterglow
candidate are as follows:
Filter T_range(days) Exp(s) 3sig_UL(mag)
V 1.831-3.555 1775 21.3
B 1.827-3.567 1572 22.3
U 1.826-3.564 1775 22.1
UVW1 1.766-3.561 1850 21.7
UVM2 1.832-3.558 1922 22.0
UVW2 1.828-3.617 2265 22.3
Where the time range of the images post-trigger is given in days.
The upper limits are not corrected for Galactic extinction.
GCN Circular 5251
Subject
GRB 060602A: Swift/XRT analysis
Date
2006-06-12T21:23:42Z (19 years ago)
From
Jamie A. Kennea at PSU/Swift-XRT <kennea@astro.psu.edu>
K. L. Page, A. P. Beardmore (U. Leicester) and J. A. Kennea (PSU) report
on behalf of the Swift/XRT team:
We have analysed 37.8 ks of XRT data obtained for the field of GRB 060602A
(Schady et al.; GCN 5196), starting 1.8 days after the trigger, when the
burst was no longer Moon constrained.
A faint source was found within the BAT error circle, at a position of
RA(J2000) = 09 58 16.80
Dec(J2000) = +00 18 14.8
with an estimated uncertainty of 4.2 arcsec (90% containment). This source
is fading with an approximate slope of alpha = 1.10, so is very likely the
X-ray afterglow.
This source is 2.3 arcsec from the possible counterpart identified by
Jensen et al. (GCN 5203).
This circular is an official product of the Swift-XRT team.
GCN Circular 6997
Subject
GRB 060602A: host redshift
Date
2007-10-25T12:44:19Z (18 years ago)
From
Pall Jakobsson at U Hertfordshire <P.Jakobsson@herts.ac.uk>
Pall Jakobsson (U. Hertfordshire), Daniele Malesani,
Johan P. U. Fynbo, Jens Hjorth, Paul M. Vreeswijk
(DARK, NBI) and Nial R. Tanvir (U. Leicester) report
on behalf of a larger collaboration:
Using FORS1 on the Very Large Telescope, we obtained
2*20 min spectra (grism 300V+GG375 covering 4000-8000 A)
of the GRB 060602A host galaxy on 28 December 2006. A firm
upper limit of z < 2.3 can be placed on the host redshift
from the lack of Ly-alpha forest lines in the combined
spectrum.
We do detect a strong emission line at 6664 A. If it
corresponds to H-alpha at z = 0.015, we would expect to
detect H-beta and the [O III] doublet in our spectrum.
However, no features are visible at their predicted
locations. In addition, this redshift would imply a very
faint absolute magnitude of M_R = -10.3.
If the emission line corresponds to [O III] 5008 at
z = 0.331, we would expect to detect [O II] 3728 which we
do not. The most probable association is with [O II] 3728,
corresponding to a redshift of z = 0.787.
Using the relations by Kennicutt (1998, ARA&A, 36, 189),
the flux of the proposed [O II] line corresponds to a star
formation rate (SFR) of approximately 1.9 M_Sun/year. This
value has not been corrected for host extinction, and is
therefore a strict lower limit to the actual SFR. The
specific SFR is around 13.6 M_Sun/year (L/L*)^-1, typical
for GRB host galaxies (Christensen et al., 2004, A&A, 425, 913).