GRB 060425
GCN Circular 5005
Subject
GRB 060425: IPN localization and KW spectrum of a short, hard burst
Date
2006-04-26T23:50:41Z (19 years ago)
From
Jay R. Cummings at NASA/GSFC/Swift <jayc@milkyway.gsfc.nasa.gov>
J. Cummings, S. Barthelmy, N. Gehrels, and H. Krimm, on behalf of
the Swift-BAT team,
S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks,
and T. Cline on behalf of the Konus-Wind team,
A. von Kienlin, G. Lichti, A. Rau, D. Gotz, and S. Mereghetti,
on behalf of the INTEGRAL GRB team,
K. Hurley, D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger,
W. Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team,
and K.Yamaoka, M.Ohno, Y.Fukazawa, T.Takahashi, M.Tashiro, Y. Terada,
T.Murakami, and K.Makishima on behalf of the Suzaku WAM team
report:
A short, hard GRB was observed at 2006-04-25 16:57:40 by Swift-BAT,
Konus-Wind, Suzaku-WAM, RHESSI, and INTEGRAL-SPI-ACS. The T90 was
0.13 +- 0.01 sec. This burst was Mars-occulted to Odyssey. The burst
had 2 main peaks of roughly similar intensity and hardness, the second
slightly shorter than the first.
The IPN triangulated error box is as follows:
----------------------
RA, deg Dec, deg (J2000)
----------------------
Center:
212.3007 -5.0667
Corners:
214.5693 -1.7277
210.9652 -7.0326
210.7765 -8.4092
213.8848 -3.1685
-----------------------
The area of the box is 2.53 sq. deg
Preliminary analysis of the Konus-Wind data yields a burst fluence of
2.57 (-1.85, +0.47) x 10^-6 erg/cm2. The peak flux measured from
T0(K-W)-0.036 s on a 16-ms time scale was
3.64 (-2.74, +1.06) x 10^-5 erg/cm2/sec. Both are quoted in the
20 keV - 10 MeV energy range. The K-W spectrum accumulated from
T0(K-W) to T0(K-W)+0.128 s is well fitted (in the 20 keV - 10 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ E^(-alpha) * exp(-(2-alpha)*E/Ep)
with alpha = 0.92 (-0.37, + 0.28) and Ep = 1403 (-594, 1273) keV
(chi^2 = 16.7/18 dof). T0(K-W) = 61063.000 s UT (16:57:43.000).
We note that the X-ray source 1RXS J140902.5-050430, and nearby galaxies
LEDA 1048719 and LEDA 1047950 are within this error box close to the
center.
GCN Circular 5008
Subject
GRB060425:MASTER survey observations
Date
2006-04-27T15:19:39Z (19 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V. Lipunov, V.Kornilov, N.Tyurina, A.Belinski, D.Kuvshinov, E.Gorbovskoy,
A.Krylov, G.Borisov, A.Sankovich, V.Vladimirov, P.Gritsyk, S.Korobkin
Sternberg Astronomical Institute, Moscow Union 'Optic'
MASTER robotic system (http://observ.pereplet.ru) observed
GRB060425 error box (GRB_TIME is 2006-04-25 16:57:40 UT, IPN
triangulation
GCN5005) in survey mode at considerable zenit distances. The weather was
good.
The first image was at 2006-04-26 18:17:03.46 UT,
1.05 days after the GRB time. The last image was at 2006-04-26
19:53:07.00 UT, 1.12 days after the GRB time.
We have 54 images.
The location of our samples you can find at
http://observ.pereplet.ru/images/GRB060425/GRB060425_ErrorBox_master.jpg
The unfiltered image is calibrated relative to USNO A2.0 (0.8 R + 0.2 B).
There is 1 bright galaxies in error box NGC5476 (14 08 08.48 -06 05 31.2).
The robot not find SN-candidate in error box brighter then 17.5 (s/n=3).
The robot find several asteroids in error box brighter then 17.5 (s/n=3)
at error box:
| number | name | coord2000 | mag
+--------+---------------+---------------------------------+------|
| 1105 | Volland | 14h 14m 10.3s , - 3d 15m 31s) | 17.5 |
| 104 | Asta | ( 14h 13m 18.7s , - 3d 57m 7s) | 14.9 |
| 111 | Euboea | ( 14h 5m 56.8s , - 6d 59m 32s) | 14.2 |
| 3652 | 2000 QZ79 | ( 14h 5m 52.7s , - 6d 50m 53s) | 17.4 |
| 1403 | 1995 HR | ( 14h 4m 5.1s , - 7d 59m 30s) | 16.4 |
So as possible OT time decay may be about 1 day
we plan additional observations.
MASTER team thanks to Konus-Wind team for collaboration.
This work is supported by RFFI 04-02-16411 grant.
This message can be cited.
Mailto: lipunov@sai.msu.ru
GCN Circular 5026
Subject
GRB060425:MASTER optical limit
Date
2006-04-28T16:19:06Z (19 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V. Lipunov, V.Kornilov, N.Tyurina, A.Belinski, D.Kuvshinov, E.Gorbovskoy,
A.Krylov, N.Shatskiy, G.Borisov, A.Sankovich, V.Vladimirov, P.Gritsyk,
S.Korobkin
Sternberg Astronomical Institute, Moscow Union 'Optic'
MASTER robotic system (http://observ.pereplet.ru) observed
GRB060425 error box (GRB_TIME is 2006-04-25 16:57:40 UT, IPN triangulation
GCN5005) in survey mode at considerable zenit distances. The weather was good.
We have two nights observations 2006-04-26 from 18:17:03.46 to
19:53:07.00 (1.05 - 1.12 days after the GRB time) (Lipunov et
al.GCN5008) and 2006-04-27 from 18:57:50.89 to 19:21:19.88.
We have 72 images. The location of our samples you can find at
http://observ.pereplet.ru/images/GRB060425/GRB060425_ErrorBox_master.jpg
The unfiltered image is calibrated relative to USNO A2.0 (0.8 R + 0.2 B).
The robot not find OT brighter then 17.0 between 1.05 -1.12 day after GRB
time in large IPN error box (J. Cummings, S. Barthelmy et al. GCN5005).
The robot not find SN brighter then 17.5 in two nights.
The search of the SN after several days is planed.
MASTER team thanks to Konus-Wind team for collaboration. This work is
supported by RFFI 04-02-16411 grant.
This message can be cited.
Mailto: lipunov@sai.msu.ru
GCN Circular 5080
Subject
GRB060425: new MASTER survey method
Date
2006-05-06T14:15:34Z (19 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V. Lipunov, V.Kornilov, N.Tyurina, A.Belinski, D.Kuvshinov, E.Gorbovskoy,
A.Krylov, N.Shatskiy, G.Borisov, A.Sankovich, V.Vladimirov, P.Gritsyk,
S.Korobkin
Sternberg Astronomical Institute, Moscow Union 'Optic'
In this circular we proposed and tested new method of optical observations
of GRBs by wide field robotic telescopes: survey search of the optical
transient like supurnovae in large error box GRBs or dark not X-ray GRB.
Especially this method is very important for bright short GRB, that
frequently detected by all sky gamma-ray detectors (Konus-Wind,
Ulysses, Odyssey, etc) and for which connection with supernovae is not
clear.
The difference between "OT" and "SN" is the following: OT - is the new
optical object without known galaxy. The SN pipe line reduction is based
on the searching of the uncatalogized candidate near known galaxies (for
example from HyperLeda, http://www-obs.univ-lyon1.fr/hypercat/).
MASTER robotic system (http://observ.pereplet.ru, 6 square degrees field)
observed GRB060425 error box (GRB_TIME is 2006-04-25 16:57:40 UT, IPN
triangulation GCN5005) in survey mode at considerable zenit distances.
The weather was good.
We have 4 nights (1-2 hours per night) observations:
Date Days after GRB Note Limit
mean
2006-04-26 1.1 (Lipunov et al.GCN5008) 17.5
2006-04-27 2.1 (Lipunov et al.GCN5026) 17.5
2006-04-30 5.2 17.8
2006-05-03 8.1 17.6
The location of our samples you can find at
http://observ.pereplet.ru/images/GRB060425/GRB060425_ErrorBox_master.jpg
The unfiltered image is calibrated relative to USNO A2.0 (0.8 R + 0.2 B).
The robot not find OT brighter then 17.0 in
large IPN error box (J. Cummings, S. Barthelmy et al. GCN5005).
The robot not find SN brighter then 17.5.
Father observations of the GRB050425 not planed.
MASTER team thanks to Konus-Wind team for collaboration. This work is
supported by RFFI 04-02-16411 grant.
This message can be cited.
Mailto: lipunov@sai.msu.ru