GRB 080229
GCN Circular 7404
Subject
GRB 080229: NIR upper limit
Date
2008-03-11T03:23:10Z (18 years ago)
From
Takeo Minezaki at U.of Tokyo/Astro <minezaki@mtk.ioa.s.u-tokyo.ac.jp>
T. Minezaki (IoA, Tokyo), P.A. Price (IfA, Hawaii), Y. Yoshii (IoA,
Tokyo), L. Cowie (IfA, Hawaii) and Y. Kakazu (IfA, Hawaii) report:
We observed the localisation of GRB 080229 with the MAGNUM telescope +
MIP dual-beam imager. We do not find any afterglow in the RIYJHK images
within the XRT error circle (GCN #7343). We estimated the upper limits
in JHK based on flux calibration with a nearby 2MASS star as follows:
Filter t - t_GRB (hour) Limit (mag)
J +19.8 20.5
H +20.7 20.0
K +20.4 19.4
This message may be cited.
GCN Circular 7380
Subject
GRB080229, optical upper limit (Correction)
Date
2008-03-10T08:25:57Z (18 years ago)
From
Ryuuji Hara at U of Miyazaki <ryuu55@astro.miyazaki-u.ac.jp>
R.Hara notes:
I stated in GCN7337$B!!(Bas
"The observation was started 17:05:03 UT, ~225 min
after the Swift trigger time."
but the correct one is
"The observation was started 19:30:40 UT, about 146 min
after the Swift trigger time."
We apologize for any inconvenience this may have caused.
GCN Circular 7377
Subject
GRB080229, optical upper limit
Date
2008-03-08T07:30:06Z (18 years ago)
From
Ryuuji Hara at U of Miyazaki <ryuu55@astro.miyazaki-u.ac.jp>
R. Hara, H.hayasi, N.Ohmori, K.Kono H. Tanaka, M.Yamauchi, E.Sonoda,
(University of Miyazaki)
We have observed the field covering the error circle of
GRB080229 (GCN 7338, C. Markwardt et al.) with
the unfiltered CCD camera on the 30-cm telescope at
University of Miyazaki.
The observation was started 17:05:03 UT, ~225 min
after the Swift trigger time.
We have compared our data of 30 sec exposures
with the USNO-A2.0 catalog,there is no new source
at the reported position.
the upper limits are as follows:
--------------------------------------------------------------
Start(UT) End(UT) Num. of frames Limit (mag.)
--------------------------------------------------------------
19:33:57 19:34:27 1 ~16.06
19:33:57 20:39:37 20 ~16.79
---------------------------------------------------------------
GCN Circular 7361
Subject
VLA possible radio detection of GRB 080229
Date
2008-03-04T13:46:24Z (18 years ago)
From
Poonam Chandra at U Virginia/NRAO <pc8s@virginia.edu>
Poonam Chandra (NRAO/UVA) and Dale A. Frail (NRAO) report on
behalf of the Caltech-NRAO-Carnegie GRB Collaboration:
"We used the Very Large Array to observe the field of view toward
GRB 080229 (GCN 7335) at a frequency of 8.46 GHz on 2008 March
01.50 UT. We detect a radio source of flux density of 635 +/- 44
uJy at a position of
RA(J2000) 15 12 52.21984, DEC(J2000) -14 42 15.3000.
This is 2.82" away from the X-ray afterglow position determined by
Swift-XRT (GCN 7343).
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."
GCN Circular 7348
Subject
GRB 080229: I-band observations from OSN
Date
2008-03-01T18:54:39Z (18 years ago)
From
Antonio Deugarte at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (ESO, Chile), F. Aceituno,
A.J. Castro-Tirado (IAA-CSIC, Spain) on behalf
of a larger colaboration report,
We have observed the field of GRB 080229 (Cannizzo et al. GCN 7335)
with the 1.5m telescope at Sierra Nevada Observatory (OSN, Granada).
The observations were obtained in I-band and range between March
1.1681 and March 1.2638 UT (mean exposure 0.5042 days after the burst).
We do not detect any new source in the error box of Swift/XRT
(Beardmore et al. GCN 7343) down to a 3-sigma limiting magnitude of
I~22.0.
This message can be cited.
GCN Circular 7347
Subject
GRB 080229: VLT NIR observations
Date
2008-03-01T18:28:34Z (18 years ago)
From
Paolo D'Avanzo at INAF-OAB <paolo.davanzo@brera.inaf.it>
P. D'Avanzo and G. Tagliaferri (INAF-OAB) on behalf of the MISTICI
collaboration report:
We observed the field of the GRB 080229 (Cannizzo et al., GCN 7335) with
the ESO-VLT on March 01.411 UT (about 16.8 hours after the burst).
Observations have been carried out in J-band with the ISAAC NIR camera
in imaging mode under very good (0.7") seeing conditions.
We do not detect any afterglow candidate inside the enhanced XRT error
box (Beardmore et al., GCN 7343) down to J > 21.6 (3sigma c.l.,
calibrated against the 2MASS catalog).
We acknowledge support from the ESO staff, in particular Thomas Szeifert.
GCN Circular 7346
Subject
GRB080229: Swift XRT refined analysis
Date
2008-03-01T12:39:34Z (18 years ago)
From
Jirong Mao at INAF-OAB <jirong.mao@brera.inaf.it>
GRB080229: Swift XRT refined analysis
J.Mao, (INAF-OAB), A. Moretti (INAF-OAB), J. Canizzo (NASA/UMBC), C.
Guidorzi
(Univ. Bicocca & INAF-OAB), A, Beardmore (U Leicester)
P. Evans (U Leicester) report on behalf of the Swift-XRT team:
We have analysed the first 2 orbits of Swift-XRT data obtained for
BAT GRB 080229 (trigger #304379, Cannizzo, et al., GCN Circ. 7335).
The data consist of 149 s in Windowed Timing (WT) mode, starting 90 s
after the BAT trigger and 8.34 ks in Photon Counting (PC) mode.
The astrometrically corrected X-ray position is given in Beardomre et
al. GCN 7324.
The XRT light-curve shows a flare peaking few seconds after the beginning
of the observation (103+/-2 s). The descending part of the flare can be
fit by a power law with
a slope of alpha1=4.45+/-0.09 up to a break at t1=192.4+/- 2.5 s, which is
followed by a flat decay with a slope of alpha2=0.18+/-0.01.
A second break is present at 2700+/-1000 s with alpha3=0.8+/-0.5
The spectrum formed from all the WT data can be modeled with a
power-law of photon index Gamma = 2.88 � 0.09, with an absorbing
column of NH = (3.1 � 0.2)e21 cm^-2 (in excess with respect to the
Galactic value of 8.97e20 cm^-2). The spectrum formed from the PC data
can be modeled with a power-law of photon index Gamma = 1.99 �
0.07, with an absorbing column of NH = (3.1 � 0.2)e21 cm^-2, which
is in agreement with the WT one.
If the light-curve continues to decay with a slope of 0.8, the
afterglow at 24 hour will be still bright with an expected count
rate of 0.3 count s^-1. This corresponds to an observed (unabsorbed) flux
of 1.41E-11(2.2e-11) erg cm-2 s-1.
This circular is an official product of the Swift-XRT team.
GCN Circular 7345
Subject
GRB 080229: TNG NIR observations
Date
2008-03-01T08:00:00Z (18 years ago)
From
Paolo D'Avanzo at INAF-OAB <paolo.davanzo@brera.inaf.it>
P. D'Avanzo, C. Guidorzi (INAF-OAB) on behalf of the CIBO collaboration
and G. Andreuzzi and Noemi Pinilla Alonso (FGG-INAF, TNG) report:
We observed the field of the GRB 080229 (Cannizzo et al., GCN 7335) with
the Italian 3.6m TNG telescope located at Canary Islands on March 01.259
UT (about 13.1 hours after the burst). Observations have been carried
out with the NICS NIR camera in imaging mode under good (1.1") seeing
conditions.
We do not detect any afterglow candidate inside the enhanced XRT error
box (Beardmore et al., GCN 7343) down to the following limiting
magnitudes (3sigma c.l., calibrated against the 2MASS catalog):
J > 20.9
H > 20.1
K > 19.5
GCN Circular 7344
Subject
GRB 080229: Deep Gemini/GMOS optical observations
Date
2008-03-01T07:53:03Z (18 years ago)
From
Edo Berger at Princton U <eberger@astro.princeton.edu>
E. Berger (Princeton/Carnegie) reports on behalf of a larger
collaboration:
"We observed the refined BAT error circle of GRB 080229 (GCN #7338) with
GMOS on the Gemini-South telescope starting on 2008 Mar 1.26 UT (13.1
hours after the burst). We obtained a total of 5x120 sec in g,r,i,z is
0.8" seeing. We do not detect any sources within the XRT error circle
(GCN #7343) to the following 3-sigma magnitude limits: g>26.0, r>25.9,
i>25.6, z>25.3."
GCN Circular 7343
Subject
GRB 080229: Enhanced Swift-XRT position
Date
2008-03-01T07:18:20Z (18 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 1276 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080229, 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 = 228.21828, -14.70467 which is equivalent
to:
RA (J2000): 15h 12m 52.39s
Dec (J2000): -14d 42' 16.8"
with an uncertainty of 1.4 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
http://www.swift.ac.uk/xrt_positions/Goad.pdf).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 7342
Subject
GRB 080229: REM NIR observations
Date
2008-03-01T07:00:23Z (18 years ago)
From
Paolo D'Avanzo at INAF-OAB <paolo.davanzo@brera.inaf.it>
P. D'Avanzo, L.A. Antonelli, S. Covino, D. Fugazza, L. Calzoletti, S.
Campana, G. Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F.
D'Alessio, F. Fiore, P. Goldoni, D. Guetta, C. Guidorzi, G.L. Israel,
E. Maiorano, N. Masetti, A. Melandri, E. Meurs, L. Nicastro, E. Palazzi,
E. Pian, S. Piranomonte, L. Stella, G. Stratta, G. Tagliaferri, G.
Tosti, V.Testa, S.D. Vergani, F. Vitali report on behalf of the REM team:
The robotic 60-cm REM telescope located at La Silla (Chile) observed
automatically the field of the GRB 080229 (Cannizzo et al., GCN 7335) on
March 01.154 UT (about 10.6 hours after the burst).
We do not detect any afterglow candidate inside the XRT error box down
to the following limiting magnitudes (3sigma c.l., calibrated against
the 2MASS catalog):
J > 16.3
H > 15.6
K > 14.4
Further analysis is in progress.
GCN Circular 7341
Subject
GRB080229: Possible optical afterglow
Date
2008-03-01T03:16:54Z (18 years ago)
From
Michitoshi Yoshida at Okayama Astrophysical Obs <yoshida@oao.nao.ac.jp>
M. Yoshida, K. Yanagisawa, Y. Shimizu, S. Nagayama, H. Toda
(OAO, NAOJ) and N. Kawai (Tokyo Tech) report on behalf of the
MITSuME collaboration:
We performed optical imaging observations (g', Rc, and Ic) of the
field of GRB 080229 (Cannizzo et al. GCN 7335) with 50cm MITSuME
telescope at Okayama Astrophysical Observatory from UT 17:06:55
(117sec after the trigger) to UT 17:24:40 on Feb 29 2008.
We found a faint fading source in the XRT error circle (Cannizzo
et al: GCN 7335) only in the Ic band. There was no source in the
g' and the Rc bands. Together with the UVOT results (Kuin and
Cannizzo GCN7339), this may suggest that this GRB is a high-
redshift one. Follow-up observations in infrared bands are
encouraged.
The magnitude of the fading source and 3-sigma upper limits are
summarized below.
Observation date 2008-02-29 UT
mid-UT exp-T g' Rc Ic
---------------------------------------------
17:09:40 5 min >17.5 >17.8 17.1+-0.3
17:18:58 11 min >17.6 >18.2 >18.0
---------------------------------------------
The values quoted above are not corrected for the Galactic
extinction.
GCN Circular 7339
Subject
UVOT analysis for GRB080229
Date
2008-03-01T00:34:09Z (18 years ago)
From
Paul Kuin at MSSL <npkuin@googlemail.com>
N.P.M. Kuin (MSSL/UCL) and J. K. Cannizzo (NASA/UMBC) report on
behalf of the Swift-UVOT team:
The Swift/UVOT observed the field of GRB 080229 (trigger #304379),
Canizzo et al. GCN CIRC. 7335) starting 2008:02:29 at 17:06:22 UT
with a 9.4 s setling image followed at 17:06:41 UT with a finding
chart. No afterglow is detected at the position of the enhanced
XRT position in the finding chart, nor in the three subsequent
exposures.
The source is near a bright star and may be affected by it.
Therefore a small aperture was used and the background was determined
for a region at equal distance to the nearby star.
The following 3-sigma upper limits (in the UVOT photometric system,
Breeveld et al., GCN Circ. 6614) were determined at the XRT
position (RA=15:12:52.53, DEC= -14:42:19.3, J2000):
Filter Tstart(s) Tstop(s) Exp(s) Mag (3-sigma Upper Limits)
wh 101 200 99.8 > 20.9
v 208 608 400.0 > 19.9
wh 856 956 99.8 > 20.9
v 962 1362 400.0 > 19.9
The values quoted above are not corrected for the expected Galactic
extinction corresponding to a reddening of E_{B-V} = 0.15 mag in the
direction of the burst (Schlegel et al. 1998).
GCN Circular 7338
Subject
GRB 080229, Swift-BAT refined analysis
Date
2008-03-01T00:15:19Z (18 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
C. Markwardt (GSFC/UMD), S. D. Barthelmy (GSFC), J. K. Cannizzo (NASA/UMBC),
J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC),
H. Krimm (GSFC/USRA), K. McLean (GSFC/UMD), D. Palmer (LANL),
A. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-239 to T+303 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080229 (trigger #304379)
(Cannizzo, et al., GCN Circ. 7335). The BAT ground-calculated position is
RA, Dec = 228.220, -14.697 deg, which is
RA(J2000) = 15h 12m 52.7s
Dec(J2000) = -14d 41' 50"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 18%.
The mask-weighted light curve shows an initial small peak starting
at ~T-3 sec, peaking at T_zero, and ending at ~T+12 sec. Then there are
two smaller peaks centered on T+18 and T+28 sec. Then comes two overlapping
large peaks on T+35 and T+39 sec with the latter tailing out to ~T+85 sec.
T90 (15-350 keV) is 64 +- 16 sec (estimated error including systematics).
The time-averaged spectrum from T-15.1 to T+64.9 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.91 +- 0.06. The fluence in the 15-150 keV band is 9.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+40.36 sec in the 15-150 keV band
is 5.7 +- 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/304379/BA/
GCN Circular 7337
Subject
GRB 080229: Faulkes Telescope South optical limit
Date
2008-02-29T20:43:58Z (18 years ago)
From
James Smith at ARI,Liverpool John Moors U <rjs@astro.livjm.ac.uk>
R.J. Smith, D.F. Bersier, S. Kobayashi, A. Monfardini, C.G. Mundell,
I. A. Steele (Liverpool JMU), A. Gomboc (U. Ljubljana),
C. Guidorzi (U. Bicocca & INAF-OAB)
P. O'Brien, E. Rol, N. Bannister (Leicester) report:
The 2-m Faulkes Telescope South (Siding Spring) robotically followed
up GRB080229 (SWIFT trigger 304379) starting 4.6 min after the GRB
trigger time. The automatic "detection mode" procedure did not find
any afterglow. In manual inspection of later observations we do not
find any optical candidate corresponding to the XRT X-ray afterglow
(Cannizzo et al., GCN 7335) to the following limiting magnitudes.
Magnitude zero points are relative to the USNO measure of R=13.3 for
the adjacent bright star.
-----------------------------------------------
Mid Time Filter Tot.Exposure Lim. Mag.
since GRB
10.95 min R 60s 18.7
28.10 min R 180s 21.9
-----------------------------------------------
[GCN OPS NOTE(29feb08): Per editor's choice, the Subject-line
was changed from "071021" to "080229".]
GCN Circular 7335
Subject
GRB 080229: Swift detection of a bright burst
Date
2008-02-29T17:31:15Z (18 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
J. K. Cannizzo (NASA/UMBC), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), J. R. Cummings (NASA/UMBC),
P. A. Evans (U Leicester), O. Godet (U Leicester), C. Gronwall (PSU),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
S. Immler (CRESST/GSFC/UMD), J. A. Kennea (PSU),
V. Mangano (INAF-IASFPA), C. B. Markwardt (CRESST/GSFC/UMD),
K. M. McLean (GSFC/UMD), A. Moretti (INAF-OAB),
P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester),
C. Pagani (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (NASA/UMBC), G. Sato (GSFC/ISAS),
B. Sbarufatti (INAF-IASFPA), M. Stamatikos (NASA/ORAU),
R. L. C. Starling (U Leicester), G. Stratta (ASDC) and
E. Troja (U Leicester/INAF-IASFPa) report on behalf of the Swift
Team:
At 17:04:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080229 (trigger=304379). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 228.217, -14.712 which is
RA(J2000) = 15h 12m 52s
Dec(J2000) = -14d 42' 43"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed three or four bright
peaks with the brightest at ~T+40 sec with a duration of about 60 sec.
The peak count rate was ~7000 counts/sec (15-350 keV), at ~40 sec
after the trigger.
The XRT began observing the field at 17:06:29.9 UT, 90.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 228.21888,
-14.70536 which is equivalent to:
RA(J2000) = 15h 12m 52.53s
Dec(J2000) = -14d 42' 19.3"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 24 arcseconds from the BAT onboard position, within the BAT
error circle.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of
8.97e+20 cm^-2 (Kalberla et al. 2005), so we cannot constrain the
redshift at this time using the relation from Grupe et al. (2007). A
summary of the promptly downlinked data is given at
http://www.swift.ac.uk/sper/304379/.
The initial flux in the 2.5 s image was 5.98e-09 erg cm^-2 s^-2 (0.2-10
keV).
UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm) filter starting 100 seconds after the BAT trigger. A 400
second image in V band was also taken 207 seconds after the trigger.
No afterglow candidate has been found in the either image. The
2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical
3-sigma upper limit has been about 18.5 mag in white and 18.0 in V.
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 0.15. There is a F0
star with R1~13.3 in the USNO catalog nearby the XRT position which
appears in DSS images.
Burst Advocate for this burst is J. K. Cannizzo (cannizzo AT milkyway.gsfc.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.)