GRB 100302A
GCN Circular 10480
Subject
GRB100302A : LOAO observations and Lulin afterglow analysis
Date
2010-03-06T02:14:20Z (16 years ago)
From
Kuiyun Huang at ASIAA <ljhuang@asiaa.sinica.edu.tw>
GRB100302A : LOAO observations and Lulin afterglow analysis
K.Y. Huang (ASIAA), Myungshin Im (CEOU/Seoul National Univ) and
Y. Urata (NCU) on behalf of EAFON team :
We observed GRB100302A afterglow position (Goad et al. GCN 10460,
Huang et al. GCN 10461 and Cucchiarar & Fox GCN 10465) in i-band
(12x300s) using 1.0 telescope at Mt. Lemmon (Arizona, US) operated by
the Korea Astronomy Space Science Institute.
No significant detection of afterglow in our i-band combined image at
11.0709 hours after the burst. The 3-sigma limiting magnitude is 20.8,
which calibrated with five nearby USNOB stars.
We also reduced R and i band images taken by Lulin 1-m telescopes. Our
photometric results, combined with the i-band detection reported by
Cucchiarar & Fox (GCN 10465), indicate the i-band power law index is
about -0.65.
Delay time filter EXPTIME Magnitude error
(hour)
---------------------------------------------------
0.450 R 300s x 5 21.54 0.22
0.780 I 300s 20.02 0.12
0.873 I 300s 20.24 0.15
0.966 I 300s 20.08 0.13
1.060 I 300s 20.17 0.17
1.153 I 300s 20.34 0.19
1.357 I 300s x 4 20.31 0.17
--------------------------------------------------
This message can be cited
GCN Circular 10469
Subject
GRB 100302A: Ondrejov 65cm limit
Date
2010-03-04T15:24:50Z (16 years ago)
From
Petr Kubanek at AIO <pkubanek@gmail.com>
K. Hornoch (Astronomical Institute, Academy of Sciences of the Czech
Republic) & P. Kubanek (IPL UV Valencia & IAA CSIC Granada, Spain)
reports on behalf of a larger collaboration:
We acquired unfiltered CCD images of GRB 100302A XRT error box
(J.R.Cummings, GCN 10458) with Ondrejov 65cm telescope + CCD. AS the CCD
is equipped with IR-block filter its sensitivity in I band is very close to 0.
Observation started March 3 00:40 UT (4h47m after the BAT trigger).
During observation which run till 03:00 UT 45 of 3 minutes exposures were
obtained. On the combined image we do not identify any new object down to
R ~22 magnitude. Particularly we do not see anything significant at the
proposed OT position (K.Y. Huang, GCN 10461).
This message can be cited
GCN Circular 10468
Subject
GRB 100302A: Swift/UVOT Upper Limits
Date
2010-03-03T19:04:52Z (16 years ago)
From
Michele Stark at PSU/Swift <stark@astro.psu.edu>
M. A. Stark (PSU) and J. R. Cummings (NASA/UMBC) report on behalf of
the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 100302A
132 s after the BAT trigger (Cummings et al., GCN 10458). No optical
afterglow consistent with the XRT position (Cummings et al., GCN
10458) is detected in the initial UVOT exposures. We do not see any
source within the XRT error circle that might correspond to the R and
I-band source reported by Huang et al. (GCN 10461) from the Lulin
1-meter telescope or the i' source reported by Cucchiara and Fox (GCN
10465) from Gemini-N.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the initial exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
---------------------------------------------------
white_FC 133 282 147 >21.06
white 133 2044 431 >21.24
v 621 1933 156 >18.82
b 547 2032 136 >19.58
u 291 2007 382 >20.10
w1 670 1982 155 >19.49
m2 645 1957 136 >19.26
w2 596 1908 156 >19.61
The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the
burst (Schlegel et al. 1998).
GCN Circular 10467
Subject
GRB 100302A: Swift-XRT refined analysis
Date
2010-03-03T17:09:17Z (16 years ago)
From
Valerio D'Elia at INAF-OAR <delia@oa-roma.inaf.it>
V. D'Elia, M. Perri (ASDC) and J.R. Cummings (NASA/UMBC) report
on behalf of the Swift-XRT team:
We have analysed the first 3 orbits of Swift-XRT data obtained from
GRB 100302A (trigger 414592; Cummings, et al., GCN Circ. 10458)
from 125 s to 28.8 ks after the BAT trigger.
The best position of the X-ray afterglow is the UVOT enhanced XRT
position given in Goad et al. (GCN Circ. 10460).
The 0.3-10 keV light curve shows a multiple peak structure, with
three main spikes at about T+200, T+250 and T+400s, followed by a
fast decay with index 3.35+-0.3 and by a break at 1ks. Later time
data are fitted by a second power law with a decay index of
0.26+-0.12.
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.28 (-0.15, +0.17). The
best-fitting absorption column is 1.1 (-0.20, +0.17) x 10^21 cm^-2, in
excess of the Galactic value of 1.9 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.3 x 10^-11 (4.7 x 10^-11) erg
cm^-2 count^-1.
If the light curve continues to decay with a power-law decay index of
0.26, the count rate at T+24 hours will be 0.01 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.3 x
10^-13 (4.7 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00414592.
This circular is an official product of the Swift-XRT team.
GCN Circular 10466
Subject
GRB 100302A: Gemini-North redshift
Date
2010-03-03T16:38:03Z (16 years ago)
From
Ryan Chornock at UC Berkeley <chornock@astro.berkeley.edu>
R. Chornock (Harvard), A. Cucchiara, D. Fox (Penn St.), and E. Berger (Harvard)
report on behalf of a larger collaboration:
Further analysis of the Gemini-North GMOS spectrum of the afterglow (Huang et
al., GCN 10461) of GRB 100302A (Cummings et al., GCN 10458) described in GCN
10465 (Cucchiara et al.) reveals that the afterglow shows a sharp increase in
continuum flux redward of 7100 Angs, with only a weak continuum detected between
5500 and 7000 Angs, consistent with absorption by H I at z~4.8.
There are several narrow absorption features superposed on the noisy red
continuum, consistent with N V, Si II, Si II*, and C II at a mean redshift of
4.813, which we identify as the redshift of this burst.
GCN Circular 10465
Subject
GRB 100302A: Gemini-N OT confirmation
Date
2010-03-03T15:22:47Z (16 years ago)
From
Antonino Cucchiara at PSU <cucchiara@astro.psu.edu>
A. Cucchiara, D. B. Fox (PSU) report on behalf of
a larger collaboration:
"On March 3.40 UT we observed the field of GRB 100302A (Cummings et
al., GCN 10458) with the Gemini-N telescope and the GMOS spectrograph.
In our 300s i'-band acquisition image we clearly identify a source
inside the XRT refined error circle (Goad et al. 10460).
Using 3 USNO-B1 stars we calibrated our photometry and obtained
i' = 22.01 +- 0.05 mag
This value is significantly below the detection reported by
Huang et al. (GCN 10461) confirming that this is the afterglow
of GRB 100302A.
We also performed a single 1200s spectroscopic observation.
No absorption or emission features have been detected over
the 4000-9000A coverage of our spectrum.
We thank the Gemini staff for performing this observation,
in particular Andrew Stephens."
GCN Circular 10464
Subject
GRB 100302A: Optical observations at Crni Vrh
Date
2010-03-03T14:31:32Z (16 years ago)
From
Bojan Dintinjana at OCV <bojan.dintinjana@fmf.uni-lj.si>
B. Dintinjana and H. Mikuz on behalf of PIKA observing program at Crni
Vrh Observatory.
We observed the field of GRB 100302A (Cummings et al., GCN 10458) from
Crni Vrh Observatory with a 60 cm robotic telescope, R filter and CCD.
Twenty consecutive exposures of 60 second duration were taken in
moonlight conditions. First exposure started at 2010-03-02 19:56:20 UT,
194 seconds after the burst (105 seconds after the SWIFT trigger).
No optical candidate was detected within the uncertainty radius on
single exposures, having R limiting magnitude 18.3, calibrated against
the nerby USNO-B R2 magnitude stars. Also we found no optical candidate
on 20 sumed R images with total exposure of 1200 seconds and limiting R
band magnitude 19.6 (calibrated against the nerby USNO-B R2 magnitude
stars).
GCN Circular 10463
Subject
GRB 100302A: MASTER-Net optical alert observations
Date
2010-03-03T11:31:50Z (16 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V.Yurkov, S.Sergienko, D.Varda,
Blagoveschensk Educational State University, Blagoveschensk
E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov, D.Zemnukhov,
M. Kornilov
Sternberg Astronomical Institute, Moscow State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory
V.Krushinski, I.Zalozhnih, T.Kopytova, A. Popov Ural State University, Kourovka
K.Ivanov, S.Yazev, N.M.Budnev, E.Konstantinov, V.Lenok
Irkutsk State University
MASTER robotic telescope (MASTER-Net: http://observ.pereplet.ru, 200
mm, FOV=8 square degrees (testing telescope) and Very Wide Field Camera
(D=50 mm, 1000 square degrees, 11 Mpx, 36" per pix, mounted on telescope)
located at Blagoveschensk was responted to the GRB 100302A (Swift Bat alert,
Cummings et al, GCN CIRC 10458) 51 sec after Notice time and 139 s
after the GRB time.
There is now OT in our images inside Swift XRT error box (Goad et al., GCN
CIRC 10460).
GRB_time start UT end UT t_exp(s) mlim Coadd?
-------------------------------------------------------------------
139s 19:55:25 19:55:55 30 16.9 no
139s-4046s 19:55:25 21:14:17 4020 18.5 68
The coadded image is available at
http://observ.pereplet.ru/images/GRB100302A/GRB_summ.jpg .
The message may be cited.
mailto: lipunov@sai.msu.ru
GCN Circular 10462
Subject
GRB 100302A, Swift-BAT refined analysis
Date
2010-03-03T03:09:06Z (16 years ago)
From
Jay R. Cummings at NASA/GSFC/Swift <james.r.cummings@nasa.gov>
J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-60 to T+243 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 100302A (trigger #414592)
(Cummings, et al., GCN Circ. 10458). The BAT ground-calculated position
is RA, Dec = 195.504, 74.568 deg which is
RA(J2000) = 13h 02m 01.0s
Dec(J2000) = +74d 34' 04.0"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 98%.
The mask-weighted light curve shows one group of multiple overlapping
peaks from T+40 to T+70. T90 (15-350 keV) is 17.9 +- 1.7 sec (estimated
error including systematics).
The time-averaged spectrum from T+47.6 to T+67.3 sec is best fit by a
simple power-law model. The power law index of the time-averaged
spectrum is 1.72 +- 0.19. The fluence in the 15-150 keV band is
3.1 +- 0.4 x 10^-07 erg/cm2. The 1-sec peak photon flux measured from
T+63.87 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.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/414592/BA/
GCN Circular 10460
Subject
GRB 100302A: Enhanced Swift-XRT position
Date
2010-03-02T23:10:26Z (16 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 478 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 100302A, 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 = 195.51524, +74.58959 which is equivalent
to:
RA (J2000): 13h 02m 3.66s
Dec (J2000): +74d 35' 22.5"
with an uncertainty of 1.9 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 10459
Subject
GRB 100302A: Skynet/DAO Observations
Date
2010-03-02T22:45:23Z (16 years ago)
From
Josh Haislip at U.North Carolina <haislip@physics.unc.edu>
J. Haislip, K. Ivarsen, A. LaCluyze, D. Reichart, R. Egger, A. Foster, J.
Moore, A. Oza, M. Schubel, J. Styblova, A. Trotter, J. A. Crain, and M.
Nysewander report:
Skynet observed the Swift/BAT localization of GRB 100302A (Cummings et al.,
GCN 10458) with the 16" telescope at the Dolomiti Astronomical Observatory
in Italy beginning 2.7 minutes after the trigger (1.3 minutes after
notification) in Red, which we have calibrated to R.
We do not detect the afterglow (Cummings et al., GCN 10458). Stacking only
images that increase the limiting magnitude yields:
mean 1-sig. 1-sig.
time 3-sig. sys. stat.
since lim. cal. cal. cal.
trig. tel. exp. fil. mag. stars unc. unc.
(m) (# x s) (mag) (mag)
73.3 DAO 28 x 160 Red 20.3 78 USNO B1 0.429 0.000
GCN Circular 10458
Subject
GRB 100302A: Swift detection of a burst
Date
2010-03-02T20:14:02Z (16 years ago)
From
Jay R. Cummings at NASA/GSFC/Swift <jayc@milkyway.gsfc.nasa.gov>
J. R. Cummings (NASA/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU),
O. Godet (U Leicester), D. Grupe (PSU),
S. T. Holland (CRESST/USRA/GSFC), S. Immler (CRESST/GSFC/UMD),
J. A. Kennea (PSU), R. Margutti (Univ Bicocca&OAB),
F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester),
M. Perri (ASDC), M. H. Siegel (PSU), M. A. Stark (PSU),
E. Troja (NASA/GSFC/ORAU), T. N. Ukwatta (GSFC/GWU) and
L. Vetere (PSU) report on behalf of the Swift Team:
At 19:53:06 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100302A trigger=414592). Swift slewed immediately to the
burst. The BAT on-board calculated location is
RA, Dec 195.344, +74.581 which is
RA(J2000) = 13h 01m 23s
Dec(J2000) = +74d 34' 51"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single broad peak
with a duration of about 35 sec, beginning about 40 sec after the trigger
time (the beginning of the 64-second interval for this "image trigger").
The peak count rate was ~500 counts/sec (15-350 keV), at ~55 sec after
the trigger.
The XRT began observing the field at 19:55:11.9 UT, 125.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
195.5146, 74.5895 which is equivalent to:
RA(J2000) = 13h 02m 3.50s
Dec(J2000) = +74d 35' 22.1"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 166 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
1.92e+20 cm^-2 (Kalberla et al. 2005).
The initial flux in the 2.5 s image was 1.96e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 132 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag.
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
0.02.
Burst Advocate for this burst is J. R. Cummings (jayc 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.)