GRB 130215A
GCN Circular 14204
Subject
GRB 130215A: Swift detection of a burst
Date
2013-02-15T01:50:26Z (12 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@milkyway.gsfc.nasa.gov>
V. D'Elia (ASDC), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (NASA/GSFC) and B. Sbarufatti (INAF-OAB/PSU) report on
behalf of the Swift Team:
At 01:31:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130215A (trigger=548760). Swift did not slew because of Moon constraint.
The BAT on-board calculated location is
RA, Dec 43.479, +13.371 which is
RA(J2000) = 02h 53m 55s
Dec(J2000) = +13d 22' 14"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows a single peak
with a duration of about 40 sec. The peak count rate
was ~1300 counts/sec (15-350 keV), at ~1 sec after the trigger.
Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 14:00 UT on 2013 February 18. There will thus be no XRT
or UVOT data for this trigger before this time.
Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it).
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.)
GCN Circular 14207
Subject
GRB 130215A: Redshift estimate
Date
2013-02-15T02:57:36Z (12 years ago)
From
Antonino Cucchiara at UCSC/UCO Lick <acucchia@ucolick.org>
A. Cucchiara (UCSC/UCO Lick), M. Fumagalli (Carnegie Observatory/
Princeton University), report on behalf of a larger collaboration
reports:
On February 15.1 UT (~50 minutes after the BAT trigger) we observed
the field of GRB 130215A (D'Elia et al., GCN 14204, Zheng et al GCN
14205) using the KAST Spectrograph on the Lick Shane 3-m telescope.
The optical candidate is clearly detected.
We obtained a 2x600s spectrum, covering the wavelength range 3500-8000A
The spectrum reveals strong absorption lines of MgII2796, MgII2803,
MgI2853, FeII2586, FeII2600, and Ca H&K.
A provisional reduction gives a redshift of z=0.597, which we believe
is most likely the redshift of this burst.
We thank the Lick Observatory staff for their prompt support.
GCN Circular 14208
Subject
GRB 130215A: ROTSE-III data analysis
Date
2013-02-15T04:07:03Z (12 years ago)
From
Weikang Zheng at U.of Michigan <zwk@umich.edu>
W. Zheng (UC Berkeley), H. Flewelling (IfA/Hawaii), T. Guver (Sabanci
U), F. Yuan (Australian National University), report on behalf of the
ROTSE collaboration:
Further analysis of ROTSE-IIIb data revealed that the OT of GRB 130215A
(Swift trigger 548760; D'Elia et al., GCN 14204; Zheng et al GCN 14205;
LaCluyze et al. 14206) peaked around 750s after the burst, followed with
a single power-law decay with index alpha = -1.24 up to ~4ks after the
burst. Observation is on going.
Interestingly the GRB is also triggered by Fermi-GBM (trigger
382584689). The GBM trigger arrived ~600s earlier than Swift-BAT trigger
and ROTSE-IIIb responded to GBM trigger at first. A 4x4 tiling follow-up
mode was performed before BAT-trigger interrupted it and a total of 22
images were obtained to GBM trigger. Unfortunately, our effort of the
tiling follow-up still didn't cover the OT location in these images
since the GBM trigger is about 3.78 degree away, just a bit away from
one of the corner.
GCN Circular 14209
Subject
GRB 130215A: P60 Observations
Date
2013-02-15T04:15:55Z (12 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. B. Cenko (UC Berkeley) reports on behalf of a larger collaboration:
We imaged the location of the Swift GRB130215A (D'Elia et al., GCN 14204)
with the robotic Palomar 60 inch telescope. Images were obtained in the
SDSS r', i', and z' filters beginning at 02:29 UT on 2013 Feb 15 (~ 1 hr
after the Swift trigger).
We detect a bright point source at the location of the optical counterpart
(Zheng et al., GCN 14205) in all filters. Using several nearby point
sources from the USNO-B1 for reference, we measure a magnitude of R = 15.9
at this time.
Observations are ongoing.
GCN Circular 14210
Subject
GRB 130215A: CARMA 3mm detection
Date
2013-02-15T06:21:53Z (12 years ago)
From
Daniel Perley at Caltech <dperley@astro.caltech.edu>
D. A. Perley (Caltech) and G. Keating (UC Berkeley) report on behalf of
a larger collaboration:
We began observations of the position of GRB 130215A (D'Elia et al., GCN
14204) with the Combined Array for Research in Millimeter Astronomy at a
frequency of 93 GHz (3mm) starting at 03:28 UT, 1.95 hours after the
burst. Observations continued until 05:03 UT (midpoint t=2.73 hours.)
A provisional reduction of the data shows a strong detection of a source
consistent with the location of the optical afterglow (Zheng et al., GCN
14205). We estimate a preliminary flux at this time of 2.99 +/- 0.39
mJy. Follow-up observations are planned.
We thank the CARMA staff for executing these rapid observations.
GCN Circular 14211
Subject
GRB 130215A: REM NIR observations
Date
2013-02-15T06:38:27Z (12 years ago)
From
Stefano Covino at Brera Astronomical Observatory <stefano.covino@gmail.com>
S. Covino, D. Fugazza, V. d'Elia, on behalf of the REM team report:
We imaged the field of GRB130215A (D'Elia et al., GCN 14204) with the
REM NIR camera with the J, Hand Ks filters.
Observations started at 2013/02/15 01:43:21, i.e. about 12 min after
the prompt event.
The optical counterpart detected by ROTSE-IIIb (Zheng et al., GCN
14205) was well detected and still fairly bright at H=11.6+-0.1
(preliminary calibration) at the beginning of our observations.
[GCN OPS NOTE(14may13): Per author's request, the line
"2013/02/15 01:38:40, i.e. about 7 min"
was changed to
"2013/02/15 01:43:21, i.e. about 12 min", due to a clock error correction.]
GCN Circular 14212
Subject
GRB 130215A: RATIR Optical and NIR Observations
Date
2013-02-15T10:48:09Z (12 years ago)
From
Nat Butler at Az State U <natbutler@asu.edu>
Nat Butler (ASU), Antonino Cucchiara (UCSC), William H. Lee (UNAM),
Alexander Kutyrev (GSFC), Alan M. Watson (UNAM), Michael G. Richer (UNAM),
Chris Klein (UCB), Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom
(UCB), Eleonora Troja (GSFC), Enrico Ramirez���Ruiz (UCSC), Jos�� A. de Diego
(UNAM), Leonid Georgiev (UNAM), Jes��s Gonz��lez (UNAM), Carlos Rom��n-Z����iga
(UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:
We observed the field of GRB 130215A (D'Elia et al.; GCN 14204) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astron��mico Nacional on
Sierra San Pedro M��rtir from 2013/02 15.13 to 2013/02 15.18 UTC (1.58 to
2.88 hours after the BAT trigger) through intermittent clouds, obtaining a
total of 25 minutes of useful exposure in the r' and i' bands and 19
minutes of useful exposure in the Z and J bands.
We detect the optical counterpart discovered by ROTSE (Zheng et al.; GCN
14205). In comparison with USNO-B1 and 2MASS, we derive the following
magnitudes in the AB system:
r' = 17.86 +/- 0.05
i' = 17.10 +/- 0.04
Z = 16.86 +/-0.04
J = 16.67 +/- 0.04
These magnitudes are not corrected for Galactic extinction in the direction
of the GRB. Compared to the earlier observation at Palomar (Cenko et al;
GCN 14209), our r band magnitude implies a temporal fade by >1 mag on a
timescale of 2 hours, with a corresponding power law fade f ~ t^(-1.5)
between 1 and 3 hours after the GRB.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 14213
Subject
GRB 130215A: TAROT La Silla observatory optical observations
Date
2013-02-15T11:08:54Z (12 years ago)
From
Bruce Gendre at ASDC <bruce.gendre@gmail.com>
Gendre B. (Artemis/IRAP), Dereli, H. (Artemis/OCA), Atteia J.L.
(IRAP-CNRS-OMP), Boer M. (UNS-CNRS-OCA), Klotz A. (IRAP-CNRS-OMP) report:
We imaged the field of GRB 130215A detected by SWIFT (trigger 548760,
D'Elia et al., GCN 14204) with the TAROT robotic telescope located at
the European Southern Observatory, La Silla observatory, Chile.
The observations started 15.5s after the GCN notice (704.3s after the
SWIFT trigger). The elevation of the field decreased from 20 degrees
above horizon and weather conditions were good.
At the position reported by Zheng et al. (GCN 14205) we clearly detect
the afterglow between 704s and 5481 seconds after the trigger. We also
confirm the peak in the light curve around 750s post-trigger announced
by Zheng et al. (GCN 14208).
We obtained the following magnitudes, calibrated with three different
USNO-B1 objects (statistical 3 sigma errors are of the order of
0.1-0.2), and not corrected for galactic extinction.
MidTime (s) R mag
719 13.8
1192 14.4
1795 15.0
2723 15.7
4439 16.3
N.B. Galactic coordinates are lon=163.0747 lat=-39.7685 and the galactic
extinction in R band is 0.3 magnitudes estimated from D. Schlegel et al.
1998ApJ...500..525S.
This message may be cited.
GCN Circular 14214
Subject
GRB 130215A: Swift-BAT refined analysis
Date
2013-02-15T13:03:30Z (12 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
V. D'Elia (ASDC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130215A (trigger #548760)
(D'Elia, et al., GCN Circ. 14204). The BAT ground-calculated position is
RA, Dec = 43.486, 13.387 deg which is
RA(J2000) = 02h 53m 56.7s
Dec(J2000) = +13d 23' 13.6"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 8%.
The mask-weighted light curve starts at ~T-10 sec, peaks at ~T+10 sec,
and slowly returns to baseline at ~T+170 sec.
T90 (15-350 keV) is 65.7 +- 10.8 sec (estimated error including systematics).
The time-averaged spectrum from T-5.83 to T+73.38 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.59 +- 0.14. The fluence in the 15-150 keV band is 5.4 +- 0.5 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+11.16 sec in the 15-150 keV band
is 2.5 +- 0.7 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/548760/BA/
We note that the BAT trigger occurred during a telemetry downlink session
during which the real-time TDRSS messages (that GCN uses) are buffered on-board
until the end of the downlink. For this trigger the minimum bufferring delay
to the ground was 692 sec.
GCN Circular 14215
Subject
GRB 130215A: Xinglong optical observations
Date
2013-02-15T13:14:33Z (12 years ago)
From
Dong Xu at DARK/NBI <dong.dark@gmail.com>
D. Xu (DARK/NBI) and T.M. Zhang (NAOC) report on behalf of a larger
collaboration
We observed the field of GRB 130215A (D'Elia et al., GCN 14204) using
the Xinglong 2.16m telescope, located in Heibei China and equipped
with the BFOSC camera. Observations started at 10:57:59 UT on
2013-02-15 (i.e., 9.941 hr after the BAT trigger), and 3x300s R-band
and I-band frames were obtained, respectively.
The optical afterglow (Zheng et al., GCN 14205; LaCluyze et al., GCN
14206; Cenko, GCN 14209; Butler et al., GCN 14212; Gendre et al., GCN
14213) is clearly detected in each of our images. Compared with the
measurements in previous GCN reports, it decayed to R=19.1 mag at the
mean time of 10.08 hr post-trigger, in the staked image and calibrated
with nearby USNO B1 stars.
We thank Feng Xiao for carrying out these observations.
GCN Circular 14216
Subject
GRB 130215A: iTelescope T11 observations
Date
2013-02-15T13:46:08Z (12 years ago)
From
Veli-Pekka Hentunen at Taurus Hill Obs,A95 <veli-pekka.hentunen@varkaus.fi>
Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill
Observatory, Varkaus, Finland) report:
T11 (iTelescope Observatory, Mayhill, New Mexico) TEL T11 0.50-m/6.8
astrograph (0.50 m) f/6.5 and FLI ProLine PL11002M CCD camera were
used to detect GRB 130215A optical afterglow. The observations were
started at 2013-02-15 02:20:23 (UT) and stopped at 2013-02-15 03:22:20
(UT). Three unfiltered, two photometric R filter and two photometric V
filter observations with different exposure times were made.
The afterglow was detected at following position RA 02:54:00.73 and
DEC +13:23:43.4.
The following magnitudes were obtained from the observations using
NOMAD1 1034-0036172 (R = 14.220, V = 15.030) as the comparison:
Tmid(s)+T0 Filter Exp (sec) Mag Mag err Limit
2993 unfiltered 120 15.56CR 0.02 19.66
3156 unfiltered 120 15.70CR 0.03 19.66
4595 Rc 300 16.44R 0.04 19.22
4936 Rc 300 16.54R 0.05 19.32
5586 V 300 17.27V 0.05 19.92
5910 V 300 17.34V 0.06 19.92
6500 unfiltered 300 16.62CR 0.03 19.64
--
*************************************************************************
Viesti on tarkastettu roskapostinsuodatus- ja virustorjuntaohjelmistolla.
*************************************************************************
GCN Circular 14217
Subject
GRB 130215A: GMG optical observation
Date
2013-02-15T14:56:14Z (12 years ago)
From
Xiao-hong Zhao at Yunnan Obs <zhaoxiaohong78@gmail.com>
X.-H. Zhao (YNAO), J.-M. Bai
(YNAO) report on behalf of 2.4m telescope group:
We observed the field of GRB 130215A (D'Elia et al., GCN 14204) with 2.4m Gao-Mei-Gu (GMG) telescope. Observations
started at 11:59:03 UT on 2013-02-15 (i.e., 10.46 hrs after the burst) and 5x300s R-band images were obtained. The optical afterglow of this burst was clearly detected in each image. The mag is R~19.2 calibrated with USNO B1 stars.
We thank the GMG staff, especially Wen-Bo Xu, De-Qing Wang for
performing these observations.
GCN Circular 14218
Subject
GRB 130215A: RAPTOR Measurements
Date
2013-02-15T17:56:46Z (12 years ago)
From
James Wren at LANL <jwren@nis.lanl.gov>
J. Wren, W.T. Vestrand, P. Wozniak, and H. Davis,
of Los Alamos National Laboratory report:
The RAPTOR network of robotic optical telescopes made follow-up observations
of Swift trigger 548760 (D'Elia, et al., GCN 14204). Our narrow-field
instruments in Los Alamos, NM USA, began imaging at 01:43:07.0 UT, 696.8 s
after the Swift BAT trigger. We detect the optical counterpart initially
reported by the ROTSE team (Zheng, et al., GCN 14205). Our unfiltered images
are calibrated to the USNO-B1 r-band. The following table gives a sample of
our observations.
T-Start Exp-Time Mag +/- error
------------------------------------
696.85 5.0 13.73 +/- 0.014
725.35 5.0 13.70 +/- 0.015
762.35 5.0 13.74 +/- 0.014
796.75 10.0 13.80 +/- 0.009
927.55 10.0 13.98 +/- 0.010
1089.9 30.0 14.13 +/- 0.006
GCN Circular 14219
Subject
GRB 130215A: Fermi GBM detection
Date
2013-02-15T21:10:57Z (12 years ago)
From
George A. Younes at USRA/NASA/MSFC <younes.ge@gmail.com>
George Younes (USRA) and P. N. Bhat (UAH)
report on behalf of the Fermi GBM Team:
"At 01:31:26.02 UT on 15 February 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130215A (trigger 382584689 / 130215063).
which was also detected by the Swift/BAT (D'Elia et al. 2013, GCN 14204)
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 86 degrees.
The GBM light curve consists of single FRED like pulse
with a duration (T90) of about 140 s (50-300 keV).
The time-averaged spectrum from T0-7.0 s to T0+124 s is
adequately fit by a Band function with Epeak= 155 +/- 63 keV,
alpha = -1.0 +/- 0.2 and beta = -1.60 +/- 0.03.
The event fluence (10-1000 keV) in this time interval is
(2.02 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+10.56 s in the 10-1000 keV band
is 3.5 +/- 0.3 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 14220
Subject
GRB 130215A: MITSuME Okayama Optical Observation
Date
2013-02-15T21:25:50Z (12 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:
We observed the field of GRB 130215A (D'Elia et al., GCN 14204)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2013-02-15 10:40:36 UT (~9.2 h after the burst).
We detected the previously reported afterglow (Zheng et al., GCNC 14205)
in Rc and Ic bands.
Photometric results and three sigma upper limits of the OT are listed below.
We used GSC2.3 catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' Rc Rc_err Ic Ic_err
-----------------------------------------------------------------------
0.39422 10:59:09 4080.0 >20.3 19.5 0.2 18.4 0.2
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 14221
Subject
GRB 130215A: GROND Detection of the Optical/NIR Afterglow
Date
2013-02-16T03:38:47Z (12 years ago)
From
Fabian Knust at MPE/GROND <fabian.knust@hotmail.de>
F. Knust, K. Varela, J. Greiner (all MPE Garching), and D. A. Kann (TLS Tautenburg) report on behalf of the GROND team:
We observed the field of GRB 130215A (Swift trigger 548760; D'Elia et al., GCN 14204) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla Observatory (Chile).
Observations started at 00:50 UT on 16.02.13, 23.3 hrs after the GRB trigger They were performed at an average seeing of 1".8 and at an average airmass of 1.98.
We detect a point source in most bands at position:
RA (J2000.0) = 02:54:00.70
Dec. (J2000.0) = +13:23:43.4
with an uncertainty of 0".4, close to the position reported by Zheng et al. (GCN 14205).
Based on the first 13 min of total exposures in g'r'i'z' and 14 min in JHK, we estimate preliminary magnitudes (all in AB system) of
g' = 21.0 +- 0.1 mag,
r' = 20.5 +-0.1 mag,
i' = 20.2 +- 0.1 mag,
z' = 19.9 +- 0.1 mag,
J = 19.4 +- 0.2 mag,
H = 19.0 +- 0.1 mag
and
K > 18.0 mag.
Given magnitudes are calibrated against GROND zeropoints as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.16 mag in the direction of the burst (Schlegel et al. 1998).
GCN Circular 14222
Subject
GRB 130215A: P200 NIR observations
Date
2013-02-16T10:11:26Z (12 years ago)
From
Daniel Perley at Caltech <dperley@astro.caltech.edu>
D. A. Perley (Caltech) reports:
I observed the location of GRB 130215A (D'Elia et al., GCN 14204) with
the Wide-Field Infrared Camera (WIRC) on the Palomar 200-inch telescope
on 2013-02-16 UT between 02:14 and 03:17. A series of nine 60-second
images each were taken in Ks, J, and H filters, followed by a second
series in Ks. High winds were present and seeing significantly degraded
over the course of the observations.
The optical/NIR afterglow (Zheng et al., GCN 14205, Covino et al., GCN
14211) is well-detected in a preliminary reduction of the Ks-band
images. Photometry (calibrated relative to 2MASS standards in the
field) gives the following magnitudes:
t_mid=24.89 hours : Ks = 17.23 +/- 0.05 mag (19.07 AB)
t_mid=25.65 hours : Ks = 17.34 +/- 0.08 mag (19.18 AB)
Further observations are planned.
GCN Circular 14227
Subject
GRB 130215A: Additional P200 NIR observations
Date
2013-02-17T10:56:45Z (12 years ago)
From
Daniel Perley at Caltech <dperley@astro.caltech.edu>
D. A. Perley (Caltech) reports:
I re-observed the location of GRB 130215A with the Wide-Field Infrared
Camera (WIRC) on the Palomar 200-inch telescope on 2013-02-17 UT between
02:09 and 02:37 and between 04:29 and 04:56. Images were again taken in
J, H, and Ks-bands; transmission and seeing conditions were good.
The NIR afterglow remains well-detected in the most recent images.
Photometry of the Ks-band images gives the following magnitudes (Vega):
t_mid=48.75 hours : Ks = 17.57 +/- 0.05 mag
t_mid=51.07 hours : Ks = 17.60 +/- 0.07 mag
Relative to the previous night (GCN 14222), these observations show
remarkably little fading (decay index alpha~0.4 between 25-50 hours,
compared to alpha~1.5 earlier; Butler et al., GCN 14212). This could
indicate contribution from a bright host galaxy, but no obvious
extension of the source is seen (in 1" seeing). Alternatively it could
indicate a bump, plateau or flare in the light curve. Further
observations with WIRC are not planned, but observations elsewhere are
encouraged to constrain further evolution of the afterglow.
GCN Circular 14237
Subject
GRB 130215A: Continued RATIR Optical and NIR Monitoring
Date
2013-02-18T09:24:53Z (12 years ago)
Edited On
2024-11-07T19:00:22Z (7 months ago)
From
Nat Butler at Az State U <natbutler@asu.edu>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Enrico Ramirez-Ruiz (UCSC), José A. de Diego (UNAM),
Leonid Georgiev (UNAM), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM),
Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:
We continue to observe the field of GRB 130215A (D'Elia et al.; GCN 14204)
with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org)
on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico
Nacional on Sierra San Pedro Mártir. From 2013/02 18.13 to 2013/02
18.21UTC (73.5 to 75.5 hours after the BAT trigger), we obtained a
total of 1.40
hours exposure in the r' and i' bands and 0.53 hours of exposure in the Z,
Y, J, and H bands.
In comparison with USNO-B1 and 2MASS, we derive the following AB
magnitudes, not corrected for Galactic extinction in the direction of the
GRB, for the afterglow:
r' 21.92 +/- 0.09
i' 20.92 +/- 0.07
Z 20.21 +/- 0.12
Y 20.38 +/- 0.15
J 20.37 +/- 0.13
H 19.59 +/- 0.11
We thank the staff of the Observatorio Astronómico Nacional in San Pedro
Mártir.
GCN Circular 14244
Subject
GRB 130215A: PTF P48 optical detection
Date
2013-02-21T06:08:29Z (12 years ago)
From
Leo Singer at CIT/PTF <lsinger@caltech.edu>
L. P. Singer (Caltech), S. B. Cenko (UC Berkeley), and D. A. Brown
(Syracuse) report on behalf of a larger collaboration:
We have imaged the 3-sigma Swift BAT error circle (S. Barthelmy, GCN
14214) of GRB130215A (Swift548760, S. Barthelmy, GCN 14204) with the
Palomar 48 inch Oschin telescope (P48) as part of the Palomar
Transient Factory (PTF).
Images were obtained in the Mould R filter on 2013-02-15 at 02:35:05
and 04:05:52 UTC, 1.1 and 2.6 hours after the trigger. We detect a
fading point source that is absent in the USNO B-1 catalog at
magnitudes of 16.38 and 17.59 at
RA(J2000) = 2h 54m 00.73s
DEC(J2000) = +13d 23' 43.0"
, matching the ROTSE-IIIb position (GCN 14205, Zheng & Flewelling).
Assuming a power-law decay, these two P48 observations give us an index
alpha=-1.25, consistent with the index of alpha=-1.24 reported by ROTSE
analysis (GCN 14208, Zheng et al.).
GCN Circular 14245
Subject
GRB 130215A: Suzaku WAM observation of the prompt emission
Date
2013-02-21T09:10:52Z (12 years ago)
From
Makoto Tashiro at Saitama U/Swift <tashiro@phy.saitama-u.ac.jp>
Y. Ishida, M. Tashiro, Y. Terada, W. Iwakiri, T. Yasuda, K. Takahara, M.
Asahina, S. Kobayashi, A. Sakamoto, H. Ueno, S. Sugimoto (Saitama U.),
M. Akiyama, N. Ohmori, E. Mochinaga, M. Yamauchi (Univ. of Miyazaki), K.
Yamaoka, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Hanabata, T. Kawano,
K. Takaki, R. Nakamura, Y. Tanaka, M. Ohno, Y. Fukazawa (Hiroshima U.),
S. Sugita (Nagoya U.), Y. E. Nakagawa (Waseda U.), Y. Urata, P. Tsai
(NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the
Suzaku WAM team, report:
The long GRB 130215A (Elia et al GCN14204; George et al GCN14219) was
detected by the the Suzaku Wide-band All-sky Monitor (WAM) which covers
an energy range of 50 keV - 5 MeV at 01:31:25.437 UT (=T0).
The observed light curve shows a single peak with a duration (T90) of
about 46.0 seconds. The fluence in 100 - 1000 keV was
1.04 (+0.13/-0.13) x 10^-5 erg/cm^2.
The 1-s peak flux measured from T0+1 s was
0.69 (+0.28/-0.36) photons/cm^2/s in the same energy range.
Preliminary result shows that the time-averaged spectrum from T0-7 s to
T0+55 s is well fitted by a single power-law with a photon index of
1.61 (+0.08/-0.07) (chi2/d.o.f = 13.9/14).
All the quoted errors are at statistical 90% confidence level, in which
the systematic uncertainties are not included.
The light curves for this burst will be available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html
GCN Circular 14303
Subject
GRB 130215A: Detection of the SN with the 10.4m GTC
Date
2013-03-14T13:30:03Z (12 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC),
J. Gorosabel (IAA-CSIC, UPV/EHU), R. Sanchez-Ramirez (IAA-CSIC),
G. Leloudas (OKC, Stockholm), Z. Cano (U. Iceland), D. Xu (DARK/NBI),
K. Wiersema (U. Leicester), J.P.U. Fynbo, D. Malesani, J. Hjorth (DARK/NBI),
P. Jakobsson (U. Iceland), O.E. Hartoog (U. Amsterdam) report on behalf of
a larger collaboration:
We have observed the optical counterpart of GRB 130215A (D'Elia et al.,
GCN 14204, Zheng et al., GCN 14205) with the 10.4 m GTC telescope
equipped with the OSIRIS imager and spectrograph. A spectroscopic
observation was performed on 12 March 2013 at a mean time of 20:52 UT,
25.8 days after the burst, corresponding to 16.2 days after the burst in the
rest frame, considering a redshift of z=0.597 (Cucchiara et al. GCN 14207).
The total exposure was 3x1200s using a low resolution grating (R~600)
covering a wavelength range 5000-10000 A. Due to its current location,
observations had to be carried out at high airmass, between 1.6 and 2.2.
There were thin cirrus but seeing was very good, at 0.6".
At this epoch, the spectrum presents undulations typical of SN spectra,
including a prominent bump at ~8200 A. Using SNID (Blondin & Tonry 2007,
ApJ, 666, 1024), we have compared the spectrum to a series of SN templates.
The spectrum gives a good match to a number of SNe Ic, including
broad-lined and normal events such as SN 2002ap and SN 1994I, around
maximum light or slightly after. By leaving the redshift unconstrained we
obtain the same template fit and derive a redshift of z=0.58+/-0.02, fully
consistent with the absorption line redshift.
We acknowledge excellent support from the GTC staff, in particular
Carlos A. Alvarez Iglesias.