GRB 110213B
GCN Circular 11716
Subject
GRB 110213B: MAXI/GSC detection of a probable GRB
Date
2011-02-13T17:15:58Z (14 years ago)
From
Nobuyuki Kawai at Tokyo Tech <nkawai@hp.phys.titech.ac.jp>
H. Negoro, M. Nakajima, H. Ozawa, F. Suwa (Nihon U.), N. Kawai, M. Morii,
K. Sugimori, R. Usui, T. Toizumi (Tokyo Tech), M. Serino, T. Mihara,
Y.E. Nakagawa, M. Sugizaki, T. Yamamoto, T. Sootome, M. Matsuoka (RIKEN),
K. Kawasaki, S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA),
A. Yoshida, K. Yamaoka, S. Nakahira (AGU), H. Tsunemi, M. Kimura (Osaka U.),
Y. Ueda, N. Isobe, S. Eguchi, K. Hiroi (Kyoto U.), A. Daikyuji (Miyazaki U.),
A. Uzawa, T. Matsumura, K. Yamazaki (Chuo U.) report on behalf of the MAXI team:
MAXI/GSC triggered at UT 2011-02-13T14:31:48 on a bright uncatalogued X-ray
transient source. Judging from its location and spectral hardness ratio,
this transient is probably a gamma-ray burst.
Since the emission was detected only for a fraction of the triangular
transit response, the uncertainty of its position along the scan direction
is large. The center of the error box is
(R.A., Dec) = (+41.768, 0.952 deg) = (02 47 04, 00 57 07)(J2000)
with an uncertainty of 0.5 deg (90% containment radius).
The preliminary flux of the transient source was 1.3 Crab (2-4 keV),
2.2 Crab (4-10 keV), and 3.5 Crab (10-20 keV).
There was no significant detection at the transit location in the
previous orbit (92 min before the detection) with an upper limit of 20 mCrab.
There is no known bright X-ray source at the detected position.
Follow-up observations are encouraged.
GCN Circular 11720
Subject
GRB 110213B: MAXI/GSC refined analysis
Date
2011-02-14T01:21:42Z (14 years ago)
From
Nobuyuki Kawai at Tokyo Tech <nkawai@hp.phys.titech.ac.jp>
M. Morii, N. Kawai, K. Sugimori, R. Usui, T. Toizumi (Tokyo Tech),
H. Negoro, M. Nakajima, H. Ozawa, F. Suwa (Nihon U.), , M. Serino, T. Mihara,
Y.E. Nakagawa, M. Sugizaki, T. Yamamoto, T. Sootome, M. Matsuoka (RIKEN),
K. Kawasaki, S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA),
A. Yoshida, K. Yamaoka, S. Nakahira (AGU), H. Tsunemi, M. Kimura (Osaka U.),
Y. Ueda, N. Isobe, S. Eguchi, K. Hiroi (Kyoto U.), A. Daikyuji (Miyazaki U.),
A. Uzawa, T. Matsumura, K. Yamazaki (Chuo U.) report on behalf of the MAXI team:
We report further analysis of MAXI/GSC GRB 110213B (GCN #11716).
The refined position of the GRB is
(R.A., Dec) = (+41.61 deg, +1.19 deg) = (02 46 27, +01 11 14)(J2000)
with a rectangular 90% statistical error box with the following corners:
(R.A., Dec) = (+41.62 deg, +1.11 deg) = (02 46 29, +01 06 23)(J2000)
(R.A., Dec) = (+41.53 deg, +1.18 deg) = (02 46 7, +01 10 48)(J2000)
(R.A., Dec) = (+41.61 deg, +1.27 deg) = (02 46 26, +01 16 2)(J2000)
(R.A., Dec) = (+41.70 deg, +1.19 deg) = (02 46 48, +01 11 37)(J2000)
Without assumptions on the source constancy,
we obtain a rectangular error box with the following corners:
(R.A., Dec) = (+41.40 deg, +0.87 deg) = (02 45 36, +00 52 14)(J2000)
(R.A., Dec) = (+41.31 deg, +0.94 deg) = (02 45 13, +00 56 41)(J2000)
(R.A., Dec) = (+41.75 deg, +1.42 deg) = (02 46 59, +01 25 10)(J2000)
(R.A., Dec) = (+41.84 deg, +1.35 deg) = (02 47 22, +01 20 45)(J2000)
There is additional systematic uncertainty of 0.2 deg (90% containment radius).
GCN Circular 11722
Subject
Konus-Wind observation of GRB 110213B
Date
2011-02-14T11:22:18Z (14 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind
team, report:
The GRB 110213B discovered and localized by MAXI/GSC (Negoro et al., GCN
11716) was detected by Konus-Wind in the waiting mode at T0(KW)=52293 s
UT (14:31:33).
The burst light curve shows a single pulse with a duration of ~50 s.
As observed by Konus-Wind, the burst had a fluence of (1.77 +/-
0.16)x10^-5 erg/cm2 (in the 20 - 1400 keV range).
Modeling the K-W 3-channel time-integrated spectrum (from T0 to
T0+50 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.52 +/- 0.25, and Ep = 123 +/- 19 keV.
All the quoted errors are estimated at the 1 sigma confidence level.
The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB110213B/
GCN Circular 11725
Subject
GRB 110213B: Swift XRT observation
Date
2011-02-14T15:22:15Z (14 years ago)
From
Nobuyuki Kawai at Tokyo Tech <nkawai@hp.phys.titech.ac.jp>
S. Nakahira (AGU), N. Kawai, M. Morii (Tokyo Tech), and H. Negoro
(Nihon U.) report on behalf of the MAXI team:
Swift observed the field of GRB 110213B (Negoro et al., GCN Circ. 11716)
centered at the refined MAXI/GSC position reported by Morii et al.
(GCN Circ. 11720) for 2 ks from 2011-02-14T03:42:19 (T0+47 ks).
We find three point sources in the XRT field of view:
Source (R.A., Dec.) J2000 flux
------ ----------------------------------------------- -------
A (41.562 deg, +1.245 deg)= (02 46 15, +01 14 42) 0.008 c/s
B (41.757 deg, +1.146 deg)= (02 47 02, +01 08 46) 0.029 c/s
C (41.550 deg, +1.391 deg)= (02 46 12, +01 23 28) 0.003 c/s
Source A is located 0.1' from 1RXS J024615.3+011427, a RASS source
identified to an AF star.
Source C is located 0.1' from a quasar Q 0243+011.
No catalogued source was found for Source B.
Source B, the brightest of the three, and found near the edge of the
field of view, is the most likely candidate for the afterglow of
GRB 110213B. Another Swift observation is planned to confirm its fading.
We thank the Swift operation team for performing a prompt TOO observation
and making the data available quickly.
GCN Circular 11732
Subject
GRB 110213B: P60 Optical Afterglow Candidate
Date
2011-02-15T06:24:24Z (14 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. B. Cenko (UC Berkeley), E. O. Ofek, S. R. Kulkarni (Caltech), and A.
Rau (MPE Garching) report on behalf of a larger collaboration:
We have imaged the location of the possible X-ray afterglow
(Source "B"; Nakahira et al., GCN 11725) of the MAXI GRB110213B (Negoro et
al., GCN 11716) with the automated Palomar 60-inch telescope.
Observations began at 3:38 UT on 2011 February 15 (~ 37.1 hours after the
burst) in the r' filter.
We detect a source near the reported XRT position with coordinates
(J2000.0):
02:47:01.41 +01:08:46.3
Using several nearby objects in the USNO-B1 catalog for reference, we
measure a magnitude at this time of R = 19.8. No object is present at
this location, either in the USNO-B1 catalog or the Digitized Sky Survey.
Given the positional coincidence and the relative brightness, we consider
it likely this is the optical afterglow of GRB110213B. However, future
observations to establish fading will be required for confirmation.
GCN Circular 11735
Subject
GRB 110213B: Possible Host Galaxy in SDSS Stripe 82 Imaging
Date
2011-02-16T01:20:22Z (14 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. B. Cenko, J. S. Bloom, and A. A. Miller (UC Berkeley) report on behalf
of a larger collaboration:
The location of the X-ray (Nakahira et al., GCN 11725) and optical (Cenko
et al., GCN 11732) afterglow of GRB 110213B (Negoro et al, GCN 11716) was
observed repeatedly over the seven year period beginning in 1998 as part
of the SDSS Stripe 82 Survey (Bramich et al., MNRAS 2008, 386, 887). We
have extracted all images covering this location from the SDSS Stripe 82
database to create stacked frames in the g, r, and i filters. A
false-color composite image of the afterglow location can be found at:
http://astro.berkeley.edu/~cenko/public/grb/GRB110213B/sdss.png
Using 10 nearby point sources from SDSS for astrometry, we measure a
revised position for the P60 optical afterglow candidate of (J2000.0):
RA: 02:47:01.45 Dec: +01:08:46.5
The measured uncertainty in the P60-SDSS astrometric tie is 100 mas in
each coordinate.
Offset by 0.9" from the location of the afterglow, we find an extended
source in the pre-outburst SDSS Stripe 82 imaging in all three filters.
We measure coordinates (J2000.0) for this source:
RA: 02:47:01.41 Dec: +01:08:47.2
Using several nearby point sources from SDSS for comparison, we measure
magnitudes of g' = 23.7, r' = 22.8, i' = 22.3 Additional emission is
marginally detected in the i' filter approximately 3" south of this
position, but its relation to this object is unclear.
This extended source could be a relatively nearby host galaxy for
GRB110213B, although the red colors are somewhat unusual for GRB hosts.
GCN Circular 11736
Subject
GRB 110213B: Gemini South Redshift
Date
2011-02-16T04:10:22Z (14 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. B. Cenko (UC Berkeley), J. X. Prochaska (UC Santa Cruz / Lick
Observatory), A. Cucchiara, D. A. Perley, and J. S. Bloom (UC Berkeley)
report on behalf of a larger collaboration:
We have obtained a spectrum of the candidate optical afterglow of GRB
110213B (Negoro et al., GCN 11716) with the Gemini Multi-Object
Spectrograph mounted on the 8-m Gemini South telescope. Observations
began at 00:44 UT on Feb. 16 and cover the wavelength range from 3900 -
6700 A.
Superposed on a smooth continuum, we detect a series of strong, narrow
absorption lines corresponding to Mg I, Mg II, Fe II, and Fe II* at a
common redshift of z = 1.083. The detection of fine structure lines
firmly establishes this as the redshift of the GRB host galaxy.
An additional, strong Mg II absorption system is also present at z =
0.717. This may be related to the potential host candidate identified in
pre-outburst SDSS Stripe 82 imaging (Cenko et al., GCN 11735).
At z = 1.083, the prompt fluence measured by Konus (Golenetskii et al.,
GCN 11722) correponds to a prompt isotropic energy release of 5.5e52 erg
(20 - 1400 keV observer-frame bandpass).
We wish to thank the staff at Gemini Observatory, in particular Fredrik
Rantakyro, for the prompt execution of these observations.
GCN Circular 11743
Subject
GRB 110213B: GROND observations of the optical/NIR afterglow
Date
2011-02-16T19:35:01Z (14 years ago)
From
Jonny Elliott at MPE/GROND <jonnyelliott@mpe.mpg.de>
J. Elliott (MPE Garching), A. Nicuesa Guelbenzu (TLS Tautenburg), T.
Kruehler and J. Greiner (both MPE Garching) report on behalf of the GROND
team:
We observed the afterglow (Cenko et al., GCNs #11732, 11736) of GRB
110213B (Negoro et al., GCN #11716 & Morii et al., GCN #11720)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2m MPI/ESO telescope at La Silla Observatory
(Chile).
Observations started at 01:22 UT on 16.02.2011, 2.45 days after the GRB
trigger and were performed at high airmass.
Based on a stacked image with exposure time of 460 s, we estimate a
preliminary r' band magnitude of r' = 20.8 +/- 0.1 calibrated against SDSS
field stars. This implies a fading with respect to the earlier measurement
of Cenko et al. (#GCN 11732). In addition, the SED of the object is
consistent with a power-law, and hence we confirm the source as the
optical afterglow of GRB 110213B.
GCN Circular 11748
Subject
GRB110213B: X-ray afterglow confirmation
Date
2011-02-18T09:11:45Z (14 years ago)
From
Raffaella Margutti at U. di Milano Bicocca <raffaella.margutti@brera.inaf.it>
R. Margutti, (INAF-OAB), Nakahira (AGU), M. Morii, N. Kawai (Tokyo Tech),
H. Negoro (Nihon U.) and A. Melandri (INAF-OAB) report on behalf of the
Swift-XRT and MAXI team:
The Swift-XRT conducted a second observation of GRB 110213B (Negoro et
al. GCN. Circ. 11716), gathering 4.9 ks of data between T0+250ks and
T0+275 ks. Source B reported by Nakahira (GCN Circ. 11725)
has faded to a level of 0.005 +/- 0.001 count/sec, with a power-law decay
index of alpha= -1.4 +/- 0.3. This source is thus confirmed as the X-ray
afterglow of GRB 110213B.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020157.
This circular is an official product of the Swift-XRT team.
GCN Circular 11749
Subject
GRB 110213B: Swift/UVOT observations
Date
2011-02-18T13:51:47Z (14 years ago)
From
Samantha Oates at MSSL <sro@mssl.ucl.ac.uk>
S. R. Oates (MSSL-UCL) & R. Margutti, (INAF-OAB) reports on behalf of
the Swift-UVOT team
The Swift/UVOT began settled observations of the field of the MAXI GRB
110213B
~13hrs after the trigger (Negoro et al., GCN Circ. 11716). The optical
afterglow
detected by P60 (Cenko et al, GCN Circ. 11732, 11735) and GROND
(Elliott et al,
GCN Circ. 11743) only lies in the UVOT field of view for 3 images, one
per
filter (white, v and u) obseved at ~3 days after the trigger.
Preliminary magnitudes using the UVOT photometric system (Poole et al.
2008,
MNRAS, 383, 627) for the single exposures at the location of the optical
afterglow are:
Filter T_start(s) T_stop(s) Exp(s) 3sigUL
#####################################################
wh 256170 256432 259 > 20.78
v 256438 256691 249 > 19.23
u 255901 256164 259 > 19.62
#####################################################
The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).