GRB 090113
GCN Circular 8804
Subject
GRB 090113: Swift detection of a burst
Date
2009-01-13T19:06:45Z (16 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
H. A. Krimm (CRESST/GSFC/USRA), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
J. A. Kennea (PSU), C. B. Markwardt (CRESST/GSFC/UMD),
P. T. O'Brien (U Leicester), K. L. Page (U Leicester),
A. M. Parsons (GSFC), B. A. Rowlinson (U Leicester),
T. Sakamoto (NASA/UMBC), E. Troja (INAF-IASFPA),
T. N. Ukwatta (GSFC/GWU), L. Vetere (PSU) and H. Ziaeepour (UCL-MSSL)
report on behalf of the Swift Team:
At 18:40:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090113 (trigger=339852). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 32.073, +33.456 which is
RA(J2000) = 02h 08m 18s
Dec(J2000) = +33d 27' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows about 4 peaks
with a duration of about 20 sec. The peak count rate
was ~5000 counts/sec (15-350 keV), at ~2 sec after the trigger.
The XRT began observing the field at 18:41:50.1 UT, 70.9 seconds after
the BAT trigger. The onboard source-detection algorithm originally
centroided on a hot column. No other source was visible in the initial
TDRSS sub-image. We are waiting for the full Malindi dataset to detect
and localise the afterglow.
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 79 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The sub-image covers 25% of the BAT
error circle. The overlap of the 8'x8' region for the list of
sources generated on-board is 100% of the BAT error circle. This source
list is usually complete to about 18th magnitude. No correction
has been made for the expected extinction corresponding to E(B-V) of 0.08.
This burst was also detected by Fermi-GBM.
This burst is not to be confused with the BAT trigger (339853)
about 12 minutes later on the 1A 1118-61 HMXB source.
Burst Advocate for this burst is H. A. Krimm (krimm 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.)
GCN Circular 8806
Subject
GRB090113: XRT position
Date
2009-01-13T22:35:51Z (16 years ago)
From
Jamie A. Kennea at PSU/Swift-XRT <kennea@astro.psu.edu>
J. A. Kennea (PSU) and H. A. Krimm (CRESST/GSFC/USRA) report on behalf of
the Swift Team:
Analysis of preliminary data from the BAT trigger 339852 (GRB090113)
reveals an uncatalogued point source at RA, Dec = 32.05816, 33.42945 which
is equivalent to:
RA(J2000) = 02h 08m 13.9s,
Dec(J2000) = +33d 25m 46.0s
with an estimated uncertainty of 8 arcseconds radius (90% confidence).
Analysis is ongoing and an improved analysis will be reported as soon as
possible.
[GCN OPS NOTE(14jan09): Per author's request, the 090213 was changed
to 090113.]
GCN Circular 8807
Subject
GRB 090113: ROTSE-III Optical Limits
Date
2009-01-13T23:23:49Z (16 years ago)
From
Heather Swan at U.of Michigan/ROTSE <hflewell@umich.edu>
H. Swan (U Mich), E.S. Rykoff (UCSB), T. Guver (U Arizona), T.A. McKay
(U Mich), F. Yuan (U Mich), B. E. Schaefer (Louisiana State), R. Quimby
(Caltech), report on behalf of the ROTSE collaboration:
ROTSE-IIId, located at the Turkish National Observatory at Bakirlitepe,
Turkey, responded to GRB 090113 (Swift trigger 339852; H. A. Krimm, GCN
8804), producing images beginning 6.4 s after the GCN notice time. An
automated response took the first image at 18:49:02.4 UT, 503.2 s after
the burst, under windy conditions. We took 10 5-sec, 10 20-sec and 30
60-sec exposures. These unfiltered images are calibrated relative to
USNO A2.0 (R). Imaging is on going.
Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle, for both single images and coadding into
sets of 10; the field is not crowded. Individual images have limiting
magnitudes ranging from 14.9-16.4; we set the following specific limits.
start UT end UT t_exp(s) mlim t_start-tGRB(s) Coadd?
--------------------------------------------------------------------
18:49:02.5 18:51:08.2 125 16.6 503.3 Y
18:51:16.6 18:55:52.3 275 17.3 637.4 Y
18:60:45.7 19:05:21.5 275 17.3 1206.5 Y
GCN Circular 8808
Subject
GRB 090113: Swift-BAT refined analysis
Date
2009-01-14T00:07:29Z (16 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
GRB 090113: Swift-BAT refined analysis
J. Tueller (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (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), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-120 to T+302 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090113 (trigger #339852)
(Krimm, et al., GCN Circ. 8804). The BAT ground-calculated position is
RA, Dec = 32.067, 33.436 deg, which is
RA(J2000) = 02h 08m 16.0s
Dec(J2000) = +33d 26' 08.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 80%.
The mask-weighted light curve shows multiple peaks starting at ~T-10 sec
and ending at ~T+30 sec. T90 (15-350 keV) is 9.1 +- 0.9 sec
(estimated error including systematics).
The time-averaged spectrum from T-0.9 to T+10.0 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.60 +- 0.10. The fluence in the 15-150 keV band is 7.6 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.46 sec in the 15-150 keV band
is 2.5 +- 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/339852/BA/
GCN Circular 8809
Subject
GRB 090113: Enhanced Swift-XRT position
Date
2009-01-14T00:31:07Z (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 752 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 090113, 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 = 32.05678, +33.42857 which is equivalent
to:
RA (J2000): 02h 08m 13.63s
Dec (J2000): +33d 25' 42.9"
with an uncertainty of 1.7 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), the current algorithm is an
extension of this method.
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 8810
Subject
GRB 090113: Observations from NOT
Date
2009-01-14T05:59:12Z (16 years ago)
From
Antonio Deugarte at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (ESO), J. Gorosabel (IAA-CSIC),
D. Malesani (DARK/NBI), J.H. Knapen, J.R. S�nchez Gallego (IAC),
P. Stiles (Obs. del Sauzal) on behalf of a larger collaboration report
We have observed the field of GRB 090113 (Krimm et al.,
GCN 8804) with the 2.5m NOT telescope at Roque de los
Muchachos Observatory (La Palma, Spain). Preliminary
analysis of a 300s R-band exposure with mid time 20:45
UT (2.08h after the burst) does not show any new source
within the enhanced XRT error box (Goad et al., GCN
8809) down to a 3-sigma limiting magnitude of R > 23.4.
[GCN OPS NOTE(14jan09): Per author's request, DM was added
to the author list.]
GCN Circular 8811
Subject
GRB 090113: Swift-XRT refined analysis
Date
2009-01-14T07:37:44Z (16 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
P.A. Evans (U. Leicester) and H. A. Krimm (CRESST/GSFC/USRA) report on behalf
of the Swift-XRT team:
We have analysed 5.5 ks of XRT data for GRB 090113 (Krimm et al. GCN Circ.
8804), beginning 93 s after the BAT trigger. The data are entirely in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given by Goad
et al. (GCN. Circ 8809).
The light curve can be modelled with a power-law decay with a decay index of
alpha=0.991 (+/-0.042).
A spectrum formed from the PC mode data can be fitted with an absorbed power-law
with a photon spectral index of 2.28 (+0.20, -0.19). The best-fitting absorption
column is 3.20 (+0.63, -0.58) x 10^21, in excess of the Galactic value of 6.7 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 4.0 x 10^-11 (7.8 x
10^-11) erg cm^-2 count^-1.
If the light curve continues to decay with a power-law decay index of 0.991, the
count rate at T+24 hours will be 0.0063 count s^-1, corresponding to an observed
(unabsorbed) 0.3-10 keV flux of 2.5 x 10^-13 (4.9 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/00339852.
This circular is an official product of the Swift-XRT team.
GCN Circular 8812
Subject
GRB 090113: GROND Upper Limits
Date
2009-01-14T08:36:44Z (16 years ago)
From
Andrea Rossi at TLS Tautenburg <rossi@tls-tautenburg.de>
F. Olivares (MPE Garching), Andrea Rossi (Tautenburg Obs.), J. Greiner,
A. Yoldas (both MPE Garching), and A. Kupcu Yoldas (ESO) report on behalf
of the GROND team:
We observed the field of GRB 090113 (Swift trigger #339852; Krimm et al.,
GCN #8804) 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 00:35 UT on January 14th, 2009, about 6.1 hrs after
the GRB trigger, and continued until the GRB location approached the 20 degree
above horizon limit of the telescope, with 8.1 min of total exposures in
g'r'i'z' and 12.0 min in JHK. They were performed at an average seeing of 1.8"
and at an average airmass of 2.6.
We do not detect any object within the 1.7'' Enhanced Swift-XRT error circle
reported by Goad et al. (GCN #8809). Co-added images yield the following
upper limits (all in AB system):
g' > 23.3 mag,
r' > 23.4 mag,
i' > 22.6 mag,
z' > 22.6 mag,
J > 21.3 mag,
H > 20.7 mag and
K > 20.0 mag.
These upper limits are derived based on calibrating the images against the
GROND zeropoints as well as 2MASS field stars.
GCN Circular 8813
Subject
GRB 090113: Swift UVOT upper limits
Date
2009-01-14T13:39:14Z (16 years ago)
From
Samantha Oates at MSSL <sro@mssl.ucl.ac.uk>
S. R. Oates (MSSL-UCL) and H.A. Krimm (CRESST/GSFC/USRA) report on
behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of
GRB 090113 79s after the BAT trigger (Krimm et al., GCN 8804).
We do not detect any source at the enhanced Swift XRT position
(Evans et al. GCN 8809). Due to trigger 339853 the automatic
target sequence was cut short and only the white and u finding charts
were taken.
In the u finding chart and in the second orbit of data the XRT position
lies outside of the UVOT images. Therefore, we can only report the 3-
sigma upper
limit for the white finding chart exposure.
The 3-sigma upper limits for the finding chart exposure is:
Filter T_start T_stop Exp(s) Mag (3-sigma upper limit)
-------------------------------------------------------------
white 79 229 147 > 20.73
-------------------------------------------------------------
The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight of E_(B-V) = 0.08 mag.
All photometry is on the UVOT photometric system described in Poole et
al. (2008, MNRAS, 383, 627).
GCN Circular 8814
Subject
GRB 090113: LOAO Detection Limits in R, I, z, Y-band
Date
2009-01-15T06:53:10Z (16 years ago)
From
Induk Lee at Seoul National U <idlee@astro.snu.ac.kr>
Induk Lee, M. Im (Seoul National University, Korea), Y. Urata (ASIAA,
Taiwan; Saitama University, Japan), and T.S. Yoon (Kyungpook National
University, Korea)
We have observed the field of GRB 090113 (Krimm et al. GCN 8804) with 1.0m
telescope at Mt. Lemmon Optical Astronomy Observatory (LOAO) in Arizona. We
took R, I, z, Y-band images beginning at UT 02:00:28 and UT 02:29:47 on
January 14 2009 respectively. On stacked images with 3 x 300 secs exposures
in R and I-band images, no new source was detected.
The starting points of observation and 3 sigma detection limits (5" aperture
mag) are as below.
-------------------------------------------------------------------------------------------------------
Band Starting point exp. detection
limit
-------------------------------------------------------------------------------------------------------
R 07h 19m 49s after trigger 3x300sec 21.1
I 07h 49m 08s after trigger 3x300sec 20.5
-------------------------------------------------------------------------------------------------------
The detection limit was calibrated by USNO B1.0 stars.
This message may be cited.
--
Induk Lee
http://astro.snu.ac.kr/~idlee
PhD. candidate in Astronomy program,
Department of Physics & Astronomy, FPRD,
Seoul National University,
Seoul, 151-747, Korea
GCN Circular 8867
Subject
GRB090113: MAGIC telescope GeV observation
Date
2009-02-01T19:34:26Z (16 years ago)
From
Markus Garczarczyk at MPI/MAGIC <garcz@mppmu.mpg.de>
Becerra Gonzalez J. (IAC Tenerife), Gaug M. (IAC Tenerife),
Antonelli L.A. (INAF Rome), Bastieri D. (Univ. Padova),
Becker J. (Univ. Dortmund), Carosi A. (INAF Rome),
Covino S. (INAF Rome), Galante N. (MPI Munich),
Garczarczyk M. (IFAE Barcelona), La Barbera A. (INAF Palermo),
Longo F. (INFN Trieste), Lorenz E. (ETH Zuerich),
Paoletti R. (Univ. Siena), Persic M. (INAF and INFN Trieste),
Scapin V. (Univ. Udine), Spiro S. (INAF Rome)
and Teshima M.(MPI Munich) for the MAGIC collaboration
The MAGIC Imaging Atmospheric Cherenkov Telescope performed a follow-up
observation of the BAT burst GRB090113 (GCN circular 8804, Krimm et al.).
We received the GCN alert at 18:41:01 UT (T0+20s), before the sunset. Data
taking with MAGIC started at 20:06:08 UT (T0+4603s), when the GRB zenith
angle reached 5 degrees. The observation continued for 9405 s.
No evidence for VHE gamma-ray emission above the analysis threshold of
94 GeV was found. The observation was carried out in (less sensitive)
moon-observation mode from 21:39:01 UT on.
A preliminary analysis, for the hypothesis of steady emission and
assumption of a differential photon spectral index of -2.5, yields the
following 95% CL differential flux upper limits, including a 30%
systematic uncertainty on the telescope efficiency.
E ( 80- 125 GeV): 0.54 * 10^-10 erg cm^-2 s^-1
E ( 125- 175 GeV): 0.99 * 10^-10 erg cm^-2 s^-1
E ( 175- 300 GeV): 0.10 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV): 0.08 * 10^-10 erg cm^-2 s^-1
for a time window from 20:06:01 UT to 21:37:01 UT
E ( 125- 175 GeV): 0.93 * 10^-10 erg cm^-2 s^-1
E ( 175- 300 GeV): 0.23 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV): 0.08 * 10^-10 erg cm^-2 s^-1
for a time window from 21:39:01 UT to 22:32:01 UT
We can also exclude emission of a constant flux in any 100s time bin
smaller than:
E ( 80- 125 GeV): 13.89 * 10^-10 erg cm^-2 s^-1
E ( 125- 175 GeV): 8.88 * 10^-10 erg cm^-2 s^-1
E ( 175- 300 GeV): 3.40 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV): 1.22 * 10^-10 erg cm^-2 s^-1
for a time window from 20:06:01 UT to 21:37:01 UT
E ( 125- 175 GeV): 13.20 * 10^-10 erg cm^-2 s^-1
E ( 175- 300 GeV): 3.88 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV): 2.30 * 10^-10 erg cm^-2 s^-1
for a time window from 21:39:01 UT to 22:32:01 UT
This message can be cited.
GCN Circular 11393
Subject
GRB 090113, the review of the sky area in plate archives
Date
2010-11-09T20:31:53Z (15 years ago)
From
Valentyna Golovnya at Main Astro Obs,Kyiv <golov_v@ukr.ne>
GRB 090113, the review of the sky area in plate archives
V.V. Golovnya, L.N. Kizyun, L.K. Pakuliak (Main Astro Obs, Kyiv)
report:
We have undertaken the review of the sky area of GRB 090113 (Evans et
al., GCN 8809) on astronegatives, collected in Ukrainian NAS Main
astronomical observatory plate archive (1976-1996). All the plates with
the possible object appearance are digitized using Microtek ScanMaker
9800XL TMA flatbed scanner and have been placed into Golosiiv Plate
Archive database DBGPA with open access to them.
The list of plates is given in the table:
YYYYMMDD UT GUA_ID Exp. LimMag
19881004 23:10:05 GUA040C001340 16.0 16.2
19891025 20:42:19 GUA040C001518A 22.5 16.0
19891025 21:38:29 GUA040C001520A 16.0 15.0
19891026 19:55:50 GUA040C001521B 19.0 15.0
19891026 21:50:31 GUA040C001525 18.0 15.3
19930924 23:42:35 GUA040C002246 20.2 15.3
GUA ID - Double Wide-angle Astrograph (D/F=40/2000, S=103"/mm)
of the Ukrainian NAS Main astronomical observatory in Kyiv
(Marsden's number - 83) the plate number [1].
Exp. - Duration of the maximum exposures (minutes).
LimMag - Limited mag, derived in the 8 minutes area around the location
given in Evans et al., GCN 8809:
RA (J2000): 02h 08m 13.63s, Dec (J2000): +33d 25' 42.9".
The preview images can be found
http://gua.db.ukr-vo.org/img/grb/090113/index.html.
The images with full resolution are available via e-mail on demand.
References:
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org/