- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Thu 22 Dec 11 14:52:21 UT
NOTICE_TYPE: Fermi-GBM Flight Position
RECORD_NUM: 47
TRIGGER_NUM: 346258317
GRB_RA: 207.617d {+13h 50m 28s} (J2000),
207.718d {+13h 50m 52s} (current),
207.191d {+13h 48m 46s} (1950)
GRB_DEC: +59.067d {+59d 03' 60"} (J2000),
+59.008d {+59d 00' 27"} (current),
+59.314d {+59d 18' 50"} (1950)
GRB_ERROR: 3.43 [deg radius, statistical plus systematic]
GRB_INTEN: 4938 [cnts/sec]
DATA_SIGNIF: 45.50 [sigma]
INTEG_TIME: 0.256 [sec]
GRB_DATE: 15917 TJD; 356 DOY; 11/12/22
GRB_TIME: 53515.02 SOD {14:51:55.02} UT
GRB_PHI: 230.00 [deg]
GRB_THETA: 150.00 [deg]
DATA_TIME_SCALE: 0.2560 [sec]
HARD_RATIO: 0.26
LOC_ALGORITHM: 3 (version number of)
MOST_LIKELY: 97% GRB
2nd_MOST_LIKELY: 1% Generic Transient
DETECTORS: 0,0,0, 0,1,0, 1,1,1, 0,0,1, 0,0,
SUN_POSTN: 270.43d {+18h 01m 44s} -23.44d {-23d 26' 11"}
SUN_DIST: 97.14 [deg] Sun_angle= 4.2 [hr] (West of Sun)
MOON_POSTN: 239.49d {+15h 57m 58s} -21.53d {-21d 31' 45"}
MOON_DIST: 84.69 [deg]
MOON_ILLUM: 6 [%]
GAL_COORDS: 109.22, 56.46 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 164.94, 61.86 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: Fermi-GBM Flight-calculated Coordinates.
COMMENTS: This trigger occurred at longitude,latitude = 92.87,18.58 [deg].
- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Thu 22 Dec 11 14:54:26 UT
NOTICE_TYPE: Fermi-GBM Ground Position
RECORD_NUM: 59
TRIGGER_NUM: 346258317
GRB_RA: 189.770d {+12h 39m 05s} (J2000),
189.898d {+12h 39m 36s} (current),
189.233d {+12h 36m 56s} (1950)
GRB_DEC: +65.840d {+65d 50' 24"} (J2000),
+65.774d {+65d 46' 28"} (current),
+66.115d {+66d 06' 53"} (1950)
GRB_ERROR: 1.95 [deg radius, statistical only]
DATA_SIGNIF: 67.10 [sigma]
DATA_INTERVAL: 0.256 [sec]
GRB_DATE: 15917 TJD; 356 DOY; 11/12/22
GRB_TIME: 53515.02 SOD {14:51:55.02} UT
GRB_PHI: 220.00 [deg]
GRB_THETA: 141.00 [deg]
E_RANGE: 44.032 - 279.965 [keV]
LOC_ALGORITHM: 4143 (Gnd S/W Version number)
SUN_POSTN: 270.43d {+18h 01m 44s} -23.44d {-23d 26' 11"}
SUN_DIST: 107.51 [deg] Sun_angle= 5.4 [hr] (West of Sun)
MOON_POSTN: 239.52d {+15h 58m 04s} -21.53d {-21d 31' 54"}
MOON_DIST: 95.01 [deg]
MOON_ILLUM: 6 [%]
GAL_COORDS: 124.95, 51.24 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 143.43, 59.85 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: Fermi-GBM Ground-calculated Coordinates.
COMMENTS: Bright hard burst in the GBM.
COMMENTS: This Notice was ground-generated -- not flight-generated.
COMMENTS:
COMMENTS: NOTE: This GBM event is temporally(3.0<100sec) coincident with the INTEGRAL_SPIACS event (trignum=6419).
- GCN Circular #12714
IPN Triangulation of GRB 111222A (short/hard/intense)
K. Hurley, on behalf of the Mars Odyssey and MESSENGER GRB teams,
I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,
J. Goldsten, on behalf of the MESSENGER NS GRB team,
S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline on behalf of the Konus-Wind team,
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
V. Connaughton, M. Briggs, and C. Meegan, on behalf of the Fermi
GBM team, and
S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on
behalf of the Swift-BAT team, report:
The short-duration, hard, intense GRB 111222A has been observed by
Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS), MESSENGER (GRNS), Mars
Odyssey (HEND), and Swift (BAT) (outside the coded field of view) so
far, at about 53515 s UT (14:51:55). We have triangulated it to a
preliminary, 3 sigma error box whose coordinates are:
---------------------------------------------
RA(2000), deg Dec(2000), deg
---------------------------------------------
Center:
179.193 (11h 56m 46s) +69.036 (+69d 02' 10")
Corners:
179.439 (11h 57m 45s) +68.877 (+68d 52' 37")
179.815 (11h 59m 16s) +69.133 (+69d 07' 59")
178.942 (11h 55m 46s) +69.195 (+69d 11' 41")
178.575 (11h 54m 18s) +68.936 (+68d 56' 11")
---------------------------------------------
The error box area is 317 sq. arcmin, and its maximum
dimension is 29 arcmin.
This box can be improved.
The time history and spectrum will be given in a forthcoming GCN Circular.
A Swift ToO observation has been requested.
- GCN Circular #12715
S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:
The short hard intense GRB 111222A
(localized by IPN: Hurley et al., GCN 12714)
triggered Konus-Wind at T0=3D53515.918s UT (14:51:55.918)
The light curve consists of a single multi-peaked pulse with
a total duration of ~300 ms.
The emission is seen up to ~3 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB111222_T53515/
As observed by Konus-Wind the burst
had a fluence of (7.2 =B1 0.7)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0 s,
of (5.1 =B1 0.7)x10-5 erg/cm2/s
(both in the 20 keV - 3 MeV energy range).
The spectrum of the burst (measured from T0 to T0+0.256 s)
is best fitted in the 20 keV - 3 MeV range
by a power law with exponential cutoff model, for which
alpha =3D -0.35 (-0.13, +0.14),
and Ep =3D 762(-89, +101) keV,
chi2 =3D 51.1/45 dof.
All the quoted results are preliminary.
All the quoted errors are at the 90% confidence level.
- GCN Circular #12716
D. Grupe (PSU) reports on behalf of the Swift-XRT team:
We have analyzed 2.3 ks of XRT data for the IPN-detected burst: GRB
111222A (Hurley et al. et al. GCN Circ. 12714), from 92.9 ks to 95.2 ks
after the IPN trigger. The data are entirely in Photon Counting (PC)
mode. An X-ray source is detected within the IPN error circle. Using
1964 s of PC mode data and 1 UVOT images, we find an enhanced XRT
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 179.21977, +69.07116 which is
equivalent to:
RA (J2000): 11h 56m 52.74s
Dec(J2000): +69d 04' 16.2"
with an uncertainty of 3.1 arcsec (radius, 90% confidence). This
position is 322 arcsec from the IPN position. We cannot determine at
the present time whether the source is fading.
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.5 (+4.9, -4.3). The
best-fitting absorption column is consistent with the Galactic value
of 1.7 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 6.8 x 10^-11 (7.0 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 0 (+2.1, -0) x 10^22 cm^-2
Galactic foreground: 1.7 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index: 1.5 (+4.9, -4.3)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020194.
This circular is an official product of the Swift-XRT team.
- GCN Circular #12717
M. H. Siegel and D. Grupe (PSU) report on behalf of the Swift/UVOT team:
We have analyzed 2.3 ks of UVOT data for the IPN-detected burst: GRB
111222A (Hurley et al. et al. GCN Circ. 12714), from 92.9 ks to 95.2 ks
after the IPN trigger. The data are entirely in the white filter. We detect a faint
optical source consistent with the XRT source reported in Grupe (GCN Circ.
12716) at a position of RA, Dec = 179.22008, Dec = 69.07096 , which
is equivalent to:
RA (J2000): 11h 56m 52.82s
Dec(J2000): +69d 04' 15.4"
with an uncertainty of 0.51 arcsec (radius, 90% confidence). Preliminary
photometry using the UVOT photometric system (Breeveld et al. 2011, AIP
Conf. Proc. 1358, 373) shows a white magnitude of 19.34+-0.03. The magnitude
is not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.01 in
the direction of the burst (Schlegel et al. 1998).
We note, however, that a source is present at this position in the DSS. Follow-up
observations will be needed to determine if the X-ray/optical source is indeed the
GRB afterglow.
- GCN Circular #12718
L.P. Xin, J.Y. Wei, Y. L. Qiu, J. Wang, J.S. Deng,
C. Wu, X. H. Han, Dong.Xu on behalf of EAFON report:
We began to observe GRB 111222A ( Hurley et al., GCN 12714)
with Xinglong TNT telescope at Dec 24th, 18:23:18.453 (UT), about 2.15d after
the burst. 15 R-band images were obtained. The exposure time is 300 sec
for each frame.
The source reported by Siegel et al. (GCN 12717)
was detected in the each R band image.
The brightness of this source was estimated
to be about 17.6 mag and without any significant change
during our observations time
relatively to the reference object in USNO B1.0 R2 mag.
The Coordinates of the reference object and its brightness are
11:56:39.863 +69:03:55.50 J2000 R2=16.86 mag, respectively.
The brightness of the reported source ( Siegel et al. GCN 12717 )
we observed is brighter than the magnitude reported by USNO B1.0 R2mag
which was R2=18.06 mag.
This message may be cited.
More observations are encouraged.
Thanks for the observation assistant of TNT telescope at Xinglong observatory.
- GCN Circular #12719
D. Xu (WIS/NAOC), X.-H. Zhao, J.-M. Bai (YNAO), J.-R. Mao (KASI/YNAO) report:
We observed the field of GRB 111222A (Hurley et al., GCN 12714; Grupe
et al., GCN 12716; Siegel et al., GCN 12717) with the 2.4m GMG
telescope equipped with YFOSC. Observations started at 17:34 UT on
2011-12-24 (i.e., 50.717 hrs after the burst) in a seeing of ~3.2",
and 3x600s SDSS r-band and 3x600s SDSS z-band images were obtained.
As noted in GCN 12717, there was a SDSS star present at the UVOT
position which has the following mags:
u=22.34+/-0.30
g=19.47+/-0.01
r=18.08+/-0.01
i=16.66+/-0.01
z=15.85+/-0.01.
The star had r=18.08+/-0.01 mag and z=15.83+/-0.02 mag in our stacked
images (calibrated with nearby SDSS stars), being consistent with the
SDSS r- and z-band archival mags.
We thank the GMG staff, especially J.-J. Zhang for performing these
observations.
- GCN Circular #12732
N. Ohmori, M. Akiyama, M. Yamauchi (Univ. of Miyazaki), M. Ohno,
Y. Hanabata, T. Uehara, T. Kawano, K. Takaki, M. Mizuno, Y. Fukazawa
(Hiroshima U.), K. Yamaoka (Aoyama Gakuin U.), W. Iwakiri, M. Tashiro,
Y. Terada, T. Yasuda, K. Takahara, M. Asahina, S. Kobayashi, A. Sakamoto
(Saitama U.), S. Sugita (Nagoya U.), M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa (Waseda U.), C-J. Chuang, Y. Urata, P. Tsai (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo),
The short hard intense GRB111222A (localized by IPN: Hurley et al., GCN 12714)
was detected by the Suzaku Wide-band All-sky Monitor (WAM) which covers
an energy range of 50 keV - 5 MeV at 14:51:55 UT (=T0).
The observed light curve shows a double-peaked structure starting at
T0 s, ending at T0+2 s with a duration (T90) of about 1 seconds.
The fluence in 100 - 1000 keV was 3.98 (-1.21, +0.74) x 10^-6 erg/cm^2.
The 1-s peak flux measured from T0 s was 4.70 (-1.18, +1.00)
photons/cm^2/s in the same energy range.
Preliminary result shows that the time-averaged spectrum from T0 to
T0+2 s is well fitted by a power-law with exponential cutoff model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha : -0.28 (-0.49, +0.43), and
Epeak : 629 (-50, +61) keV (chi^2/d.o.f. = 94.8/98).
All the quoted errors are at statistical 90% confidence level.
The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html
- GCN Circular #12805
D. Grupe (PSU) and M. Siegel (PSU) report on behalf of the
Swift team:
Swift re-observed the field of the IPN burst GRB 111222A (Hurley et
al., GCN circ. 12714) on 2011-12-31 for 5 ks. We do not detect the
X-ray source reported by Grupe (GCN circ. 12716) in a 2.5 ks
observation 27 hours after the burst anymore. The 3-sigma upper
limit at the position of the afterglow is 2.2e-3 counts/s in the
Swift XRT. We conclude that the X-ray source has faded and is the
afterglow of GRB 111222A.
Swift/UVOT observed the burst for 4.9 ks, with all data taken
in the white filter. We confirm the previously reported optical
source noted in Siegel and Grupe (GCN Circ. 12717) that was also
present in the DSS images. We find that the source has faded
significantly since the initial observation from a white magnitude
of 19.34+-0.03 to 19.89+-0.03. This implies that the previous
observation recorded light from both the host galaxy and the
optical afterglow of the burst. Further observations of the
host galaxy are strongly encouraged.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020194.
This circular is an official product of the Swift team.
- GCN Circular #12806
Arne Rau (MPE) and Charles Meegan (USRA) report on behalf of the Fermi
GBM Team:
"At 14:51:55.02 UT on 22 December 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 111222A (trigger 346258317 / 111222619). The
burst
was was also detected by the 3rd Interplanetary Network (Hurley et al.
2011, GCN 12714)
and The GBM on-ground location is consistent with the IPN position.
The angle from the Fermi LAT boresight is 136 degrees. Moreover, this
burst was bright
enough to result in a Fermi spacecraft autonomous rapid repoint (ARR)
maneuver.
The GBM light curve shows a single pulse with a duration (T90) of about
0.32 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.320 s is best fit by
a power law
function with an exponential high-energy cutoff. The power law index is
-0.38 +/- 0.06
and the cutoff energy, parameterized as Epeak, is 725 +/- 45 keV.
The event fluence (10-1000 keV) in this time interval is (1.502 +/-
0.034)E-05 erg/cm^2.
The 64-msec peak photon flux measured starting from T0+0.0 s in the
10-1000 keV band
is 60.2 +/- 3.4 ph/s/cm^2.
The spectral analysis results presented above are preliminary; final
results will be published
in the GBM GRB Catalog."
- GCN Circular #12807
V.V. Golovnya (Main Astro Obs, Kyiv)
report:
We have undertaken the review of the sky area in vicinity of=20
GRB 111222A (M. H. Siegel and D. Grupe, GCN Circ.12717) on=20
astronegatives, collected in Ukrainian NAS Main astronomical=20
observatory plate archive (1976-1996). All the plates with=20
the possible object appearance are digitized using Microtek=20
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed=20
scanners and have been placed into Golosiiv Plate Archive=20
database DBGPA with open access to them.
The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2=20
19850424/193653 GUA040C000630 16.0 15.35 1575-03212355
19860301/224314 GUA040C000837A 18.0 16.35 1575-03212664
19860409/202551 GUA040C000846 16.0 15.75 1575-03212662
Plates: =96the plates archive identifier of DWA (D/F=3D400/2000,=20
GUA040C M=3D103"/mm) of the Ukrainian NAS Main Astro obs.
(Marsden's number - 83) the plate number [1].
Exp. - Duration of the maximum exposure (minutes).=20
LimMag - Limited V mag, derived in the 20 minutes area around=20
the location given in GCN Circ.12717:=20
RA (J2000): 11h 56m 52.82s,Dec(J2000): +69d 04' 15.4"
Star USNOA2 - Comparison star.
The preview images of 3 areas together with =20
the 20x20 min.of arc area from SkyMap can be found in =20
http://gua.db.ukr-vo.org/img/grb/111222A/index.html
The images with full resolution are available via e-mail on=20
demand.
References:
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org
- GCN Circular #13001
D. Grupe and M. Siegel (PSU) report on behalf of the Swift team:
Swift re-observed the field of the IPN burst GRB 111222A (Hurley et
al., GCN circ. 12714) on 2012-02-06/07 for 5.1 ks. We do not
detect the X-ray source reported by Grupe (GCN circ. 12716) in a
2.5 ks observation 27 hours after the burst. The 3-sigma upper
limit at the position of the afterglow is 1.4e-3 counts/s in the
Swift XRT. This observation confirms our findings from a 5 ks Swift
observation obtained on 2011-12-31 (Grupe & Siegel, GCN circ.
12805) that the source has faded. We therefore conclude that the
X-ray source reported by Grupe (GCN circ. 12716) is the afterglow
of GRB 111222A.
UVOT observations show that the source reported in Grupe & Siegel
(GCN circ. 12805) has remained at constant white magnitude of
19.88 since fading by 0.48 magnitudes between the first and
second Swift/UVOT observations. Multi-color photometry confirms
that the source is very red (B-V=1.26), with only upper limits in
UV passbands). Its relation to the burst is still unknown.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020194.
This circular is an official product of the Swift team.
Previous IAU Circulars 