Gamma-ray Burst 011130

(All information courtesy of the instrument teams.)

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Results of Observations

GCN/BACODINE POSITION NOTICE


TITLE:          GCN/HETE BURST POSITION NOTICE
NOTICE_DATE:    Fri 30 Nov 01 10:53:16 UT
NOTICE_TYPE:    HETE Ground Analysis
TRIGGER_NUM:    1864,   Seq_Num: 1
GRB_DATE:       12243 TJD;   334 DOY;   01/11/30
GRB_TIME:       22775.66 SOD {06:19:35.66} UT
TRIGGER_SOURCE: Trigger on the 2-30 keV band.
WXM_SIG/NOISE:  7 sig/noise  on a 5.120 [sec] timescale
SC_-Z_RA:       244 [deg]
SC_-Z_DEC:      -21 [deg]
WXM_CNTR_RA:    44.538d {+02h 58m 09s} (J2000),
                44.563d {+02h 58m 15s} (current),
                43.872d {+02h 55m 29s} (1950)
WXM_CNTR_DEC:   +7.411d {+07d 24' 40"} (J2000),
                +7.419d {+07d 25' 07"} (current),
                +7.211d {+07d 12' 41"} (1950)
WXM_MAX_SIZE:    120.00 [arcmin] diameter
WXM_LOC_SN:      6 sig/noise (pt src in image)
SUN_POSTN:      246.35d {+16h 25m 25s}  -21.66d {-21d 39' 34"}
SUN_DIST:       154.61 [deg]
MOON_POSTN:      59.04d {+03h 56m 09s}  +17.91d {+17d 54' 27"}
MOON_DIST:       17.57 [deg]
MOON_ILLUM:     100 [%]
GAL_COORDS:     169.12,-43.81 [deg] galactic lon,lat of the burst
COMMENTS:       Possible GRB.
COMMENTS:       WXM error box is circular; not rectangular.
COMMENTS:       Burst_Validity flag is true.

GCN notice #1165
GRB011130 (=H1864): An X-Ray Rich GRB Detected by HETE
G. Ricker, D. Lamb, and S. Woosley on behalf of the HETE Science Team;
R. Vanderspek, G. Crew, J. Doty, G. Monnelly, J. Villasenor, N. Butler, T. Cline, J.G. Jernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin, J. Braga, R. Manchanda, and G. Pizzichini, on behalf of the HETE Operations and HETE Optical-SXC Teams;
N. Kawai, M. Matsuoka, Y. Shirasaki, T. Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Donaghy, and C. Graziani, on behalf of the HETE WXM Team;
J-L Atteia, M. Boer, J-F Olive, J-P Dezalay, and K. Hurley on behalf of the HETE FREGATE Team;
write:
The HETE WXM instrument has detected (>7 sigma) a GRB (trigger H1864). The burst occurred at 22775.66 SOD (6:19:35 UT) on 30 November. The burst is well-localized by the WXM but occurred before dusk and at full moon (phase >0.96); consequently the error in the spacecraft aspect is much larger than normal. The statistical error radius in the WXM localization is 14 arcmin (90% confidence). In addition, we estimate a systematic error radius at present of 60 arcmin about this location due to the uncertainty in spacecraft aspect. The resulting localization is therefore
R.A. = 02h58m09s.1, Dec = 07o24'40"
with a total error of 60 arcminutes.
The burst duration in the 2-25 keV band was ~5 s. A total of 500 counts were detected during that interval. The spectrum is soft, making an estimate of the peak flux and fluence highly uncertain.
Further refinement of the spacecraft aspect, and thus the burst localization, is in progress.
This message is quotable.

GCN/BACODINE POSITION NOTICE


TITLE:          GCN/HETE BURST POSITION NOTICE
NOTICE_DATE:    Fri 30 Nov 01 13:55:55 UT
NOTICE_TYPE:    HETE Ground Analysis
TRIGGER_NUM:    1864,   Seq_Num: 2
GRB_DATE:       12243 TJD;   334 DOY;   01/11/30
GRB_TIME:       22775.66 SOD {06:19:35.66} UT
TRIGGER_SOURCE: Trigger on the 2-30 keV band.
WXM_SIG/NOISE:  7 sig/noise  on a 5.120 [sec] timescale
SC_-Z_RA:       244 [deg]
SC_-Z_DEC:      -21 [deg]
WXM_CNTR_RA:    44.455d {+02h 57m 49s} (J2000),
                44.480d {+02h 57m 55s} (current),
                43.790d {+02h 55m 10s} (1950)
WXM_CNTR_DEC:   +7.372d {+07d 22' 18"} (J2000),
                +7.379d {+07d 22' 46"} (current),
                +7.172d {+07d 10' 19"} (1950)
WXM_CORNER1:    44.4660   6.6530 [deg]
WXM_CORNER2:    45.0080   6.9190 [deg]
WXM_CORNER3:    43.8980   7.8320 [deg]
WXM_CORNER4:    44.4480   8.0830 [deg]
WXM_MAX_SIZE:    86.67 [arcmin] diameter
WXM_LOC_SN:      6 sig/noise (pt src in image)
SUN_POSTN:      246.35d {+16h 25m 25s}  -21.66d {-21d 39' 34"}
SUN_DIST:       154.52 [deg]
MOON_POSTN:      59.04d {+03h 56m 09s}  +17.91d {+17d 54' 27"}
MOON_DIST:       17.66 [deg]
MOON_ILLUM:     100 [%]
GAL_COORDS:     169.07,-43.89 [deg] galactic lon,lat of the burst
COMMENTS:       Definite GRB.
COMMENTS:       Burst_Validity flag is true.
COMMENTS:       WXM data refined since S/C_Last Notice.

GCN/BACODINE POSITION NOTICE


TITLE:          GCN/HETE BURST POSITION NOTICE
NOTICE_DATE:    Sat 01 Dec 01 01:05:55 UT
NOTICE_TYPE:    HETE Ground Analysis
TRIGGER_NUM:    1864,   Seq_Num: 4
GRB_DATE:       12243 TJD;   334 DOY;   01/11/30
GRB_TIME:       22775.66 SOD {06:19:35.66} UT
TRIGGER_SOURCE: Trigger on the 2-30 keV band.
WXM_SIG/NOISE:  7 sig/noise  on a 5.120 [sec] timescale
SC_-Z_RA:       244 [deg]
SC_-Z_DEC:      -21 [deg]
WXM_CNTR_RA:    46.402d {+03h 05m 36s} (J2000),
                46.427d {+03h 05m 42s} (current),
                45.748d {+03h 02m 60s} (1950)
WXM_CNTR_DEC:   +3.810d {+03d 48' 36"} (J2000),
                +3.817d {+03d 49' 02"} (current),
                +3.617d {+03d 37' 01"} (1950)
WXM_MAX_SIZE:    20.00 [arcmin] diameter
WXM_LOC_SN:      6 sig/noise (pt src in image)
SUN_POSTN:      246.35d {+16h 25m 25s}  -21.66d {-21d 39' 34"}
SUN_DIST:       153.69 [deg]
MOON_POSTN:      59.04d {+03h 56m 09s}  +17.91d {+17d 54' 27"}
MOON_DIST:       18.73 [deg]
MOON_ILLUM:     100 [%]
GAL_COORDS:     174.44,-45.22 [deg] galactic lon,lat of the burst
COMMENTS:       Definite GRB.
COMMENTS:       WXM error box is circular; not rectangular.
COMMENTS:       Burst_Validity flag is true.
COMMENTS:       WXM data refined since S/C_Last Notice.

GCN notice #1169
GRB011130 (=XRF011130): Revised Localization of an X-ray Flash/X-ray Rich GRB
G. Ricker, D. Lamb, and S. Woosley on behalf of the HETE Science Team;
N. Butler, G. Crew, J. Doty, G. Monnelly, G. Prigozhin, R. Vanderspek, J. Villasenor, T. Cline, J.G. Jernigan, A. Levine, F. Martel, E. Morgan, J. Braga, R. Manchanda, and G. Pizzichini, on behalf of the HETE Operations and HETE Optical-SXC Teams;
C. Graziani, N. Kawai, M. Matsuoka, Y. Shirasaki, T. Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Tavenner, and T. Donaghy, on behalf of the HETE WXM Team;
J-L Atteia, M. Boer, J-F Olive, J-P Dezalay, and K. Hurley on behalf of the HETE FREGATE Team;
write:
The localization of H1764, an X-ray flash (XRF) reported as GRB011130 in GCN Circular 1165, has been greatly improved. The burst occurred at 22775.66 SOD (6:19:35 UT) on 30 November.
Selection by hand of optimal background and foreground time intervals, and the optimal energy interval has resulted in a 19.6 sigma detection of GRB011130 in the WXM 2-10 keV energy band. The improved statistical error radius in the WXM localization is 7.2 arcmin (90% confidence). The spacecraft aspect has been improved to lie within a circle of 3.6 arcmin radius. The revised localization of H1864 is centered at:
R.A. = 03h05m36s.45, Dec. = 3o48'37"
A circle centered on this location having a radius 10 arcmin contains the burst location with > 90% confidence.
The revised location differs significantly (~4 degrees) from the originally reported one; the contributing factors to the large difference are explained in detail in the "Special Note on Burst 1864" posted at:
http://space.mit.edu/HETE/Bursts/
A careful re-analysis of the full WXM data set indicates that the burst is considerably longer, and of higher fluence, than reported in GCN1135. In the 2-10 keV band, the duration is ~30 s, with ~3100 counts contained in the burst.
Further refinement of the spacecraft aspect, and thus the burst localization, continues.
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GCN notice #1170
D.W. Fox (Caltech) and P.A. Price (MSO/ANU), with S. Pravdo, E. Helin, K. Lawrence, and M. Hicks of the NEAT/Palomar team, report on behalf of the Caltech-NRAO-CARA GRB collaboration:
"We have observed the 10 arcmin-radius error circle of the XRF011130 (GCN 1169) with the 48-inch NEAT automated telescope on Mt. Palomar on Dec 1.24 UT. In unfavorable conditions of moon illumination and seeing, we do not find any objects not present in DPOSS images of the region. We estimate the limiting magnitude of our images as R = 18.5 mag. Further observations are planned."
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GCN notice #1171
J. Greiner (AIP, Potsdam), S. Klose (TLS, Tautenburg), A. A. Henden (USRA/USNO, Flagstaff), A. Riffeser (Universitaets-Sternwarte Muenchen), and A. J. Castro-Tirado (IAA Granada, Spain)
report:
The 30 arcmin error box of the X-ray transient 011130 (GCN/HETE BURST POSITION NOTICE; 1864, Seq_Num: 3) was surveyed with the Calar Alto 1.23-m telescope in R and I on November 30, starting 22:45 UT, i.e., about 16.5 hrs after the burst trigger. Seeing was ~ 1.2 arcsec. The images completely cover the revised error box (Ricker et al., GCN #1169). Because of the bright, full moon close to the error box, the limiting magnitude of the images is only about R, I = 18.5 to 19. A careful comparison with the DSS2 red survey did not reveal any potential OT candidate (see also Fox et al., GCN #1170). Naturally, some faint objects visible on our I-band images have no counterpart on the corresponding R-band images. Their nature remains to be checked.
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GCN notice #1173
E. Berger (Caltech) and D. A. Frail (NRAO) report on behalf of a larger collaboration:
"On December 3.73 UT we used the VLA to observe the HETE-II error circle of GRB011130 (GCN #1169), using five pointings at 4.86 GHz. Inside the error circle we find one source which is not cataloged in the NRAO VLA Sky Survey (NVSS was taken at 1.43 GHz; Condon et al. 1998, AJ, 115, 1693), with a flux density of 320+/-40 microJy. The coordinates of this source are: RA=03 05 24.71, DEC=03 46 13.1 (J2000), with an estimated uncertainty of 1.1" in each coordinate. Further observations are planned."
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GCN notice #1174
D. W. Fox and P. A. Price (Caltech), with S. S. Eikenberry (Cornell), report on behalf of a larger collaboration:
"We observed the HETE-II error circle for XRF011130 (GCN 1169) with the Palomar Hale Telescope + Wide-Field Infrared Camera during an instrument commissioning run on December 1.39 UT. Preliminary reduction of a subset of the data covering the location of the VLA source at RA 03:05:24.71, Dec +3:46:13.1 (J2000; uncertainties 1.1" in each coordinate; see GCN 1173) reveals no K'-band counterpart to a limit of roughly K'=18.5 mag. We note also the absence of any optical counterpart to the VLA source in archival DPOSS images (limits of approximately g=20.5 mag, r=20.7 mag, and i=20.3 mag) and in our Dec 1.24 UT NEAT images (limit of R=18.5 mag; see GCN 1170)."
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GCN notice #1175
B. C. Lee, D. L. Tucker, D. Q. Lamb, D. E. Vanden Berk, and E. Neilsen, on behalf of the SDSS GRB team, report:
We observed the entire revised HETE-2 error circle for GRB011130 (XRF011130) (GCN 1169) using the SDSS 0.5-m "Photometric Telescope" (PT) at APO under clear skies and a bright moon on UTC 2001 December 2 from MJD 52245.208450 to 52245.301880. We took a series of eleven 180 second i-band exposures (41.5' x 41.5' field of view) centered on the reported location of XRF011130 (GCN 1169). We have coadded the 11 images and examined the region of the variable radio source reported by Frail (GCN 1173). We find an object with a peak approximately 2 sigma above noise and an estimated magnitude of i* = 20.5 +/- 0.5 at RA=03:05:24.96, DEC=+03:46:14.58 (RMS error of approximately 1 arcsec), consistent with the location of the variable radio source. Because the object is only margninally detected in the coadded image, is slightly below the limiting magnitude of the DPOSS plates, and has not been observed as part of the SDSS imaging survey, we do not know if it is variable. Additional observations are urged.
A finding chart can be found at: http://sdss.fnal.gov:8000/grb/
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GCN notice #1176
J. Greiner (AIP, Potsdam), S. Klose (TLS, Tautenburg), A. A. Henden (USRA/USNO, Flagstaff), A. Riffeser (Universitaets-Sternwarte Muenchen), and A. J. Castro-Tirado (IAA Granada, Spain)
report:
The radio source localization described in Breger and Frail (GCN 1173) is at the intersection of our mosaic of November 30 UT with the Calar Alto 1.23-m telescope. Two R- and two I-band 180sec images overlap, along with two shorter setup R-band frames. The coadded image can be found at ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb011130.jpg The optical source mentioned in Lee, et al. (GCN 1175) is marginally detected, at about the same magnitude as shown in the figure by Lee et al. We therefore suggest that this object is most likely a constant source.
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GCN notice #1177
N. Mirabal, J. P. Halpern (Columbia), & J. Kemp (Joint Astronomy Centre/Columbia) report on behalf of the MDM Observatory GRB follow-up team:
"I-band images obtained on the MDM 1.3m for 100 minutes starting on Dec 2.30 UT also show the object reported by Lee et al. (GCN #1175) near the position of the radio source reported by Berger & Frail (GCN #1173). We have not reported this object (until now) because the position we measured for it with respect to the USNO-A2.0 is (J2000) 03:05:25.02, +03:46:13.9 with an estimated uncertainty of 0.6". This is consistent with the position measured by Lee et al., but it is 4.7" from the radio source, thus unlikely to be an optical transient."
GCN notice #1178
GRB011130 (= XRF011130): Second Revised Localization by HETE
G. Ricker, D. Lamb, and S. Woosley on behalf of the HETE Science Team;
R. Vanderspek, N. Butler, G. Crew, J. Doty, G. Monnelly, G. Prigozhin, J. Villasenor, T. Cline, J.G. Jernigan, A. Levine, F. Martel, E. Morgan, J. Braga, R. Manchanda, and G. Pizzichini, on behalf of the HETE Operations and HETE Optical-SXC Teams;
C. Graziani, Y. Shirasaki, N. Kawai, M. Matsuoka, T. Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Tavenner, and T. Donaghy, on behalf of the HETE WXM Team;
J-L Atteia, M. Boer, J-F Olive, J-P Dezalay, and K. Hurley on behalf of the HETE FREGATE Team;
write:
The localization of H1864, an X-ray flash (XRF) reported as GRB011130 (= XRF011130) in GCN Circular 1165, and as revised in Circular 1169, has been further improved. The burst occurred at 22775.66 SOD (6:19:35 UTC) on 2001 November 30.
The reduced statistical error radius in the WXM localization is 7.4 arcmin (90% confidence). The spacecraft aspect has been improved to lie within a circle of < 2 arcmin radius. The revised localization of H1864 is centered at:
R.A. = 03h 05m 26.9s, Dec. = +3d 49'30" (J2000)
A circle centered on this location having a radius 7.6 arcmin contains the burst location with > 90% confidence.
The error circle reported here has slightly more than 1/2 the area of the larger error circle reported in GCN 1169, and is almost entirely contained within the error circle reported in GCN 1169 (ie this new circle extends 12 arcsec beyond one edge of the old circle). Details of the analysis and localization history are given in the "Special Note on Burst 1864" posted at:
http://space.mit.edu/HETE/Bursts/
This message is quotable.

GCN/HETE BURST POSITION NOTICE


TITLE:          GCN/HETE BURST POSITION NOTICE
NOTICE_DATE:    Thu 06 Dec 01 00:34:13 UT
NOTICE_TYPE:    HETE Ground Analysis
TRIGGER_NUM:    1864,   Seq_Num: 5
GRB_DATE:       12243 TJD;   334 DOY;   01/11/30
GRB_TIME:       22775.66 SOD {06:19:35.66} UT
TRIGGER_SOURCE: Trigger on the 2-30 keV band.
WXM_SIG/NOISE:  7 sig/noise  on a 5.120 [sec] timescale
SC_-Z_RA:       244 [deg]
SC_-Z_DEC:      -21 [deg]
WXM_CNTR_RA:    46.362d {+03h 05m 27s} (J2000),
                46.387d {+03h 05m 33s} (current),
                45.708d {+03h 02m 50s} (1950)
WXM_CNTR_DEC:   +3.825d {+03d 49' 30"} (J2000),
                +3.832d {+03d 49' 56"} (current),
                +3.632d {+03d 37' 54"} (1950)
WXM_MAX_SIZE:    15.20 [arcmin] diameter
WXM_LOC_SN:      6 sig/noise (pt src in image)
SUN_POSTN:      246.35d {+16h 25m 25s}  -21.66d {-21d 39' 34"}
SUN_DIST:       153.67 [deg]
MOON_POSTN:      59.04d {+03h 56m 09s}  +17.91d {+17d 54' 27"}
MOON_DIST:       18.75 [deg]
MOON_ILLUM:     100 [%]
GAL_COORDS:     174.39,-45.24 [deg] galactic lon,lat of the burst
COMMENTS:       Definite GRB.
COMMENTS:       WXM error box is circular; not rectangular.
COMMENTS:       Burst_Validity flag is true.
COMMENTS:       WXM data refined since S/C_Last Notice.

GCN notice #1179
S. Jha, R. P. Kirshner (CfA) and P. M. Garnavich (Notre Dame)
We imaged the radio position of GRB 011131 (GCN 1173) with the Magellan 6.5m Baade telescope and Direct Camera on Dec. 5.23 (UT). A single 180s exposure with the R filter in 0.7" seeing reveals an unresolved source within the radio error circle. The position is 3:05:24.73 3:46:14.1 (2000) (1" from the radio position) based on the USNO.A2 catalog. The position is based on only three objects in common between the catalog and image, but is consistent with the GSC offset to the USNO.A2 in this region.
The possible afterglow has an R magnitude of 22.8+/-0.2 based on a calibration from a single Landolt standard. A star 4" east and 7" south of the OT position has R=21.5 mag (star A on finder). A finder chart can be found at http://www.nd.edu/~pgarnavi/grb011130/finder.jpg and the reduced FITS image (dec5.fits) can be obtained there as well.
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GCN notice #1180
James Rhoads, Andy Fruchter, and Ingunn Burud report:
We observed the location of the candidate radio counterpart to XRF 011130 on 2001 December 5.37 UT in the K' filter with the NASA IRTF + NSFCam.
Within the combined astrometric uncertainty of the IRTF and radio data, which we estimate at 2" radius, we find one and probably two sources. The first is clearly the same object reported by Jha et al (GCNC 1179). The second is 1.66" to the SW and considerably fainter, near the detection limit for the image.
Photometric calibration is not presently available, but further observations are planned. A very rough zero point (based on calibration on a different night with the same instrument) suggests K=18.1 for the brighter source, making the source very red (R-K ~ 4) if this zero point is correct.
Additionally, we expect to improve the astrometry shortly using comparison to wider field optical data.
GCN notice #1181
P. M. Garnavich (Notre Dame), S. Jha and R. P. Kirshner (CfA)
We have again imaged the suspected optical afterglow of GRB 011130 (Jha, Kirshner & Garnavich, GCN 1179) with the Magellan 6.5m Walter Baade telescope and Direct Camera. Three R-band images with a total exposure time of 780s were obtained on Dec 6.15 (UT). Using point spread function photometry we find that the optical source within the radio transient error circle (GCN 1173) has faded by 0.16+/-0.05 mag over 22 hours. A Landolt standard star observed at near the same airmass as the afterglow provides a magnitude estimate of R=23.0+/-0.1.
The PSF subtraction of the source leaves a faint residual that was not apparent on the short exposure of the previous night. This resolved emission may be the host galaxy. The combined R-band image is available at http://www.nd.edu/~pgarnavi/grb011130.
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GCN notice #1183
S. Jha, R. P. Kirshner, T. Matheson (CfA), P. M. Garnavich (Notre Dame), G. P. Monnelly, R. K. Vanderspek and G. R. Ricker (MIT) report:
We obtained a spectrum of the optical counterpart to the radio source (GCN 1173) that is a possible afterglow to GRB 011130 (GCN 1179) with the Magellan 6.5m Baade telescope (+ LDSS2) on Dec. 7.15 (UT). Four 1200s exposures have a resolution of 1.2 nm and cover the wavelength range 400 to 800 nm. The spectrum of the source reported on GCN 1179 is dominated by galaxy light. A strong calcium break is seen at 600 nm providing a redshift of z=0.50. No significant [OII] is detected. The brighter galaxy 4" east was also placed on the slit and has the same redshift.
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GCN notice #1184
GRB011130 (=XRF011130): Scheduled Target of Opportunity Observation with Chandra X-ray Observatory
G. Ricker, P. Ford, G. Monnelly, N. Butler, R. Vanderspek (MIT); and D. Lamb (U.Chicago)
on behalf of the Chandra ToO Team and the HETE Science Team
write:
On 10 December, from 00:38 UT - 09:27 UT, the Chandra Observatory is scheduled to observe the field of the X-ray rich gamma-ray burst XRF011130 that was localized by the HETE satellite (Ricker et al., GCN1165). The revised error circle for XRF011130 (Ricker et al. GCN1178) fits completely within the field-of-view of the ACIS-I array on Chandra.
Special arrangements have been made by the Chandra Science Center to expedite the pre-processing of the data from our observation, so that the TOO Science Team should be able to carry out the accurate astrometry needed to establish accurate locations of the brightest X-ray sources in the HETE field within a few hours of receipt of data on 10 December.
Assuming that the observation takes place as planned and that the bulk of the data are received during the morning on 10 December, the TOO Science Team will strive to disseminate the RA, DEC, and relative intensity for the 10 brightest X-ray objects in the field by GCN Circular as soon as possible -- hopefully within 12 hours after the observation is completed.
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GCN notice #1185
GRB011130 (=XRF011130): Results of a Target of Opportunity Observation with the Chandra X-ray Observatory
G. Ricker, P. Ford, G. Monnelly, N. Butler, R. Vanderspek (MIT); and D. Lamb (U.Chicago)
on behalf of the Chandra ToO Team and the HETE Science Team
write:
On 10 December, from 00:38 UT - 09:27 UT, the Chandra Observatory targeted the field of the X-ray rich gamma-ray burst XRF011130 that was previously localized by the HETE satellite (Ricker et al., GCN1165). The revised error circle for XRF011130 (Ricker et al. GCN1178) fit completely within the field-of-view of the ACIS-I array on Chandra. The observation duration was 30 ksec.
As a result of the special arrangements made by the Chandra Science Center to expedite the pre-processing of the data from our observation, the TOO Science Team has been able to establish the location and relative intensity for the 10 brightest X-ray sources within the HETE field.
The following table lists the J2000 coordinates of the 10 brightest sources we have established in the HETE Field:
```
     Chandra Name          RA          DEC     dRA(s)  dDEC('')  Cts 
CXOU J030527.9+034657   3 5 27.88  3 46 57.04  0.061     0.96    110 
CXOU J030532.5+035140   3 5 32.50  3 51 40.37  0.061     0.96    101 
CXOU J030534.3+034958   3 5 34.26  3 49 58.94  0.061     0.96     33 
CXOU J030514.2+034854   3 5 14.21  3 48 54.19  0.061     0.96     30 
CXOU J030550.1+035009   3 5 50.10  3 50  9.38  0.064     0.99     27 
CXOU J030458.7+034702   3 4 58.68  3 47  2.92  0.069     1.03     27 
CXOU J030541.4+034808   3 5 41.43  3 48  8.02  0.061     0.97     26 
CXOU J030534.2+034208   3 5 34.22  3 42  8.75  0.070     1.10     23 
CXOU J030512.9+034936   3 5 12.91  3 49 36.35  0.062     0.97     22 
CXOU J030536.0+035303   3 5 36.01  3 53  3.58  0.062     0.97     21 
```
The astrometry was calibrated by correlating against four USNO A2 catalog stars.
In the table, delta(RA), the uncertainty in RA, and delta(DEC),the uncertainty in DEC, were established by summing the following in quadrature for each coordinate: the error reported by celldetect, the error reported by the correlation code, and the error estimate from the star reference catalog.
We gratefully acknowledge the timely assistance of the personnel at the Chandra Science Center in the preparation of these data.
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GCN notice #1186
N. Mirabal & J. P. Halpern (Columbia) report on behalf of the MDM Observatory GRB follow-up team:
"We obtained R-band images on the MDM 1.3m for 2 hours on each of the following nights, covering the positions of all ten Chandra X-ray sources listed by Ricker et al. (GCN #1185):
```
Dec. 6.18
Dec. 7.24
Dec. 9.27
```
We detect constant optical counterparts of nine of the ten sources. The source CXOU J030458.7+034702 is not detected in any of our images to an approximate limiting magnitude R > 23. Deeper optical images of this location would be useful.
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GCN notice #1187
N. Mirabal & J. P. Halpern (Columbia) report on behalf of the MDM Observatory GRB follow-up team:
"Here are further details of the R-band optical counterparts of the Chandra X-ray sources listed by Ricker et al. (GCN #1185), as measured on Dec. 7.24, including estimated magnitudes using Landolt star calibration, and morphological comments:

Source			Optical Position	   R	 Comment 
-------------------------------------------------------------------------
CXOU J030527.9+034657   03 05 27.85 +03 46 56.9   20.0   galaxy
CXOU J030532.5+035140   03 05 32.46 +03 51 40.0   19.8   stellar
CXOU J030534.3+034958   03 05 34.21 +03 49 58.2    ?	 blended galaxy
CXOU J030514.2+034854   03 05 14.18 +03 48 54.4   21.7   galaxy?
CXOU J030550.1+035009   03 05 50.02 +03 50 08.5   21.6   stellar
CXOU J030458.7+034702                            >23
CXOU J030541.4+034808   03 05 41.53 +03 48 07.4   21.5?  near bright star
CXOU J030534.2+034208   03 05 34.18 +03 42 08.9   22.3   galaxy?
CXOU J030512.9+034936   03 05 12.89 +03 49 36.3   21.6   ?
CXOU J030536.0+035303   03 05 35.95 +03 53 02.9   22.9   ?
-------------------------------------------------------------------------

A finding chart is at http://www.astro.columbia.edu/~jules/mdmchart.ps
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GCN notice #1190
GRB011130 (=XRF011130): Further analysis of Chandra Target of Opportunity Observations
G. Monnelly, N. Butler, G. Ricker, P. Ford, R. Vanderspek (MIT); and D. Lamb (U.Chicago)
on behalf of the Chandra ToO Team and the HETE Science Team
write:
On 10 December, from 00:38 UT - 09:27 UT, the Chandra Observatory targeted the field of the X-ray rich gamma-ray burst XRF011130 that was previously localized by the HETE satellite (Ricker et al., GCN 1165). The revised error circle for XRF011130 (Ricker et al. GCN 1178) fits completely within the field-of-view of the ACIS-I array on Chandra. The observation duration was 30 ksec.
In Ricker et al. (GCN 1185), we reported the locations of the brightest 10 X-ray sources established in our Chandra observation. In this Circular, we complete the list of detected sources by presenting all sources found in the entire ACIS-I detector field-of-view down to a limit of 10 detected counts, including the sources presented in GCN Circular #1185. The information for sources outside the 7.6' radius HETE error circle are presented in a separate table for clarity. The analysis reported here is based on wavedetect, whereas GCN 1185 was based on celldetect. The results are similar: nine of the celldetect sources appear among the top ten wavedetect sources.
The following table includes all sources above a limit of 10 detected counts found within the HETE error circle (radius 7.6'). Sources marked with a * were found by celldetect and distributed in GCN 1185.
```
       Chandra Source ID       RA         DEC      dRA(s) dDEC('') Cts
   * CXOU J030527.7+034656  3 5 27.70  3 46 56.46  0.057    1.18   128
   * CXOU J030532.3+035139  3 5 32.32  3 51 39.79  0.057    1.18   105
   * CXOU J030534.1+034958  3 5 34.08  3 49 58.35  0.057    1.18    37
   * CXOU J030514.0+034853  3 5 14.03  3 48 53.56  0.057    1.19    32
   * CXOU J030458.5+034702  3 4 58.46  3 47  2.31  0.067    1.28    31
   * CXOU J030549.9+035008  3 5 49.88  3 50  8.80  0.058    1.20    28
   * CXOU J030541.2+034807  3 5 41.25  3 48  7.26  0.057    1.19    23
   * CXOU J030534.1+034208  3 5 34.07  3 42  8.24  0.062    1.33    22
   * CXOU J030535.8+035302  3 5 35.83  3 53  2.99  0.058    1.19    20
     CXOU J030534.7+035147  3 5 34.68  3 51 47.96  0.057    1.19    18

     CXOU J030502.4+034522  3 5  2.44  3 45 22.41  0.071    1.30    18
     CXOU J030532.4+034301  3 5 32.44  3 43  1.87  0.062    1.29    17
     CXOU J030540.5+034936  3 5 40.45  3 49 36.96  0.057    1.19    15
     CXOU J030516.5+035229  3 5 16.48  3 52 29.34  0.059    1.19    14
     CXOU J030522.2+035354  3 5 22.21  3 53 54.43  0.059    1.19    14
   * CXOU J030512.8+034936  3 5 12.75  3 49 36.22  0.057    1.19    12
     CXOU J030530.3+035224  3 5 30.31  3 52 24.48  0.057    1.18    11
     CXOU J030532.9+034927  3 5 32.86  3 49 27.94  0.057    1.19    11
     CXOU J030537.0+034406  3 5 37.04  3 44  6.95  0.059    1.25    10
     CXOU J030501.6+034613  3 5  1.65  3 46 13.94  0.061    1.24    10
```
The following table includes all sources above a limit of 10 detected counts found in the ACIS-I field-of-view outside the HETE error circle (radius 7.6'), but within 10' of the center of the HETE error circle.
```
       Chandra Source ID       RA         DEC      dRA(s) dDEC('') Cts
     CXOU J030539.8+034148  3 5 39.79  3 41 48.82  0.060    1.23   132
     CXOU J030454.4+035149  3 4 54.39  3 51 49.41  0.066    1.25    52
     CXOU J030519.7+035711  3 5 19.67  3 57 11.99  0.062    1.21    50
     CXOU J030539.1+035652  3 5 39.09  3 56 52.21  0.063    1.21    42
     CXOU J030529.8+035711  3 5 29.79  3 57 11.93  0.063    1.21    36
     CXOU J030537.4+035744  3 5 37.41  3 57 44.79  0.065    1.22    32
     CXOU J030538.3+035825  3 5 38.28  3 58 25.95  0.067    1.26    24
     CXOU J030453.0+035144  3 4 53.04  3 51 44.28  0.070    1.25    16
     CXOU J030602.8+034737  3 6  2.77  3 47 37.64  0.074    1.39    16
     CXOU J030529.0+034115  3 5 29.02  3 41 15.90  0.065    1.38    11
```
The astrometry was calibrated using five USNO A2 catalog stars.
In the table, delta(RA), the uncertainty in RA, and delta(DEC),the uncertainty in DEC, were established by summing the following in quadrature for each coordinate: the error reported by wavedetect, the error reported by the correlation code, and the error estimate from the star reference catalog.
It is notable that during our Chandra observation there were no counts detected from within the error circle of the VLA radio source reported by Berger and Frail (GCN 1173).
Further information about the Chandra observations, including 23 additional sources down to the detection limit of the observation, can be found on the HETE web page:
http://space.mit.edu/HETE/Bursts/GRB011130.
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GCN notice #1207
D. A. Frail (Caltech/NRAO) reports on behalf of a larger collaboration:
"We have continued to monitor the entire HETE-II error circle of GRB011130 (GCN #1169, 1178) with the VLA at 4.86 GHz. Observations have been made on 2001 December 4, 6, 7, 9 and 11. In addition, observations were made at a frequency of 8.46 GHz towards an un-cataloged radio source noted earlier by Berger and Frail (GCN #1173). The flux density is similar (350 uJy) at both frequencies and no strong variability is seen at either frequency. We suggest that this source is a flat spectrum AGN which is too weak at 1.43 GHz to be cataloged in the NRAO VLA Sky Survey (NVSS; Condon et al. 1998, AJ, 115, 1693).
A search was carried out in all the radio images for counterparts of the X-ray sources identified by Chandra. None of the initial 10 bright X-ray sources (GCN #1185) have radio counterparts. Two radio/X-ray pairs are present in a deeper X-ray search (GCN #1190). These are:
```
CXOU J030534.7+035147  3 5 34.68  3 51 47.96     Radio double, NVSS src
CXOU J030532.4+034301  3 5 32.44  3 43  1.87	 Weak (200 uJy) pt-like src
```
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GCN notice #1208
J. P. Halpern, N. Mirabal, E. V. Gotthelf (Columbia), & J. Kemp (Joint Astronomy Centre/Columbia) report on behalf of the MDM Observatory GRB follow-up team:
"R-band images of this field taken on three nights and previously described in GCNs #1186 and #1187 also cover the positions of the two radio sources described by Frail (GCN #1207). Optical images of both sources are shown on the web page given below. Neither show evidence of variability. The point radio source corresponding to CXOU J030532.4+034301 is approximately equidistant (3") from three optical objects. It is not clear which, if any, is the counterpart.
Examination of the I-band images obtained on the MDM 1.3m on Dec. 2.30 UT (GCN #1177) under bright lunar conditions shows marginal detections of the two brightest Chandra sources on the list of Ricker et al. (GCN #1185), CXOU J030527.9+034657 and CXOU J030532.5+035140. The combined I-band image is slightly deeper than the POSS-II IVN plate, but does not provide any evidence for variability of the detected objects. In addition, we note that examination of blue and red POSS II plates shows blue objects at the locations of CXOU J030532.5+035140 and CXOU J030534.3+034958.
Details of MDM images are posted at http://www.astro.columbia.edu/~jules/grb/011130/
This message may be cited."
GCN notice #1212
Julie McEnery on behalf of the Milagro collaboration reports:
Milagro observed GRB 011130 and GRB 011212 at GeV/TeV energies during the burst durations reported by the HETE WXM (30 seconds and 80 seconds respectively). No evidence for prompt GeV/TeV emission was found from either of these bursts. A preliminary analysis (assuming a differential photon spectral index of -2.4) gives an upper limit on the fluence at the 99% confidence level of:
```
J(E > 2 TeV) < 6 * 10^(-7) erg cm^(-2) for GRB 011130 and,
J(E > 2 TeV) < 1 * 10^(-6) erg cm^(-2) for GRB 011212
```
We expect that TeV photons will be attenuated by pair production with infrared photons in intergalactic space so we also calculate an upper limit on the fluence, assuming a spectrum truncated at 150 GeV. In this case we find an upper limit on the fluence at the 99% confidence level of:
```
J(100-150 GeV) < 5 * 10^(-4) erg cm^(-2) for GRB 011130 and,
J(100-150 GeV) < 1 * 10^(-3) erg cm^(-2) for GRB 011212
```
These upper limits are preliminary and will be refined with further analysis. These limits do not incorporate systematic uncertainties which may be of order 50%.
GCN notice #1272
GRB011130 (=XRF011130): Results of a Second Epoch Observation with the Chandra X-ray Observatory
N. Butler, G. Monnelly, G. Ricker, J. Doty, P. Ford, R. Vanderspek, G. Crew, A. Dullighan (MIT); D. Lamb (U.Chicago); and P. Plucinsky (CFA)
on behalf of the Chandra GRB ToO Team and the HETE Science Team
write:
On 20 February, from 10:02 UT - 14:30 UT, the Chandra Observatory targeted the field of the X-ray rich gamma-ray burst XRF011130, localized by the HETE satellite (Ricker et al., GCN1165) This was a 16 ksec observation with ACIS-I, following up the 30 ksec observation performed with ACIS-I on 10 December (Ricker et al., GCN 1185).
Of the 20 brightest sources reported in GCN 1190 (Monnelly et al.), none were observed to fade in a manner that is consistent with the power-law behavior that is characteristic of gamma-ray burst afterglows. (A power law index of -1.3 implies a fade by a factor ~15, between our 1st and 2nd epoch observations.) Corrected for exposure, the largest fade for any of the sources in the list was by a factor of 3. We note that our brightest epoch 1 source (CXOU J030527.9+034657), which appears to be associated with a 20th magnitude galaxy (Mirabal & Halpern, GCN 1187), faded by a factor of approximately 2.
Beyond the top 20 brightest, we note that our 24th and 27th brightest 1st epoch sources (see partial table below) faded to levels consistent with the background. We estimate a 50% probability for chance fading to the background in one or more of our 24 brightest sources; we estimate a 75% probability for chance fading to the background in one or more of our 27 brightest sources.
```
Chandra Name               RA          DEC     E1C  E1B    E2C  E2B
CXOU J030515.1+034457  3 5 15.12  3 44 57.02   8.1  2.9   4.0  -0.7  0.7
CXOU J030527.8+035548  3 5 27.81  3 55 48.09  13.8  4.2   6.5  -1.3  4.3
```
Here E1C denotes the epoch 1 net counts for the source, E1B the epoch 1 background counts estimate, the expected epoch 2 net number of counts based on epoch 1, E2C the observed net counts in epoch 2, and E2B the epoch 2 background counts estimate. A complete table in this form, containing all of our 1st epoch sources, can be found at:
http://space.mit.edu/HETE/Bursts/GRB011130/epoch2_table.html
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Jochen Greiner, last update: 15-Mar-2002 [Disclaimer]