Fermi Gamma-ray Space Telescope Education and Public Outreach

This page uses the WorldWide Telescope to show the location of gamma-ray bursts (GRBs) detected by the Fermi telescope against real astronomical images from ground and space-based telescopes. Use your mouse to select the GRB for which you would like additional information, which will then be displayed under the Description column. The virtual telescope will then "slew" over to the location of the GRB. The field of view when the telescope comes to a rest is 0.25°. This data is extracted from Gamma-ray Burst Real-time Sky Map. To see the gamma ray sky as seen by Fermi Space Telescope, check the "Show UI" box and select Fermi from the "Imagery" menu. You may be prompted to download the Silverlight plugin if you do not already have it.

To celebrate the one-year anniversary of Fermi's launch, we created a WorldWide Telescope tour of some of the objects that Fermi has studied. To view the tour, please click the "Run Tour" button below.

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GRB ID Date Time RA Dec Constellation Description GRB 120402B 2012/04/02 16:04:00.76 14:55:00 -10:24:00 Libra The GBM light curve for this burst showed a soft, bright pulse, followed by weaker sustained emission. The duration of the burst was about 17.5 seconds. The spectrum of the burst was fit equally well by either a Comptonized power law or a Band function. The parameters of the power law are alpha = -1.35 +/- 0.11, Epeak = 37.2 +/- 2.2 keV. For the Band function they are alpha = -0.48 +/- 0.37, beta = -2.44 +/- 0.09 and Epeak = 27.5 +/.- 2.45 keV. GRB 120323A 2012/03/23 12:10:19.72 23:07:00 27:12:00 Pegasus "The GBM light curve for this burst had a double-peaked FRED profile and lasted about half a second. The spectrum was fitted with a Band function with alpha = -0.82+/-0.07, beta=-2.01+/-0.02 and Epeak=64.8+/-3.8 keV. The burst was also detected by INTEGRAL, Konus-Wind, MESSENGER and Swift as part of the IPN." GRB 120302A 2012/03/02 01:55:39 08:09:48.14 29:39:35.3 Cancer "This burst was detected by the Fermi GBM and in ground analysis of Swift BAT data, where it had a significance of 8.2 sigma. There was no automated trigger from the BAT, and so no XRT of UVOT data were initially available. The Swift light curve showed at least two peaks, with possibly a third. The total duration was 35 to 40 seconds (GCN 13002). A possible afterglow to this burst was detected in GROND images taken 22.6 hours after the burst. The source is slightly outside outside the ToO XRT error circle (cf. GCN 13012). Though the source does not fade between two epochs of GROND observations, it is not visible in DSS images, so it seems to be a new object in the field. Second epoch magnitudes, taken about 48 hours after the burst, are (GCN 13003): g' = 22.5 +/- 0.3 r' = 21.9 +/- 0.2 i' = 21.9 +/- 0.3 z' = 21.4 +/- 0.1 J = 20.9 +/- 0.4 H = 20.3 +/- 0.3 K = 19.7 +/- 0.4 " GRB 120226A 2012/02/26 20:54:17.03 20:11:43 48:39:55 Cygnus "This burst was detected in ground analysis using a non-standard LAT detection. The excess counts in the LAT (50 counts over background over a 60 second interval) were seen to coincide with a GBM trigger. The GRB was detected with standard LAT selection criteria over longer timescales. The GBM light curve contained several peaks and a duration of T90 = 57 +/- 2 seconds. The spectrum was fit by a Band function with alpha = -1.00 +/- 0.02, beta = -2.28 +/- 0.10 and Epeak = 296.70 +/- 13.60 keV (GCN 12995)." GRB 120114A 2012/01/14 16:20:09 21:11:37.03 57:02:08.9 Cepheus This burst was found in ground analysis of a failed trigger event. The burst was also detected by the Fermi/GBM (trigger 348250807). The Swift/BAT light curve for the burst has a duration of about 35 second. The burst occurred too close to the Sun for any followup observations to be undertaken. GRB 120107A 2012/01/07 09:12:15 17:53:40 -23:22:18 Sagittarius This burst was seen by the Fermi LAT and GBM, and also by Konus-Wind, Suzaku/WAM and MESSENGER/GRNS. The Konus-Wind light curve contained multiple peaks that partially overlapped. The burst duration was about 25 seconds. Both Fermi/GBM Suzaku/WAM and Konus-Wind detected similar shapes and durations for the light curve. GRB 111017A 2011/10/17 15:45:23.72 00:32:24 -07:36:00 Cetus The GBM light curve ad a single symmetric peak with emission extending up to 1 MeV. The burst was bright enough to trigger the spacecraft to repoint. Its duration was about 11 seconds. The spectrum was fit by a Band function, with alpha = -0.91 +/- 0.02, beta = -2.7 +/- 0.40 and Epeak = 692.5 +.- 48.3 keV. GRB 110825A 2011/08/25 06:22:11.44 2:59:35.1 15:24:25 Aries "This was an IPN localized event, with Fermi/GBM, AGILE/MCAL, MESSENGER/GRNS, Mars Odyssey/HEND, Suzuku/WAM and Swift/BAT contributing to the triangulated coordinates. The Fermi/GBM light curve lasted about 4 seconds. A Swift Target of Opportunity observations was made starting about 23 hours after the GRB. In 2.9 kiloseconds of observations (~48 minutes) an x-ray source was seen within the IPN error box. There was no known source at the position of this source, though current catalogs do not go deep enough to have included it. No UVOT source was found to v > 19.19 (GCN 12308). A possible afterglow with R~23.6 was obtained using the Nordic Optical Telescope (NOT) /ALFOSC. The imaging was done in poor weather conditions and brightening morning twilight, so only one image was obtained and it was not possible to determine if the object was fading (GCN 12311). The 2.4 meter Gau-Mei-Gu telescope in Yunan, China was used to observe the field approximately 19 hours after the burst. The R-band object reported in the NOT observations was not present to a limiting magnitude R~23.9 (GCN 12314). No optical afterglow was seen in early times, within the first 5 to 15 minutes, as reported from the ROTSE-IIId telescope of the Turkish National Observatory at Bakirlitepe, Turkey. Limiting magnitudes are between 15.6 at early times and 14.4 in the later observations (GCN 12313)." GRB 110815A 2011/08/15 09:40:57 05:41:11.2 32:36:31 Auriga This IPN localized burst included data from SuperAGILE, Konus-Wind, MESSENGER, Mars Oddysey, RHESSI, Suzaku and Swift. The Konus-Wind light curve had two peaks separated by about 13 seconds. The total burst duration was 20 seconds. Emission was seen up to 8 MeV and the spectrum was best fit by a Band function with alpha = -0.85 +/- 0.1, beta = -2.5 +0.2/-0.3 and Epeak = 251 +/- 25 keV (GCN 12278). GRB 110812A 2011/08/12 00:20:08 23:53:38.15 72:12:23.32 Cepheus This burst lasted about 30 seconds and a multi-peak structured light curve. GRB 110721A 2011/07/21 04:47:43.75 22:05:00 -36:25:00 Grus "This burst had a FRED light curve with duration about 24 seconds long. The spectrum was best fit by a Band Function with alpha = -0.94 +/- 0.02, beta = -1.77 +/- 0.02 and Epeak = 372.50 +26.50/-23.60 keV. This burst was 40 degrees from the LAT boresight at the time of the trigger, and the satellite automatically repointed to put the source closer to the LAT field center. The LAT then observed the source for the following 2.5 hours, subject to Earth limb constraint. The LAT showed a significant increase in emission that correlated in both space and time with the GBM data. More than 20 photons were seen to have energies in excess of 100 MeV, with the highest energy photon recorded being at 1.7 GeV. The light curve in the LAT had a similar FRED shape to that in the GBM, though the duration was only about 16 seconds long (GCN 12188)." GRB 110705A 2011/07/05 03:37:11.94 10:42:00 24:00:00 Leo Minor This was a short burst, with the GBM light curve showing a single spike of 0.2 second duration. The spectrum was fit by a Band function with alpha = -0.17 +/- 0.07, beta = -3.0 +0.2/-0.4 and Epeak = 1010 +90/-80 keV. The burst was also detected by INTEGRAL, Konus-Wind and Suzaku, as well as satellites of the IPN. GRB 110529A 2011/05/29 00:48:42.87 07:53:19 67:54:36 Camelopardalis "This burst had two short bright peaks. The total duration for the GRB was 0.41 seconds. The spectrum was fit using a Band function with alpha = -0.88+/-0.06, beta = -2.05+/-0.15 and Epeak = 1161+/-265 keV. This burst was also seen in the LAT (GCN 12044) and by the Konus-Wind Satellite, which detected emission up to about 5 MeV (GCN 12045). " GRB 110428A 2011/04/28 09:18:30 00:22:22.22 64:50:57.1 Cassiopeia "This burst was detected by both the Fermi GBM and LAT. The LAT detected emission all the way up to 3 GeV, and the LAT detection lasted for about 200 seconds. Automatic reporting of the burst was hindered because of the effects of powerful thunderstorms and tornadoes in Alabama (Huntsville). This field was observed by the Swift XRT as a Target Of Opportunity starting about 16 hours after the Fermi trigger. Two sources were found within the Fermi/LAT error circle. One is a known ROSAT x-ray source and is also seen in the Digitized Sky Survey. We list the coordinates of the second, uncatalogued source. See circular GCN 11984 for the coordinates of the other source and for further information about the XRT observations. In additional observations from Swift/XRT taken approximately two days after the trigger, the first source (seen by ROSAT and DSS) was still detected at the same flux as the initial observations. The second source was no longer seen, suggesting that it was the x-ray afterglow of the GRB (GCN 11989)." GRB 110406A 2011/04/06 03:44:10 01:09:21 35:48:32 Andromeda This burst had a single smooth peak lasting about 3 seconds. It was also detected by Konus-Wind (GCN 11893) and the IPN (GCN 11900). Because of the proximity of the GRB to the Sun, no followup observations will be possible from Swift. It is noted that the position of the GRB coincides with the position of the dwarf lenticular galaxy NGC 404, which is undergoing vigorous star formation (GCN 11909). GRB 110401A 2011/04/01 22:04:19.63 17:54:00 26:52:00 Hercules The light curve for this burst contained two strong pulses and lasted about 2 seconds. The spectrum for the burst was fit using a Band function with alpha = -0.66+/-0.15, beta = -2.36+/-0.53 and Epeak = 1194 +/- 406 keV. The burst was originally classified as “Below Horizon” by the onboard flight software. GRB 110328B 2011/03/28 12:29:19.19 07:50:24 43:12:00 Lynx This burst had a single pulse and a duration of about 120 seconds. The spectrum was fit by a power law with exponential cutoff. The power law index was -1.17+/-0.04 and the cutoff energy was Epeak=538+96/-70 keV. This source was also see in the LAT, though the typical energy cutoff had to be lowered from 100 MeV to 50 MeV for the object to be seen. The spectrum of the LAT data has a steeper slope than reported by the GBM, which suggests a break in the spectrum between the low and high energy regimes (GCN 11835). GRB 110319B 2011/03/19 19:34:02 21:44:17.8 -56:46:24 Indus "This burst triggered the Fermi/GBM during a Swift slew. An alert to the IPN prompted an examination of the BAT data taken during the slew, which revealed a strong source. The position of the object remained in the SwiftBAT filed of view from the time of the trigger until the end of the slew. The light curve had a duration of about 18 seconds, with a single FRED profile. Followup observations with the XRT begun about 7.5 hours after the trigger showed an x-ray source within the BAT error circle. It was not clear from these initial data if the source was fading or not (GCN 11814). Only faint upper limits were reported from ground-based observations. The GROND multi-band imager was used to observe the GRB field. No optical afterglow was seen to g’>23.1, nor was any object seen in any of the other filters (GCN 11815)." GRB 110301A 2011/03/01 05:08:43.07 15:17:24 15:17:24 Serpens This burst lasted about five minutes. Its light curve consisted of a single pulse with internal structure. The GBM trigger caused an automatic repointing of Fermi to follow the burst, but because of an Earth constraint, the repoint maneuver was not completed until 40 minutes after the trigger. GRB 110125A 2011/01/25 21:27:28.39 22:05:00 -46:12:00 Grus This burst had a single pulse lasting about 5 seconds. The spectrum was fit by a power law of index -1.93 +/- 0.05. GRB 110123A 2011/01/23 19:17:45.03 17:40:00 28:02:00 Hercules This burst had a single main peak with substructure. It lasted about 18 seconds. The spectrum was fit by a Band function with alpha = -0.64 +/- 0.03, beta = -1.96 +/- 0.05 and Epeak = 280 +/- 15 keV. GRB 110120A 2011/01/20 15:59:39.23 04:06:24 -12:00:00 Eridanus "This burst had a 5 second peak followed by a longer, 40 second tail. The T90 duration was about 27 seconds. The spectrum could be fit by a power law with exponential cutoff. The power law index was -0.87 +/- 0.04, and the cutoff energy was Epeak = 1156 +/- 172 keV. This burst was also seen in the LAT. Emission was detected up to about 2 GeV, with the highest energies detected about 72 seconds after the trigger. The LAT emission lasted more than 100 seconds" GRB 110107A 2011/01/07 21:15:51 19:59:33.6 41:53:19 Cygnus This burst was detected by the Fermi GBM, but it was also caught in Swift BAT data during a Swift satellite slew: A strong source is seen in a mosaic of BAT images taken during the slew. The burst lasted about 100 seconds, starting at about T-70 seconds and continuing to about T+40 seconds. The BAT data ended at T+21 seconds. The burst contained multiple peaks, and the highest flux rate occurred near T0 (the time of the GBM trigger). GRB 101123A 2010/11/23 22:51:34.97 08:45:32 05:33:47 Hydra The burst was initiated by a weak pulse that was followed by three separate emission peaks. The total duration was about 105 seconds (T90). The spectrum was fit by a Band function with alpha = -0.75+/-0.01, beta = -2.14+/-0.03, Epaek = 476 +/- 11 keV. This burst was also observed by INTEGRAL, AGILE, Swift, Konus-Wind and other IPN spacecraft. GRB 101014A 2010/10/14 04:11:52.62 01:47:00 -51:04:00 Eridanus "The GBM light curve for this burst contained multiple pulses lasting a total of about 450 seconds (T90). The spectrum was best fit by a Band function with alpha = -1.27 +/-0.01, beta = -2.07 +/- 0.02 and Epeak = 181.40+5.66/-5.44 keV. The burst was seen by the LAT as well as the GBM (GCN 11349)." GRB 100916A 2010/09/16 18:41:12.49 10:08:00 -59:23:00 Carina This burst was originally classified as Distance Particle trigger, but subsequent analysis showed that it was a GRB. The burst occurred close to the Earth’s limb, which caused the initial confusion. The GBM light curve showed a short ~0.5 second spike situated atop a broader, weaker bulge of emission lasting about 20 seconds. GRB 100910A 2010/09/10 19:37:43.96 15:24:24 -34:37:00 Lupus This burst had 4 pulses. It’s total duration was about 15 seconds, and its spectrum was best fit by a Band function with alpha=-0.92+/-0.4, beta=-2.26+/-0.08 and Epeak = 143+/-7.0 keV. GRB 100814B 2010/08/14 08:25:25.75 08:11:00 18:30:00 Cancer The GBM showed a single pulse lasting about 6 seconds. The burst spectrum was best fit by a Band function with alpha = -0.62 +0.14/-0.11, beta = -2.49 +0.15/-0.20 and Epeak = 81.0 +6.2/-6.7 keV. GRB 100724B 2010/07/24 00:42:05.98 08:00:09.6 76:44:24 Camelopardalis "This burst had several pulses and lasted nearly 112 seconds. The source was tracked for five hours following the trigger, but the observations were delayed by ~45 minutes due to observing constraints. The spectrum was best-fit by a Band function with alpha = 0.84 +/- 0.01, beta = -1,84 +/- 0.01 and Epeak = 467.8 +15.3/-13.1 KeV. This burst was also detected by INTEGRAL and Konus-Wind (GCN 10981)." GRB 100722A 2010/07/22 02:18:37.24 15:55:00 -15:36:00 Libra The light curve for this burst had several peaks. Its total duration was about 6.6 seconds. The satellite was able to track the GRB source for 5 hours after the burst, subject to Earth constraints. The GRB spectrum was best fit by a Band function with alpha=-1.01 -0.06/+0.07, beta = -3.54 -0.1/+0.08, Epeak = 68.1 -3.5/+3.4 keV. GRB 100707A 2010/07/07 00:46:38.99 23:24:00 -06:34:00 Aquarius This burst had a FRED light curve with a duration of 82 seconds. The spectrum was best fit by a power law with exponential cutoff: index = -0.91 +/- 0.02, Epeak = 283 +/- 7 keV. The Fermi/LAT also detected this burst. The object was 90 degrees off the LAT boresight, so non-standard analyses had to be used. The LAT showed a single sharp pulse with a gradual decay, similar to the GBM light curve. The total burst duration seen by the LAT was less than 30 seconds, but it’s possible this is due to the noisier data in the LAT, with the background swamping the late-time signal. GRB 100703A 2010/07/03 17:43:37.4 00:38:05 -25:42:36 Sculptor This burst was extremely short, lasting only 70 milliseconds. It was too low in significance to trigger automatic distribution and was discovered during interactive analysis of the data. GRB 100701B 2010/07/01 11:45:23.070 03:02:00 -03:26:00 Eridanus This burst lasted about 27 seconds. Its light curve showed six or more main pulses. The spectrum for the burst was fit by a power law with exponential cutoff. The poser law index was -0.99 _/- 0.2, and the cutoff was Epeak = 1.85 +/-0.16 MeV. A Band function could also fit the spectrum. GRB 100511A 2010/05/11 11:50:39 07:17:12 -04:39:00 Monoceros The GBM showed several pulses in the burst light curve, which lasted 38 seconds. The spectrum was fit by a power law with exponential cutoff: index = -1.32 +/- 0.02, Epeak = 946.6 +134/-110 keV. GRB 100503A 2010/05/03 13:18:03.89 09:50:00 04:00:00 Sextans The GBM showed a multi-peaked light curve with a total duration of about 130 seconds. The spectrum was best fit by a power-law with exponential cutoff: index = -0.99 +0.06/-0.05, Epeak = 211.60 +18.30/-15.50 keV. GRB 100423B 2010/04/23 05:51:25 07:58:00 05:46:00 Canis Minor This burst had a single pulse lasting about 22 seconds. The spectrum was fit using a power law with exponential cutoff: index = -0.84 +/- 0.05, Epeak = 1034 +144/-117 keV. GRB 100414A 2010/04/14 02:20:21.99 12:48:27.04 08:41:35.1 Virgo "This burst had a single pulse lasting about 26 seconds. The spectrum was fit with a power law and exponential cutoff: index = -0.58 +/- 0.01, Epeak = 627.6 +12.5/-12.1 keV. This burst occurred 70 degrees off the LAT bore sight, and an automatic repointing of the telescope was triggered. The LAT detected emission from the GRB source for 300 seconds following the GBM trigger, with 20 photons more energetic than 100 MeV detected. The most energetic photon from the source was 4 GeV (40 seconds after the trigger, GCN 10594). This field was observed by the Swift/XRT beginning about 48 hours after the trigger. An uncatalogued x-ray source was detected in 1.4 kiloseconds of observations. In these initial observations it was not possible to tell if the source was fading (GCN 10601). The Swift/UVOT also imaged the field. Observations were obtained 40.4 hours after the trigger and 53.2 hours after. There was some evidence for fading over that period: Filter T_start (hr) Exp(s) Mag Err White 40.38 765 20.54 +/- 0.10 White 53.20 3531 20.86 +/- 0.06 The Gemini North telescope (Hawaii) was able to obtain spectroscopy on the object on April 17.26, about 2.5 days after the burst. They detect an i’=20.37 +/- 0.03 object. Spectra in the range 4000 to 8000 angstroms show metal absorption line features from FeII 2374; FeII 2383; FeII 2587; MnII 2594; FeII 2600; MgII 2796, 2803, MgI 2853 all at z = 1.368 (GCN 10606). " GRB 100325A 2010/03/25 06:36:08.02 22:09:00 -28:36:00 Piscis Austrinus The GBM light curve had a single, structured pulse lasting 8.3 +/- 1.9 seconds. The spectrum was best fit by a power law with exponential cutoff: index = -0.45 +0.12/-0.11, Epeak = 159.3 +12.7/-10.8 KeV. GRB 100322A 2010/03/22 01:05:09 23:20:00 -10:13:00 Aquarius The GBM light curve had multiple peaks, and the burst had a duration of 37 seconds. The spectrum was best fit by a Band function with alpha = -0.88 +/- 0.02, beta = -2.15 +/- 0.05 and Epeak = 309 +/- 16 keV. GRB 100224B 2010/02/24 02:40:55.48 17:58:00 -17:05:00 Sagittarius The light curve for this burst had three distinct peaks. Its total duration was about 77 seconds, starting at T-5.6 seconds. The spectrum was fit by a power law with exponential cutoff: index = -1.36 +0.07 / -0.06, Epeak = 181.40 +31.50 / - 23.60 keV. GRB 100223A 2010/02/23 02:38:09.31 06:56:00 02:48:00 Monoceros A short, soft peak triggered the GBM for this burst. It had a duration of 0.05 seconds and was followed after a few milliseconds by a harder one. The total duration for the burst was 0.206 seconds. The spectrum was fit by a power law with exponential cutoff: index = -0.31 +/- 0.08, Epeak = 1143 +/- 109 keV. GRB 100131A 2010/01/31 17:30:57.67 08:02:00 16:29:00 Cancer This burst lasted 6.2 seconds. It consisted of a single bright spike with substructure. The spectrum was best fit by a Band function: alpha = -0.63 +/- 0.05, beta = -2.21 +/- 0.05, Epeak = 132.10 +/- 6.28. GRB 100122A 2010/01/22 14:47:37.31 05:16:48 -02:42:00 Orion "This burst had two pulses, the first a weak one, followed by a much stronger one beginning 21 seconds later and lasting 6.6 seconds. The spectrum is fit by a Band function with alpha = -0.98 +/- 0.05, beta = -2.31 +/- 0.03 and Epeak = 45.6 +/- 1.5 keV. Ground-based imaging was done using the MASTER robotic telescope in Blagoveschensk, Russia. The images are from the telescope itself, with a limiting magnitude of m ~ 17, and from the Very Wide Field Camera which has a limit of m ~ 11.5. An image showing the region of the burst with the Fermi error boxes superimposed in linked." GRB 100116A 2010/01/16 21:31:00.24 20:20:04.8 16:24:00 Sagitta This burst had two separate peaks separated by more than 60 seconds. There was essentially no emission evident between the peaks. The total duration of the burst was approximately 110 seconds. Both peaks were best fit with a power law plus high energy cutoff for the spectra. The first peak had an index of -0.92 +/- 0.15 and Epeak = 240 +60/-40 keV. The second peak had an index of -1.02 +/- 0.017 and Epeak = 1240 +/- 90 keV. The burst was also seen by the LAT, which saw an increase in the flux coincident with the second peak. Most of the energy was detected below 100 MeV (GCN 10333). GRB 100130A 2010/01/10 17:29:24.14 01:19:00 -25:12:00 Sculptor This GRB had an initial soft, weak peak. A second stronger peak followed at T+50, and then another weaker one at T+75 seconds. The total duration of the burst was about 106 seconds. The spectrum was fit by a power law with exponential cutoff: index = -0.97 +/- 0.06, Epeak = 100.50 +/- 4.77 keV. GRB 100130B 2010/01/10 18:38:35.46 05:10:00 20:21:00 Taurus This burst had four peaks, with a total duration of about 90 seconds. The spectrum by a power law with exponential cutoff: the index is -1.22 +/- 0.04, with Epeak = 208.00 +/- 17.10 keV. GRB 091128 2009/11/28 06:50:34.64 08:30:00 01:42:00 Hydra The GBM light curve shows a single structured peak lasting about 97 seconds. The spectrum was best fit by a power law with exponential cutoff: index = -0.99 +/- 0.02, Epeak = 178.8 +/- 5.6 keV. GRB 091126 2009/11/26 07:59:24.76 05:33:00 -19:18:00 Lepus This burst had a single pulse with a duration of 0.3 seconds. The spectrum was fit by a power-law with exponential cutoff: index = -0.60 +0.24/-0.21, Epeak = 458 +215/-107 keV. GRB 091123 2009/11/23 07:08:37.26 19:48:00 -29:12:00 Sagittarius This burst was extremely unusual. The GBM light curve showed four emission peaks separated by long quiet periods. However, comparison with Konus-Wind data showed that the burst was already occurring when its position rose above the limb of the Earth as seen from Fermi. Using only the GBM data the burst duration was 650 seconds. It’s spectrum was fit by a power-law with exponential cutoff: index = -1.-8 +/- 0.05, Epeak = 101.30 +5.16/-4.52 keV. GRB 091120 2009/11/20 04:34:40.23 15:59:00 -24:48:00 Scorpius "This burst had multiple peaks and lasted about 52 seconds. The spectrum was fit by a power law function with exponential cutoff. The power law index was -1.17 +/- 0.02, with cutoff at Epeak = 129 +.- 3 keV. A Band function fit the spectrum equally well (GCN 10187). This object was also detected as a hard x-ray transient by the Gas Slit Camera (GSC) on the MAXI mission. The position is consistent with the GBM position, though MAXI positions should be improved after the spacecraft completes its commissioning phase (GCN 10188)." GRB 091104 2009/11/04 08:49:22 13:55:01.50 47:24:37.9 Canes Venatici This was a BAT image trigger, so no variation was evident in the light curve. The satellite slewed immediately and started observing with the XRT 131.5 seconds after the trigger. A bright, uncatalogued x-ray source was found within the BAT error circle. The UVOT also imaged the field, but no OC was found. GRB 091031 2009/10/31 12:00:28 04:42:00 -59:06:00 Dorado The GGM light curve showed many pulses with substructure. The duration of the burst was about 35 seconds. The spectrum was best fit by a Band function with alpha = -0.91 +/- 0.04, beta = -2.34 +0.19/-0.31 and Epeak = 503.10 +47.30/-46.60 keV. GRB 091030 2009/10/30 19:52:26.86 17:40:12 21:32:00 Hercules The GBM showed two bright peaks followed by two dimmer ones. The burst duration was 160 seconds. The spectrum was fit by a Band function with alpha = -0.88 +/- 0.02, beta = -2.2 +/- 0.1 and Epeak = 507 +/- 30 keV. GRB 091003A 2009/10/03 04:35:45.58 16:46:04.687 36:37:30.76 Hercules "This burst had multiple peaks. It lasted approximately 21 seconds. The spectrum was fit by a Band function with alpha = -1.13 +/- 0.01, beta = -2.64 +/- 0.24 and Epeak = 486.2 +/- 23.6 keV. The burst was bright enough to cause a Fermi spacecraft repointing maneuver, and 5 hours of pointed observations were made. The LAT showed a significant increase in emission after the GBM trigger (GCN 9985). Observations with the Swift XRT were begun 15.5 hours after the Fermi/GBM trigger. A total of 2.5 kiloseconds were observed, revealing an uncatalogued x-ray source 6.85 arcminutes from the LAT position (GCN 9986). Subsequent observations taken up to 168 kiloseconds after the trigger showed that this source was fading, and thus was the GRB afterglow (GCN 9991). The Swift UVOT observed the source contemporaneously with the XRT. In the initial set of observations a faint, fading source was found inside the XRT error circle. The observations were taken in the uvw2 filter, and the object’s magnitude was 21.02 +/- 0.27. No extinction correction has been applied (GCN 9987). The afterglow was also seen by observers using the William Herschel Telescope and ACAM. In 60 and 250 second exposures started 1.69 days after the trigger, an r = 21.33 _/- 0.11 object was detected. A spectrum was also taken, but only faint continuum emission was seen. No strong or absorption lines were present, but the continuum seen at 4000A implies an upper limit of z = 2.3 for the redshift (GCN 9995)." GRB 090929A 2009/09/29 04:33:03.97 03:45:57.9 -05:57:50 Eridanus "The GBM light curve showed multiple short peaks, with the burst lasting a total of about 8.5 seconds. The spectrum was fit by a power law with exponential cutoff: index = -0.52 +/- 0.06, Epeak = 610.9 +/- 44.5 keV. This burst was also seen by the Swift/BAT instrument during a preplanned slew of the satellite. The BAT light curve had three successively weaker peaks. They occurred at T+1 second, T+4 seconds and T+8 seconds. The duration measured by the BAT was about 10 seconds, with the burst commencing at 04:33:08 UT." GRB 090927 2009/09/27 10:07:16 22:55:53.50 -70:58:49.2 Indus "This was a short burst, lasting only about 1.5 seconds. It had a single peak. An observing constraint prevented the satellite from slewing to the burst for 33 minutes, so no prompt XRT/UVOT data was obtained. The UVOT began observing the field beginning 2141 seconds (~70 minutes) after the trigger. In a 150 second finder chart exposure (unfiltered) there is an afterglow candidate with m = 19.10 +/- 0.15 (GCN 9946). Images were also obtained from the 1 meter Zadko telescope which showed a fading source within the XRT error circle 110 minutes after the trigger. Magnitudes were measured as follows GCN 9956): tmid(min) Exp. Time R Magnitude ------------------------------------- 110 42s >16 126 540s 19.8 +/- 0.5 158 360s 20.0 +/- 0.5 The VLT/FORS2 was used to obtain a spectrum of the OC starting 16.5 hours after the trigger. At that time the OC had a magnitude of R = 21.7. The spectrum shows absorption from Mg II and Fe II at z = 1.37. No evidence was seen for higher redshift systems, nor for Lyman-alpha, indicating that this is indeed the redshift of the GRB (GCN 9958). " GRB 090926A 2009/09/26 04:20:26.99 23:33:36.18 -66:19:25.9 Tucana "This burst had a single pulse lasting about 20 seconds. The spectrum was fit by a Band function with alpha = -0.75 +/- 0.01, beta = -2.59 +0.04/-0.05, and Epeak = 314 +/- 4 keV. The burst was bright enough to initiate a spacecraft repointing maneuver. It was also detected independently by INTEGRAL. This burst occurred at the edge of the LAT field, and that instrument also detected the burst. The LAT observed GeV photons coming from the burst for more than 200 seconds after the trigger (GCN 9934). The Swift UVOT observed the field beginning 13 hours after the burst. They find an m = 18.78 +/- 0.04 object. The burst was also observed with the XRT (GCN 9936). Observers using the PROMPT telescopes at Cerro Tololo in Chile reported detecting the optical afterglow. In images collected approximately 19 hours after the burst, the measured the following magnitudes (GCN 9937): mean time since cal. trig. tel. exp. fil. magnitude stars (h) (# x s) 19.9 PROMPT-2 22 x 80 V 18.81 +0.10 -0.09 52 NOMAD 20.0 PROMPT-5 22 x 80 I 18.24 +0.04 -0.04 165 USNO B1 20.0 PROMPT-4 24 x 80 R 18.06 +0.03 -0.03 230 USNO B1 A redshift was obtained for this afterglow from the VLT/X-shooter. These observations, which where done a part of the science verification for the new X-shooter single object spectrograph, were begun 22 hours after the burst. The afterglow had R = 17.9 at that time, and four 1800 second exposures were taken to produce the spectra. The final spectrum contained many absorption features, including CIV 1548 and 1550, Si II 1304 and 1526, Si II* 1533, FeII 1608, MgII 2798 and 2803 and unspecified others. There was also a broad absorption near 3780 which was interpreted as damped Lyman-alpha. These lines are all seen at a common redshift of z = 2.1062. The wavelength solution for these lines is based on archival calibration data, so minor corrections might be needed (GCN 9942). GRB 090925 2009/09/25 09:20:33.67 22:13:00 14:18:00 Pegasus This burst had a FRED-like light curve that lasted about 50 seconds. The spectrum was fit by a Band function with alpha = -0.60 +0.14 / - 0.13, beta = -1.91 +0.07 / - 0.09 and Epeak = 156 +25 / -20 keV. GRB 090922A 2009/09/22 12:56:42.14 01:08:00 74:18:00 Cassiopeia "The main pulse of this burst lasted 10 seconds, and it was followed by a weaker pulse approximately 60 seconds later. The total burst duration was about 92 seconds. The time-averaged spectrum was fit by a Band function with alpha = -0.77 +/- 0.05, beta = -2.28 +/- 0.07 and Epeak = 139.3 +/- 6.6 keV. This burst was 19 degrees from the LAT boresight, and it was bright enough that the spacecraft repositioned itself to better observe with the LAT… results of those observations are not yet reported. " GRB 090910 2009/09/10 19:29:48.81 19:44:00 72:18:00 Draco The burst had 3 pulses between T0-5 seconds to T0-45 seconds. A smaller pulse was seen at T0+70 seconds. The duration (T90) was 62 seconds. The spectrum was fit by a Band function with alpha = -0.9 +/- 0.1, beta = -2.0 +/- 0.2 and Epeak = 274.8 +/- 56.1 keV. GRB 090902A 2009/09/02 09:38:05.49 19:24:00 53:06:00 Cygnus This burst had a single peak and lasted approximately 1.2 seconds. The spectrum was fit using a Band function with alpha = 0.30 +0/5/-0.26, beta = -2.05 +0.29/-0.24 and Epeak = 388 +82/-102 keV. GRB 090904B 2009/09/02 11:05:08 17:39:45.26 27:19:28.1 Hercules "This burst had a single bright pulse lasting about 21 seconds. It was also independently detected by the INTEGRAL SPI-ACS. The spectrum was fit by a Band function with alpha =-0.696 +/- 0.012, beta = -3.85 +0.21/-0.31 and Epeak = 775 +/- 11 keV. The burst was also seen in the LAT (GCN 9867). Ongoing analysis with the Fermi GBM and LAT showed that the burst was detected in the LAT for at least 300 seconds. The Swift satellite began TOO observations 12.5 hours after the GBM trigger. It found an uncatalogued x-ray source within the GBM error circle (GCN 9868). Analysis of the observations, taken over ~4.5 hours, confirms that the object was fading, and thus was likely the GRB afterglow (GCN 9876). Swift UVOT observations were done simultaneously to the XRT ones, and a faint (m = 20.41 +/- 0.2) object was found within the XRT error circle. Though the object is not visible in the DSS image of the field, there is another faint object nearby, so it was not possible to make a positive identification between the two (GCN 9869). Observations taken with the 1 meter Nickel telescope at Lick Observatory were consistent with the source found by the UVOT, but no fading was evident, so the identification of the source with the GRB was still uncertain (GCN 9870). A spectrum obtained using the Gemini North telescope showed metal absorption from MgII[2796,2803], MgI[2853],MnII[2606], FeII[2600], MnII[2594], FeII[2586], FeII[2260], SiII[1808], SiII*[1816], all at a redshift of z = 1.822 (GCN 9873). This field was observed on September 03.94 from the Very Large Array radio telescope in New Mexico. The GRB was detected at 8.46 GHz (GCN 9889)." GRB 090831A 2009/08/31 07:36:36.58 09:40:00 51:00:00 Ursa Major This burst had two structured main peaks. Its total duration was about 69 seconds. The spectrum was fit by a power law with exponential cutoof. The power law index was -1.57 +/- 0.03, and the cutoff energy was Epeak = 399.6 keV. A Band function could also fit the spectrum: alpha = -1.52 +/- 0.06, beta = -1.96 +/-0.14, Epeak = 243.8 +-85.3. GRB 090829A 2009/08/29 16:07:38.86 21:57:00 34:11:00 Pegasus This burst lasted 85 seconds. It had a weak precursor followed by a single bright peak. The spectrum was fit by a Band function with alpha = -1.44 +/- 0.04, beta = -2.1 +/- 0.1 and Epeak = 183 +/- 31 keV. GRB 090829B 2009/08/29 16:50:40.13 23:40:00 -09:22:00 Aquarius This burst lasted approximately 100 seconds and had two widely separated peaks. The spectrum was fit by a Band function with alpha = -0.7 +/- 0.2, beta = -2.4 +/- 0.5 and Epeak = 143 +/- 30 keV. GRB 090828 2009/08/28 02:22:48.20 08:18:00 -26:06:00 Puppis This light curve had three pulses with a total duration of ~100 seconds. The spectrum was fit by a Band function with alpha = -1.23 +0.06/-0.05, beta = -2.12 +0.08/-0.11 and Epeak = 136.5 +16.0/-13.7. GRB 090826 2009/08/26 01:37:31.85 09:22:00 -00:06:00 Hydra The burst had two pulses with a total duration of approximately 8.5 seconds. The spectrum was fit using a power law with exponential cutoff. The power law index was -0.96 +0.32/-0.28. The cutoff energy was Epeak = 172 +132/-64 keV. GRB 090820A 2009/08/20 00:38:16.19 05:51:00 27:00:00 Taurus "This burst had a weak precursor, then, 30 seconds later, a bright pulse that lasted 30 seconds. The spectrum was fit by a Band function with alpha = -0.69 +/- 0.01, beta = -2.61 +/- 0.05 and Epeak = 215 +/- 3 keV. The burst was so bright that Fermi repositioned to do a pointed observation beginning 3100 seconds after the trigger. Earth constraint prevented an earlier pointed observation. This burst was also detected by the RT-2 Experiment (both detectors RT-2/S and RT-2/G) aboard CORONAS-PHOTON. A precursor followed by single peak at T0+34 seconds was seen, consistent with the behavior seen by Fermi. The burst width was seen to diminish with increasing energy (GCN 9833)." GRB 090820B 2009/08/20 12:13:16.70 21:13:00 -18:36:00 Capricornus The light curve had two narrow peaks and a duration of about 11.2 seconds. The spectrum was fit by a power law with exponential cutoff. The power law index was -1.44 +/- 0.18, with cutoff energy 38.8 +/- 4.4 keV. GRB 090815A 2009/08/15 07:12:12.45 02:47:00 -02:00:00 Eridanus This burst was quite long, lasting 200 seconds. It had a single broad pulse. The spectrum was fit by a simple power-law with an index of -1.15 +/- 0.1. GRB 090815B 2009/08/15 10:30:41.85 01:26:00 53:24:00 Cassiopeia This burst had two peaks, lasting a total of 30 seconds. The spectrum was fit by a power law with exponential cutoff at Epeak = 15.1 +/- 10.8 keV. The index was -1.89 +/- 0.12. GRB 090814C 2009/08/14 08:49:41.22 22:10:00 58:54:00 Cepheus The GBM light curve had a single peak lasting 0.25 seconds. The spectrum was fit by a power law with exponential cutoff at Epeak = 790 +/- 120 keV. The power law index was -0.39 +/- 0.11. GRB 090809B 2009/08/09 23:28:14.61 06:21:00 00:08:00 Monoceros This burst consisted of a single pulse in the GBM. It lasted approximately 15 seconds. The spectrum was fit using a Band function with alpha=-0.85 +/- 0.04, beta = -2.02 +/- 0.06 and Epeak = 198 +/- 13 keV. GRB 090807B 2009/08/07 19:57:59.02 21:48:00 07:12:00 Pegasus This burst had a single pulse with structure. The pulse lasted about 3 seconds. The spectrum was fit by a Band function with alpha = -0.6 +/- 0.4, beta = -2.4 +/- 0.1 and Epeak = 37 +/- 5 keV. GRB 090802A 2009/08/02 05:39:03.08 03:24:00 37:54:00 Perseus The BGM light curve had a single FRED peak lasting 128 milliseconds. The spectrum was fit by a Band function with alpha = -0.42 (-0.17 +0.21), beta = -2.4 (-0.7 +0.3) and Epeak = 283 (-53 +58) keV. GRB 090802B 2009/08/02 15:58:23.44 17:48:00 -71:46:00 Apus This was a weak source, and no additional information is given. GRB 090720 2009/07/20 06:38:08.28 13:18:00 -16:24:00 Virgo The light curve for this burst had a single peak lasting about 7 seconds. The spectrum for this burst was fit by a power law with exponential cutoff: index = -0.75 +/- 0.10, Epeak = 117.5 +/- 7.12. GRB 090720B 2009/07/20 17:02:56.910 13:32:00 -54:48:00 Centaurus This GRB had two bright peaks. It lasted about 20 seconds. The spectrum was fit by a power-law with exponential cutoff: index =-1.01 +/- 0.5, Epeak = 982 +/- 186 keV. It could be fit equally well using a Band function with alpha = -1.00 +/- 0.05, beta = -2.43 +/- 0.47 and Epeak = 924 +/- 201 keV. GRB 090719 2009/07/19 01:31:26.61 22:45:00 -67:52:00 Indus The GBM light curve had a bright pulse with substructure and a duration of approximately 16 seconds. The spectrum was fit by a Band function with alpha = -0.68 +/- 0.02, beta = -2.92 +/- 0.16 and Epeak = 254 +/- 6 keV. GRB 090718A 2009/07/18 17:16:42.93 16:10:00 -06:35:00 Ophiuchus This was a weak source, and no additional information is available. GRB 090718B 2009/07/18 18:17:42.84 18:16:00 -36:23:00 Sagittarius The light curve had a total duration of approximately 28 seconds and exhibited several peaks. The spectrum was fit by a power law with exponential cutoff. The power law index is -1.21 +/- 0.02 and the cutoff energy is Epeak = 198 +/- 9 keV. A Band function also fits the spectrum: alpha = -1.18 +/- 0.03, beta = -2.59 +/- 0.26 and Epeak = 184 +/- 9 keV. GRB 090717A 2009/07/17 00:49:32.11 05:47:00 -64:12:00 Dorado The GBM showed two peaks, with a total duration of approximately 70 seconds. The spectrum was fit by a Band function with alpha = -0.88 +/- 0.04, beta = -2.33 +/- 0.06 and Epeak = 120 +/- 5 keV. GRB 090717B 2009/07/17 02:40:31.79 16:28:00 23:00:00 Hercules The GBM light curve had a single peak lasting 0.9 seconds. The spectrum was fit by a simple power law with index -1.02 +/- 0.04. GRB 090713 2009/07/13 00:29:28.06 18:59:00 -03:20:00 Aquila This burst had multiple peaks and lasted approximately 113 seconds. The spectrum was fit by a power law with exponential cutoff: index = -0.34 +/- 0.12, Epeak = 99 +/- 5 keV. GRB 090706 2009/07/06 06:47:40.43 13:40:00 -47:06:00 Centaurus The GBM showed two peaks lasting a total of ~100 seconds. The spectrum was fit by a simple power law with index -2.16 +/- 0.09. GRB 090703 2009/07/03 07:54:02.48 00:03:00 09:42:00 Pisces The GBM light curve showed a single peak lasting about 9 seconds. The spectrum was fit by a simple power-law with index -1.72 +/- 0.06. GRB 090701 2009/07/01 07:54:02.48 07:39:00 -42:06:00 Puppis A single pulse lasting 12 seconds was seen in the GBM. The spectrum was fit by a simple power law with index 1.84 +/- 0.09. GRB 090630 2009/06/30 07:27:21.17 09:24:00 -46:36:00 Vela The GBM light curve had a single peak lasting approximately 5.1 seconds. The spectrum was fit by a power-law with exponential cutoff: index = -1.5 +/- 0.1, Epeak = 79 +/- 13 keV. A Band function could also be used to fit the spectrum, with alpha -1.5 +/- 0.2, beta = -2.3 +/- 0.4 and Epeak = 71 +/- 24 keV. GRB 090626 2009/06/26 04:32:08.88 11:17:00 -36:06:00 Centaurus The GBM light curve had four main peaks and lasted approximately 70 seconds. The spectrum was fit by a Band function with alpha = -1.29 +/- 0.02, beta = -1.98 +/- 0.02 and Epeak = 175 +/- 12 keV. GRB 090625A 2009/06/25 05:37:00.21 01:21:00 -06:24:00 Cetus This GRB had multiple weak pulses. It lasted approximately 51 seconds. The spectrum was fit by a power-law with exponential cutoff. The power-law index was -0.6 +/- 0.2 and the cutoff energy was Epeak = 198 +/- 36 keV. GRB 090623 2009/06/23 02:34:17.56 20:36:00 -43:12:00 Microscopium At least five peaks were seen in the GBM light curve, which lasted 72 seconds. The spectrum was fit by a power law with exponential cutoff. The index was -0.73 +/- 0.04 and the cutoff energy was Epeak = 476 +/- 39 keV. GRB 090623 2009/06/23 02:34:17.56 20:36:00 -43:12:00 Microscopium At least five peaks were seen in the GBM light curve, which lasted 72 seconds. The spectrum was fit by a power law with exponential cutoff. The index was -0.73 +/- 0.04 and the cutoff energy was Epeak = 476 +/- 39 keV. GRB 090621C 2009/06/21 10:00:52.10 17:10:00 -28:28:00 Ophiuchus The burst had multiple short peaks and a duration of ~59.9 seconds. The spectrum was fit by a power-law plus exponential cutoff. The index is -1.4 +/- 0.1 and the cutoff energy is Epeak = 148 +/- 34 keV. GRB 090621D 2009/06/21 10:43:45.14 00:49:00 -22:36:00 Cetus This burst had two peaks and it lasted 39.9 seconds. The spectrum was fit by a simple power-law with index -1.66 +/- 0.05. GRB 090620 2009/06/20 09:36:23.47 15:50:00 61:12:00 Draco This had a single peak lasting approximately 16.5 seconds. The spectrum was fit by a Band function with alpha = -0. 40 +/- 0.04, beta = -2.44 +/- 0.10 and Epeak = 156 +/- 6 keV. The burst was independently detected by INTEGRAL. GRB 090616 2009/06/16 03:45:42.53 06:52:00 -03:42:00 Monoceros This burst had a single pulse that lasted approximately 2.7 seconds. The spectrum was fit by a power law with index -1.27 +/- 0.07. GRB 090612 2009/06/12 14:50:50.490 05:24:18 17:45:00 Taurus The GBM light curve showed a single strong pulse which was preceded by a weak pre-trigger. The total duration of the burst was ~ 58 seconds. The spectrum was fit using a Band function with alpha = -0.6 +/- 0.1, beta = -1.9 +/- 0.1 and Epeak = 357 +/- 59 keV. GRB 090610A 2009/06/10 15:33:25.94 05:37:00 35:24:00 Auriga This burst had a single pulse lasting 6.5 seconds. The spectrum was fit using a power law with index -1.30 +/- 0.03. GRB 090610B 2009/06/10 17:21:31.90 18:24:00 -42:06:00 Corona Austrina This burst was triggered by single short pulse which was followed by a broad pulse at T+80. The total burst duration was 202.5 seconds. The spectrum during the the ~10 seconds centered at T0 was fit by a power law with exponential cutoff. The index was -0.46 +/- 0.36 and the cutoff energy Epeak = 104.90 +/- 16.70 keV. The spectrum of the second pulse was fit by a simple power law with index -1.66 +/- 0.07. GRB 090610C 2009/06/10 21:12:07.73 04:42:00 30:18:00 Auriga This burst had a single peak lasting approximately 18.1 seconds. The spectrum was fit with a simple power law of index -1.62 +/- 0.08. GRB 090608 2009/06/08 01:15:26.60 06:41:00 -37:25:00 Puppis The GBM showed multiple peaks lasting a total of about 61 seconds. The spectrum was fit by a power law with index = -1.83 +/- 0.07. GRB 090606 2009/06/06 11:18:08.00 09:48:00 -70:30:00 Carina This was a long weak pulse in the GBM, lasting approximately 60 seconds. The spectrum was fit by a power law with index -1.63 +/- 0.09. GRB 090602 2009/06/02 13:32:22.85 16:36:00 -65:00:00 Triangulum Australe The GBM light curve had a broad single peak with a duration of 16 seconds. The spectrum was fit using a power law with exponential cutoff: index = -0.56 +/- 0.14, Epeak = 503 +/- 91 keV. GRB 090530B 2009/05/30 18:14:24.42 04:53:00 13:47:00 Orion This was a long, soft burst lasting 194 seconds (T90). It had a FRED shape with a double peak. The spectrum was fit by a Band function with alpha = -0.71 +/- 0.06, beta = -2.42 +/- 0.05 and Epeak = 67 +/- 3 keV. GRB 090529B 2009/05/29 07:26:22.41 15:25:00 32:12:00 Corona Borealis The GBM light curve was a double-peaked FRED profile with a duration of 194 seconds. The spectrum was fit by a Band function with alpha = -0.71 +/- 0.06, beta = -2.42 +/- 0.05 and Epeak = 67 +/- 3 keV. GRB 090529C 2009/05/29 13:32:00.49 10:51:00 47:18:00 Ursa Major This GBM light curve had two narrow pulses and a duration of about 10.4 seconds. The spectrum was fit by a Band function with alpha = -0.84 +/- 0.05, beta = -2.1 +/- 0.1 and Epeak = 188 +/- 15 keV. GRB 090528A 2009/05/28 04:09:01.14 09:00:00 -35:48:00 Pyxis This burst lasted ~ 68 seconds. The light curve had one major pulse with structure. The spectrum was fit by a power law with exponential cutoff. The index is -1.7 +/- 0.1 and the cutoff energy is Epeak = 99 +/- 26 keV. GRB 090528B 2009/05/28 12:22:31.29 20:49:00 32:42:00 Cygnus The GBM light curve showed multiple peaks with a weak structured tail. The duration of the burst was 102 seconds. The spectrum was fit with a power law and exponential cutoff: index = -1.10 +- 0.04, Epeak = 172 +/- 12 keV. GRB 090524 2009/05/24 08:17:56.23 21:58:00 67:24:00 Cepheus The burst had two main peaks and a total duration of 72 seconds. The spectrum was fit by a Band function with alpha = -1.00 +/- 0.08, beta = -2.30 +/- 0.09 and Epeak = 82.6 +/- 6.3 keV. GRB 090522 2009/05/22 08:15:49.33 18:31:00 19:36:00 Hercules This burst lasted 22 seconds and had a single pulse. The spectrum was fit by a power law with exponential cutoff. The power law index is -1.03 (+ 0.41 / - 0.53) with energy cutoff Epeak = 75.8 (+36.9 / - 15.9) keV. GRB 090520B 2009/05/20 19:57:53.98 22:08:00 43:12:00 Lacerta This burst lasted 1.5 seconds and had a single peak light curve. The spectrum is fit by a simple power law with index -1.4 +/- 0.1. GRB 090520C 2009/05/20 20:23:19.31 07:24:48 -19:42:00 Canis Major The burst had a single peak lasting 4.9 seconds. The spectrum was fit with a Band function with alpha = -0.73 +/- 0.09, beta = -1.96 +/- -.10 and Epeak = 204.2 +/- 27.9. GRB 090520D 2009/05/20 21:01:37.14 08:45:12 -18:00:00 Hydra The burst had a single pulse lasting 12 seconds. The spectrum was fit using a power law with exponential cutoff: index = -1.03 +/- 0.22, Epeak =47.4 +/- 4.1 keV. It was fit equally well with a Band function: alpha = -0.99 +/- 0.28, beta = -3.25 +/- 1.23 and Epeak = 46.3 +/- 5.3 keV. GRB 090519B 2009/05/19 11:05:27.54 07:04:00 56:42:00 Lynx This burst had a single peak lasting 4 seconds. This was superimposed on a lower level continuum that lasted a total of 87 seconds. The spectrum was fit by a power law with index -1.63 +/- 0.05. GRB 090518B 2009/05/18 05:51:04.67 14:05:00 -16:42:00 Virgo The light curve had a duration of about 12 seconds and showed a single peak. The spectrum can be fit with either a power law with exponential cutoff: index = -0.74 +/- 0.13, Epeak = 127 +/- 12 keV, or a Band Function with Epeak = 86 +/- 15 keV, beta = -2.10 +/- 0.14 and alpha not constrained. GRB 090516C 2009/05/16 20:28:40.05 01:03:00 -13:41:00 Cetus The GBM light curve contained a single short spike with some smaller peaks. The duration of the burst was about 15 seconds. The spectrum was fit by a power-law with exponential cutoff. The index was -1.51 +/- 0.08, and the cutoff energy was Epeak = 210 +/- 68 keV. A Band function provided a better fit, but the low energy index (alpha) is poorly constrained: alpha = -0.44 +/- 0.81, beta = -1.81 +/- 0.06 and Epeak = 38 +/- 14 keV. GRB 090516B 2009/05/16 03:17:20.17 08:09:00 -71:37:00 Volans This burst contained several overlapping peaks lasting approximately 140 seconds. Additional weak emission was detected to as long as 350 seconds. The spectrum for this burst was fit by a power law with exponential cutoff: index = -1.01 +/- 0.06, Epeak = 327.0 +/- 58.7 keV. GRB 090514 2009/05/14 00:08:39.16 00:49:00 -10:54:00 Cetus The GBM light curve had multiple peaks and lasted 49 seconds. The spectrum was fit by a power law with index -1.92 +/- 0.4. GRB 090513 2009/05/13 21:58:47.92 17:59:00 -31:36:00 Sagittarius The GBM light curve showed a broad peak lasting 23 seconds. The spectrum was fit by a power law with exponential cutoff: index = -0.9 +/- 0.1, Epeak = 850 +/- 390 keV. GRB 080513B 2009/05/13 22:35:35.34 06:36:00 -72:54:00 Volans Because this burst was quite weak no additional information is available. GRB 090511 2009/05/11 16:25:16.37 10:48:00 51:18:00 Ursa Major The burst had a single pulse lasting 14 seconds. The spectrum was fit with a power law plus exponential cutoff: index = -0.95 +/- 0.18, Epeak = 391 +/- 157 keV. GRB 090510B 2009/05/10 7:47:39.510 17:57:00 -57:56:00 Pavo The burst lasted 7 seconds. It had a single peak. The source was weak, so the spectrum was not well constrained. GRB 090502 2009/05/02 18:39:34.64 17:51:00 -20:18:00 Sagittarius The burst lasted about 66 seconds and showed multiple peaks. The spectrum was fit by a power law with exponential cutoff: index = -1.1 +/- 0.3, Epeak = 63.2 +/- 8.7 keV. GRB 090428B 2009/04/29 13:15:11.06 00:03:00 06:30:00 Pisces The GBM light curve had a single broad peak lasting approximately 30 seconds. The spectrum can be fit by a power law with exponential cutoff: index = -1.86 +/- 0.07, Epeak = 65 +/- 16 keV. It can be fit equally well by a Band function: alpha = -1.81 +/- 0.13, beta = -2.17 +/- 0.21, Epeak = 53 +/- 19 keV. GRB 090429C 2009/04/29 12:43:25.70 17:26:00 55:30:00 Draco The GBM showed two pulses and a total duration of 13 seconds. The spectrum was fit by a power law of index -1.43 +/- 0.04. GRB 090429D 2009/04/29 18:03:57.51 08:20:48 06:12:00 Hydra Three short pulses are seen in this light curve, two occurring before the trigger. The duration of the burst was T90 = 11 seconds. The spectrum could be fit by a power law with exponential cutoff: index -0.87 +/- 0.27, Epeak = 223 +/- 72.5 keV. A Band function also fit the spectrum: alpha = -0.66 +/- 0.53, beta = -1.88 +/- 0.32 and Epeak = 152.8 +/- 92.4. GRB 090428A 2009/04/28 10:34:38.46 14:10:00 37:18:00 Bootes The GBM light curve has two peaks and lasts approximately 8 seconds. The spectrum could be fit by a power law with exponential cutoff (index -0.59 +/- 0.16, Epeak = 97 +/- 7 keV) or a Band function with alpha =-0.40 +/- 0.25, beta = -2.7 +/- 0.4 and Epeak = 85 +/- 10 keV. GRB 090427B 2009/04/27 15:27:00.86 14:00:00 -45:42:00 Centaurus The GBM showed a single peak with a duration of 7 seconds. The spectrum was fit by a power of index -1.1 +/- 0.1. GRB 090427C 2009/04/27 16:30:23.81 23:45:00 -34:35:00 Sculptor The light curve had two peaks and a duration of 12.5 seconds. The spectrum was fit by a power law and exponential cutoff: index = 0.35 +/- 0.16, Epeak = 75 +/- 3 keV. GRB 090426B 2009/04/26 01:35:35.23 01:10:00 -19:12:00 Cetus The light curve has a single peak with a long tail. Duration is approximately 3.8 seconds. The spectrum was best bit by a power law with index -1.60 +/- 0.08. GRB 090426C 2009/04/26 16:33:49.27 05:31:00 -09:40:00 Orion The light curve had one main pulse lasting 12 seconds. The spectrum was fit by a power law with exponential cutoff with index -1.31 +/- 0.09, Epeak = 351 +150/-81 keV. GRB 090412 2009/04/12 01:28:05.25 00:01:00 -48:48:00 Phoenix This burst was weak, with a pulse lasting 0.5 seconds. Because it was so weak there was no spectral fit possible. GRB 090411A 2009/04/11 20:06:36.89 10:37:00 68:21:00 Ursa Major The duration of this burst was ~25 seconds. It had two main pulses. The spectrum was best fit by a Band function with Epeak = 141 +/- 35 keV and indices alpha = -0.88 +/- -.15 and beta = -1.82 +/- 0.08. GRB 090411B 2009/04/11 23:47:44.88 02:28:00 03:15:00 Cetus A single “spiky” peak lasting 19 seconds describes this burst. The spectrum was fit by a Band function with alpha = -0.8 +/- 0.1, beta = -2.0 /- 0.2 and Epeak = 189 +/- 37 keV. GRB 090409 2009/04/09 06:54:01.44 20:08:00 01:06:00 Aquila GRB 090403 2009/04/03 07:32:42.13 04:21:00 47:06:00 Perseus GRB 090331 2009/03/31 16:20:20.39 14:09:00 00:31:00 Virgo This was a weak burst. No spectral or other information has been provided. GRB 090328 2009/03/28 09:36:46 06:02:39.58 -43:52:57.5 Pictor "Fermi detected this burst in both the GBM and the LAT. Emission was seen up to several GeV in the LAT. The burst had a complicated multi-peak light curve, with emission extending longer than 100 seconds in total. The object was following with the LAT for five hours after the trigger. Followup observations of the LAT field using the Swift XRT revealed an uncatalogued x-ray source within the LAT error circle. The observations were begun approximately 16 hours after the GBM trigger (GCN 9045, 9046). Swift also performed observations with the UVOT and detected an optical OC with magnitudes listed below (GCN 9048): Filter T_mid (hrs) Exposure(s) Mag Err ------------------------------------------------------------ u 16.0 793 19.04 +/- 0.13 white 16.1 173 19.56 +/- 0.14 GRB 090324 2009/03/24 02:48:09 17:08:42.73 -48:08:47.59 Ara This burst had a 30 second duration and a FRED type light curve. GRB 090323 2009/03/23 00:02:42.63 12:42:50.26 17:03:14.2 Coma Berenices "This burst was detected by Fermi in both the GBM and the LAT. In the LAT, emission was seen to extend up to a few GeV, with the high energy emission beginning several seconds after the GBM trigger. The light curve contained multiple peaks and lasted ~150 seconds, but there is marginal evidence that the high energy emission lasted for a couple of kiloseconds. The burst location was tracked by Fermi for five hours, subject to Earth angle constraints. The Swift observatory began a TOO observation of this GRB at 19:27UT on 2009/03/23. With 1137 seconds of XRT in photon counting mode an uncatalogued x-ray source was found within the Fermi LAT error circle (GCN 9024). From the ground, observers using the GROND multiband imager detected an afterglow candidate in the NIR. The observations started 26 hours 48 minutes after the trigger. The observations confirm the Swift XRT point source. With 8 minutes of exposure the following magnitudes were obtained (GCN 9026): g' = 21.64 +/- 0.07 mag, r' = 20.03 +/- 0.03 mag, i' = 19.64 +/- 0.02 mag, z' = 19.39 +/- 0.02 mag, J = 19.24 +/- 0.02 mag, H = 18.86 +/- 0.02 mag, and K = 18.58 +/- 0.03 mag The object was also detected in observations from the Palomar 60” telescope at r’ = 20.5, I’ = 20.0. These observations began 28 hours 18 minutes after the trigger (GCN 9027). A redshift for the afterglow was obtained using the Gemini South Telescope. Spectra obtained about 30 hours after the trigger showed strong absorption blueward of 5580 Ang. This was taken to be the onset of the Lyman Alpha forest, suggesting z = 3.6. In addition, multiple narrow absorption features were seen from C IV, O I, C II and Si IV at a similar redshift (z = 3.57, GCN 9028) " GRB 090320A 2009/03/20 10:01:04 16:10:00 -51:54:00 Norma This burst had a single peak and lasted about 10 seconds. However, the duration was not well-measured because of strong background fluctuations. No other information is available. GRB 090320B 2009/03/20 19:13:46.10 12:15:18 57:33:00 Ursa Major This burst lasted 52 seconds. It had one main pulse and several subsequent weaker pulses. The spectrum was fit by a power law with exponential cutoff: index -1.1 +/- 0.3, Epeak = 72 +/- 14 keV. GRB 090320C 2009/03/20 1:05:10.530 07:13:00 -43:18:00 Puppis This burst had a duration of about 4 seconds, but because it was weak there is no spectrum fit available. GRB 090319 2009/03/19 14:55:35.220 18:18:00 -11:24:00 Serpens The burst had two distinct peaks of duratoin ~6 seconds which sat atop a smooth component lasting ~68 seconds. The first peak was centered at T0+13 and T0+30 seconds, respectively. The spectrum was best fit by a power law with exponential cutoff: index = 0.90 +/- 0.10 and Epeak = 187.3 +/- 20.4 keV. GRB 090310 2009/03/10 04:32:49.90 12:07:00 -38:42:00 Centaurus This light curve consisted of a single narrow peak which lasted ~ 4 seconds. This was follows by several fainter peaks. The total burst duration was T90 ~ 125 seconds. The spectrum over the first four seconds was fit by a power law with exponential cutoff: index = -0.65 +/- 0.13, Epeak = 279 +/- 43 keV. GRB 090309B 2009/03/09 18:25:07.19 11:13:00 -55:01:00 Centaurus Two main peaks were seen in this burst, which had a duration of 10 and 25 seconds, respectively. The spectrum was best fit by a power law with exponential cutoff: index = -1.52 +/- 0.10, Epeak = 197 +/- 65 keV. GRB 090308B 2009/03/08 17:36:24.70 01:30:00 58:05:00 Cassiopeia This burst showed two peaks with substructure. It had a duration of about 2.1 seconds. The spectrum was fit using a power law with exponential cutoff: index = -0.54 +/- 0.11, Epeak = 710.3 +/- 100 keV. GRB 090307B 2009/03/07 10:34:00 14:36:00 04:00:58.60 Virgo This GRB had a FRED-like pulse with substructure. It began at T0-6 seconds and had a duration of T90 ~ 30 seconds. Its spectrum was fit with a power law having index -0.7 +/- 0.3 and cutoff Epeak = 212 +/- 80 keV. GRB 090306C 2009/03/06 05:52:05.35 09:00:00 51:36:00 Ursa Major The light curve for this burst had a single main peak that lasted 5 seconds. This was followed by a broad tail lasting 39 seconds. The spectrum was fit by a power law with exponential cutoff: index = -0.58 +/- 0.29, Epeak = 107 +/- 16 keV. A Band function fit the spectrum as well: alpha = -0.32 +- 0.54, beta = -2.28 +/- 0.43, Epeak = 87 +/- 25 keV. GRB 090305B 2009/03/05 01:14:35.72 10:20:00 68:06:00 Ursa Major The lightcurve had a single peak lasting 2 seconds. The spectrum for the burst was fit by a Band function with Epeak = 770 +/- 230 keV, alpha = -0.50 +/- 0.17, beta = -1.9 +/- 0.2. GRB 090304 2009/03/04 05:10:48.16 16:25:00 -80:54:00 Apus Because this burst was quite weak no additional information is available. GRB 090301B 2009/03/01 07:33:37.98 23:21:00 09:00:00 Pegasus The GBM showed a single peak lasting 5 seconds. This was atop a broader, low level burst lasting 28 seconds. The spectrum was fit by a power law with exponential cutoff. The index is -1.03 +/- 0.09 with Epeak = 546 +/- 133 keV. The spectrum could be fit as well with a Band function having Epeak 427 +/- 147 keV, alpha = -0.98 +/- 0.12, beta = -1.93 +/- 0.24. GRB 090228 2009/02/28 04:53:20.91 07:07:00 -24:18:00 Canis Major The duration of this burst was 0.8 seconds. The pulse had a single bright pulse with a subsequent much fainter one. It’s spectrum was fit by a Band function with Epeak = 849 +/- 44 keV, alpha = -0.35 +/- 0.04 and beta = -2.98 +/- 0.25. GRB 090227 2009/02/27 07:25:57.00 00:13:00 -43:06:00 Phoenix The single FRED-like peak on this burst contained substructure and had a duration of 50 seconds, with some detectable emission continuing out to 80 seconds. The spectrum was fit by a power law with exponential cutoff. The power law index is -0.91 +/- 0.06 and the cutoff energy is Epeak = 1355 +/- 259 keV. The spectrum can be fit equally well by a Band function with alpha = -0.92 +/- 0.06, beta = -3.6 +/- 2.9 and Epeak = 1357 +/- 284 keV. GRB 090227B 2009/02/27 18:31:01.41 11:48:36 32:10:12 Ursa Major A 0.9 second spike characterizes this burst light curve. The spectrum was best fit by a Band function with alpha = -0.53 +/- 0.02, beta = -3.04 +/- 0.23 and Epeak = 2255 +/- 116 keV. GRB 080226 2009/02/26 14:52:42.17 10:29:00 14:30:00 Leo A single peak with duration ~0.8 seconds defines this burst. The spectrum was fit by a power-law with exponential cutoff. The index was -0.65 +/- 0.14, Epeak = 710 +/- 170 keV. The burst was independently detected by INTEGRAL. GRB 090222 2009/02/22 04:17:09.58 08:01:00 43:24:00 Lynx This burst had a single main peak with substructure. The duration was ~18 seconds. The spectrum was fit using a power law with exponential cutoff. The index was -1.00 +/- 0.11, Epcak = 157.7 +/- 19.8 keV. A Band function fit the spectrum equally well: Epeak = 147.9 +/- 27.1, alpha = -0.97 +/- 0.14, beta = -2.56 +/- 0.66. GRB 090219 2009/02/19 01:46:18.15 01:05:36 60:12:00 Cassiopeia "This burst lasted about half a second and had two closely spaced, narrow peaks. The spectrum was fit by a simple power law with index -1.43 +/- 0.05. " GRB 090217 2009/02/17 04:56:42.56 14:08:00 -02:48:00 Virgo "A single peak lasting 32.8 seconds characterized this burst. The spectrum was fit by an power law with exponential cutoff: index = -0.85 +/- 0.02, Epeak = 626 +/- 29 keV. The spectrum was fit equally well by a Band function with alpha = -0.845 +/- 0.023, beta = -2.86 +/- 0.36 and Epeak = 610 +/- 32 keV. This burst was detected not only by the GBM, but also by the LAT. In the LAT the emission continued for 20 seconds after the GBM trigger, but it did not begin until several seconds after the trigger (GCN 8903). The XRT aboard Swift was used to observe this field starting 10.8 hours after the trigger. Three sources with S/N > 3 were detected, but these were all associated with previously known sources and were not thought likely to be associated with the GRB (GCN 8907)." GRB 090213 2009/02/13 05:39:25.46 21:48:00 -53:30:00 Indus This was a weak burst. No spectral or other information has been provided. GRB 090207 2009/02/07 18:39:10.84 16:19:00 36:49:00 Corona Borealis This burst had a fast rise and slow decay. Its duration was ~10 seconds. The spectrum was fit by a power law with index -1.59 +/- 0.04. GRB 090202 2009/02/02 08:19:30.40 17:56:00 -02:30:00 Ophiuchus A single peak light curve was seen for this burst. It had a duration of approximately 66 seconds. The spectrum was fit by a power law with an exponential cutoff: index = -1.31 +/- 0.06, Epeak = 570 +/- 170 keV. The notice says that the burst was independently detected by INTEGRAL, though no circular has been posted. GRB 090126B 2009/01/26 05:26:22.23 19:42:00 33:12:00 Cygnus This burst had a single peak and a duration of ~11 seconds. The spectrum was best fit by a power law with exponential cutoff; the index is -0.99 +/- 0.18, with Epeak = 47.5 +/- 3.4 keV. GRB 090126C 2009/01/26 05:52:33.73 14:52:00 39:12:00 Bootes This burst was quite weak, and it lasted only ~ 1 second. As a result, the spectrum is not well constrained. No report of an afterglow has been made. GRB 090117B 2009/01/17 08:02:02.23 15:32:00 27:36:00 Corona Borealis The burst had two separate peaks, the first lasting ~1.5 seconds and the seconds approximately 25 seconds later and lasting ~2.5 seconds. The total length of the burst was ~27 seconds. Both peaks were fit with a simple power law spectrum. The index for the first was -1.55 +/- 0.08, and for the second it was -1.55 +/- 0.07. GRB 090117C 2009/01/17 15:10:40.18 07:50:00 -40:18:00 Puppis The burst had a long precursor, lasting tens of seconds. This was followed by a single, complex burst event with a duration of ~35 seconds. The total burst duration was ~86 seconds. The spectrum was best fit by a Band function with alpha = -1.0 +/- 0.1, beta = -2.1 +/- 0.2 and Epeak = 247 +/- 41 keV. The precursor spectrum between T0-55 seconds and T0-6 is best fit using a power law of index -1.3 +/- 0.1 and high energy cutoff at Epeak = 147 +/- 38 keV. GRB 090112A 2009/01/12 07:57:23.11 07:27:00 -30:17:00 Puppis This burst had two peaks with substructure. It lasted approximately 65 seconds, and there was some evidence of a precursor near T0-20 seconds. The spectrum was fit by a Band function with alpha = -0.94 +/- 0.20, beta = -2.01 +/- 0.19 and Epeak = 150 +/- 40 keV. GRB 090112B 2009/01/12 17:30:15.45 12:15:00 22:12:00 Coma Berenices The Fermi GBM triggered on this single peaked burst which lasted 12 seconds. The spectrum was best fit by a Band function with alpha = -0.75 +/- 0.06, beta = -2.43 +/- 0.14 and Epeak = 139 +/- 9 keV. GRB 090109 2009/01/09 07:58:29.49 08:11:00 54:48:00 Lynx This burst had a single, weak peak of duration 5 seconds. The spectrum was fit using a simple power law of index -1.50 +/- 0.08. GRB 090108A 2009/01/08 00:29:02.37 17:32:00 52:28:00 Draco This burst had a single bright pulse followed by a much fainter one. The total duration of the burst was approximately 0.9 seconds. The spectrum is best fit by a Band function with alpha = -0.47 +/- -.20, beta = -1.97 +/- 0.09 and Epeak = 104.9 +/- 16.4 keV. GRB 090108B 2009/01/08 07:43:23.36 00:15:00 -32:12:00 Sculptor This burst had a single peak lasting 0.8 seconds. The spectrum is fit by a power law of index -0.99 +/- 0.06. GRB 081231 2008/12/31 03:21:01.93 14:35:00 -38:43:00 Centaurus The GBM detected three main peaks with total duration of 29 seconds. The spectrum was best fit by a Band function with alpha = -0.80 +/- 0.06, beta = -2.03 +/- 0.07 and Epeak = 152.3 +/- 11.9 keV. GRB 081229 2008/12/29 04:29:01.8 11:22:00 55:06:00 Ursa Major A single pulse of duration 0.5 seconds was detected by the Fermi GBM. The spectrum was fit by a power law with exponential cutoff. The power law index was -0.42 +/- 0.18 and the cutoff energy is Epeak = 807 +/- 186 keV. A Band function could fit the spectrum as well, with alpha = -0.27 +/- 0.27, beta = -2.0 +/- 0.3 and Epeak = 585 +/- 188 keV. GRB 081226C 2008/12/26 03:44:52.41 12:38:00 27:48:00 Coma Berenices This long GRB had two main pulses, with weak emission extending back to T0-45 seconds. The burst lasted approximately 60 seconds in total. The spectrum is best fit by a power law with exponential cutoff. The power law index is -1.04 +/- 0.11, and the cutoff energy is Epeak = 82 +/- 7 keV. GRB 081224 2008/12/24 21:17:55 00:13:50.00 73:18:00 Cepheus This FRED burst lasted approximately 50 seconds. It had a FWHM of 15 seconds. Initially, a simultaneous detection and localization from the LAT was reported, but this was later retracted (GCN 8726). The Swift XRT was used to make follow-up observations beginning 18 kiloseconds after the trigger. A faint x-ray source was detected, but it was not certain that this was the afterglow, as the XRT FOV is smaller than the GBM/LAT error circle (but see above regarding the LAT detection). This set of observations was not sufficient to tell whether or not the source was fading (GCN 8725). GRB 081223 2008/12/23 10:03:57 07:47:00 33:30:00 Gemini The duration of this burst was 890 milliseconds. It had a single-peaked structure and its spectrum was fit by a power law with exponential cutoff: power law index was -0.63 +/- 0.10, Epeak = 280 +/- 30 keV. GRB 081217 2008/12/17 23:34:49 07:47:00 26:44:00 Gemini This broad burst had a duration of 39 seconds. The spectrum was fit by a Band function with Epeak = 167 +/- 11 keV, alpha = -0.61 +/- 0.09 and beta = -2.7 +/- 0.6. GRB 081216 2008/12/16 12:44:00 08:40:49 11:48:57 Cancer This burst was localized by the IPN, Suzaku-WAM, INTEGRAL-SPI-ACS and Konus-Wind. It corresponds to the Fermi trigger cited. The burst had a single peak lasting 0.2 second. GRB 081215 2008/12/15 18:48:37 09:00:00 53:48:00 Ursa Major This was an extremely bright burst, so bright that scattered radiation from the Earth prevented proper localization of the burst in the initial GCN notices. The burst duration was 7.7 seconds, and the spectrum is best fit by a Band function with Epeak = 304 +/- 11 keV, alpha = -0.585 +/- 0.022 and beta = -2.066 +/- 0.038. GRB 081213 2008/12/13 04:09:42 01:42:00 -35:18:00 Sculptor This single peak burst had a duration of 50 milliseconds. The spectrum is not well-constrained because of the weak signal in the burst. GRB 081209 2008/12/09 23:31:56 05:09:05 17:20:47 Taurus This burst was localized by the IPN. AGILE-MCAL, Swift-BAT and Konus-Wind observed this short duration (0.2 second) hard burst. The burst corresponded to Fermi-GBM trigger 250558317. It had a single peak. No afterglow has been reported. GRB 081206A 2008/12/06 06:35:53 08:00:00 32:42:00 Gemini Fermi detected this 24 second long burst. Its spectrum was well fit by a power law with exponential cutoff: power law index is -0.11 +/- 0.24, Epeak = 180 +/- 23 keV. A Band function is an equally good fit: Epack = 151 +/- 29 keV, alpha = 0.13, beta = -2.2 +/- 0.4. GRB 081206B 2008/12/06 14:29:30 23:05:00 -33:06:00 Piscis Austrinus This was a weak source. It showed a single peak with a duration of ~10 seconds. No other information is available. GRB 081206C 2008/12/06 23:41:50 02:44:00 -14:25:00 Cetus The GBM showed a pulse of duration ~20 seconds that began approximately 11 seconds before the trigger. Weak emission from the burst continued until ~T0+83 seconds. The spectrum was fit using a power law of index -1.35 +/- 0.04. GRB 081204B 2008/12/04 12:24:26 12:06:00 32:06:00 Ursa Major The burst had a single peak with duration of 320 milliseconds. A single power law best fits the spectrum, with index -1.18 +/- 0.05. GRB 081129 2008/11/29 03:52:04 03:40:00 -63:00:00 Reticulum Fermi detected this 2 - peaked burst. It had duration of about 59 seconds. The spectrum was best fit by a Band function with Epeak = 150 +/- 30 keV, alpha = -0.5 +/- 0.2 and beta = -1.84 +/- 0.08. GRB 081124 2008/11/24 01:26:11 22:26:00 -15:32:00 Aquarius This 35 second long burst had two distinct pulses. Its spectrum was best-fit by a Band function with Epeak = 22.8 +/- 0.7 keV, alpha = -0.6 +/- 0.2 and beta = -2.83 +/- 0.80. GRB 081122 2008/11/22 12:28:12 22:35:00 38:24:00 Lacerta The light curve for this burst had 3 pulses and a duration of 26 seconds. The spectrum was fitted by a power law with high energy cutoff: index = -0.77 +/- 0.07, Epeak = 200.7 +/- 15.7. The burst occurred only 21 degrees from the LAT boresight, and so observations with the LAT with a duration of 5 hours were commenced. GRB 081122B 2008/11/22 14:43:26 10:06:00 -02:06:00 Sextans The burst had a single peak with duration of 0.3 seconds. A single power law best fits the spectrum, with index -1.5 +/- 0.1. GRB 081120 2008/11/20 14:49:34 13:42:00 -09:06:00 Virgo The GRB had two peaks and a duration of 12 seconds. The spectrum is best-fit by a Band function with Epeak = 44 +/- 5 keV, alpha = 0.4 +/- 0.5 and beta = -2.18 +/- 0.10. GRB 081119 2008/11/19 04:25:27 22:46:00 29:42:00 Pegasus The duration of this burst was 0.8 seconds. It consisted of a single peak, and its spectrum was fitted with simple power law of index 1.3 +/- 0.1. GRB 081113 2008/11/13 05:31:32 09:47:00 68:54:00 Ursa Major The GRB on Fermi detected this burst. It had a duration of 0.5 seconds, with two short peaks, the first approximately 250 milliseconds long, and the second lasting 150 milliseconds. The spectrum is fit by a power law of index -1.28 +/- 0.05. The burst was also detected by INTEGRAL. GRB 081110 2008/11/10 14:25:43 08:14:00 21:12:00 Cancer Duration of this burst was 20 seconds. The light curve had three pulses, the first being the brightest and lasting 5 seconds. The subsequent pulses became progressively fainter. Optical imaging performed with the MASTER telescope did not detect any afterglow candidate to m=19 (unfiltered). The observations were done at T+6:42 (GCN 8519). GRB 081105 2008/11/05 13:26:12 00:15:48.5 03:28:15 Pisces This long soft burst triggered Konus-Wind, prompting them to inform the IPN. Swift, AGILE, Suzaku and INTEGRAL all had coincident detections. Subsequent observations with the XRT revealed an x-ray source within the BAT error circle 15.8 hours after the burst GCN 8487). No object was seen by the UVOT to limits of m > 20.76 (unfiltered, GCN 8488), and no other observers have reported observations of this object. GRB 081101B 2008/11/01 12:45:24 14:10:00 -31:06:00 Centaurus This GRB had several overlapping pulses with a duration of approximately 8 seconds. The spectrum is best fit by a power law with exponential high energy cutoff at 550 +/- 30 keV and spectral index -0.63 +/- 0.05. GRB 081024B 2008/10/24 21:22:41 21:31:36 21:12:14.4 Pegasus This Fermi-detected burst was seen both in the LAT and the GBM. It had a duration of 800 milliseconds and showed two main peaks. The first peak lasted 200 ms and its spectrum was fit by a power-law with exponential cutoff. The power-law index was -0.7 +/- 0.13 and the cutoff energy was 1583 +/- 520 keV. The second peak lasted 600 ms and was fit by a power-law of index -1.28 _/- 0.04. LAT observations showed emission from this burst up to 3 GeV in the first 5 seconds following the trigger. . Swift was able to slew to this source and begin observing 70.3 ks after the trigger, It detected three uncatalogued x-ray sources within the LAT error-circle. Subsequent observations undertaken approximately 1.5 days after the trigger showed two of the three sources. The other source was not detected, but due to photon statistics the observations could not unequivocally confirm fading. Additional observations performed 6 days after the trigger also did not detect this source (while still detecting the other two). However, these observations, when combined with the earlier ones, did detect the second source (R = 22.6), and suggested a 12% probability that it was not fading. It also suggested a possible association with a variable optical object (see below). Nonetheless, these observations could not confirm this source as the x-ray afterglow candidate (GCN 8454). In the meantime, observers using the Palomar 200 inch Hale Telescope imaged the LAT error circule in Sloan r’ and i’, starting approximately 30 hours after the burst. They detected 4 sources close to the possible x-ray afterglow candidate (see above). These ranged in brightness from R = 20.6 to 23.4. None of the detected objects showed any sign of variability, and one of them was seen on the DSS (GCN 8417). This burst was also detected by the SUZAKU instrument. It showed a double-peaked structure, as in the GBM, but it’s duration was 0.4 second (T90). (GCN 8444) GRB 081006A 2008/10/06 14:29:34 09:30:00 -67:24:00 Carina Fermi detected this 7 second long burst. Its spectrum was best fit by a Band function with alpha = -0.77 +/- 0.24, beta = -1.80 +/- 0.22 and Epeak = 1135 +/- 826 keV. GRB 081006B 2008/10/06 20:55:35 09:40:00 -57:30:00 Carina This Fermi GBM burst had a duration of 9 seconds. Its spectrum was best-fit by a power law of index -1.30+/-0.09. GRB 081003C 2008/10/03 15:27:17 18:00:00 20:54:00 Hercules This 30 second duration burst had several peaks. The spectrum was fit with a power law of index -1.41 +/- 0.06. GRB 081001 2008/10/01 21:17:42 18:26:21.78 -08:43:08.5 Scutum The duration of this SuperAGILE detected burst was 40 seconds. It had a two-peak structure, with an initial 10 second peak, followed by an additional one after a 20 second delay. Swift began XRT observations of the field 15.5 ks after the trigger. It found a fading source inside the SuperAGILE error circle (GCN 8307). The Swift UVOT also observed the field beginning 14.5 ks after the trigger. No optical counterpart was seen to v = 19.84 (GCN 8308). GRB 080927 2008/09/27 11:30:32 03:51:00 30:00:00 Taurus This GRB was single-peaked with a duration of approximately 25 seconds. The spectrum is fit with a power law of index -1.5 +/- 0.1, or by a Band model with Epeak = 40 +/- 10 keV and beta = -1.7 +/- 0.1, but alpha is poorly constrained. GRB 080925 2008/09/25 18:35:55 06:24:00 18:12:00 Gemini This multipeaked burst had a duration of 29 seconds. The spectrum is best fit by a band spectrum with E_peak 120 +/- 5 keV, alpha = -0.53 +/- 0.05 and beta = -2.26 +/- 0.08. GRB 080916C 2008/09/16 00:12:45 07:59:23.29 -56:38:16.4 Carina The Fermi GBM detected this burst. It had a duration of 66 seconds and a four-peaked structure. This burst was also the first one to be detected by the LAT, which captured more than 10 photons with energy above 1 GeV (GCN 8246). This detection makes this the only burst to ever be seen at such high energies. GRB 080912 2008/09/12 08:38:55 01:44:00 -05:06:00 Cetus This burst had a single peak with a duration of 17 seconds. The spectrum in the 50 - 300 keV band is well fit by a power law with index -1.74+/-0.07. GRB 080906B 2008/09/06 05:05:11 12:22:00 -08:36:00 Virgo This burst was detected by the GBM aboard the Fermi Gamma-ray Space Telescope. The duration was 5 seconds in the 50-300 keV bandpass. The spectrum was best fit by a band function with alpha = -0.07 +/- 0.09 beta = -2.10 +/- 0.07 Epeak = 125.3 +/- 6.6 keV GRB 080905C 2008/09/05 13:41:29 06:28:00 -69:48:00 Dorado The GBM aboard Fermi detected this burst. It had a duration of 28 seconds, with most of the energy being emitted in the first 11 seconds. The power law fit to the spectrum has an index of -0.9+/-0.17 and a cutoff at 78.8 keV. GRB 080904 2008/09/04 01:52:43 14:20:00 -32:18:00 Centaurus The Fermi GBM detected this burst, which had a duration of 22 seconds and a single peak. The is best fit by a band function with alpha= 0.0 +/- 0.17 beta = -2.70 +/- 0.08 Epeak = 35 +/- 1 keV GRB 080830 2008/08/30 08:50:16 10:33:00 33:36:00 Leo Minor The Fermi GBM detected this burst. It had four pulses totaling 45 seconds.The spectral index for the power law spectrum was -0.88 +/- 0.12, and the high energy cutoff was at 154 +/- 57 keV. No optical counterpart was reported. GRB 080825B 2008/08/25 17:46:40 13:57:07.42 -68:56:34 Circinus SuperAGILE localized this burst. It had a duration of ~50 seconds and a multipeaked structure. A possible optical counterpart was reported by observers using the Danish 1.54 m telescope on La Silla (GCN 8135). The object had a magnitude I = 17.4 +/- 0.2. In further observations, these same observers confirmed that the object was fading, and from it SED in UBVRI estimate a lower limit of z>3 for its redshift (GCN 8137). Observations made with the XRT aboard Swift also confirmed the reality of the source, and its fading (GCN 8140). GRB 080825C 2008/08/25 14:13:48 15:29:00 -04:54:00 Libra The Fermi GBM (formerly GLAST GBM) detected this burst. It had a duration of 22 seconds and a spectral index (8 - 910 keV) of -0.39+/-0.04 and a cutoff energy of 155+/- 5 keV. No optical counterpart has been reported. GRB 080824 2008/08/24 21:48:54 08:01:00 -03:10:00 Monoceros The Fermi GBM detected this burst, which had a duration of 28 seconds and a single peak. The spectral index for the burst (50 - 300 keV) was -0.4 +/- 0.2. The cutoff energy was 100 +/- 16 keV. No optical counterpart was reported. GRB 080823 2008/08/23 08:42:13 06:07:00 -40:36:00 Columba The Fermi GBM triggered on this burst. It had a duration of 46 seconds, with an initial small pulse followed by a larger main pulse. The spectral index had a power law index -1.2 +/- 0.2 and high energy cutoff at 164.7 +/- 34.2 keV. GRB 080818A 2008/08/18 13:54:24 03:41:00 -05:00:00 Eridanus This GRB had a duration of about 50 seconds. It was double peaked and well-fit by a power law of index -1.57+/- in the energy range from 10 keV to 300 keV. No optical counterpart was seen, as the burst alert was not sent out automatically, which caused a substantial delay in the notification. GRB 080818B 2008/08/18 22:40:49 06:32:00 07:24:00 Monoceros This GBM-detected burst was 10 seconds long. It had a single peak and a power law index of -1.3+/-0.1. The spectral cutoff occurred at 80+/-11 keV. No optical counterpart was found since the alert was not sent out promptly. GRB 080817A 2008/08/17 03:52:10 10:05:00 -19:15:00 Hydra This is the second GRB reported from the GLAST Burst Monitor. It had a duration of ~70 seconds and a double-peak structure in the main burst, with a weaker peak at T+50 seconds. Since these bursts were processed manually, no prompt alert was made, so no followup optical observations were done. GRB 080817B 2008/08/17 17:17:07 04:51:00 -11:48:00 Eridanus This was the third burst detected by the GLAST Burst Monitor. It had a duration of 6 seconds and three peaks. No followup optical observations were made, as all the initial GBM bursts were handled manually, without prompt reporting in place. GRB 080816A 2008/08/16 12:03:19 10:28:00 +54:36:00 Ursa Major This is the first reported GRB from GLAST. It had a duration of 70 seconds and a 4 peak structure. The spectrum from 10 keV to 500 keV is a power-law of index -0.57+/-0.14. The high energy cutoff occurs at 146.7+/-14.5 keV. Since these first bursts were not yet being sent out automatically, there was a large time delay between the burst and its reporting. As a result, there are no optical followups data. GRB 080816B 2008/08/16 23:44:01 19:14:00 -06:30:00 Aquila This burst had a duration of 5 seconds. It was double-peaked, with a spectral index -0.37+/-0.17 in the range 6 keV to 3500 keV. The cutoff in the spectrum occurs at 1230 +/- 230 keV. No optical counterpart was obtained in these first GLAST alerts because they were processed by hand. Thus, no prompt notifications were sent out. GRB 080812 2008/08/12 21:19:33 11:37:00 -41:18:00 Centaurus This GLAST GBM detected burst was 15 seconds long. It was multipeaked and had a power-law spectrum with index 0.17+/-0.27 with cutoff at 140+/-14 keV. No optical counterpart was found, as the burst notification was not sent out until after quite a long delay for these first GLAST bursts. Description

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