//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28594 SUBJECT: Swift detection of a new SGR 1830-0645 or a short GRB 201010A DATE: 20/10/10 15:16:16 GMT FROM: Scott Barthelmy at NASA/GSFC K. L. Page (U Leicester), S. D. Barthelmy (GSFC), N. J. Klingler (PSU), N. P. M. Kuin (UCL-MSSL) and A. Y. Lien (GSFC/UMBC) report on behalf of the Neil Gehrels Swift Observatory Team: At 14:49:24 UT, the Swift Burst Alert Telescope (BAT) triggered and located SGR 1830-0645 or GRB 201010A (trigger=999571). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 277.675, -6.758, which is RA(J2000) = 18h 30m 42s Dec(J2000) = -06d 45' 30" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single peak structure with a duration of no more than 0.128 sec. The peak count rate was ~1600 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 14:50:30.9 UT, 67.0 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 277.6702, -6.7550 which is equivalent to: RA(J2000) = 18h 30m 40.85s Dec(J2000) = -06d 45' 18.0" with an uncertainty of 2.2 arcseconds (radius, 90% containment). This location is 20 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 1.11 x 10^22 cm^-2 (Willingale et al. 2013). UVOT took a finding chart exposure of 150 seconds with the White filter starting 71 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the sub-image. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the region. No correction has been made for the large, but uncertain, extinction expected. Due to its short duration (BAT trigger duration of 8 ms, although the immediately available lightcurve is only available at 128 ms resolution), the soft spectrum (not visible above 50 keV) and its location in the Galactic bulge near the plane (lon,lat) = (24.5, 1.5) we suspect that this event may be a new Soft Gamma Repeater, which we would name SGR 1830-0645. Burst Advocate for this burst is K. L. Page (klp5 AT leicester.ac.uk). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28597 SUBJECT: SGR 1830-0645 / GRB 201010A: Kitab optical non-detection DATE: 20/10/11 12:42:25 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), A. Pozanenko (IKI), A. Zhornichenko (KIAM), N. Pankov (HSE), A. Novichonok (Petrozavodsk State University, KIAM), Sh. Ehgamberdiev (UBAI) report on behalf of IKI-GRB-FuN: We observed the field of new SGR 1830-0645 (Page et al., GCN 28594; Gogus et al., ATEL 14085) originally detected by Swift (trigger=999571) and also named as GRB 201010A with Kitab-ISON RC-36 telescope in R-filter. Observation started on Oct. 10 (UT) 15:21:08, i.e. 31.7 minutes after trigger. The field is extremely crowded. Within enhanced XRT position (Osborne et al., GCN 28596) we found a source which is also presented in the DSS2 (R) image but not listed in USNO-B1.0. In our images we cannot discriminate the sources. We performed aperture photometry which include this source and nearby Northern source listed in USNO-B1.0 0832-0432584 (R2=13.54) in two stacked images. The image A is at midpoint 0.02343 days and the image (B) is at midpoint 0.03835 days after trigger. By comparison of the two photometric results (A) R=14.16 +/- 0.06 and (B) R=14.20 +/- 0.07 we do not observe any variability and hence we do not detect optical activity of SGR 1830-0645. Formal photometry of the field in both epochs (A,B) is following Date, UT start, t-T0, Exp., Filter, OT, Err., UL (mid, days) (A)2020-10-10 15:21:08 0.02343 240 R n/d n/d 17.0 (B)2020-10-10 15:21:08 0.03835 2480 R n/d n/d 18.0 The photometry is based on nearby USNO-B1.0 star, R2 magnitude USNO_B10_id R2 0832-0432530 15.34 0832-0433055 13.04 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28599 SUBJECT: SGR 1830-0645: Swift-BAT refined analysis DATE: 20/10/11 17:36:47 GMT FROM: Amy Lien at GSFC H. A. Krimm (NSF), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from the recent telemetry downlink, we report further analysis of SGR 1830-0645 (trigger #999571) (Page et al., GCN Circ. 28594). The BAT ground-calculated position is RA, Dec = 277.697, -6.761 deg which is RA(J2000) = 18h 30m 47.3s Dec(J2000) = -06d 45' 40.0" with an uncertainty of 2.9 arcmin, (radius, sys+stat, 90% containment). The partial coding was 89%. The mask-weighted light curve shows a single-pulse structure that starts at ~T0, peaks at ~T+0.005 s, and ends at ~T+0.008 s. There may be another short pulse (~ 10 ms) at ~ T-2.76 s, which has an image significance of ~ 5.1 sigma in 15-25 keV. T90 (15-350 keV) is ~0.008 sec (due to the extremely short duration, standard bayesian block analysis does not produce a meaningful uncertainty). The time-averaged spectrum from T+0.00 to T+0.008 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.22 +- 0.47. The fluence in the 15-150 keV band is 7.8 +- 2.5 x 10^-9 erg/cm2. The 1-sec peak photon flux measured from T+0.00 sec in the 15-150 keV band is 17.2 +- 4.8 ph/cm2/sec. A single blackbody fit to the time-averaged spectrum shows the blackbody temperature of 9.3 +- 2.1 keV (chi squared 28.52 for 57 d.o.f.). All the quoted errors are at the 90% confidence level. The spectral and temporal properties are more consistent with an SGR, instead of a short GRB. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/999571/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28601 SUBJECT: SGR 1830-0645 / GRB 201010A: 1.5m OSN optical upper limit DATE: 20/10/11 19:35:27 GMT FROM: Youdong HU at IAA-CSIC Y.-D. Hu, A. Sota, A. J. Castro-Tirado, E. Fernandez-Garcia (IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de Malaga) on behalf of a larger collaboration, report: Following the detection of SGR 1830-0645/GRB201010A by Swift (Page et al. GCNC 28594), optical images in the I-band were obtained at the 1.5m OSN telescope in Granada (Spain) starting at 20:35 (Oct 10), i.e. ~5.8 h postburst. No optical afterglow is detected in the image within the enhanced Swift/XRT error box (Osborne et al. GCNC 28596) down to I=20.1, which is in agreement with the non-detections reported by Lipunov et al. (GCNC 28595) and Belkin et al. (GCNC 28597). We thank the staff at OSN for their excellent support. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28603 SUBJECT: SGR 1830-0645: pre-discovery detection in Swift/BAT DATE: 20/10/11 22:39:41 GMT FROM: Aaron Tohuvavohu at U Toronto SGR 1830-0645 was discovered by Swift/BAT trigger #999571 on 2020-10-10T14:29:24 UTC (GCN 28594, ATEL 14083). The hypothesis of magnetar origin was strengthened by measurement of a spin-period in the Swift/XRT data (Gogus et al. ATEL 14085). We performed a sub-threshold search in the Swift/BAT data, and find that BAT detected a soft (<50 keV), short (~20 ms), flare from this source at 2020-10-05T18:20:35.566 UTC, 5 days before the discovery trigger. The origin of this flare is confirmed to come from SGR 1830-0645 from time-tagged event data recorded by Swift/BAT. This TTE data was saved by BAT triggering on this flare in the rates domain in real-time, with failed trigger #998860. This was not promoted to a successful trigger as BAT failed to find a source location in the associated image produced on-board. This was due to a suboptimal foreground interval selection by the real time analyses. The close proximity to the SAA, and elevated background, likely also contributed. We cleaned the TTE data of hot/noisy detectors. We detect the flare from SGR 1830-0645 with a rates significance of >10 sigma, and confirm the source location in the image domain at >7 sigma. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28606 SUBJECT: GRB 201011A: Fermi GBM detection of a likely Long GRB in the direction of SGR 1830-0645 DATE: 20/10/12 21:10:54 GMT FROM: Oliver J Roberts at USRA/NASA O.J. Roberts (USRA) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 15:06:24.66 UT on 11 October 2020, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 201011A (trigger 624121589 / 201011629), which was also detected by the AGILE (Ursi et al. 2020, GCN 28605). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 281.1, Dec = -5.7 (J2000 degrees, equivalent to J2000 18h 44m , -05d 43'), with a statistical uncertainty of 2.4 degrees. The angle from the Fermi LAT boresight at the GBM trigger time is 35 degrees. The GBM light curve consists of multiple pulses with a duration (T90) of about 126.2 s (50-300 keV). The time-averaged spectrum from T0-1.8 s to T0+124.2 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.18 (+0.09/-0.08) and the cutoff energy, parameterized as Epeak, is 138.0 (+19.6/-14.4) keV. The event fluence (10-1000 keV) in this time interval is (9.25 +/- 0.52)E-06 erg/cm^2. The 1s peak photon flux measured starting from T0+5.44 s in the 10-1000 keV band is 5.8 +/- 0.3 ph/s/cm^2. We note that this event is in the direction of SGR 1830-0645 (K.L. Page et al. 2020, GCN 28594). While we cannot conclusively rule out an association with SGR 1830-0645, the GBM spectrum and time history are suggestive of a long GRB and not a Magnetar transient. Analysis is ongoing to confirm the source. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog: https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/" //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28610 SUBJECT: SGR 1830-0645: Swift/UVOT Upper Limits DATE: 20/10/13 14:20:18 GMT FROM: Paul Kuin at MSSL Paul Kuin (UCL-MSSL) and Kim Page (U.Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of SGR 1830-0645/ GRB 201010 71 s after the BAT trigger (Page et al., GCN Circ. 28594). This field is crowded with sources. Near the XRT position (Osborne et al. GCN Circ. 28596) we find two sources which were both observed not to vary within our measuring accuracy of 0.07 mag. Hence, no optical afterglow consistent with the XRT position is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 71 221 147 >17.6 u_FC 284 534 246 >18.1 white 71 757 186 >17.6 v 614 5462 216 >16.4 b 540 733 39 >17.6 u 284 6049 434 >18.0 w1 664 5872 216 >18.6 m2 639 5667 216 >19.7 w2 590 5257 216 >19.3 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 1.78 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28838 SUBJECT: Swift Trigger 1004219: Detection of SGR 1830-0645 DATE: 20/11/05 02:40:36 GMT FROM: David Palmer at LANL J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), M. J. Moss (GWU), D. M. Palmer (LANL) and B. Sbarufatti (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 02:22:03 UT, the Swift Burst Alert Telescope (BAT) triggered and located SGR 1830-0645 (trigger=1004219). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 277.679, -6.754 which is RA(J2000) = 18h 30m 43s Dec(J2000) = -06d 45' 13" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of <~ 0.1 sec. The peak count rate was ~5000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 02:23:38.0 UT, 94.8 seconds after the BAT trigger. Using promptly downlinked data we find a X-ray source with an enhanced position: RA, Dec 277.6736, -6.7550 which is equivalent to: RA(J2000) = 18h 30m 41.67s Dec(J2000) = -06d 45' 17.9" with an uncertainty of 2.3 arcseconds (radius, 90% containment). This location is 19 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. We cannot determine whether the source is fading at the present time. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (1.11 x 10^22 cm^-2, Willingale et al. 2013), with an excess column of 2 (+2.39/-1.60) x 10^22 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 97 seconds after the BAT trigger. No credible counterpart has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any counterpart in the sub-image. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any counterpart in the region. No correction has been made for the large, but uncertain, extinction expected. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28879 SUBJECT: Swift Trigger 1005428: Detection of SGR 1830-0645 DATE: 20/11/11 10:04:46 GMT FROM: Kim Page at U.of Leicester J.D. Gropp (PSU), N. J. Klingler (PSU), N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC) and K. L. Page (U Leicester) report on behalf of the Neil Gehrels Swift Observatory Team: At 09:45:06 UT, the Swift Burst Alert Telescope (BAT) triggered and located SGR 1830-0645 (trigger=1005428). Swift slewed immediately to the source. The BAT on-board calculated location is RA, Dec 277.701, -6.741 which is RA(J2000) = 18h 30m 48s Dec(J2000) = -06d 44' 27" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a very short duration. The peak count rate was ~6480 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 09:45:57.7 UT, 51.5 seconds after the BAT trigger. Using promptly downlinked data we find an X-ray source with an enhanced position: RA, Dec 277.6736, -6.7548 which is equivalent to: RA(J2000) = 18h 30m 41.66s Dec(J2000) = -06d 45' 17.2" with an uncertainty of 2.1 arcseconds (radius, 90% containment). This location is 109 arcseconds from the BAT onboard position, within the BAT error circle, and consistent with the known location of SGR 1830-0645. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (1.11 x 10^22 cm^-2, Willingale et al. 2013), with an excess column of 1.1 (+0.80/-0.68) x 10^22 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 55 seconds after the BAT trigger. No credible counterpart has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any counterpar in the sub-image. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any counterpart in the region. Swift first triggered on SGR 1830-0645 on 2020 October 10 (GCN Circ. 28594), although a sub-threshold flare was also detected on October 05 (GCN 28603). The source again triggered Swift-BAT on November 05 (GCN Circ. 28838). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29500 SUBJECT: Swift Trigger 1032350: Detection of SGR 1830-0645 DATE: 21/02/13 00:39:23 GMT FROM: David Palmer at LANL J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL), D. M. Palmer (LANL) and B. Sbarufatti (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 00:10:13 UT, the Swift Burst Alert Telescope (BAT) triggered and located a burst form the soft gamma repeater SGR 1830-0645 (trigger=1032350). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 277.660, -6.748 which is RA(J2000) = 18h 30m 38s Dec(J2000) = -06d 44' 52" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single short peak in one 0.128 s timebin. The peak count rate was ~8000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 00:11:14.4 UT, 60.6 seconds after the BAT trigger. Using promptly downlinked data we find an X-ray source with an enhanced position: RA, Dec 277.6734, -6.7541 which is equivalent to: RA(J2000) = 18h 30m 41.61s Dec(J2000) = -06d 45' 14.9" with an uncertainty of 2.2 arcseconds (radius, 90% containment). This location is 52 arcseconds from the BAT onboard position, within the BAT error circle, and consistent with the known location of SGR 1830-0645. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (1.11 x 10^22 cm^-2, Willingale et al. 2013), with an excess column of 8.1 (+9.28/-7.67) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 63 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of the BAT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the sub-image. The 8'x8' region for the list of sources generated on-board covers 100% of the BAT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the region. No correction has been made for the large, but uncertain, extinction expected. BAT's most recent detection of this SGR was on 2020-11-22, following its discovery by Swift on 2020-11-10 (Page et al., GCN Circ. 28594). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29516 SUBJECT: Swift Trigger 1033144: Detection of SGR 1830-0645 DATE: 21/02/17 08:28:25 GMT FROM: Kim Page at U.of Leicester N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC) and K. L. Page (U Leicester) report on behalf of the Neil Gehrels Swift Observatory Team: At 08:11:21 UT, the Swift Burst Alert Telescope (BAT) triggered and located the soft gamma repeater SGR 1830-0645 (trigger=1033144). Swift slewed immediately to the source. The BAT on-board calculated location is RA, Dec 277.646, -6.735 which is RA(J2000) = 18h 30m 35s Dec(J2000) = -06d 44' 05" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 0.1 sec. The peak count rate was ~10000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 08:12:33.2 UT, 71.9 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 277.67287, -6.75438 which is equivalent to: RA(J2000) = 18h 30m 41.49s Dec(J2000) = -06d 45' 15.8" with an uncertainty of 4.2 arcseconds (radius, 90% containment). This location is 118 arcseconds from the BAT onboard position, within the BAT error circle, and consistent with the known location of SGR 1830-0645. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (1.11 x 10^22 cm^-2, Willingale et al. 2013), with an excess column of 2.7 (+4.47/-2.40) x 10^22 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 76 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers none of the XRT error circle. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the region. No correction has been made for the large, but uncertain, extinction expected. BAT most recently triggered on SGR 1830-0645 on 2021 Feb 13 (GCN 29500). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29524 SUBJECT: Fermi/GBM observation of a burst from SGR 1830-0645 DATE: 21/02/18 02:21:02 GMT FROM: Cori Fletcher at USRA C. Fletcher (USRA) reports on behalf of the Fermi GBM Team: "At 08:11:21.50 UT on 17 February 2021 the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located a burst from SGR 1830-0645 (trigger 635242286/ 210217341)). This SGR J1830 burst has also been reported by Swift-BAT (Klingler et al., GCN 29516). The GBM on-ground location is consistent with the known position of the SGR. The burst has a duration (T90) of about 0.1 seconds. It is adequately fit by a power law function with an exponential high-energy cutoff. The power law index is -0.7 +/- 0.9 and the cutoff energy, parameterized as Epeak, is 28.07 +/- 5.74 keV. The event fluence (10-300 keV) from T0-0.144s to T0+0.003s is (4.4 +/- 0.7)E-08 erg/cm^2. The average photon flux in the 10-300 keV band during this period is 7.6 +/- 0.9 ph/s/cm^2. The spectral analysis results presented above are preliminary. For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"