//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27078 SUBJECT: GRB 200215A: Fermi GBM Final Real-time Localization DATE: 20/02/15 14:49:48 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 14:39:31 UT on 15 Feb 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200215A (trigger 603470376.849696 / 200215611). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 30.5, Dec = 10.0 (J2000 degrees, equivalent to J2000 02h 01m, 10d 00'), with a statistical uncertainty of 4.5 degrees. The angle from the Fermi LAT boresight is 84.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200215611/quicklook/glg_skymap_all_bn200215611.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200215611/quicklook/glg_healpix_all_bn200215611.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200215611/quicklook/glg_lc_medres34_bn200215611.gif //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27079 SUBJECT: GRB 200215A: Swift detection of a burst DATE: 20/02/15 15:14:13 GMT FROM: Kim Page at U.of Leicester M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB), J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU), H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL), S. Laha (GSFC/UMBC/CRESST), A. Melandri (INAF-OAB), K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sbarrato (INAF-OAB) and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 14:39:31 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 200215A (trigger=956639). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 34.122, +12.781 which is RA(J2000) = 02h 16m 29s Dec(J2000) = +12d 46' 50" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve up to T+8s showed a single-peaked structure with a duration of about 20 sec. (The light curve after T+8s is not immediately available.) The peak count rate was ~4000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 14:40:59.0 UT, 87.1 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source with an enhanced position: RA, Dec 34.0794, 12.7704 which is equivalent to: RA(J2000) = 02h 16m 19.05s Dec(J2000) = +12d 46' 13.6" with an uncertainty of 2.1 arcseconds (radius, 90% containment). This location is 154 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 in excess of the Galactic value (1.21 x 10^21 cm^-2, Willingale et al. 2013), with an excess column of 4.2 (+3.73/-3.12) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 90 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. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.15. Burst Advocate for this burst is M. G. Bernardini (grazia.bernardini AT brera.inaf.it). 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: 27080 SUBJECT: Swift GRB200215.61: Global MASTER-Net observations report DATE: 20/02/15 15:16:16 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D.Kuvshinov, D. Cheryasov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov, A. Gabovich, Yu. Sergienko (Blagoveschensk Educational State University) MASTER-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the Swift GRB200215.61 (trigger No 956639,02h 16m 29.28s , +12d 46m 51.6s, R=0.05) errorbox 20 sec after notice time and 40 sec after trigger time at 2020-02-15 14:40:12 UT, with upper limit up to 18.5 mag. The observations began at zenith distance = 70 deg. The sun altitude is -39.9 deg. The galactic latitude b = -45 deg., longitude l = 154 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=1288551 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 46 | MASTER-Tunka | P| | 10 | 15.3 | 75 | MASTER-Tunka | P| | 10 | 15.2 | 110 | MASTER-Tunka | P| | 20 | 15.5 | 160 | MASTER-Tunka | P| | 30 | 16.1 | 215 | MASTER-Tunka | P| | 40 | 16.0 | 279 | MASTER-Tunka | P| | 50 | 16.4 | 354 | MASTER-Tunka | P| | 60 | 16.6 | 443 | MASTER-Tunka | P| | 80 | 16.7 | 553 | MASTER-Tunka | P| | 100 | 16.7 | 682 | MASTER-Tunka | P| | 120 | 16.8 | 837 | MASTER-Tunka | P| | 150 | 16.9 | 1021 | MASTER-Tunka | P| | 180 | 17.1 | 1221 | MASTER-Tunka | P| | 180 | 17.0 | 1420 | MASTER-Tunka | P| | 180 | 16.9 | 1761 | MASTER-Tunka | C | 180 | 18.5 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27081 SUBJECT: GRB 200215A: Nanshan/NEXT optical upper limit DATE: 20/02/15 16:08:10 GMT FROM: Dong Xu at NAOC/CAS D. Xu, Z.P. Zhu, X. Liu, B.Y. Yu, Y. Ma (NAOC), X. Gao (Urumqi No.1 Senior High School) report: We observed the field of GRB 200215A (Bernardini et al., GCN 27079) using the NEXT 0.6m optical telescope located at Nanshan, Xinjiang, China. Observations automatically started at 14:40:59 UT on 2002-02-15, i.e., 88 s after the BAT trigger. We obtained 3x40 s, 4x60 s, and 5x90 s frames in the Sloan r-filter. Observations then ended due to follow-ups of LIGO/Virgo S200213t. No optical afterglow is detected in our images at the XRT position (Bernardini et al., GCN 27079) down to a limiting magnitude of r~18.0, calibrated with the nearby PanSTARRS field. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27083 SUBJECT: GRB 200215A Possible host galaxy in PanSTARRS DATE: 20/02/15 18:13:07 GMT FROM: Alexander Kann at IAA-CSIC D. A. Kann (HETH/IAA-CSIC), and A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI) report: In PanSTARRS imaging of the field of GRB 200215A (Bernardini et al., GCN 27079), we find a bright, extended object (1".5 x 1".7) at the edge of the enhanced XRT error circle given in Bernanrdini et al. According to the PanSTARRS catalog, the source lies at: RA = 02:16:19.065 (J2000) Dec. = +12:46:09.67 (J2000) The Kron magnitudes in the catalog are given as: g_PS = 21.73 +/- 0.06, r_PS = 20.90 +/- 0.07, i_PS = 20.26 +/- 0.06, z_PS = 19.89 +/- 0.05, y_PS = 19.58 +/- 0.10 We suggest this galaxy may be the host galaxy of GRB 200215A, implying a low redshift. There is another clear extended galaxy to the east of this source, the relationship between the two is unclear at this time. Spectroscopy of these galaxies is encouraged. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27086 SUBJECT: GRB 200215A: Liverpool Telescope upper limits DATE: 20/02/15 20:37:20 GMT FROM: Daniel Perley at Liverpool JMU D. A. Perley and A. M. Cockeram (LJMU) report: We observed the field of GRB 200215A (Bernardini et al., GCN 27079) with the IO:O imager on the 2m robotic Liverpool Telescope between 19:56 and 20:14 UT on 2019-02-15. We acquired 3x150s exposures in each of the i and z filters. No counterpart is detected within the XRT error circle in either filter. Calibrating relative to nearby standards from the Pan-STARRS 1 catalog, we place upper limits (3-sigma) of: i > 22.90 (t = 0.2204 days) z > 21.95 (t = 0.2264 days) DisclaimerNone //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27087 SUBJECT: GRB 200215A: Fermi GBM detection DATE: 20/02/15 22:21:54 GMT FROM: Suraj Poolakkil at UAH S.Poolakkil (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 14:39:31.85 UT on 15 February 2020, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 200215A (trigger 603470376 / 200215611), which was also detected by the Swift/BAT (Bernardini et al. 2020, GCN 27079). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 86 degrees. The GBM light curve consists of a single bright pulse followed by some extended emission with a duration (T90) of about 24 s (50-300 keV). The time-averaged spectrum from T0-4.09 s to T0+5.12 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.76 +/- 0.16 and the cutoff energy, parameterized as Epeak, is 162 +/- 25 keV. The event fluence (10-1000 keV) in this time interval is (1.858 +/- 0.175)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.06 s in the 10-1000 keV band is 3.7 +/- 0.3 ph/s/cm^2. 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: 27088 SUBJECT: GRB 200215A: Optical observations form Calar Alto 2.2m DATE: 20/02/15 23:21:56 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D. A. Kann, M. Blazek, F. Agui Fernandez, C. Thoene (all HETH/IAA-CSIC), I. Hermelo, B. Arroyo (both CAHA), Y. Ascasibar, A. Gutierrez Adame, A. Cayrol Bernardo, A. Rodriguez Ortega, A. Rayo Mato, M. Rocamora Bernal, M. A. Diaz Teodori, P. Nuñez Yebra, S. Ortega Martinez, G Meeus, D. Barba Gonzalez, L Brenes Gil, J. Ferrer Ereza, H. Garcia Escudero, S. Jaraba Gómez, D. Lopez Cano, P. Sanchez Alarcon, P Santamarina Guerrero, A. Romar Tejeiro (UAM) report: We observed the field of GRB 200215A (Bernardini et al., GCN 27079) with CAFOS on the 2.2m telescope at Calar Alto Observatory, in Almeria (Spain). Our observation started at 19:15 UT (4.591 hr after the burst) and consisted of 5x720 s in Rc band. We detect no optical counterpart within the XRT error circle down to a 3-sigma limit of 24.0 mag. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27089 SUBJECT: GRB 200215A: Enhanced Swift-XRT position DATE: 20/02/16 00:34:14 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 3846 s of XRT Photon Counting mode data and 3 UVOT images for GRB 200215A, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 34.07940, +12.77079 which is equivalent to: RA (J2000): 02h 16m 19.06s Dec (J2000): +12d 46' 14.9" with an uncertainty of 1.5 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27090 SUBJECT: GRB 200215A: Swift/UVOT Upper Limits DATE: 20/02/16 01:29:30 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (UCL-MSSL) and M. G. Bernardini (INAF-OAB) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 200215A 90 s after the BAT trigger (Bernardini et al., GCN Circ. 27079). No optical afterglow consistent with the XRT position (Evans et al. GCN Circ. 27089) 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 90 240 147 >20.0 u_FC 302 552 246 >20.0 white 90 7290 581 >21.2 v 634 5070 294 >18.5 b 559 7092 294 >19.8 u 302 6885 481 >20.3 w1 1087 6680 216 >19.2 w2 10534 11091 547 >19.8 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.15 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27091 SUBJECT: GRB 200215A: Swift-XRT refined Analysis DATE: 20/02/16 02:00:45 GMT FROM: Phil Evans at U of Leicester M. Perri (ASDC), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester) and M.G. Bernardini report on behalf of the Swift-XRT team: We have analysed 7.4 ks of XRT data for GRB 200215A (Bernardini et al. GCN Circ. 27079), from 72 s to 35.0 ks after the BAT trigger. The data comprise 24 s in Windowed Timing (WT) mode (the first 9 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN Circ. 27089). The light curve can be modelled with a power-law decay with a decay index of alpha=0.93 (+/-0.04). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.47 (+0.18, -0.17). The best-fitting absorption column is 1.7 (+0.8, -0.5) x 10^21 cm^-2, consistent with the Galactic value of 1.2 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.9 x 10^-11 (5.5 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.7 (+0.8, -0.5) x 10^21 cm^-2 Galactic foreground: 1.2 x 10^21 cm^-2 Excess significance: <1.6 sigma Photon index: 1.47 (+0.18, -0.17) If the light curve continues to decay with a power-law decay index of 0.93, the count rate at T+24 hours will be 7.5 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.6 x 10^-13 (4.1 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00956639. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27098 SUBJECT: GRB 200215A: Swift-BAT refined analysis DATE: 20/02/16 11:49:41 GMT FROM: Hans Krimm at NSF/NASA-GSFC S. D. Barthelmy (GSFC), M. G. Bernardini (INAF-OAB), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), 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-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 200215A (trigger #956639) (Bernardini, et al., GCN Circ. 27079). The BAT ground-calculated position is RA, Dec = 34.100, 12.775 deg which is RA(J2000) = 02h 16m 24.1s Dec(J2000) = +12d 46' 31.7" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 73%. The mask-weighted light curve shows a single symmetrical peak from roughly -10 sec to +6 sec, peaking at T+0 sec. T90 (15-350 keV) is 11.7 +- 2.2 sec (estimated error including systematics). The time-averaged spectrum from T-9.97 to T+5.37 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.41 +- 0.09. The fluence in the 15-150 keV band is 1.1 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-0.16 sec in the 15-150 keV band is 2.7 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/956639/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27099 SUBJECT: GRB 200215A: UKIRT H-band observations DATE: 20/02/16 11:58:15 GMT FROM: Dong Xu at NAOC/CAS D. Xu, Z.P. Zhu, X. Liu, H.J. Wang, L. Ge (NAOC) report: We observed the field of GRB 200215A (Bernardini et al., GCN 27079) using the United Kingdom Infra-Red Telescope (UKIRT). Observations started at 05:02:05 UT on 2020-02-16 (i.e., 14.38 hr after the BAT trigger), and 3600 s H-band imagining was obtained. No afterglow is detected within the Enhanced XRT error circle (Evans et al., GCN 27089) in our stacked image down to a limiting magnitude of H~20.0. From the PanSTARRS archive, there exists an extended object outside and south to the Enhanced XRT error circle by ~5.1 arcsec, as reported in Kann & de Ugarte Postigo (GCN 27083). It's thus dubbed PS021619+124609 here. As the GRB field is in the previous UKIRT H-band survey, we performed photometry of PS021619+124609 in both epochs. Any significant brightening for PS021619+124609 is ruled out, and we're inclined to think it is not related to the GRB. We thank the great support of the UKIRT staff, in particular Michael Pohlen. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27105 SUBJECT: GRB 200215A: RATIR Optical Observations DATE: 20/02/16 16:57:12 GMT FROM: Alan M Watson at UNAM Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (U. Wash.), and Vicki Toy (UMD) report: We observed the field of GRB 200215A (Bernardini et al., GCN Circ. 27079) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir from 2020/02 16.11 to 2020/02 16.23 UTC (11.91 to 14.78 hours after the BAT trigger), obtaining a total of 1.79 hours exposure in the r and i bands. For a source within the enhanced Swift-XRT error circle (Evans et al., GCN Circ. 27089), in comparison with the SDSS DR9 catalog, we obtain the following 3-sigma upper limits: r > 22.01 i > 23.15 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27113 SUBJECT: GRB 200215A: CALET Gamma-Ray Burst Monitor detection DATE: 20/02/17 09:01:26 GMT FROM: Valentin Pal'shin at AGU T. Sakamoto, A. Yoshida, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), Y. Asaoka, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 200215A (Swift detection: Bernardini et al., GCN Circ. 27079, Barthelmy et al., GCN Circ. 27098; Fermi GBM detection: Poolakkil and Meegan, GCN Circ. 27087) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 14:39:28.087 UTC on 15 February 2020. The burst signal was seen by all CGBM detectors. The burst light curve shows a multi-peaked structure which starts at T+0.1 sec, peaks at T+4.0 sec and ends at T+8.3 sec. The T90 and T50 durations measured by the SGM data are 7.1 +- 1.6 sec and 2.2 +- 1.5 sec (40-1000 keV), respectively. The ground processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1265812510/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27150 SUBJECT: GRB 200215A: LCO Optical Upper Limits DATE: 20/02/20 05:44:06 GMT FROM: Robert Strausbaugh at U. of the Virgin Islands R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (U. of the Virgin Islands/College of Marin) report on behalf of a larger collaboration: We observed Swift GRB 200215A (Bernardini et al., GCN 27079) with the LCO 1-m Sinistro instrument at the McDonald Observatory, Texas, USA site, on February 16, from 01:37 to 01:46 UT (corresponding to 10.97 to 11.12 hours from the GRB trigger time) with the Bessel I filter. We performed a series of 3x120s exposures. We do not detect any sources in the individual frames (nor in stacked images) in the Swift error region. Using the USNO-B.1 catalog as reference, we obtain the following 3-sigma upper limit: I > 18.8 R.S. is funded by NSF AST grant #1831682