//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27101 SUBJECT: GRB 200216B: Fermi GBM Final Real-time Localization DATE: 20/02/16 13:42:51 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 13:32:34 UT on 16 Feb 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200216B (trigger 603552759.75478 / 200216564). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 159.2, Dec = 21.0 (J2000 degrees, equivalent to J2000 10h 36m, 21d 00'), with a statistical uncertainty of 6.5 degrees. The angle from the Fermi LAT boresight is 78.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200216564/quicklook/glg_skymap_all_bn200216564.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/bn200216564/quicklook/glg_healpix_all_bn200216564.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200216564/quicklook/glg_lc_medres34_bn200216564.gif //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27102 SUBJECT: GRB 200216B: Swift detection of a burst DATE: 20/02/16 13:57:44 GMT FROM: Paolo D'Avanzo at INAF - OAB P. D'Avanzo (INAF-OAB), M. G. Bernardini (INAF-OAB), J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC), T. Sbarrato (INAF-OAB) and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift Observatory Team: At 13:32:33 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 200216B (trigger=956824). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 160.461, +19.454 which is RA(J2000) = 10h 41m 51s Dec(J2000) = +19d 27' 15" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed one long peak with a duration of about 30 sec, there is possible evidence for weaker emission out to T0+60 seconds. The peak count rate was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 13:34:29.0 UT, 115.1 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec 160.4343, 19.4757 which is equivalent to: RA(J2000) = 10h 41m 44.23s Dec(J2000) = +19d 28' 32.4" with an uncertainty of 2.0 arcseconds (radius, 90% containment). This location is 119 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 (2.03 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 9.9 (+3.22/-2.80) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 1.33e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 124 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. The typical 3-sigma upper limit has been about 19.6 mag. 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 0.02. Burst Advocate for this burst is P. D'Avanzo (paolo.davanzo AT 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: 27103 SUBJECT: GRB 200216B: GMG upper limit DATE: 20/02/16 14:36:13 GMT FROM: Jirong Mao at Yunnan Obs J. Mao, D.-Q. Wang, and J.-M. Bai (YNAO) report: We observed the field of GRB 200216B (D'Avanzo et al. GCN circ. 27102) with the 2.4-meter optical telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatories. The observation began at UT 13:46:56, 16th, Feb, 2020, about 14 min after the trigger. We did not detect any optical source in the Swift-XRT error circle. A preliminary measurement provided an upper limit of R~21.8. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27104 SUBJECT: GRB 200216B: Nanshan/NEXT early optical upper limit and possible host galaxy DATE: 20/02/16 15:09:41 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 200216B (D'Avanzo et al., GCN 27102) using the NEXT 0.6m optical telescope located at Nanshan, Xinjiang, China. Observations automatically started at 13:33:46 UT on 2002-02-16, i.e., 73 s after the BAT trigger. We obtained 3x40 s, 4x60 s, 3x90 s and onging 200 s frames in the Sloan r-filter. The altitude for the GRB and the weather has been improving. No optical afterglow is detected in our images at the XRT position (D'Avanzo et al., GCN 27102) down to a limiting magnitude of r~20.0. Meanwhile, we note that there exists a very marginally detected blob (thus noise fluctuation not ruled out yet), extended and being positionally consistent with the XRT position both in PanSTAR r-band field, centred at coordinates: R.A. (J2000) = 10:41:44.23, Dec. (J2000) = +19:28:33.18. The source would be of r~23 in depth, and might be the host galaxy of the GRB. Deep imaging would identify the nature of the blob. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27106 SUBJECT: GRB 200216B: Enhanced Swift-XRT position DATE: 20/02/16 19:50:33 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 1480 s of XRT Photon Counting mode data and 2 UVOT images for GRB 200216B, 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 = 160.43469, +19.47516 which is equivalent to: RA (J2000): 10h 41m 44.32s Dec (J2000): +19d 28' 30.6" with an uncertainty of 1.7 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: 27108 SUBJECT: GRB 200216B: Swift/UVOT Upper Limits DATE: 20/02/16 22:15:58 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (UCL-MSSL) and P. D'Avanzo (INAF-OAB) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 200216B 124 s after the BAT trigger (D'Avanzo et al., GCN Circ. 27102). No optical afterglow consistent with the XRT position (Goad et al. GCN Circ. 27106) 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 124 274 147 >21.0 white 124 1535 334 >21.5 w1 1095 1635 39 >20.2 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27109 SUBJECT: GRB 200216B: Fermi GBM observation DATE: 20/02/16 23:24:33 GMT FROM: Christian Malacaria at NASA-MSFC/USRA C. Malacaria (NASA-MSFC/USRA), B. Mailyan (UAH) and C. Meegan (UAH), report on behalf of the Fermi GBM Team: "At 13:32:34.75 UT on 16 February 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200216B (trigger 603552759 / 200216564), which also triggered the Swift/BAT (D'Avanzo et al. 2020, GCN 27102). The Fermi GBM Final Real-time Localization (GCN 27101) is consistent with the Swift position. The angle from the Fermi LAT boresight is 78 degrees. The GBM light curve consists of a single bright pulse followed by some extended emission with a duration (T90) of about 12.0 s (10-1000 keV). The time-averaged spectrum from T0-1.0 to T0+15.4 s is best fit by by a power law function with an exponential high-energy cutoff. The power law index is 0.07 +/- 0.30, and the cutoff energy, parameterized as Epeak, is 69.5 +/- 4.9 keV. The fluence (10-1000 keV) in this time interval is (1.141 +/- 0.074)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+2.3 s in the 10-1000 keV band is 1.95 +/- 0.2 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: 27110 SUBJECT: GRB 200216B: z-band limit from NOT DATE: 20/02/17 01:20:29 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Martikainen (NOT and U. Helsinki), D. Perley (LJMU), K.E. Heintz (U. Iceland), D. Xu (NAOC), A. Levan (Radboud U.) report on behalf of a larger collaboration: We observed the field of GRB 200216B (Fermi GBM team GCN 27101; D’Avanzo et al. GCN 27102) with the 2.5 m Nordic Optical Telescope equipped with AlFOSC. Observations consisted of 5x200s imaging in z-band, with mean epoch 17 Feb 2020 00:11:22 UT (10.647 hr after the burst). We do not detect any source within the refined XRT error box (Goad et al. GCN 27106) down to a 3-sigma limit of z > 23.3 mag. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27114 SUBJECT: GRB 200216B - possible IR counterpart from VLT DATE: 20/02/17 11:37:45 GMT FROM: Andrew Levan at U.of Leicester A. J. Levan (Radboud Univ), A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D. Xu (NAOC), D. A. Kann (HETH-IAA/CSIC), J. P. U. Fynbo (DAWN/NBI/DTU), K. E. Heinz (Univ. Iceland), N. R. Tanvir (Univ. Leicester), G. Pugliese (API, Univ. Amsterdam), D. H. Hartmann (Clemson University) report on behalf of the Stargate Consortium: "We observed the localisation of GRB 200216B (D’Avanzo et al. GCN 27102) with the Very Large Telescope and the HAWK-I instrument in the JHK bands beginning on 17 Feb 2020 at 02:44 UT, approximately 13.2 hours after the burst. In our K-band images we identify a candidate IR counterpart within the refined XRT localisation (Goad et al. GCN 27106). The location of the source is RA(J2000) 10:41:44.28 DEC(J2000) 19:28:31.3 With an uncertainty of ~0.3”. The source has a magnitude of K(AB)~22. The source is not well detected in either the J or H-band observations, but the depths are such that these observations offer limited constraints on the colour of the source. Given the inferred high X-ray column a high redshift origin is unlikely. We cannot make any statements regarding variability at this stage. We thank the staff at the VLT, in particular Bin Yang and Trystyn Berg for their work in acquiring these data." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27117 SUBJECT: GRB 200216B: Swift-BAT refined analysis DATE: 20/02/17 21:26:59 GMT FROM: Hans Krimm at NSF/NASA-GSFC H. A. Krimm (NSF), S. D. Barthelmy (GSFC), P. D'Avanzo (INAF-OAB), 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+908 sec from the recent telemetry downlink, we report further analysis of BAT GRB 200216B (trigger #956824) (D'Avanzo, et al., GCN Circ. 27102). The BAT ground-calculated position is RA, Dec = 160.452, 19.468 deg which is RA(J2000) = 10h 41m 48.4s Dec(J2000) = +19d 28' 05.5" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 84%. The mask-weighted light curve shows a single bright pulse followed by some extended emission. The main pulse has a FRED shape, starting at T-2 sec, peaking around T+2 sec and decaying by T+18 sec. Lower-level extended emission with some weak pulses lasts until around T+100 sec. T90 (15-350 keV) is 81.3 +- 13.0 sec (estimated error including systematics). The time-averaged spectrum from -0.72 to +100.33 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.81 +- 0.52, and Epeak of 47.6 +- 6.6 keV (chi squared 48.83 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 1.6 +- 0.1 x 10^-6 erg/cm2 and the 1-sec peak flux measured from T+2.80 sec in the 15-150 keV band is 1.5 +- 0.2 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.90 +- 0.10 (chi squared 65.47 for 57 d.o.f.). 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/956824/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27120 SUBJECT: GRB 200216B: Swift-XRT refined Analysis DATE: 20/02/18 10:07:24 GMT FROM: Paolo D'Avanzo at INAF - OAB P. D'Avanzo (INAF-OAB) and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: We have analysed 1.6 ks of XRT data for GRB 200216B (D'Avanzo et al. GCN Circ. 27102), from 105 s to 1.7 ks after the BAT trigger. The data comprise 90 s in Windowed Timing (WT) mode (the first 8 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 Goad et al. (GCN Circ. 27106). The light curve can be modelled with a power-law decay with a decay index of alpha=1.91 (+0.07, -0.06). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.18 (+0.20, -0.19). The best-fitting absorption column is 7.3 (+2.3, -1.9) x 10^21 cm^-2, in excess of the Galactic value of 2.0 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.63 (+0.27, -0.26) and a best-fitting absorption column of 9.2 (+2.9, -2.5) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5.8 x 10^-11 (8.5 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 9.2 (+2.9, -2.5) x 10^21 cm^-2 Galactic foreground: 2.0 x 10^20 cm^-2 Excess significance: 6.0 sigma Photon index: 1.63 (+0.27, -0.26) If the light curve continues to decay with a power-law decay index of 1.91, the count rate at T+24 hours will be 5.4 x 10^-5 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x 10^-15 (4.6 x 10^-15) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00956824. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27122 SUBJECT: GRB 200216B: Mondy and AbAO optical upper limits DATE: 20/02/18 16:01:19 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI), S. Belkin (IKI), E. Klunko (ISTP), R. Ya. Inasaridze (AbAO), E. Mazaeva (IKI), A. Volnova (IKI), I. Molotov (KIAM) report on behalf of IKI-GRB-FuN: We observed the field of GRB 200216B (D'Avanzo et al. GCN 27102; Fermi GBM team, GCN 27101) with AZT-33IK telescope of Sayan observatory (Mondy) starting on Feb. 16 (UT) 13:47:34 i.e. 15 minutes after GRB trigger. We also observed the GRB 200216B with AS-32 (0.7m) telescope of Abastumani Observatory starting on Feb. 16 (UT) 20:00:20. We do not detect any object in the enhanced Swift-XRT position (Goad et al. GCN 27106). In particular we do not detect possible IR-counterpart (Levan et al., GCN 27114). Preliminary photometry of the field is following. Date UT start t-T0 Filter Exp. OT UL(3sigma) (mid, days) (s) 2020-02-16 13:47:34 0.06915 R 30*60 n/d 22.0 2020-02-16 20:00:20 0.29256 R 67*60 n/d 21.8 Photometry is based on the USNO-B2.0 nearby stars. We note the presense the optical object at coordinates (J2000) 10:41:44.54 +19:28:19.3 and brightess of R=21.75 +/- 0.25 at 0.06915 days (mid time) after triger, and do not detect the object in the secod epoch R > 21.8 at 0.29256 days. The object is absent in both SDSS ans Pan-SARRS catalogues. The object is apart 14.5 arcsec from center of enhanced XRT erro circle (Goad et al. GCN 27106) and the object lies within 90% BAT ground-calculated position (Krimm et al., GCN 27117). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27128 SUBJECT: GRB 200216B: second epoch optical upper limit at Mondy observatory DATE: 20/02/19 12:01:00 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), E. Mazaeva (IKI), A. Volnova (IKI) report on behalf of IKI-GRB-FuN: We observed the field of GRB 200216B (D'Avanzo et al., GCN 27102: Fermi GBM team, GCN 27101) with AZT-33IK telescope of Sayan observatory (Mondy) starting on Feb. 18 (UT) 16:02:31. We did not detect any object in the enhanced Swift-XRT position (Goad et al., GCN 27106). In particular we do not detect possible IR-counterpart (Levan et al., GCN 27114). Upper limit is 22.8R. We detected the object reported earlier (Pozanenko et al., GCN 27122) with coordinates (J2000) 10:41:44.54 +19:28:19.3 which is 14.5 arcsec apart from center of enhanced XRT error circle (Goad et al., GCN 27106). Preliminary photometry of the object is following: Date UT start t-T0 Filter Exp. OT Err. UL(3sigma) (mid, days) (s) 2020-02-18 16:02:31 2.12497 R 30*120 22.7 0.3 22.8 Power law index of a light curve of the object calculated between the two epochs is about -0.3. Therefore the object might not be related to GRB 200216B.