//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28823 SUBJECT: GRB 201104A: Fermi GBM Final Real-time Localization DATE: 20/11/04 00:11:18 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 00:00:56 UT on 4 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201104A (trigger 626140861.749996 / 201104001). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 60.4, Dec = -72.7 (J2000 degrees, equivalent to J2000 04h 01m, -72d 42'), with a statistical uncertainty of 1.0 degrees. The angle from the Fermi LAT boresight is 65.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201104001/quicklook/glg_skymap_all_bn201104001.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/bn201104001/quicklook/glg_healpix_all_bn201104001.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201104001/quicklook/glg_lc_medres34_bn201104001.gif //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28824 SUBJECT: Fermi GRB 201104A: Global MASTER-Net observations report DATE: 20/11/04 00:15:27 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), 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-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 201104A ( Fermi GBM team, GCN 28823) errorbox 80 sec after trigger time at 2020-11-04 00:02:17 UT, with upper limit up to 17.8 mag. Observations started at twilight. The observations began at zenith distance = 59 deg. The sun altitude is -13.0 deg. The galactic latitude b = -38 deg., longitude l = 287 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=1475503 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 90 | 2020-11-04 00:02:17 | MASTER-OAFA | (03h 58m 14.15s , -74d 30m 15.1s) | C | 20 | 17.4 | 130 | 2020-11-04 00:02:56 | MASTER-OAFA | (03h 58m 07.55s , -74d 31m 15.8s) | C | 20 | 17.3 | 174 | 2020-11-04 00:03:35 | MASTER-OAFA | (03h 58m 15.37s , -74d 30m 56.0s) | C | 30 | 17.4 | 228 | 2020-11-04 00:04:25 | MASTER-OAFA | (03h 58m 11.98s , -74d 29m 19.8s) | C | 40 | 17.6 | 293 | 2020-11-04 00:05:24 | MASTER-OAFA | (03h 58m 12.40s , -74d 30m 55.2s) | C | 50 | 17.8 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28825 SUBJECT: GRB 201104B: Swift detection of a burst DATE: 20/11/04 18:10:07 GMT FROM: Jamie A. Kennea at PSU/Swift-XRT B. Sbarufatti (PSU), J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC), K. L. Page (U Leicester) and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift Observatory Team: At 17:33:46 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 201104B (trigger=1004168). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 5.217, 7.820 which is RA(J2000) = 00h 20m 52s Dec(J2000) = 07d 49' 12" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). Due to GCN downtime, no BAT light curves are available at this moment. The XRT began observing the field at 17:35:28.2 UT, 102 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec = 5.21528, 7.84257 which is equivalent to: RA(J2000) = 00h 20m 51.7s Dec(J2000) = +07d 50' 33.3" with an uncertainty of 5 arcseconds (radius, 90% containment). This location is 81.5 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. Due to GCN downtime, no UVOT data are available at this time. Burst Advocate for this burst is B. Sbarufatti (bxs60 AT psu.edu). 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: 28826 SUBJECT: GRB 201104B: MASTER optical observation DATE: 20/11/04 19:56:02 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, E.Gorbovskoy, N.Tiurina, P.Balanutsa,A.Kuznetsov,K.Zhirkov, F.Balakin, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, A.Chasovnikov,A.Pozdnyakov, V.Topolev, D.Cheryasov(Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O.A. Gres, N.M. Budnev (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V.Yurkov, Yu. Sergienko (Blagoveschensk Educational State University) MASTER-SAAO started GRB 201104B (Sbarufatti et al. GCN 28825, Ttrig=2020-11-04 17:33:46) observation by MASTER-II (2x4sq.deg.) in 2020-11-04 19:14:43UT (unfiltered, manual pointing) and by MASTER very wide field cameras (Lipunov et al. 2010, Advances in Astronomy,vol.2010, 30L), started at 48deg. altitude in clouds (the sun altitude was -25deg) There is no OT at Swift-XRT position with mlim=16.1 Observation and reduction will continue. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28827 SUBJECT: GRB 201104B: Swift/UVOT Detection DATE: 20/11/04 20:16:09 GMT FROM: Frank Marshall at Swift/UVOT F. E. Marshall (NASA/GSFC), S. R. Oates (U.Warwick) and B. Sbarufatti (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 201104B 56 s after the BAT trigger (Sbarufatti et al., GCN Circ. 28825). A source consistent with the XRT position (Sbarufatti et al. GCN Circ. 28825) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 00:20:51.65 = 5.21520 (deg.) Dec (J2000) = +07:50:29.4 = 7.84150 (deg.) with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence). Preliminary detections using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 56 206 147 18.63 +/- 0.06 u 268 459 188 19.45 +/- 0.23 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.045 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28828 SUBJECT: GRB 201104A: Fermi-LAT detection DATE: 20/11/04 20:30:07 GMT FROM: Masanori Ohno at Hiroshima University M. Ohno (Hiroshima U./Eotvos U.), N. Omodei (Stanford University), F. Longo (University & INFN Trieste) and M. Axelsson (KTH & Stockholm Univ.) report on behalf of the Fermi-LAT Collaboration: On November 4, 2020, Fermi-LAT detected high-energy emission from GRB 201104A, which was also detected by Fermi-GBM (trigger 626140861/201104001) (Fermi-GBM team; GCN Circ. 28823). The best LAT on-ground location is found to be RA, Dec = 81.4, -71.1 (degrees, J2000) with an error radius of 0.24 deg (90% containment, statistical error only). This was 6.7 deg from the LAT boresight at the time of the GBM trigger: T0 = 00:00:56 UT. The source quickly went out from the LAT FoV but the data from the Fermi-LAT show a significant increase in the event rate after the GBM trigger that is spatially and temporally correlated with the GBM emission with high significance. The photon flux above 100 MeV in the time interval 0-100 s after the GBM trigger is (2.6+/-0.4)e-4 ph/cm2/s. The estimated photon index above 100 MeV is -2.5 +/- 0.2. The highest-energy photon is a 3.7 GeV event which is observed 16 seconds after the GBM trigger. A Swift ToO has been requested for this burst The Fermi-LAT point of contact for this burst is Masanori Ohno (ohno@astro.hiroshima-u.ac.jp). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28829 SUBJECT: GRB 201104A: AGILE/MCAL detection DATE: 20/11/04 20:46:45 GMT FROM: Alessandro Ursi at INAF/IAPS A. Ursi (INAF/IAPS), F. Verrecchia, C. Pittori (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Argan, M. Cardillo, C. Casentini, Y. Evangelista, G. Piano (INAF/IAPS), F. Lucarelli (SSDC, and INAF/OAR), A. Bulgarelli, V. Fioretti, F. Fuschino, N. Parmiggiani (INAF/OAS-Bologna), M. Marisaldi (INAF/OAS-Bologna, and Bergen University), M. Pilia, A. Trois (INAF/OA-Cagliari), I. Donnarumma (ASI), F. Longo (Univ. Trieste and INFN Trieste), A. Giuliani (INAF/IASF-Mi), report on behalf of the AGILE Team: The AGILE Mini-CALorimeter (MCAL) detected GRB 201104A at T0 = 2020-11-04 00:00:56.77 +/- 0.01 s (UTC), reported by Fermi/GBM (GCN #28823) and INTEGRAL/SPI-ACS (trigger ID 8789,0). The event lasted about 8 s and released a total number of ~7200 counts in the detector (in the 0.4-100 MeV energy range), above an average background rate of 640 Hz. The light curve shows sveral episodes and can be found at http://www.agilescienceapp.it/notices/GRB_070287_531532856.770000.png . The time-integrated spectrum of the burst can be fitted in the energy range 0.4-20 MeV with a single power-law with ph.ind. = -2.26 -0.15/+0.18, resulting in a reduced chi-squared of 1.06 (75 d.o.f.) and a fluence of 3.57e-06 ergs/cm^2 (90% confidence level), in the same energy range. The burst is clearly visible in the AGILE scientific ratemeters of the MCAL detector. The event released a total number of 25100 counts, above a background rate of 1255 Hz. The AGILE ratemeter light curves can be found at http://www.agilescienceapp.it/notices/GRB_201104A_AGILE_RM.png . The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive in the energy range 0.4-100 MeV. Additional analysis of AGILE data is in progress. Automatic MCAL GRB alert Notices can be found at: https://gcn.gsfc.nasa.gov/agile_mcal.html. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28830 SUBJECT: GRB 201104A: Fermi GBM observation DATE: 20/11/04 20:51:58 GMT FROM: Christian Malacaria at NASA-MSFC/USRA E. Bissaldi (Politecnico and INFN Bari) and C. Malacaria (NASA-MSFC/USRA) report on behalf of the Fermi GBM Team: "At 00:00:56.75 UT on 4 November 2020, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 201104A (trigger 626140861 / 201104001, which was also detected by the Fermi-LAT (Ohno et al. 2020, GCN 28828) and AGILE (Ursi et al. 2020, GCN 28829). The GBM on-ground location is consistent with the LAT position. The angle from the Fermi LAT boresight at the GBM trigger time is 57 degrees. The GBM light curve shows a bright emission episode with a duration (T90) of about 8.4 s (50-300 keV). The time-averaged spectrum from T0 to T0+9 s is best fit by a Band function with Epeak = 1140 +/- 130 keV, alpha = -0.76 +/- 0.04, and beta = -2.24 +/- 0.17. The event fluence (10-1000 keV) in this time interval is (1.55 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0 in the 10-1000 keV band is 12.1 +/- 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: 28832 SUBJECT: GRB 201104A: Tiled Swift observations DATE: 20/11/04 21:22:19 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a series of observations, tiled on the sky, of the Fermi/LAT GRB 201104A. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00094 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. The probability of finding serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28833 SUBJECT: GRB 201104C: Fermi GBM Final Real-time Localization DATE: 20/11/04 21:35:03 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 19:23:25 UT on 4 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201104C (trigger 626210610.205754 / 201104808). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 240.3, Dec = -36.7 (J2000 degrees, equivalent to J2000 16h 01m, -36d 42'), with a statistical uncertainty of 7.7 degrees. The angle from the Fermi LAT boresight is 90.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201104808/quicklook/glg_skymap_all_bn201104808.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/bn201104808/quicklook/glg_healpix_all_bn201104808.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201104808/quicklook/glg_lc_medres34_bn201104808.gif //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28834 SUBJECT: GRB 201104A: BALROG localization (Fermi Trigger 626140861 / GRB 201104001) DATE: 20/11/04 22:35:07 GMT FROM: Jochen Greiner at MPE,Garching F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 626140861 at 00:00:56 on 04 Nov. 2020 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position (1 sigma statistical errors) is: RA(2000.0) = 67.9+/-10.4 deg Decl.(2000.0) = -73.2+/-1.6 deg We estimate an additional systematic error of 2 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB201104001/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB201104001/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB201104001/json //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28835 SUBJECT: GRB 201104A: BALROG localization (Fermi Trigger 626140861 / GRB 201104001) DATE: 20/11/04 22:35:09 GMT FROM: Jochen Greiner at MPE,Garching F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 626140861 at 00:00:56 on 04 Nov. 2020 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position (1 sigma statistical errors) is: RA(2000.0) = 67.9+/-10.4 deg Decl.(2000.0) = -73.2+/-1.6 deg We estimate an additional systematic error of 2 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB201104001/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB201104001/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB201104001/json //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28836 SUBJECT: GRB 201104A: BALROG localization (Fermi Trigger 626140861 / GRB 201104001) DATE: 20/11/04 22:37:25 GMT FROM: Jochen Greiner at MPE,Garching F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 626140861 at 00:00:56 on 04 Nov. 2020 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position (1 sigma statistical errors) is: RA(2000.0) = 67.9+/-10.4 deg Decl.(2000.0) = -73.2+/-1.6 deg We estimate an additional systematic error of 2 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB201104001/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB201104001/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB201104001/json //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28837 SUBJECT: GRB 201104A: BALROG localization (Fermi Trigger 626140861 / GRB 201104001) DATE: 20/11/05 01:40:31 GMT FROM: Jochen Greiner at MPE,Garching F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 626140861 at 00:00:56 on 04 Nov. 2020 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position (1 sigma statistical errors) is: RA(2000.0) = 67.9+/-10.4 deg Decl.(2000.0) = -73.2+/-1.6 deg We estimate an additional systematic error of 2 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB201104001/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB201104001/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB201104001/json //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28839 SUBJECT: GRB 201104B: Swift-BAT refined analysis DATE: 20/11/05 02:50:15 GMT FROM: Amy Lien at GSFC A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), B. Sbarufatti (PSU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+302 sec from the recent telemetry downlink, we report further analysis of BAT GRB 201104B (trigger #1004168) (Sbarufatti et al., GCN Circ. 28825). The BAT ground-calculated position is RA, Dec = 5.215, 7.834 deg which is RA(J2000) = 00h 20m 51.5s Dec(J2000) = +07d 50' 03.6" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 53%. The mask-weighted light curve shows several overlapping pulses that start at ~T-9 s and end at ~T+1 s. The main peak occurs at ~T-8 s. T90 (15-350 keV) is 8.66 +- 0.16 sec (estimated error including systematics). The time-averaged spectrum from T-8.86 to T+0.88 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.47 +- 0.07. The fluence in the 15-150 keV band is 1.8 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-8.52 sec in the 15-150 keV band is 4.1 +- 0.3 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/1004168/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28840 SUBJECT: GRB 201104B: VLT/X-shooter redshift DATE: 20/11/05 03:03:00 GMT FROM: Alexander Kann at IAA-CSIC J.-B. Vielfaure (GEPI, Paris Observatory), D. B. Malesani (DTU Space), D. A. Kann (HETH/IAA-CSIC), B. Sbarufatti (PSU), N. R. Tanvir (Univ. Leicester), and D. H. Hartmann (Clemson University) report on behalf of the Stargate Consortium: We observed the optical afterglow (Marshall et al., GCN 28827) of GRB 201104B (Sbarufatti et al., GCN 28825) using the ESO VLT UT3 (Melipal) equipped with the X-shooter spectrograph. Our spectra cover the wavelength range 3000-21000 AA, and consist of 2 exposures of 1200 s each. The observation mid-time was 2020 Nov 5.0831 UT (8.431 hr after the GRB). In a 60 s image taken with the acquisition camera on Nov 5.0596 UT, we detect the optical afterglow, for which we measure a magnitude r = 21.01 +/- 0.02 mag (AB magnitude, calibrated against nearby stars from the Pan-STARRS catalog; Chambers et al. 2016, arXiv:1612.05560). We clearly detect continuum over the entire wavelength range. A trough is visible around 3590 AA, which we identify as due to H I. From detection of multiple absorption features, which we interpret as due to SiII, CI, CII, SiIV, CIV, FeII, AlII, AlIII, MgII, we infer a redshift z = 1.954. In particular, fine structure lines from Fe II* are visible, which confirm the association of the absorption system with the GRB. Emission lines are also detected, which we interpret as due to [O II], Hbeta, [O III], and Halpha at the same redshift. We acknowledge excellent support from the ESO observing staff in Paranal, in particular Florian Rodler, Ivan Aranda, and Matias Jones. [GCN OPS NOTE(06nov2020): Per author's request, has two changes: 1) from "which we interpret as due to [O II], [O III], ad Halpha" to "which we interpret as due to [O II], Hbeta, [O III], and Halpha" 2) adding Ivan Aranda, and Matias Jones to the acknowledgement list.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28848 SUBJECT: GRB 201104C: Swift ToO observations DATE: 20/11/06 07:51:21 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the ZTF GRB 201104C. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021039 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. These are not necessarily related to the ZTF event. Any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28850 SUBJECT: GRB 201104B: Swift-XRT refined Analysis DATE: 20/11/06 09:09:44 GMT FROM: Phil Evans at U of Leicester J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), A. Melandri (INAF-OAB), T. Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB) and B. Sbarufatti report on behalf of the Swift-XRT team: We have analysed 4.9 ks of XRT data for GRB 201104B (Sbarufatti et al. GCN Circ. 28825), from 105 s to 131.7 ks after the BAT trigger. The data comprise 347 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. Using 546 s of PC mode data and 3 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 5.21441, +7.84185 which is equivalent to: RA (J2000): 00h 20m 51.46s Dec(J2000): +07d 50' 30.7" with an uncertainty of 2.3 arcsec (radius, 90% confidence). The light curve can be modelled with an initial power-law decay with an index of alpha=0.11 (+0.11, -0.12), followed by a break at T+338 s to an alpha of 1.21 (+0.05, -0.04). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.80 (+/-0.07). The best-fitting absorption column is 1.12 (+0.30, -0.28) x 10^22 cm^-2, at a redshift of 1.954, in addition to the Galactic value of 5.7 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (4.5 x 10^-11) erg cm^-2 count^-1. A summary of the WT-mode spectrum is thus: Galactic foreground: 5.7 x 10^20 cm^-2 Intrinsic column: 1.12 (+0.30, -0.28) x 10^22 cm^-2 at z=1.954 Photon index: 1.80 (+/-0.07) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01004168. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28851 SUBJECT: GRB 201104B: Swift/UVOT Detection DATE: 20/11/06 09:41:59 GMT FROM: Samantha Oates at MSSL S. R. Oates (U.Birmingham) and B. Sbarufatti (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 201104B 56 s after the BAT trigger (Sbarufatti et al., GCN Circ. 28825). A source consistent with the XRT position (Sbarufatti et al. GCN Circ. 28825) and UVOT position (Marshall et al. GCN Circ. 28827) is detected in the initial UVOT exposures. Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white (FC) 56 206 147 17.98 +/- 0.05 white 20890 21385 484 >21.1 b 3718 3777 57 >19.0 u (FC) 268 459 188 18.72 +/- 0.16 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.048 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28852 SUBJECT: GRB 201104B: TSHAO optical observation DATE: 20/11/06 11:11:37 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), N. Pankov (HSE), I. Reva (FAPHI), A. Pozanenko (IKI) report on behalf of GRB-IKI-FuN: We observed the field of GRB 201104B (Sbarufatti et al., GCN 28825) with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting on Nov. 05 (UT) 12:51:33. The optical afterglow (Marshall et al., GCN 28827; Vielfaure et al., GCN 28840; Oates et al., GCN 28851) at redshift z = 1.954 (Vielfaure et al., GCN 28840) is detected in stacked image in R-filter. Preliminary photometry of the afterglow is following. Date UT start t-T0 Filter Exp. OT Err. UL(3 sigma) (mid, days) (s) 2020-11-05 12:51:33 0.82641 R 43*90 21.20 0.1 22.2 The photometry is based on nearby USNO-B1.0 stars. USNO-B1.0_id R2 0979-0003163 17.51 0979-0003223 17.47 We note the presence of a galaxy 3.6" South-East from the afterglow. The galaxy is clearly visible in Pan-STARRS and SDSS and detected in USNO-B1.0, PS1 and SDSS DR12 (J002051.50+075026.5). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28856 SUBJECT: GRB 201104B: Kitab optical observations DATE: 20/11/06 17:01:34 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), A. Zhornichenko (KIAM), A. Pozanenko (IKI), V. Agletdinov (KIAM), Sh. Ehgamberdiev (UBAI) report on behalf of IKI-GRB-FuN: We observed the field of GRB 201104B (Sbarufatti et al., GCN 28825) with Kitab-ISON RC-36 telescope in Clear filter. Observation started on Nov. 4 (UT) 18:44:28, i.e. 77 minutes after trigger. The optical afterglow (Marshall et al., GCN 28827; Vielfaure et al., GCN 28840; Oates et al., GCN 28851) at redshift z = 1.954 (Vielfaure et al., GCN 28840) is marginally (S/N = 1.8) detected in stacked image. Preliminary photometry of the afterglow is following. Date, UT start, t-T0, Exp., Filter, OT, S/N UL(3 sigma) (mid, days) 2020-11-04 18:44:28 0.0741 72*60 CR 20.4 1.8 20.0 The photometry is based on nearby USNO-B1.0 stars, R magnitude. USNO-B1.0_id R2 0979-0003163 17.51 0979-0003223 17.47 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28859 SUBJECT: GRB 201104A: Swift-XRT observations DATE: 20/11/06 17:46:49 GMT FROM: Boris Sbarufatti at PSU V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), D.N. Burrows (PSU), J. D. Gropp (PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB) and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/LAT-detected burst GRB 201104A (Ohno et al. GCN Circ. 28828) in a series of observations tiled on the sky. The total exposure time is 4.7 ks, distributed over 3 tiles; the maximum exposure at a single sky location was 2.4 ks. The data were collected between T0+67.6 ks and T0+80.9 ks, and are entirely in Photon Counting (PC) mode. One uncatalogued X-ray source has been detected, it is not above the RASS limit or shows definitive signs of fading. Furthermore, it is coincident with a known optical source and the XRT data are possibly affected by stray light. Therefore we believe that XRT has not detected any viable candidate afterglow. Details of the sources are given below: Source 3: RA (J2000.0): 80.9041 = 05:23:36.99 Dec (J2000.0): -71.0096 = -71:00:34.6 Error: 4.1 arcsec (radius, 90% conf. [Enhanced position]) Count-rate: (5.3 [+2.7, -2.0])e-3 ct s^-1 Distance: 664 arcsec from Fermi/LAT position. Flux: (1.53 [+0.77, -0.59])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) A catalogued source was also detected inside the LAT error circle, and two more sources were detected outside of it. The 3 sigma upper limit at the LAT GRB position is 7.6×10-3 ct s-1. The results of the XRT-team automatic analysis of the tiled XRT observations, including a position-specific upper limit calculator, are available at https://www.swift.ac.uk/xrt_products/TILED_GRB00094. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28860 SUBJECT: GRB 201104B: 1.3m DFOT optical observations DATE: 20/11/06 19:56:54 GMT FROM: Rahul Gupta at ARIES, India Rahul Gupta (ARIES), Dimple (ARIES), Amit Kumar (ARIES), Ankur Ghosh (ARIES), Amar Aryan (ARIES), Shubham Kishore (ARIES) , Shashi B. Pandey (ARIES), Kuntal Misra (ARIES), and Alok C. Gupta (ARIES ) report: We observed the optical afterglow ( Marshall et al., GCN 28827 ; Vielfaure et al., GCN 28840; Oates et al., GCN 28851; and Belkin et al., GCN 28852, GCN 28856) of Swift triggered GRB 201104B (Sbarufatti et al., GCN 28825) using the 1.3m Devasthal Fast Optical Telescope (DFOT) at Devasthal observatory of Aryabhatta Research Institute of Observational Sciences (ARIES), India. The observations were started on 2020-11-05 at 17:44:45 UT . Multiple frames having an exposure time of 60 s were taken in the R filter. We clearly detected the optical counterpart in the stacked images. The preliminary photometric estimate of the afterglow in the stacked images is the following : Date Start_UT T_start-T0 (hrs) Filter Exp time (s) Magnitude Mag_err ------------------------------ ------------------------------ ------------------------------ ------------------------------ ------------------------------ ------------------ 2020-11-05 17:44:45 24.18 R 30*60 22.40 0.23 ------------------------------ ------------------------------ ------------------------------ ------------------------------ ------------------------------ ------------------ The magnitude is not corrected for the Galactic and Host extinction in the direction of the burst. Photometric calibration is performed using the standard stars from the USNO-B1.0 catalog. This circular may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28870 SUBJECT: GRB 201104B: MITSuME Akeno optical observation DATE: 20/11/09 09:47:55 GMT FROM: Ryohei Hosokawa at Tokyo Institute of Technology R. Hosokawa, R. Adachi, K. L. Murata, M. Niwano, F. Ogawa, N. Nakamura, N. Ito, S. Ogata, H. Takamatsu, H. Hara, Y. Yatsu, and N. Kawai (TokyoTech) report on behalf of the MITSuME collaboration: We observed the field of GRB 201104B (B. Sbarufatti et al., GCN #28825) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started at 2020-11-05 08:14:33 UT. The first 29 images were heavily affected by twilight at Akeno Observatory. We marginally detected the point source at the position consistent with the afterglow detected previously (Marshall et al., GCN #28827, Vielfaure et al., GCN #28840, Oates et al., GCN #28851, Belkin et al., GCN #28852, Belkin et al., GCN #28856, and Gupta et al., GCN #28860). We measured the magnitudes as follows. T0+[hour] MID-UT T-EXP[sec] measured magnitudes ------------------------------------------------------------------------------------------------ 15.2 2020-11-05 12:59:59 21360 g'=21.5+/-0.3, Rc=20.7+/-0.2, Ic=20.3+/-0.3 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., https://doi.org/10.1093/pasj/psaa091, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28871 SUBJECT: GRB 201104B: continued TSHAO optical observation DATE: 20/11/09 12:57:32 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), A. Kusakin (FAP), N. Pankov (HSE), I. Reva (FAP), A. Pozanenko (IKI) report on behalf of GRB-IKI-FuN: We continued observations of the GRB 201104B (Sbarufatti et al., GCN 28825) with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting on Nov. 06 (UT) 15:04:58. The optical afterglow (Marshall et al., GCN 28827; Vielfaure et al., GCN 28840; Oates et al., GCN 28851; Belkin et al., GCNs 28852, 28856; Gupta et al., GCN 28860; Hosokawa et al., GCN 28870) at redshift z = 1.954 (Vielfaure et al., GCN 28840) is detected in stacked image in R-filter. Preliminary photometry of the afterglow is following. Date UT start t-T0 Filter Exp. OT Err. UL(3 sigma) (mid, days) (s) 2020-11-06 15:04:58 1.92271 R 50*90 22.20 0.21 22.4 The photometry is based on nearby USNO-B1.0 stars. USNO-B1.0_id R2 0979-0003163 17.51 0979-0003223 17.47 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28873 SUBJECT: GRB 201104A: AstroSat CZTI detection DATE: 20/11/09 20:42:02 GMT FROM: Soumya Gupta at IUCAA/ASTROSAT S. Gupta, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (IUCAA/TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: The AstroSat CZT Imager recorded a transient event in all four of its CsI anticoincidence (Veto) detectors in the 100-500 keV energy range, coincident with the long GRB 201104A reported by Fermi GBM (GCN #28823), Global MASTER-Net (Lipunov V. et al., GCN #28824), Fermi LAT (Ohno M. et al., GCN #28828), AGILE/MCAL (Ursi A. et al., GCN #28829), Fermi GBM (Bissaldi E. et al., GCN #28830), Tiled Swift (Evans P. et al., GCN #28832), BALROG (Kunzweiler F. et al., GCN #28834) and Swift-XRT (D'Elia V. et al., GCN #28859). There was a weak detection in the main CZT detectors in the 40-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-11-04 00:00:55.000 UT. The measured peak count rate is 1757 +/- 68 cts/s above the background in the combined Veto data of four quadrants, with a total of 6949 +/- 80 cts. The local mean background count rate was 2774 +/- 5 cts/s. We measure a T90 of 8.18 +/- 0.13 s from the cumulative Veto light curve. In the main CZT detectors, the light curve showed multiple peaks of emission with the strongest peak at 2020-11-04 00:00:56.000 UT. The measured peak count rate associated with the burst is 330 +/- 33 cts/s above the background in the combined data of four quadrants, with a total of 1170 +/- 23 cts. The local mean background count rate was 792 +/- 2 cts/s. Using cumulative rates, we measure a T90 of 7.36 +/- 0.11 s. CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29198 SUBJECT: GRB 201104B: Maidanak and CrAO optical observations DATE: 20/12/29 22:49:38 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), A. Pozanenko (IKI), V. Rumyantsev (CrAO), O. Burhonov (UBAI), Sh. Ehgamberdiev (UBAI) report on behalf of IKI GRB FuN: We observed GRB 201104B (Sbarufatti et al., GCN 28825) with AZT-22 telescope of Maidanak Observatory and ZTSh telescope of CrAO. The optical afterglow (Marshall et al., GCN 28827; Vielfaure et al., GCN 28840; Oates et al., GCN 28851; Belkin et al., GCNs 28852, 28856, 28871; Gupta et al., GCN 28860; Hosokawa et al., GCN 28870) at redshift z = 1.954 (Vielfaure et al., GCN 28840) is detected in stacked images. Preliminary photometry of the afterglow is following. Date UT start t-T0 Filter Exp. OT Err. UL(3 sigma) (mid, days) (s) 2020-11-09 15:57:43 4.95413 R 12*300 22.89 0.09 24.3 AZT-22 2020-11-13 19:50:05 9.12784 R 45*120 23.20 0.12 24.0 ZTSh The photometry is based on nearby USNO-B1.0 stars. A light curve base on our observations including reported earlier (Belkin et al., GCNs 28852, 28856, 28871) can be found in http://grb.rssi.ru/GRB201104B/GRB201104B_LC_R.png