GRB201015A

This page lists all entries on GRB201015A in GRBweb

Summary IPN Swift GCN 28632 GCN 28634 GCN 28635 GCN 28637 GCN 28639 GCN 28645 GCN 28647 GCN 28649 GCN 28653 GCN 28656 GCN 28658 GCN 28659 GCN 28660 GCN 28661 GCN 28662 GCN 28663 GCN 28664 GCN 28668 GCN 28673 GCN 28674 GCN 28676 GCN 28677 GCN 28680 GCN 28681 GCN 28688 GCN 28721 GCN 28822 GCN 28857 GCN 28939 GCN 28945 GCN 29028 GCN 29033 GCN 29306

Summary table
Variable Value Source
T0 22:50:13 UTC GCN_circulars,Swift Det
ra 354.3186° Swift
decl 53.4160° Swift
pos_error 2.20e-04° Swift
T90 9.78 s Swift
T90_start 22:50:13 UTC Swift
fluence 2.00e-07 erg/cm² Swift
redshift 0.4260
T100 9.78 s
GBM_located False
mjd 59137.95153935185 GCN_circulars,Swift Det
IPN table
GRB_name GRB201015A
ra 354.3417°
decl 53.4000°
pos_error 5.00e-02°
redshift 0.4260
Swift table
GRB_name GRB201015A
t_trigger 22:50:13 UTC
ra 354.3186°
decl 53.4160°
pos_error 2.20e-04°
T90 9.78 s
fluence 2.00e-07 erg/cm²
redshift 0.4260
GCN 28632 table
GRB_name GRB201015A
GCN_number 28632
Detection_method Swift Det
t_trigger 22:50:13 UTC
ra 354.3430°
decl 53.3930°
Circular_text TITLE: GCN CIRCULAR NUMBER: 28632 SUBJECT: GRB 201015A: Swift detection of a burst DATE: 20/10/15 22:58:36 GMT FROM: David Palmer at LANL V. D'Elia (SSDC), E. Ambrosi (INAF-IASFPA), S. D. Barthelmy (GSFC), A. D'Ai (INAF-IASFPA), J.D. Gropp (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL), B. Sbarufatti (PSU) and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 22:50:13 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 201015A (trigger=1000452). Swift did not slew immediately to the burst due to an observing constraint. The BAT on-board calculated location is RA, Dec 354.343, +53.393 which is RA(J2000) = 23h 37m 22s Dec(J2000) = +53d 23' 36" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a duration of about 10 sec. The peak count rate was ~700 counts/sec (15-350 keV), at ~0 sec after the trigger. Due to an observing constraint, Swift will not slew until T0+51.6 minutes. There will be no XRT or UVOT data until this time. Burst Advocate for this burst is V. D'Elia (delia AT ssdc.asi.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/)
GCN 28634 table
GRB_name GRB201015A
GCN_number 28634
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 28634 SUBJECT: Swift GRB 201015A: Global MASTER-Net observations report DATE: 20/10/15 23:02:53 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-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 201015A ( V. D'Elia et al., GCN 28632) errorbox 88 sec after trigger time at 2020-10-15 22:51:41 UT, with upper limit up to 18.5 mag. The observations began at zenith distance = 33 deg. The sun altitude is -50.5 deg. The galactic latitude b = -8 deg., longitude l = 112 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=1462183 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 98 | MASTER-Tavrida | C | 20 | 17.8 | 123 | MASTER-Tavrida | C | 70 | 18.5 | Coadd 138 | MASTER-Tavrida | C | 20 | 17.9 | 184 | MASTER-Tavrida | C | 30 | 18.1 | 239 | MASTER-Tavrida | C | 40 | 18.3 | 305 | MASTER-Tavrida | C | 50 | 18.4 | 385 | MASTER-Tavrida | C | 70 | 18.5 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 28635 table
GRB_name GRB201015A
GCN_number 28635
Detection_method Swift-XRT Other
ra 354.3207°
decl 53.4146°
Circular_text TITLE: GCN CIRCULAR NUMBER: 28635 SUBJECT: GRB 201015A: Swift-XRT observations DATE: 20/10/16 00:11:29 GMT FROM: Phil Evans at U of Leicester J.A. Kennea (PSU), G. Tagliaferri (INAF-OAB), S. Campana (INAF-OAB), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester) and D.N. Burrows (PSU) report on behalf of the Swift-XRT team: The XRT began observing the field of GRB 201015A at 23:43:47.2 UT, 3214.1 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source located at RA, Dec 354.32067, 53.41460 which is equivalent to: RA(J2000) = 23h 37m 16.96s Dec(J2000) = +53d 24' 52.6" with an uncertainty of 3.8 arcseconds (radius, 90% containment). This location is 91 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 3.60 x 10^21 cm^-2 (Willingale et al. 2013).
GCN 28637 table
GRB_name GRB201015A
GCN_number 28637
Detection_method Optical
ra 354.3184°
decl 53.4157°
Circular_text TITLE: GCN CIRCULAR NUMBER: 28637 SUBJECT: GRB 201015A: NOT optical afterglow confirmation DATE: 20/10/16 01:21:02 GMT FROM: Daniele B Malesani at DTU Space D. B. Malesani (DTU Space), A. de Ugarte Postigo (HETH, IAA/CSIC), T. Pursimo (NOT), report on behalf of a larger collaboration: We observed the field of GRB 201015A (D'Elia et al., GCN 28632) using the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. Our first image was taken at 23:25:12 UT (35 min after the trigger). At the location of the afterglow candidate reported by Lipunov et al. (GCN 28633), also consistent with the XRT position (Kennea et al., GCN 28635), we detect a source not visible in the Pan-STARRS images of the same area. We report for this target the following, refined coordinates: RA(J2000) = 23:37:16.41 Dec(J2000) = +53:24:56.5 with an uncertainty of 0.3" (calibrated against the Gaia catalog). Our image was taken with a non-standard, broad filter (~3700-9000 AA), and the target is affected by a saturation defect from a star. We cannot provide a reliable magnitude at the present time, but a rough estimate yields ~19.
GCN 28639 table
GRB_name GRB201015A
GCN_number 28639
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 28639 SUBJECT: GRB 201015A: GOTO confirmation of afterglow detection DATE: 20/10/16 03:18:47 GMT FROM: Kendall Ackley at Monash University K. Ackley (1); D. K. Galloway (1); Y-L Mong (1); M. Dyer (2); J. Lyman (3); K. Ulaczyk (3); D. Steeghs (3); V. Dhillon (2); P. O'Brien (4); G. Ramsay (5); S. Poshyachinda (6); R. Kotak (7); L. Nuttall (8); D. Pollacco (3); R. Breton (9) ((1) Monash University, (2) University of Sheffield, (3) Warwick University, (4) University of Leicester, (5) Armagh Observatory & Planetarium, (6) National Astronomical Research Institute of Thailand, (7) University of Turku, (8) University of Portsmouth, (9) University of Manchester) report on behalf of the GOTO collaboration: We carried out observations with the Gravitational-wave Optical Transient Observer (GOTO) on La Palma in response to GRB 201015A (Swift; D'Elia et al; GCN 28632). We made a series of 4x90 s exposures using our wide L-band filter (400-700 nm) covering the Swift XRT error box (Swift; Kennea et al.; GCN 28635), beginning at 51 minutes after trigger, with midtime of the first observation 23:41:54.25 UT on 15 October 2020. Using a difference imaging analysis with recent survey observations of the same pointings as reference, we detect an uncatalogued source located at (J2000): RA 23:37:16.42 Dec +53:24:55.89 confirming the OT reported by MASTER (Lupinov et al.; GCN 28633) and NOT (Malesani et al.; GCN 28637). We find an equivalent magnitude of g ~ 20.2 mag based on cross-calibration of our L-band magnitudes against the ATLAS catalogue. Observations are continuing. GOTO is operated at the La Palma observing facilities of the University of Warwick on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT) and the Instituto de Astrofisica de Canarias (IAC) (https://goto-observatory.org )
GCN 28645 table
GRB_name GRB201015A
GCN_number 28645
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 28645 SUBJECT: GRB 201015A: BOOTES-1 early optical afterglow detection DATE: 20/10/16 05:18:34 GMT FROM: Youdong HU at IAA-CSIC Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado (IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco, I. Perez-Garcia, A. Reina (Univ. de Malaga) and F. Rendon (IAA-CSIC and INTA-CEDEA) on behalf of a larger collaboration, report: Following the Swift/BAT trigger of GRB 201015A (D'Elia et al., GCNC 28632), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva), southern Spain, automatically responded to this burst. A series of images were taken starting on 15 Oct at 22:50:48UT (35 s after trigger). We confirm the OT reported by MASTER (Lipunov et al., GCNC 28633) in our co-added 30x1s clear filter images at a similar epoch (T_mid = 205 s) with 17.0 mag, at a position consistent with the reported Swift/XRT X-ray (Kennea et al., GCNC 28635) and late-time optical afterglows position reported by NOT (Malesani et al., GCNC 28637) and GOTO (Ackley et al., GCNC 28639). Further analysis is ongoing. We thank the staff at INTA-CEDEA for their excellent support.
GCN 28647 table
GRB_name GRB201015A
GCN_number 28647
Detection_method Swift-XRT Det
ra 354.3186°
decl 53.4160°
Circular_text TITLE: GCN CIRCULAR NUMBER: 28647 SUBJECT: GRB 201015A: Enhanced Swift-XRT position DATE: 20/10/16 06:48:24 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 1576 s of XRT Photon Counting mode data and 4 UVOT images for GRB 201015A, 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 = 354.31859, +53.41603 which is equivalent to: RA (J2000): 23h 37m 16.46s Dec (J2000): +53d 24' 57.7" 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.
GCN 28649 table
GRB_name GRB201015A
GCN_number 28649
Detection_method Swift-BAT Det
redshift 0.4260
Circular_text TITLE: GCN CIRCULAR NUMBER: 28649 SUBJECT: GRB 201015A: Redshift from GTC/OSIRIS DATE: 20/10/16 09:13:32 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D.A. Kann, M. Blazek, J.F. Agui Fernandez, C. Thoene (all HETH/IAA-CSIC), G. Gomez Velarde (GTC) report: We observed the afterglow of GRB 201015A (D’Elia et al. GCN 28632, Lipunov et al. GCN 28633) with the 10.4m GTC telescope, at Roque de los Muchachos Observatory (La Palma, Spain) equipped with OSIRIS. The observation started at 4:07 UT (5.28 hrs after the GRB onset) and consisted of 3x900s with the R1000B grism, covering the range between 3700 and 7800 Å. The spectrum shows a featureless continuum throughout the full spectral range. However, we do identify emission features superposed on the trace, which we identify as [OIII], [OII], and H-beta at a common redshift of 0.426. The automatic BAT analysis shows that this is a peculiar short but soft spectrum burst. We encourage follow-up to search for the associated supernova that could confirm the long nature of the burst, or the lack of such a supernova which would indicate a possible short origin.
GCN 28653 table
GRB_name GRB201015A
GCN_number 28653
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 28653 SUBJECT: GRB201015A: Nanshan/NEXT early optical observations DATE: 20/10/16 14:16:04 GMT FROM: Dong Xu at NAOC/CAS Z.P. Zhu (NAOC/HUST), X. Liu, S.Y. Fu, D. Xu (NAOC), X. Gao (Urumqi No.1 Senior High School), J.Z. Liu (XAO) report: We observed the field of GRB 201015A (D'Elia et al., GCN 28632) using the NEXT-0.6m optical telescope located at Nanshan, Xinjiang, China. Observations automatically started at 22:51:31 UT on 2020-10-15, i.e., 78 s after the BAT trigger. We obtained 3x40s, 4x60s and 12x90s frames in the Sloan r-filter until the sky brightens. The optical afterglow (e.g., Lipunov et al., GCN 28633; Kennea et al., GCN 28635; Malesani et al., GCN 28637; Ackley et al., GCN 28639; Hu et al., GCN 28645) is clearly detected in our images. The lightcurve rises from r = 18.34 +/- 0.08 at T-mid=98 s to the peak of r = 16.97 +/- 0.03 at T-mid=226 s, and then decays roughly in a powerlaw with the index of alpha ~ 1.2. Photometry is calculated with the Pan-STARRS field.
GCN 28656 table
GRB_name GRB201015A
GCN_number 28656
Detection_method Optical
redshift 0.4260
Circular_text TITLE: GCN CIRCULAR NUMBER: 28656 SUBJECT: GRB 201015A: CrAO/ZTSH optical observations DATE: 20/10/16 15:31:16 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), N. Pankov (HSE), A. Pozanenko (IKI), V. Rumyantsev (CrAO), A. Volnova (IKI) report on behalf of larger GRB follow-up collaboration: We observed the GRB 201015A (D'Elia et al., GCN 28632) with ZTSH 2.6m telescope of CrAO observatory between Oct. 16 (UT) 01:02:14 -- 02:52:23. The optical afterglow (e.g., Lipunov et al., GCN 28633; Kennea et al., GCN 28635; Malesani et al., GCN 28637; Ackley et al., GCN 28639; Hu et al., GCN 28645; Zhu et al., GCN 28653) at redshift z=0.426 (de Ugarte Postigo et al., GCN 28649) is clearly detected in each frame of 120 s exposure in R filter. The exact photometry of the afterglow depends on the underlying object visible and presented in PS1 catalogue (i'=19.6), which may be a host galaxy (PS1 magnitude i'=19.6). Preliminary photometry of the afterglow in a combined image is following Date UT start t-T0 Filter Exp. OT err UL(3sigma) (mid, days) (s) 2018-10-16 02:19:26 0.15501 R 12*120 20.66 0.05 23.0 The photometry is based on several nearby USNO-B1.0 stars USNO-B1.0_id R2 1434-0471702 17.51 1434-0471746 18.23
GCN 28658 table
GRB_name GRB201015A
GCN_number 28658
Detection_method Swift-BAT Det
ra 354.3100°
decl 53.4460°
Circular_text TITLE: GCN CIRCULAR NUMBER: 28658 SUBJECT: GRB 201015A: Swift-BAT refined analysis (a soft short pulse with a tail emission) DATE: 20/10/16 16:04:58 GMT FROM: Amy Lien at GSFC C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), V. D'Elia (SSDC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC), 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 201015A (trigger #1000452) (D'Elia et al., GCN Circ. 28632). The BAT ground-calculated position is RA, Dec = 354.310, 53.446 deg which is RA(J2000) = 23h 37m 14.4s Dec(J2000) = +53d 26' 45.0" with an uncertainty of 2.9 arcmin, (radius, sys+stat, 90% containment). The partial coding was 30%. The mask-weighted light curve shows a short-soft structure with several overlapping pulses that start at ~T0 and end at ~T+1 s, followed by a weak-soft tail that lasts till ~T+10 s. T90 (15-350 keV) is 9.78 +- 3.47 sec (estimated error including systematics). The time-averaged spectrum from T+0.02 to T+10.35 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 3.03 +- 0.68. The fluence in the 15-150 keV band is 2.0 +- 0.6 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+0.08 sec in the 15-150 keV band is 1.8 +- 0.4 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The BAT spectrum of this event does not appear to be a short hard burst. However, the quickly fading X-ray and optical afterglows are consistent with those from a short GRB. If this is a short GRB, this is one of the softest short bursts detected by BAT (based on a sample with constrained spectral fits from the 3rd BAT GRB catalog; Lien & Sakamoto et al. 2016). Other BAT-detected short GRBs with similar softness include GRB190326A and GRB140622A. GRB190326A has an ambiguous origin due to an observing constraint, but late time XRT/UVOT followup observations suggest that the source is more consistent with a GRB (Sbarufatti et al., GCN Circ. 24129). GRB140622A was classified to be a short GRB because the XRT light curve is consistent with the normal behavior of a short burst (Sakamoto et al. GCN Circ. 16438; Burrows et al. GCN Circ. 16439). The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/1000452/BA/
GCN 28659 table
GRB_name GRB201015A
GCN_number 28659
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 28659 SUBJECT: MAGIC observations of GRB 201015A: hint of very high energy gamma-ray signal DATE: 20/10/16 16:48:37 GMT FROM: Oscar Blanch at MAGIC Collaboration O.Blanch (IFAE-BIST Barcelona), M. Gaug (UAB Barcelona), K. Noda (ICRR University of Tokyo), A. Berti (INFN Torino), E. Moretti (IFAE-BIST Barcelona), D. Miceli (University of Udine and INFN Trieste), P. Gliwny (University of Lodz) S. Ubach (UAB Barcelona), B. Schleicher (University of Wuerzburg), M. Cerruti (University of Barcelona) and A. Stamerra (INAF Rome) on behalf of the MAGIC collaboration report: On October 15, 2020, the MAGIC telescopes observed GRB 201015A following the Swift-BAT trigger (D’Elia et al., GCN 28632). MAGIC started observations under good conditions about 40 seconds after the initial Swift trigger, revealing a hint of signal with significance >3 sigma in the very high energy band. Refined off-line analyses of the data are ongoing. Further MAGIC observations on GRB 201015A are planned in the coming night. We strongly encourage follow-up observations by other instruments at all wavelengths. The MAGIC point of contact for this burst is O. Blanch (blanch@ifae.es). Burst Advocate for this burst is M. Gaug (Markus.Gaug@uab.cat) MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Observatory Roque de los Muchachos on the Canary island La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV. -- Avís - Aviso - Legal Notice - (LOPD) - http://legal.ifae.es
GCN 28660 table
GRB_name GRB201015A
GCN_number 28660
Detection_method Swift-XRT Other
redshift 0.4260
Circular_text TITLE: GCN CIRCULAR NUMBER: 28660 SUBJECT: GRB 201015A: Swift-XRT refined Analysis DATE: 20/10/16 17:26:09 GMT FROM: Phil Evans at U of Leicester A. D'Ai (INAF-IASFPA), J. D. Gropp (PSU), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), A. Melandri (INAF-OAB) and V. D'Elia report on behalf of the Swift-XRT team: We have analysed 7.2 ks of XRT data for GRB 201015A (D'Elia et al. GCN Circ. 28632), from 3.2 ks to 57.3 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN Circ. 28647). The light curve can be modelled with a power-law decay with a decay index of alpha=1.49 (+0.24, -0.21). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.2 (+/-0.4). The best-fitting absorption column is 2.3 (+4.6, -2.3) x 10^21 cm^-2, at a redshift of 0.426, in addition to the Galactic value of 3.6 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 4.0 x 10^-11 (7.7 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Galactic foreground: 3.6 x 10^21 cm^-2 Intrinsic column: 2.3 (+4.6, -2.3) x 10^21 cm^-2 at z=0.426 Photon index: 2.2 (+/-0.4) If the light curve continues to decay with a power-law decay index of 1.49, the count rate at T+24 hours will be 10.0 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.0 x 10^-14 (7.7 x 10^-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01000452. This circular is an official product of the Swift-XRT team.
GCN 28661 table
GRB_name GRB201015A
GCN_number 28661
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 28661 SUBJECT: GRB 201015A: redshift confirmation DATE: 20/10/16 18:15:26 GMT FROM: Daniele B Malesani at DTU Space L. Izzo (DARK/NBI), D. B. Malesani (DTU Space), Z.P. Zhu (NAO/CAS, HUST), D. Xu (NAO/CAS), A. de Ugarte Postigo (HETH, IAA-CSIC), T. Pursimo, report on behalf of a larger collaboration: We observed the optical counterpart of GRB 201015A (D'Elia et al., GCN 28632; Lipunov et al., GCN 28634) with the Nordic Optical Telescope, equipped with the ALFOSC spectrograph. Spectroscopic observations started on 2020 Oct 15.978 UT (38 min after the GRB trigger) and consisted of four 900-s exposures with grism #4, covering the wavelength range 3800-9400 AA. A trace is visible across the full spectral range. In the blue part, weak absorption features are detected which can be interpreted as Mg II, Mg I and Ca II at z = 0.423. Faint emission lines are also detected at a consistent redshift, identified as [O II] and Halpha. Our data allow thus to confirm the redshift value reported by de Ugarte Postigo et al. (GCN 28649) using the GTC. We note that the detection of absorption features sets a firm lower limit to the GRB redshift, excluding a chance superposition with a background galaxy. This work made use of the GRBspec database grbspec.iaa.es.
GCN 28662 table
GRB_name GRB201015A
GCN_number 28662
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 28662 SUBJECT: GRB 201015A: Swift/UVOT Detection DATE: 20/10/16 20:49:02 GMT FROM: Frank Marshall at Swift/UVOT F. E. Marshall (NASA/GSFC) and V. D'Elia (SSDC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 201015A 3217 s after the BAT trigger (D'Elia et al., GCN Circ. 28632). A weak source consistent with the optical position (Malesani et al. GCN Circ. 28637) 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 3217 3367 147 20.69 +/- 0.28 white 4402 4602 197 20.33 +/- 0.16 v 3375 4949 331 >19.3 b 4197 4397 197 20.47 +/- 0.33 u 3991 4191 197 >19.7 w1 3786 3986 197 >19.3 m2 3579 3779 197 >18.8 w2 4608 4808 197 >19.4 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.34 in the direction of the burst (Schlegel et al. 1998).
GCN 28663 table
GRB_name GRB201015A
GCN_number 28663
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 28663 SUBJECT: Fermi GBM Sub-Threshold Detection of GRB 201015A DATE: 20/10/16 21:25:33 GMT FROM: Cori Fletcher at USRA C. Fletcher (USRA) and P. Veres (UAH) report on behalf of the Fermi-GBM Team: Swift-BAT detected GRB 201015A at 22:50:13 UT (GCN 28632). There was no Fermi-GBM onboard trigger around the event. An automated, blind search for short gamma-ray bursts below the onboard triggering threshold in Fermi-GBM identified no counterparts. The GBM targeted search [1], the most sensitive, coherent search for GRB-like signals was run from +/-30 s around the BAT trigger time. A transient source was identified whose most significant timescale according to the automated search is 1.024 s, with a log likelihood ratio of 76 and a location consistent with the Swift-BAT event. The time-averaged spectrum from T0-0.256 s to T0+0.896 s is adequately fit by a Band function with Epeak = 14 +/- 6 keV, alpha = -1.0 (fixed), and beta = -2.40 +/- 0.21. Because the peak energy is close to the low energy threshold of GBM, the low energy photon index is unconstrained. We fix it to the median value of the GBM GRB sample, however it has no significant effect on the values for Epeak and beta. The event fluence (10-1000 keV) in this time interval is(2.25 +/- 0.38)E-07 erg/cm^2. T0 here is 2020-10-15T22:50:13.22 UT = 624495018.22 (MET) [1] Goldstein et al. 2019 arXiv:1903.12597
GCN 28664 table
GRB_name GRB201015A
GCN_number 28664
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 28664 SUBJECT: GRB 201015A: FRAM-ORM afterglow detection DATE: 20/10/17 06:24:03 GMT FROM: Martin Jelinek at Astro.Inst-AVCR,Ondrejov Martin Jelinek and Jan Strobl (ASU CAS Ondrejov, CZ), Sergey Karpov, Martin Masek, Petr Janecek, Jakub Jurysek, Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza (Institute of Physics, Prague, CZ) report: The 25cm robotic telescope FRAM-ORM at La Palma (Spain) reacted robotically to the alert of GRB201015A (D'Elia et al GCNC 28632), obtaining a series of 20 s unfiltered images starting at 22:50:50.8 UT, i.e. 37.6s post trigger. We clearly detect the source reported by other telescopes (Lipunov et al. GCN 28633, Malesani et al GCN 28637, Ackley et al GCN 28639 and others). As reported before, the brightness of the object reaches a maximum about 5 minutes after the trigger with R ~ 16.5 and then decays until the end of our dataset 2.4 h after the trigger.
GCN 28668 table
GRB_name GRB201015A
GCN_number 28668
Detection_method Optical
redshift 0.4260
Circular_text TITLE: GCN CIRCULAR NUMBER: 28668 SUBJECT: GRB 201015A: classification as long GRB DATE: 20/10/17 12:55:23 GMT FROM: Alexei Pozanenko at IKI, Moscow P. Minaev (IKI) and A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We analyzed GRB 201015A detected by Swift (D'Elia et al., GCN 28632) using GBM/Fermi spectral data (Fletcher et al., GCN 28663) and redshift of z = 0.426 (de Ugarte Postigo et al., GCN 28649; Izzo et al., GCN 28661). GRB 201015A has a low luminosity, Eiso = (1.1 +/- 0.2)*10^50 erg, and well consistent with the Ep,i – Eiso correlation (Amati relation) for type II (long) bursts, see [1] for details and Figure at http://grb.rssi.ru/GRB201015A/GRB201015A_Epi_Eiso.png The position of the burst is within 1-sigma confidence area of the cluster of type II (long) bursts on the EH – T90,i diagram (see [2] for details), indicating strong association with type II bursts, see Figure at http://grb.rssi.ru/GRB201015A/GRB201015A_EH_T90i.png We encourage follow-up optical observations to search for associated supernova. [1] - Minaev et al., MNRAS, 492, 1919, 2020 [2] - Minaev et al., arXiv:2008.12752
GCN 28673 table
GRB_name GRB201015A
GCN_number 28673
Detection_method Optical
redshift 0.4260
Circular_text TITLE: GCN CIRCULAR NUMBER: 28673 SUBJECT: GRB 201015A: Assy and Mondy optical observations DATE: 20/10/17 15:56:12 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), V. Kim (AFIF, Pulkovo Observatory), A. Pozanenko (IKI), E. Klunko (ISTP), M. Krugov (AFIF), N. Pankov (HSE), A. Volnova (IKI) report on behalf of IKI GRB FuN: We observed GRB 201015A (D'Elia et al., GCN 28632) with AZT-33IK telescope of Mondy observatory in R-filter starting on Oct. 16 (UT) 13:42:54 and with AZT-20 telescope of Assy-Turgen observatory starting on Oct. 16 (UT) 14:51:35 in g',r',i'-filters. The optical afterglow (e.g., Lipunov et al., GCN 28633; Kennea et al., GCN 28635; Malesani et al., GCN 28637; Ackley et al., GCN 28639; Hu et al., GCN 28645; Zhu et al., GCN 28653) at redshift z=0.426 (de Ugarte Postigo et al., GCN 28649; Izzo et al., GCN 28661) is detected in stacked images in each filter. Preliminary photometry of the afterglow is following Date UT start t-T0 Filter Exp. OT Err. UL (3sigma) (mid, days) (s) 2020-10-16 13:42:54 0.64075 R 30*120 21.70 0.25 22.0 2020-10-16 14:51:35 0.68081 r'(AB) 36*60 21.85 0.14 23.5 2020-10-16 15:02:53 0.68796 g'(AB) 36*60 22.10 0.10 23.7 The photometry is based on the nearby stars of PanSTARRS-PS1 catalog. RA, DEC, g, r, i 23:37:17.49934 +53:24:05.6357 18.6327 17.7832 17.4125 23:37:21.06032 +53:24:57.1308 19.4472 18.4947 18.0340
GCN 28674 table
GRB_name GRB201015A
GCN_number 28674
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 28674 SUBJECT: GRB 201015A NUTTelA-TAO / BSTI Early Measurements (Preliminary) DATE: 20/10/18 00:01:47 GMT FROM: Bruce Grossan at LBNL/UCB SSL B. Grossan (UCB, NU) , Z. Maksut (NU), A. Kim (NU), M. Krugov (FAI), G. F. Smoot (HKUST, UCB, NU), E. Linder (UCB, NU), report on behalf of the Energetic Cosmos Laboratory: The Nazarbayev University Transient Telescope at Assy-Turgen Astrophysical Observatory (NUTTelA-TAO) pointed at GRB201015A on receipt of an automated GCN / BAT position alert. We report measurements made with the Burst Simultaneous Three-Channel Imager (BSTI; Grossan, Kumar & Smoot 2019, JHEA, 32,14) instrument ***during commissioning phase*** and we note cautions with these measurements below. Calibration with bright Pan-STARRS catalog I stars on our images, for our standard SDSS filters yields, without color corrections, the following photometric values for the OT: tc-t0(s) g'(mag) r'(mag) i'(mag) -------- ------- -------- ------------ 73.2 UL17.8 17.79 17.67 103.2 UL17.8 18.16 17.86 157.6 17.91 16.81 16.96 202.6 17.76 16.63 16.75 247.6 17.94 16.86 16.85 292.6 17.89 17.29 16.87 337.6 17.76 17.02 17.01 382.6 18.21 17.31 17.05 427.6 18.07 17.49 17.16 472.6 18.08 17.56 17.29 517.6 18.31 17.60 17.48 562.6 18.14 17.90 17.66 607.6 18.61 18.00 17.49 652.6 UL18.2 18.13 17.85 697.6 UL18.2 18.37 18.00 742.6 UL18.2 18.53 18.02 787.6 UL18.2 18.45 18.06 832.6 UL18.2 18.41 18.34 877.6 UL18.2 18.71 UL17.9 922.6 UL18.2 18.85 18.21 967.6 UL18.2 UL18.2 18.26 1012.6 UL18.2 UL18.2 UL17.8 1057.6 UL18.2 UL18.2 UL17.8 1102.6 UL18.2 UL18.2 UL17.8 1147.6 UL18.2 UL18.2 UL17.8 1192.6 UL18.2 UL18.3 UL17.8 UL = 5 sigma upper limit Uncertainties are estimated at ~ 0.1 mag for r',i'; unfortunately at this time we have indications of errors ~ 0.15 mag for g'. tc-t0 = trigger time minus image center time. We have not yet established the accurracy of our times. The first two co-adds are 30 s in duration; the rest are 45 s. The peak in r' at ~200 s is roughly consistent with that of other observers (e.g. see Dong Xu, 2020, GCN 28653), but for precise comparisons see cautionary notes below. These measurements are likely among the earliest multi-channel simultaneous optical measurements of GRBs. We encourage additional measurements at all wavelengths to add to these data. We caution the reader that the BSTI instrument is in commissioning phase, with known imperfections, and we have not extensively tested our results, e.g. against other simultaneous measurements, or near our detection limits. Please also note that the times are approximate. We anticipate additional refinement and improvement in analysis in 15-30 days posted at http://ecl.nu.edu.kz/gamma-ray-burst/grb201015A. ---------------------------------- UCB = University of California, Berkeley, USA NU = Nazarbayev University, Nur-Sultan, Kazakhstan HKUST = Hong Kong University of Science and Technology FAI = Fesenkov Astrophysical Institute, Kazakhstan The NUTTelA-TAO Team acknowledges the support of the staff of the Assy-Turgen Astrophysical Observatory, Almaty, Kazakhstan, and the Fesenkov Astrophysical Institute, Almaty, Kazkhstan.
GCN 28676 table
GRB_name GRB201015A
GCN_number 28676
Detection_method Optical
ra 354.3181°
decl 53.4155°
Circular_text TITLE: GCN CIRCULAR NUMBER: 28676 SUBJECT: GRB 201015A: MMT afterglow imaging DATE: 20/10/18 03:28:43 GMT FROM: Jillian Rastinejad at Northwestern Univ. J. Rastinejad, K. Paterson, C. D. Kilpatrick and W. Fong (Northwestern) report: ''We observed the location of Swift GRB 201015A (D'Elia et al., GCN 28632; Markwardt et al., GCN 28658) with the Binospec imager and spectrograph mounted on the MMT 6.5-meter telescope on Mount Hopkins, Arizona. We obtain 6x120-sec imaging in the i-band and 9x120-sec imaging in the z-band at mid-times of 2020 October 17.365 (1.41 days post-burst) and 2020 October 17.342 (1.39 days post-burst), respectively. Within the XRT position (Evans et al. GCN 28647), we detect the previously reported optical afterglow (Lipunov et al. GCN 28633; Malesani et al; GCN 28637, Hu et al.; GCN 28645, Zhu et al.; GCN 28653; Belkin et al. GCN 28656; Jelinek et al., GCN 28664; Belkin et al., GCN 28673). Calibrated to PS1, we measure i = 22.2 +/- 0.1 mag and z = 21.9 +/- 0.1 mag (AB system and not corrected for Galactic extinction in the direction of the burst). In addition to the afterglow, emission extending directly to the southwest of the afterglow position is weakly detected in both bands, at around RA(J2000) = 23:37:16.35, Dec(J2000)=+53:24:55.7. Given its proximity to the afterglow, this may be the host galaxy of GRB 201015A; however our imaging cannot resolve the afterglow from this extended emission. We also detect the brighter galaxy, previously mentioned in Belkin et al. (GCN 28656) and also detected in archival PS1 imaging at an offset of 2.3'' from the afterglow position (Malesani et al., GCN 28637). Given the large offset from the afterglow (13 kpc at z=0.42; de Ugarte Postigo et al., GCN 28649, Izzo et al., GCN 28661), we consider that this source is less likely to be related to the GRB. Further observations are planned. We thank Skyler Self and Ben Weiner at the MMT for the rapid scheduling and execution of these observations.''
GCN 28677 table
GRB_name GRB201015A
GCN_number 28677
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 28677 SUBJECT: GRB 201015A: Xinglong-2.16m optical observations DATE: 20/10/18 06:29:12 GMT FROM: Dong Xu at NAOC/CAS Z.P. Zhu (NAOC, HUST), X. Liu, S.Y. Fu, D. Xu (NAOC) report: We observed the field of GRB 201015A (D'Elia et al., GCN 28632; Kennea et al., GCN 28635) using the Xinglong-2.16m telescope equipped with the BFOSC. Observations were carried out starting at 10:35:46 UT on 2020-10-16 (i.e., about 11.2 hr after the BAT trigger), and 13x300s R-band frames were obtained. The GRB optical afterglow (e.g., Lipunov et al., GCN 28633; Malesani et al., GCN 28637; Ackley et al., GCN 28639; Hu et al., GCN 28645; Zhu et al., GCN 28653; Belkin et al., GCN 28673; Jelinek et al., GCN 28664; Marshall et al., GCN 28662; Belkin et al., GCN 28656; Grossan et al., GCN 28674) is weakly detected in our stacked image, with R = 22.0 +/- 0.3 at T-mid=12.10 hr, calibrated with the nearby Pan-STARRS field. We acknowledge the support of the staff of the Xinglong-2.16m telescope, in particular J. Zheng and A.Y. Zhou.
GCN 28680 table
GRB_name GRB201015A
GCN_number 28680
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 28680 SUBJECT: GRB 201015A: HCT optical photometric follow-up DATE: 20/10/18 15:11:04 GMT FROM: Harsh Kumar at Indian Inst of Tech,Bombay H. Kumar (IITB), D. K. Sahu (IIA), R. Gupta (ARIES), V. Shenoy (IITB), B. Kumar (ARIES), S. Kiran (IIA), G. C. Anupama (IIA), V. Bhalerao (IITB), S.B. Pandey (ARIES), S. Barway (IIA), report on behalf of the HCT team: We observed GRB 201015A reported by Swift-BAT (V. D'Elia et al., GCN 28632; also see: V. Lipunov et al., GCN 28633; J.A. Kennea et al., GCN 28635; D. B. Malesani et al., GCN 28637; K. Ackley et al., GCN 28639; Y.-D. Hu et al., GCN 28645; P.A. Evans et al., GCN 28647; A. de Ugarte Postigo et al., GCN 28649; Z.P. Zhu et al., GCN 28653; S. Belkin et al., GCN 28656; C. B. Markwardt et al., GCN 28658; A. D'Ai et al., GCN 28660; L. Izzo et al., GCN 28661; F. E. Marshall et al., GCN 28662; C. Fletcher et al., GCN 28663; Martin Jelinek and Jan Strobl et al., GCN 28664; P. Minaev et al., GCN 28668; S. Belkin et al., GCN 28673; B. Grossan et al., GCN 28674; J. Rastinejad et al., GCN 28676; Z.P. Zhu et al., GCN 28677) with 2.0 m Himalayan Chandra Telescope (HCT). The field was observed in the V and Rc filter starting at 2020-10-16T17:54:14.936 UT i.e. ~19 hrs after the event detection by Swift-BAT. We obtained 9 x 60 sec in Rc and 120 x 9 in the V band. We clearly detected the source in the stacked image. We obtained the following photometric results:- ------------------------------------------------------------------ JD(Mean) | Filter | Mag | Total exposure (sec) | ------------------------------------------------------------------ 2459139.250567 | V | 21.56 +/- 0.1 | 60 x 9 2459139.262356 | Rc | 21.33 +/- 0.04 | 120 x 9 ------------------------------------------------------------------ These observations were carried out under the ToO program HCT-2020-C3-P6. We thank HCT staff for conducting the observations.
GCN 28681 table
GRB_name GRB201015A
GCN_number 28681
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 28681 SUBJECT: GRB 201015A: GROWTH-India Telescope (GIT) upper limit DATE: 20/10/18 19:03:03 GMT FROM: Harsh Kumar at Indian Inst of Tech,Bombay H. Kumar (IITB), U. Stanzin(IAO), V. Bhalerao (IITB), G. C. Anupama (IIA), S. Barway (IIA) report on behalf of the GROWTH-India collaboration: We observed GRB 201015A reported by Swift-BAT (V. D'Elia et al., GCN 28632; also see: V. Lipunov et al., GCN 28633; J.A. Kennea et al., GCN 28635; D. B. Malesani et al., GCN 28637; K. Ackley et al., GCN 28639; Y.-D. Hu et al., GCN 28645; P.A. Evans et al., GCN 28647; A. de Ugarte Postigo et al., GCN 28649; Z.P. Zhu et al., GCN 28653; S. Belkin et al., GCN 28656; C. B. Markwardt et al., GCN 28658; A. D'Ai et al., GCN 28660; L. Izzo et al., GCN 28661; F. E. Marshall et al., GCN 28662; C. Fletcher et al., GCN 28663; Martin Jelinek and Jan Strobl et al., GCN 28664; P. Minaev et al., GCN 28668; S. Belkin et al., GCN 28673; B. Grossan et al., GCN 28674; J. Rastinejad et al., GCN 28676; Z.P. Zhu et al., GCN 28677, H. Kumar et al., GCN 28680) with 0.7m GROWTH-India Telescope (GIT). The field was observed in the SDSS r’ filter starting at 2020-10-16T20:21:44.41 UT i.e. ~ 21.5 hrs after the event detection by Swift-BAT. We obtained 10 exposures of 300 sec each. We did not find any source in the stacked image up to r’ > 20.97 mag (5-sigma) within the uncertainty region, calibrated against PanSTARRs PS1 data release (Flewelling et al., 2018). The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics and the Indian Institute of Technology Bombay with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA).
GCN 28688 table
GRB_name GRB201015A
GCN_number 28688
Detection_method Optical
ra 354.3184°
decl 53.4157°
Circular_text TITLE: GCN CIRCULAR NUMBER: 28688 SUBJECT: GRB 201015A: 6 GHz VLA radio afterglow candidate detection DATE: 20/10/19 14:53:30 GMT FROM: Wen-fai Fong at Northwestern U W. Fong, G. Schroeder, J. Rastinejad, and A. Hajela (Northwestern) report: "We observed the position of GRB 201015A (D'Elia et al., GCN 28632; Markwardt et al., GCN 28658) with the Karl G. Jansky Very Large Array (VLA) beginning on 2020 Oct 17.364 UT (1.41 days post-burst) at a mean frequency of 6 GHz. We detect a bright, uncatalogued radio source with a flux density of ~0.13 milliJy at the position: RA(J2000) = 23:37:16.41 Dec(J2000) = +53:24:56.4 with an uncertainty of ~0.3" in each coordinate. This position is consistent with optical afterglow position reported by NOT (Malesani et al., GCN 28637), and the XRT position (Evans et al. GCN 28647). We propose this source as the radio afterglow of GRB 201015A. We thank the VLA staff for quickly approving and executing these observations."
GCN 28721 table
GRB_name GRB201015A
GCN_number 28721
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 28721 SUBJECT: GRB 201015A: SAO RAS optical observations DATE: 20/10/21 13:48:37 GMT FROM: Moskvitin Alexander at SAO RAS A. S. Moskvitin, V. N. Aitov (SAO RAS) on behalf of GRB follow-up team report. We observed the field of the GRB 201015A (D'Elia et al., GCN #28632) with the 1-m telescope of SAO RAS, Zeiss-1000 + Multi-Mode Photometer-Polarimeter on October 16, 19:46:23--20:49:31 UT, t_mid - T0 = 0.89426 days. The GRB OT (Lipunov et al., GCN #28633; Malesani et al., GCN #28637; Ackley et al., GCN #28639; Hu et al., GCN #28645; de Ugarte Postigo, GCN #28649; Zhu et al., GCN #28653; Belkin et al., GCN #28656; Izzo et al., GCN #28661; Marshall & D'Elia, GCN #28662; Jelinek et al., GCN #28664; Belkin et al., GCN #28673; Grossan et al., GCN #28674; Rastinejad et al., GCN #28676; Zhu et al., GCN #28677; Kumar et al, #GCN 28680) is detected in the stacked image. Preliminary photometry of the OT is R = 21.69 +/- 0.05 (based on standards from Belkin et al., GCNs #28656, #28673).
GCN 28822 table
GRB_name GRB201015A
GCN_number 28822
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 28822 SUBJECT: GRB 201015A: Late X-ray Detections with Chandra DATE: 20/11/03 16:45:05 GMT FROM: Ben Gompertz at U of Warwick B. Gompertz (1); A. Levan (2); N. Tanvir (3); A. Fruchter (4); A. Cucchiara (5); J. Greiner (6); J. Hjorth (7); T. Kangas (4); G. Lamb (3); J. Lyman (1); S. Oates (8); P. O'Brien (3); J. Osborne (3); K. Page (3); D. Perley (9); E. Pian (10); D. Steeghs (1); K. Wiersema (1); G. Wynn (3) ((1) University of Warwick, (2) Radboud University, (3) University of Leicester, (4) Space Telescope Science Institute, (5) University of the Virgin Islands, (6) MPE Garching, (7) University of Copenhagen, (8) University of Birmingham, (9) Liverpool John Moores University, (10) INAF-OAS) report: We observed the position of GRB 201015A (D'Elia et al., GCN 28632) with the Chandra X-ray Observatory with epochs 8.4 and 13.6 days after trigger. The X-ray afterglow is clearly detected with a flux around 100x brighter than expected based on the extrapolation of the early XRT data taken between 0.03 and 0.8 days after burst. The source is seen to fade between the two Chandra epochs with a power-law index of approximately -0.8. A Swift ToO has been approved.
GCN 28857 table
GRB_name GRB201015A
GCN_number 28857
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 28857 SUBJECT: GRB 201015A: Swift-XRT late time observations DATE: 20/11/06 17:24:55 GMT FROM: Valerio D'Elia at ASDC V. D’Elia (SSDC) reports on behalf of the Swift team: Following the Chandra late time detection (Gompertz et al., GCN Circ. 28822) of GRB 201015A (D’Elia et al., GCN Circ. 28632), Swift performed a ToO observation of its X-ray afterglow. 13 ks of data were acquired between 3 and 6 November, i.e., 18-21 days after the trigger. Consistent with the prediction reported by Gompertz et al., XRT detected the afterglow at a level of (7+/-3)E-4 cts/s. This is an official product of the Swift-XRT team. [GCN OPS NOTE(06nov2020): Per author's request, the tail end containing the signiture block was removed.]
GCN 28939 table
GRB_name GRB201015A
GCN_number 28939
Detection_method Other
ra 354.3184°
decl 53.4157°
Circular_text TITLE: GCN CIRCULAR NUMBER: 28939 SUBJECT: GRB 201015A radio afterglow with e-MERLIN DATE: 20/11/21 09:28:54 GMT FROM: Stefano Giarratana at University of Bologna S. Giarratana (Univ. of Bologna, INAF/IRA), M. Giroletti (INAF/IRA), B. Marcote (JIV-ERIC), G. Ghirlanda (INAF/OABrera), M. Ribó (Univ. of Barcelona), J.M. Paredes (Univ. of Barcelona) On UT 2020 November 5 and 8 we observed the radio counterpart of the GRB 201015A (D’Elia V. et al., GCN Circ. 28632) with e-MERLIN at 5 GHz. We detect a point-like source at a position consistent with the VLA GRB 201015A afterglow coordinates (RA(J2000) = 23:37:16.41, Dec(J2000)= +53:24:56.4, Fong W. et al., GCN Circ. 28688). Preliminary analysis indicates a significance of the detection of 4.5 and 3.3 sigma confidence for November 5 and 8 observations respectively. We note that the noise level in the November 8 observation is 20% higher than on November 5. Additional radio observations are in progress. We would like to thank the e-MERLIN personnel for approving, executing, and processing these observations.
GCN 28945 table
GRB_name GRB201015A
GCN_number 28945
Detection_method VLA Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 28945 SUBJECT: GRB 201015A L-band observations with e-MERLIN DATE: 20/11/23 10:44:45 GMT FROM: Lauren Rhodes at Oxford L. Rhodes, R. Fender (Oxford), J. Bray and D.R.A. Williams (JBCA) report: e-MERLIN observed the position of GRB 201015A (D'Elia et al., GCN Circ. 28632) at 1.5GHz at 19 and 23 days post burst. Both epochs show a point source with coordinates consistent with those from the VLA detection (Fong et al., GCN Circ. 28688). The flux densities of the detections are 214+/-25uJy and 256+/-27uJy for epochs 1 and 2, respectively. We tentatively attribute the observed emission to the GRBs host galaxy as there is very little variation in the flux density between our two epochs. There is also no significant variation between our detections and that from Fong et al., when using an optically thin spectrum to scale between the two observing bands. We are in the process of obtaining further radio observations. We thank the e-MERLIN staff for the time allocation and their assistance with the observations.
GCN 29028 table
GRB_name GRB201015A
GCN_number 29028
Detection_method Other
ra 354.3184°
decl 53.4157°
Circular_text TITLE: GCN CIRCULAR NUMBER: 29028 SUBJECT: GRB 201015A: 5-GHz radio afterglow detection with the EVN DATE: 20/12/11 17:07:03 GMT FROM: Benito Marcote at JIVE B. Marcote (JIVE), M. Ribó (Univ. of Barcelona), J. M. Paredes (Univ. of Barcelona), M. Giroletti (INAF/IRA), S. Giarratana (Univ. of Bologna, INAF/IRA), G. Ghirlanda (INAF/OABrera) We observed the radio counterpart of GRB 201015A (D'Elia et al., GCN 28632) with the European VLBI Network (EVN) on 9 November 2020 and 1 December 2020 at a central frequency of 5.0 GHz. Preliminary analysis reports the detection of a compact radio source at a >8-sigma confidence level in both epochs at a consistent position of: RA (J2000) = 23h37m16.4223s Dec (J2000) = +53d24'56.439" With an uncertainty of ~1 mas on each coordinate. The synthesized beams are 1.1 x 2.1 mas (PA = 7.1 deg) and 3.1 x 3.6 mas (PA = -29 deg) for the first and second epoch, respectively. We note that this position is consistent with the one previously reported by the VLA (Fong et al. GCN 28688) and eMERLIN (Giarratana et al. GCN 28939). Further analysis is in progress. We thank the directors and staff of all the EVN telescopes for making this target of opportunity observation possible. The European VLBI Network is a joint facility of independent European, African, Asian, and North American radio astronomy institutes. Scientific results from data presented in this publication are derived from the following EVN project code: RM016. e-VLBI research infrastructure in Europe is supported by the European Union’s Seventh Framework Programme (FP7/2007-2013) under grant agreement number RI-261525 NEXPReS. e-MERLIN is a National Facility operated by the University of Manchester at Jodrell Bank Observatory on behalf of STFC.
GCN 29033 table
GRB_name GRB201015A
GCN_number 29033
Detection_method Optical
redshift 0.4260
Circular_text TITLE: GCN CIRCULAR NUMBER: 29033 SUBJECT: GRB 201015A: optical observations and supernova identification DATE: 20/12/12 23:11:17 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI), S. Belkin (IKI, HSE), A. Volnova (IKI), A. Moskvitin (SAO RAS), O. Burhonov (UBAI), V. Kim (FAI), M. Krugov (FAI), V. Rumyantsev (CrAO), E. Klunko (ISTP), R. Ya. Inasaridze (AbAO), I. Reva (FAI), P. Minaev (IKI), N. Pankov (HSE), Sh. Ehgamberdiev (UBAI) report on behalf of GRB IKI FuN: We observed the GRB 201015A (D'Elia et al., GCN 28632) with ZTSh 2.6m telescope of CrAO observatory, AZT-33IK of Mondy observatory, AZT-20 of Assy observatory, AS-32 of Abastumani observatory, Zeiss-1000 of SAO RAS, AZT-22 of Maidanak observatory, and Zeiss-1000(E) of TSHAO. The optical transient of GRB 201015A (Lipunov et al., GCN 28633; Kennea et al., GCN 28635; Malesani et al., GCN 28637; Ackley et al., GCN 28639; Hu et al., GCN 28645; Zhu et al., GCN 28653; Belkin et al., 28656; Marshall et al., GCN 28662; Jelinek et al., GCN 28664; Belkin et al., GCN 28673; Grossan et al., GCN 28674; Rastinejad et al., GCN 28676; Zhu et al., GCN 28677; Kumar et al., GCN 28680; Kumar et al., GCN 28681; Moskvitin et al., GCN 28721) at redshift z=0.426 (de Ugarte Postigo et al., GCN 28649; Izzo et al., GCN 28661) is not spatially resolved in most of our images besides a few imaging in Maidanak observatory between Oct. 26 - Nov. 6 when observations were carried out under good weather conditions (FWHM = 0.8 - 0.9 arcsec). The finding chart of stacked image obtained in Maidanak observatory on Oct. 26, Nov. 4 and Nov. 6 is presented in the left panel of the Figure 1. http://grb.rssi.ru/GRB201015A/GRB201015A_SN_imaging.png (In all of the stacked images in the Figure 1 we subtracted nearby stars which positions are designated by white and green circles. The white circles denote the stars presented in PS DR1 catalogue, and the green circle denote the star is not presented in PS DR1. Stacked images of Zeiss-1000 of SAO RAS observations on 32 days (central panel) and 47 days (right panel) are also presented in the Figure 1.) Using the stacked image of Maidanak observations (left panel of the Figure 1, an upper limit of the image is R=24.6) we obtained photometry of the nearby stars. The photometry of the stars is used for flux subtraction to obtain R-magnitudes of unresolved optical transient in all of observations, and a light curve of the optical transient is presented in Figure 2 http://grb.rssi.ru/GRB201015A/GRB201015A_SN_LC.png The light curve is preliminary and represent the joint photometry of the optical transient and a possible host galaxy. The source raised on in the left panel of the Figure 1 (red circle) coincides with an afterglow coordinates of GRB 201015A reported by NOT observation (Malesani et al., GCN 28637). We suggest the object clearly visible on Oct.26 - Nov.6 at the place of the afterglow is a supernova associated with GRB 201015A. The light curve in the Figure 2 suggests the supernova maximum between 12 and 20 days after GRB trigger. The supernova identification rules out the GRB 201015A as a questionable short burst with extended emission (Markwardt et al., GCN 28658) and corroborates the GRB 201015A as a long duration burst (Minaev et al., GCN 28668). The afterglow in the first two days after the trigger can be approximated by a power law with the index of -0.91 ± 0.03. We apologize for late report due to delay of Maidanak data which is critical for supernova identification.
GCN 29306 table
GRB_name GRB201015A
GCN_number 29306
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 29306 SUBJECT: GRB 201015A: evidence of supernova in LBT spectra DATE: 21/01/17 02:05:04 GMT FROM: Andrea Rossi at INAF A. Rossi (INAF/OAS), S. Benetti (INAF-Padova), E. Palazzi (INAF/OAS), P. D'Avanzo (INAF-OAB), V. D'Elia (SSDC), and M. De Pasquale report on behalf of the CIBO collaboration: We report the results of the photometric and spectroscopic follow-up of GRB 201015A (D'Elia et al. GCN 28632) at z = 0.42 (Izzo et al. GCN 28661, de Ugarte Postigo et al. GCN 28649) obtained with the Multi-Object Double Spectrographs (MODS) instrument mounted on the 2x8.4-m LBT telescope (Mt Graham, AZ, USA). Data were obtained at the mid time of 04:00 UT on 2020-11-13, ~28.8 days after the burst trigger. Spectroscopy of the source was obtained for a total of 8x900 s, covering the wavelength range 3200-10000 AA. All the spectra have been corrected for the Galactic extinction (A_V = 0.93). The low S/N spectrum shows a peak around 5400 AA (rest frame) and is consistent with type Ic-BL supernova spectra around maximum light, in agreement with the results presented by Pozanenko et al. (GCN 29033). Together with the spectroscopy we also obtained g and r-band imaging of the supernova, which thanks to the good seeing of 0.6" it is separated enough from the host galaxy to avoid contamination. We find r=23.5+-0.1 for the SN and r=22.9+-0.2 for the host galaxy, calibrated against Pan-STARRS field stars. We acknowledge the excellent support from the LBTO in particular D. Thompson, and from the LBT-INAF staff, particularly S. Paiano, F. Cusano, D. Paris and L. Cassarà in obtaining and reducing these observations.