GRB170105A

This page lists all entries on GRB170105A in GRBweb

Summary IPN GCN 20387 GCN 20389 GCN 20406 GCN 20412 GCN 20413 GCN 20415 GCN 20417 GCN 20421 GCN 20425 GCN 20434 GCN 20507

Summary table
Variable Value Source
T0 6:14:07 UTC GCN_circulars,IPN Triangulation
ra 138.3042° IPN
decl 61.1000° IPN
pos_error 5.00e-02° IPN
GBM_located False
mjd 57758.25980324074 GCN_circulars,IPN Triangulation
IPN table
GRB_name GRB170105A
ra 138.3042°
decl 61.1000°
pos_error 5.00e-02°
GCN 20387 table
GRB_name GRB170105A
GCN_number 20387
Detection_method Konus-Wind Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 20387 SUBJECT: GRB 170105A: POLAR Observation DATE: 17/01/07 06:44:37 GMT FROM: Radek Marcinkowski at PSI/POLAR R. Marcinkowski (PSI), H. Xiao (PSI) and W. Hajdas (PSI) report on behalf of the POLAR collaboration: At 2017-01-05T06:14:07.0 UT(T0), during a routine on-ground search of data, POLAR detected the GRB 170105A, which was also observed by SPIACS at 2017-01-05T06:14:06 and Konus-Wind at 22450.264s UT (06:14:10.264). The POLAR light curve consists of 1 peak with duration (T90) of 2.0 +/- 0.5 s measured from T0. The 0.5 s peak flux at T0 + 0.8 s is equal to 2490 +/- 90 counts/sec. POLAR recorded 3600 +/- 160 events from the burst. Above measurements are in the energy range of about 80 - 500 keV. LC_URL: http://polar.psi.ch/triggers/GRB_170105A_raw.png or http://polar.psi.ch/pub/lc.php?event=GRB+170105A The analysis results presented above are preliminary. Calibration of the instrument is ongoing. POLAR is a dedicated Gamma-Ray Burst polarimeter which was launched on-board the Chinese space laboratory Tiangong-2 (TG-2) on Sep 15, 2016. The energy detection range of POLAR is ~ 50-500 keV. More information about POLAR can be found at http://polar.psi.ch/pub , http://polar.ihep.ac.cn/en/ and http://isdc.unige.ch/polar/ . This message is quotable in publications.
GCN 20389 table
GRB_name GRB170105A
GCN_number 20389
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 20389 SUBJECT: GRB 170105A: AstroSat CZTI detection DATE: 17/01/07 13:28:52 GMT FROM: Vidushi Sharma at IUCAA V. Sharma, V. Bhalerao and D. Bhattacharya (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data showed clear detection of GRB170105A (POLAR Observation: R. Marcinkowski et al., GCN Circ. 20387) in the 40-200 keV energy range. The light curve shows a single peak structure with main peak at 06:14:06 UT in the quadrant A and B only, ~1 sec before the POLAR trigger at 06:14:07 UT. The measured peak count rate is 305.46 counts/sec above the background in combined data of four quadrants, with a total of 762 counts. The local mean background count rate was 287.54 counts/sec. Using cumulative rates, we measure a T90 of 2.86 secs. 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.
GCN 20406 table
GRB_name GRB170105A
GCN_number 20406
Detection_method IPN Triangulation
t_trigger 6:14:07 UTC
ra 129.7490°
decl 27.9040°
Circular_text TITLE: GCN CIRCULAR NUMBER: 20406 SUBJECT: LIGO/Virgo G268556: IPN Triangulation of GRB 170105A (association with ATLAS17aeu) DATE: 17/01/09 16:38:27 GMT FROM: Dmitry Svinkin at Ioffe Institute D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Tsvetkova, A. Kozlova, and T. Cline on behalf of the Konus-Wind team, K. Hurley, on behalf of the IPN, and A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, report: The long-duration, soft-spectrum GRB 170105A was detected by POLAR (Marcinkowski et al., GCN Circ. 20387), AstroSat (CZTI; Sharma et al., GCN Circ. 20389), Konus-Wind, and INTEGRAL (SPI-ACS) at about 22447 s UT (06:14:07). We have triangulated this GRB to a Konus-INTEGRAL annulus centered at RA(2000)=129.749 deg (08h 38m 60s) Dec(2000)=+27.904 deg (+27d 54' 14"), whose radius is 34.255(-14.832,+1.812) deg (3 sigma). This localization may be improved. The distance between the annulus center line and the ATLAS17aeu optical transient reported by Tonry et al. (LVC Circ. 20382) is 0.57 degrees, strengthening the association of the transient with the GRB initially suggested by Kasliwal et al. (LVC Circ. 20393). A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB170105_T22450/IPN/. As observed by Konus-Wind, the burst had a fluence of 2.56(-0.13,+0.18)x10^-6 erg/cm2, and a 64-ms peak energy flux, measured from T0-0.204 s, of 2.47(-0.30,+0.58)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB170105_T22450/.
GCN 20412 table
GRB_name GRB170105A
GCN_number 20412
Detection_method AstroSat CZTI
ra 60.0000°
decl 80.0000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 20412 SUBJECT: GRB170105A: AstroSat CZTI localisation DATE: 17/01/10 05:46:39 GMT FROM: Varun Bhalerao at IUCAA V. Bhalerao and D. Bhattacharya (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Detailed analysis of AstroSat CZTI data for GRB170105A (POLAR Observation: R. Marcinkowski et al., GCN Circ. 20387; CZTI detection: Sharma et al., GCN Circ. 20389) was carried out for localising the GRB. We modelled the counts in various quadrants using a raytracing code based on the instrument geometry. The GRB is localised to a 550 sq. deg. area, centred roughly on RA, Dec = 60, +80. While spectral fits are not possible at the current stage, the data indicate a rather soft spectrum, with strongest detection around 60-80 keV and almost no counts above 100 keV. Along with the T90 measurement in Sharma et al., GCN Circ. 20389, this suggests that GRB170501A was a long GRB. A pdf showing the localisation region is available at: http://www.iucaa.in/~astrosat/czti_grb/GRB170105A/heal/GRB170105A_localisation.pdf A healpix map with the localisation region is available at: http://www.iucaa.in/~astrosat/czti_grb/GRB170105A/heal/GRB170105A_localisation.fits 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.
GCN 20413 table
GRB_name GRB170105A
GCN_number 20413
Detection_method IPN Triangulation
Circular_text TITLE: GCN CIRCULAR NUMBER: 20413 SUBJECT: LIGO/Virgo G268556: ATLAS17aeu position is consistent with GRB170105A DATE: 17/01/10 06:15:41 GMT FROM: Varun Bhalerao at IUCAA Varun Bhalerao (IUCAA), Sujay Mate (IUCAA), Dipankar Bhattacharya (IUCAA), Sukanta Bose (IUCAA), Gulab Chand Dewangan (IUCAA), Ranjeev Misra (IUCAA), Sanjit Mitra (IUCAA), A R Rao (TIFR), Tarun Souradeep (IUCAA), Santosh Vadawale (PRL), on behalf of the Astrosat CZTI team report: Bhalerao et al. (GCN Circ. 20412) have used AstroSat CZTI to infer that GRB170105A is a long GRB, and have localised it to a ~550 square degree region (1-sigma). This region includes 3.9% probability of containing the LIGO trigger G268556, based on the revised LALInference sky map (Greco et al, 20385). The overlap with the IPN triangulation (Svikin et al., GCN Circ. 20406) is about 50 square degrees. The position of ATLAS17aeu (Tonry et al., GCN Circ. 20382) is marginally outside the AstroSat CZTI error region, consistent at better than 1.1 sigma. This further indicates that ATLAS17aeu is the afterglow of GRB170105A (Kasliwal et al., GCN Circ. 20393).
GCN 20415 table
GRB_name GRB170105A
GCN_number 20415
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 20415 SUBJECT: LIGO/Virgo G268556: Swift-XRT confirms that ATLAS17aeu is fading in X-rays DATE: 17/01/10 09:45:26 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester), J.A. Kennea (PSU), S.D. Barthelmy (NASA/GSFC), A.P. Beardmore (U. Leicester), A.A. Breeveld (UCL-MSSL), D.N. Burrows (PSU), S. Campana (INAF-OAB), S.B. Cenko (NASA/GSFC), G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA), P. D'Avanzo (INAF-OAB), V.D'Elia (ASDC), N. Gehrels (NASA/GSFC), P. Giommi (ASI), C. Gronwall (PSU), H.A. Krimm (CRESST/GSFC/USRA), N.P.M. Kuin (UCL-MSSL), A.Y. Lien (GSFC/UMBC), D. Malesani (DARK/NBI), F.E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), B. Mingo (U. Leicester), J.A. Nousek (PSU), S.R. Oates (U. Warwick), P.T. O'Brien (U. Leicester), J.P. Osborne (U. Leicester), C. Pagani (U. Leicester), K.L. Page (U.Leicester), D.M. Palmer (LANL), M. Perri (ASDC), J.L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU), M.H. Siegel (PSU), G. Tagliaferri (INAF-OAB), E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team: Swift has continued to observed ATLAS17aeu (Tonry et al., LVC Circ. 20382), gathering a total of 21.3 ks of data, from T0+222 ks to T0+470 ks (where T0 is the GW trigger time). The X-ray counterpart (Evans et al., LVC Circ. 20390) is now confirmed to be fading. Assuming the trigger time from the GW event (LVC Circ. 20364) the light curve is decaying with a power-law index of 2.2 (+1.1, -1.2). If instead we take T0 from GRB 170105A (Marcinkowski et al., GCN Circ. 20387), the decay index is 1.7 (+1.1, -0.9). At the mid-point of the latest observation, GW_T0+453 ks (=GRB_T0+381 ks) the 0.3-10 keV XRT count-rate was 0.0017 (+/- 0.0006) ct/sec. A spectrum compiled from the data can be fitted with an absorbed power-law, with NH consistent with the Galactic value of 4.6e20 cm^-2 (Willingale et al. 2013) and photon index Gamma=1.60 (+0.4, -0.3). Using this spectrum the count-rate above corresponds to an observed (unabsorbed) 0.3-10 keV flux of (6.7+/-2.4)e-14 ( [7.2+/-2.6]e-14) erg cm^-2 s^-1. The spectral and temporal indices are consistent with the values typically seen for X-ray GRB afterglows (e.g. the Swift-XRT GRB catalogue: http://www.swift.ac.uk/xrt_live_cat/; Evans et al. 2009). This circular is an official product of the Swift GW follow up team.
GCN 20417 table
GRB_name GRB170105A
GCN_number 20417
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 20417 SUBJECT: LIGO/Virgo G268556: NOWT of EWE, Xinglong 0.6/0.9m, Xuyi 1m optical upper limits of ATLAS17aeu and a reminder of GCN 20394 DATE: 17/01/10 15:22:53 GMT FROM: Jinzhong Liu at Xinjiang Astronomical Observatory D. Xu (NAOC/CAS), J.Z. Liu, H.B. Niu, Y. Zhang, X. Zhang, G.X. Pu, S.G. Ma, T.Z. Yang, F.F. Song (XAO), X. Zhou, T.M. Zhang (NAOC/CAS), H.B. Zhao, B. Li, G.T. Zhaori (PMO), J.M. Bai, J.R. Mao (YNAO) report on behalf of a Chinese Gravitational Wave collaboration: We have performed tiled observations of LIGO/Virgo G268556 (LVC, GCN 20364) using the Nanshan One-meter Wide field Telescope (NOWT), Xinjiang, China, the 0.6/0.9-m Schmidt telescope at Xinglong, Hebei, China, and the 1-m telescope at Xuyi, Jiangsu, China. The Nanshan 1-m has a FOV of 1.3x1.3 deg^2, and covered the position of ATLAS17aeu (Tonry et al. GCN 20382), the potential optical afterglow of GRB 170105A (e.g., Marcinkowski et al., GCN 20387; Sharma et al., GCN 20389; Kasliwal, et al., GCN 20393), in a single night. We obtained an upper limit of m(V)>20.0 mag (3 sigma) at 14:55 UT on 2017-01-07. The 0.6/0.9-m Schmidt telescope has a FOV of 1.5x1.5 deg^2, and covered the position of ATLAS17aeu also in a single night. We obtained an upper limit of m(White)>18.8 mag (5 sigma) at 18:26 UT on 2017-01-08. The Xuyi 1-m has a FOV of 3.0x3.0 deg^2, and covered the position of ATLAS17aeu in a single night. We obtained an upper limit of m(r)>14 mag (3 sigma) at 14:32 UT on 2017-01-09. In addition, we note that the two sources, dubbed EWE001 and EWE002, in GCN 20394, are obviously known sources in several surveys such as DSS II and SDSS. -- N: Jinzhong Liu, Dr. O: Main building, 213 P: 150, Science 1-Street, Urumqi, Xinjiang 830011, China T: 86 991 3689027 D: 2012-07-14 E: optics@xao.ac.cn
GCN 20421 table
GRB_name GRB170105A
GCN_number 20421
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 20421 SUBJECT: LIGO/Virgo G268556: Lijiang Observatory GMG Telescope Upper Limit on ATLAS17aeu DATE: 17/01/10 23:03:21 GMT FROM: Mansi M. Kasliwal at Caltech A.K.H. Kong (NTHU/Oxford), J. Mao, X. Hou, J. Wang, and J.-M. Bai (YNAO) We observed the field of the optical transient ATLAS17aeu (Tonry et al., LVC GCN 20382; Kasliwal et al., GCN 20398) that is within the error region of LIGO/Virgo G268556 (LVC, GCN 20364) with the 2.4-m GMG telescope at the Lijiang Observatory in Yunnan, China. We obtained an R-band image with the Yunnan Faint Object Spectrograph and Camera (YFOSC) on 2017-01-07 14:55:35 UT. ATLAS17aeu was not detected with a 3-sigma limit of about R~23 mag. ATLAS17aeu was detected with i=21.9 mag on 2017-01-07 08:05:33 UT (Kasliwal et al., GCN 20398) and was proposed to be the afterglow of GRB 170105A. Our observation indicates that the source is fainter than the suggested power-law decay. However, due to the use of different filters in ATLAS, Palomar, and Lijiang, the lightcurve should be treated with caution.
GCN 20425 table
GRB_name GRB170105A
GCN_number 20425
Detection_method AMI
Circular_text TITLE: GCN CIRCULAR NUMBER: 20425 SUBJECT: LIGO/Virgo G268556: AMI 15 GHz detection of ATLAS17aeu DATE: 17/01/11 12:58:07 GMT FROM: Kunal Mooley at U of Oxford K. P. Mooley, R. P. Fender (Oxford), A. Horesh (HUJI) report on behalf of a larger collaboration We observed the optical transient ATLAS17aeu (Tonry et al., LVC GCN 20382) located in the error region of LIGO/Virgo G268556 (LVC GCN 20364) with the AMI Large Array on 2017 Jan 07.04 UT. At 15.5 GHz, the flux density of the source is 336+/-20 uJy. We are currently monitoring this source. We thank the AMI staff for scheduling this observation. Since this source is likely the afterglow of GRB 170105A (e.g. Kasliwal et al., LVC GCN 20393; Chambers et al., LVC GCN 20407), we will be updating the AMI-GRB database (http://4pisky.org/ami-grb/) with the measurements.
GCN 20434 table
GRB_name GRB170105A
GCN_number 20434
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 20434 SUBJECT: LIGO/Virgo G268556: Early SWASP limits of ATLAS17aeu DATE: 17/01/11 22:56:15 GMT FROM: Danny Steeghs at U of Warwick/GOTO D.Steeghs, D.Pollacco, K.Ulaczyk, R.Cutter, R.West, A.Levan (U. Warwick), D.K. Galloway, E.Rol, E.Thrane (Monash U.), V.Dhillon, M.Dyer, S.Littlefair, E.Daw, J.Maund, J.Mullaney (U. Sheffield), G.Ramsay (Armagh O.), P.O'Brien, R.Starling (U. Leicester) On behalf of the GOTO collaboration: We have analysed our SWASP imaging related to G268556 (GCN #20364, spanning MJD 57758.043-57758.210) for evidence of ATLAS17aeu. Our first imaging window following G268556 spans 9-5 hours before the reported detections in Tonry et al. (GCN #20382) and end 1 hour before GRB170105A (GCN #20387). We do not find any evidence for an optical source at the ATLAS17aeu position. We combined 3 sets of images not affected by clouds and achieve the following 5-sigma upper limits: MJD (mid): g limit: r limit: 57758.05948013 >17.7 >17.0 57758.09198558 >17.6 >16.9 57758.20992235 >17.0 >16.3 These photometric limits were derived by crossmatching field stars with the APASS survey. Considering the reported optical flux evolution of ATLAS17aeu (GCN #20382, #20393, #20397, #20407, #20416) and extrapolating to earlier times, we would have expected to detect ATLAS17aeu if its peak optical flux preceded GRB170105A. Our non-detections thus further corroborate associating ATLAS17aeu with the optical afterglow of GRB170105A.
GCN 20507 table
GRB_name GRB170105A
GCN_number 20507
Detection_method MAXI Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 20507 SUBJECT: LIGO/Virgo G268556/GW170104: MAXI/GSC observations DATE: 17/01/23 02:51:51 GMT FROM: Motoko Serino at RIKEN/MAXI M. Serino (RIKEN), N. Kawai, S.Sugita (Tokyo Tech), H. Negoro (Nihon U.), S. Ueno, H. Tomida, S. Nakahira, M. Ishikawa, Y. Sugawara (JAXA), Y. E. Nakagawa (JAMSTEC), T. Mihara, M. Sugizaki, W. Iwakiri, M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), N.Isobe, T. Yoshii, Y. Tachibana, Y. Ono, T. Fujiwara, S. Harita, Y. Muraki (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Kawakubo, Y. Kitaoka (AGU), H. Tsunemi, R. Shomura (Osaka U.), M. Nakajima, K. Tanaka, T. Masumitsu, T. Kawase (Nihon U.), Y. Ueda, T. Kawamuro, T. Hori, A. Tanimoto, S. Oda (Kyoto U.), Y. Tsuboi, Y. Nakamura, R. Sasaki (Chuo U.), M. Yamauchi, K. Furuya (Miyazaki U.), K. Yamaoka (Nagoya U.) report on behalf of the MAXI team: We examined the MAXI/GSC all-sky X-ray images (2-20 keV) obtained in the orbit and the day after the LVC trigger G268556/GW170104 at 2017-01-04 10:11:58.599 UTC (GCN 20364). In the 92-min orbit, MAXI/GSC scanned more than 80% of the whole sky, which includes 89.3% of the 90% regions in the bayestar skymap. One day image covers 95.2% of the 90% regions in the bayestar skymap. No significant new source was found in these images. The upper limits for the X-ray flux are different depending on the part of the sky. For instance, typical 2-20 keV 1-sigma (3-sigma) upper limits obtained from the one-orbit and oneday images are 19 (56) mCrab and 5 (16) mCrab, respectively. MAXI/GSC also observed the position of GRB 170105A (GCN Circ. 20377, 20390, 20406). The first scan after the burst was at 2017-01-05T06:47 (UT). No significant emission was observed at the position at the scan. The 1-sigma (3-sigma) upper limits in 2-20 keV are 18 (54) mCrab.