//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22292 SUBJECT: GRB 180102A: Swift detection of a burst DATE: 18/01/02 16:01:33 GMT FROM: David Palmer at LANL K. L. Page (U Leicester), A. A. Breeveld (UCL-MSSL), D. N. Burrows (PSU), A. Deich (PSU), C. Gronwall (PSU), J.D. Gropp (PSU), J. A. Kennea (PSU), H. A. Krimm (NSF/USRA), N. P. M. Kuin (UCL-MSSL), A. Y. Lien (GSFC/UMBC), A. Melandri (INAF-OAB), D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report on behalf of the Swift Team: At 15:49:44 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 180102A (trigger=802999). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 203.115, +62.148 which is RA(J2000) = 13h 32m 28s Dec(J2000) = +62d 08' 53" 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 40 sec. The peak count rate was ~1800 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 15:50:54.4 UT, 70.2 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 203.06761, 62.17091 which is equivalent to: RA(J2000) = 13h 32m 16.23s Dec(J2000) = +62d 10' 15.3" with an uncertainty of 3.8 arcseconds (radius, 90% containment). This location is 114 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 http://www.swift.ac.uk/sper. We cannot determine whether the source is fading at the present time. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 1.88 x 10^20 cm^-2 (Willingale et al. 2013). UVOT took a finding chart exposure of 150 seconds with the White filter starting 73 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers none of the XRT error circle. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.01. Burst Advocate for this burst is K. L. Page (klp5 AT leicester.ac.uk). 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/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22293 SUBJECT: GRB 180102A: Prompt enhanced Swift-XRT position DATE: 18/01/02 16:38:02 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Using promptly downlinked XRT event data for GRB 180102A, we find an enhanced XRT position of the afterglow: RA, Dec: 203.0669, 62.1718 which is equivalent to: RA (J2000) = 13 32 16.07 Dec (J2000) = +62 10 18.6 with an uncertainty of 2.1 arcseconds (radius, 90% confidence). Analysis of the promptly available data is online at http://www.swift.ac.uk/sper/802999. Position enhancement is is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22294 SUBJECT: GRB 180102A: Enhanced Swift-XRT position DATE: 18/01/02 19:39:31 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 611 s of XRT Photon Counting mode data and 1 UVOT images for GRB 180102A, 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 = 203.06658, +62.17177 which is equivalent to: RA (J2000): 13h 32m 15.98s Dec (J2000): +62d 10' 18.4" with an uncertainty of 2.0 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22295 SUBJECT: GRB 180102A: Fermi GBM detection DATE: 18/01/02 20:38:51 GMT FROM: Peter Veres at UAH P. Veres (UAH) reports on behalf of the Fermi GBM Team: "At 15:49:47.21 UT on 2 January 2018, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 180102A (trigger 536600992 / 180102660) which was also detected by Swift/BAT (Page et al., GCN 22292). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 60 degrees. The GBM light curve consists of a single pulse with a duration (T90) of about 16 s (50-300 keV). The time-averaged spectrum from T0-6.1 s to T0+2.0 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.40 +/- 0.44 and the cutoff energy, parameterized as Epeak, is 54.9 +/- 6.7 keV. The event fluence (10-1000 keV) in this time interval is (4.31 +/- 0.45)E-7 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.7 s in the 10-1000 keV band is 1.76 +/- 0.19 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 41.8 +/- 9.2 keV, alpha = 0.59 +/- 1.18 and beta = 2.52 +/- 0.35. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22296 SUBJECT: GRB 180102A: Swift-XRT refined Analysis DATE: 18/01/02 23:26:33 GMT FROM: Phil Evans at U of Leicester A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), D.N. Burrows (PSU), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), J.P. Osborne (U. Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo (INAF-OAB) and K.L. Page report on behalf of the Swift-XRT team: We have analysed 6.7 ks of XRT data for GRB 180102A (Page et al. GCN Circ. 22292), from 82 s to 19.2 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Beardmore et al. (GCN Circ. 22293). The light curve can be modelled with a power-law decay with a decay index of alpha=0.55 (+/-0.06). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.31 (+0.32, -0.30). The best-fitting absorption column is 4.0 (+1.4, -1.2) x 10^21 cm^-2, in excess of the Galactic value of 1.9 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 3.3 x 10^-11 (6.3 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 4.0 (+1.4, -1.2) x 10^21 cm^-2 Galactic foreground: 1.9 x 10^20 cm^-2 Excess significance: 5.2 sigma Photon index: 2.31 (+0.32, -0.30) If the light curve continues to decay with a power-law decay index of 0.55, the count rate at T+24 hours will be 6.5 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x 10^-13 (4.1 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00802999. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22297 SUBJECT: GRB 180102A: MASTER-Net robotic report DATE: 18/01/03 08:10:16 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, N.Tyurina, V.Kornilov, D.Kuvshinov, A.V.Krylov, I.Gorbunov, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D. Vlasenko Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU V.Yurkov, Yu.Sergienko Blagoveschensk Educational State University, Blagoveschensk R.Podesta, C.Lopez, F. Podesta Observatorio Astronomico Felix Aguilar (OAFA), National University of San Juan, Argentina H. Levato, C. Saffe Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE), San Juan, Argentina D.Buckley, S. Potter, A.Kniazev, M.Kotze South African Astronomical Observatory R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres The Instituto de Astrofisica de Canarias O.Gres, K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk, Irkutsk State University A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov Kislovodsk Solar Station of the Pulkovo Observatory MASTER-Kislovodsk robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Kislovodsk was pointed to the GRB180102A 23 sec after notice time and 43 sec after trigger time at 2018-01-02 15:50:27 UT (Page et al., GCN #22292; Veres GCN22295). On our first (10s exposure) set we haven`t found optical transient within Swift error-box (D'Ai et al., GCN #22296; Beardmore et al., GCN 22294). The 5-sigma upper limit has been about 13.7 mag The message may be cited. The observations made on zenit distance = 74 degrees, galaxy latitude b = 55 degree. The moon (99 % bright part) is 14 degrees above the horizon. The distance between moon and object is 73 The sun altitude is -22.3 degree. The object can be observed till sunrise at 2018-01-03 04:41:55. MASTER-Tavrida robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Crimea was pointed to the GRB180102.66 3221 sec after notice time and 3247 sec after trigger time at 2018-01-02 16:43:51 UT. On our 22-th (180s exposure) set we haven`t found optical transient within SWIFT error-box (ra=203.113 dec=62.1472 r=0.05). The message may be cited. The observations made on zenit distance = 73 degrees, galaxy latitude b = 55 degree. The moon (99 % bright part) is 18 degrees above the horizon. The distance between moon and object is 73 The sun altitude is -25.8 degree. The object can be observed till sunrise at 2018-01-03 05:20:03. MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Blagoveschensk was pointed to the GRB180102.66 21451 sec after notice time and 21471 sec after trigger time at 2018-01-02 21:47:35 UT. We not optical transient within SWIFT error-box (ra=203.113 dec=62.1472 r=0.05) brighter then 16.7. The 5-sigma upper limit has been about 16.24mag The message may be cited. The observations made on zenit distance = 12 degrees, galaxy latitude b = 55 degree. The moon (99 % bright part) is 20 degrees above the horizon. The distance between moon and object is 72 Observations started at twilight. The sun altitude is -15.2 degree. The object can be observed till sunrise at 2018-01-03 23:26:49 This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22298 SUBJECT: GRB 180102A: NOT optical observations DATE: 18/01/03 08:20:40 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst D. Malesani (DARK/NBI), K. E. Heintz (Univ. Iceland and DARK/NBI), A. Sagues Carracedo (NOT), Andreas Kjaer Dideriksen (Aarhus Univ.), report on behalf of a larger collaboration: We observed the field of GRB 180102A (Page et al., GCN 22292; Veres, GCN 22295) with the Nordic Optical Telescope (NOT) equipped with the AlFOSC camera. Observations were carried out in the SDSS r and z filters (900 and 1000 s exposure, respectively), with a seeing of 1.5", and started on 2018 Jan 3.1769 UT (12.42 hr after the GRB trigger). At the position of the X-ray counterpart (D'Ai et al., GCN 22296), no objects are detected down to (preliminary) limiting magnitudes r = 22.5, z = 22.0 (all AB, calibrated with reference to nearby Pan-STARRS stars). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22299 SUBJECT: GRB 180102A: Swift/UVOT Upper Limits DATE: 18/01/03 12:37:47 GMT FROM: Alice Breeveld at MSSL-UCL A. A. Breeveld (UCL-MSSL) and K. L. Page (U. Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 180102A 74 s after the BAT trigger (Page et al., GCN Circ. 22292). No optical afterglow consistent with the XRT position (Beardmore et al. GCN Circ. 22294) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 74 224 147 >20.8 u_FC 286 535 246 >19.9 white 74 7508 824 >21.3 v 616 6484 352 >19.3 b 541 7303 529 >20.3 u 286 7098 717 >20.4 w1 665 6893 529 >20.1 m2 640 6688 350 >19.7 w2 591 7692 528 >20.1 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.01 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22300 SUBJECT: GRB 180102A: Swift-BAT refined analysis DATE: 18/01/03 16:06:40 GMT FROM: Amy Lien at GSFC T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-61 to T+243 sec from the recent telemetry downlink, we report further analysis of BAT GRB 180102A (trigger #802999) (Page et al. GCN Circ. 22292). The BAT ground-calculated position is RA, Dec = 203.078, 62.161 deg which is RA(J2000) = 13h 32m 18.8s Dec(J2000) = +62d 09' 38.1" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 95%. The mask-weighted light curve shows two overlapping pulses that starts at ~ T-8 s and ends at ~ T+6 s. The main peak occurs at ~T+1 s. T90 (15-350 keV) is 10.8 +- 1.7 sec (estimated error including systematics). The time-averaged spectrum from T-7.62 to T+6.30 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.01 +- 0.18. The fluence in the 15-150 keV band is 3.5 +- 0.4 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+0.80 sec in the 15-150 keV band is 1.0 +- 0.1 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/802999/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22301 SUBJECT: GRB 180102A: TSHAO optical upper limit DATE: 18/01/03 17:34:05 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), A. Pozanenko (IKI), I. Reva (FAPHI), M. Krugov (FAPHI), A. Volnova (IKI), A. Kusakin (FAPHI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 180102A (Page et al., GCN 22292) with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting on Jan. 02 (UT) 21:34:54. We took several images in R-filter. We do not detect any new sources within enhanced XRT error circle (Beardmore et al., GCN 22294). Preliminary photometry of the field is following. Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2018-01-02 21:34:54 0.25428 R 21*120 n/d n/d 20.6 The photometry is based on several nearby USNO-B1.0 stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22303 SUBJECT: GRB 180102A AROMA-N optical observation DATE: 18/01/06 00:57:23 GMT FROM: Takanori Sakamoto at AGU Y. Kitaoka, T. Sakamoto (AGU) We observed the field of GRB 180102A detected by Swift (Page et al. GCN circ. 22292) with the 0.3 m AROMA-N telescope located at Aoyama Gakuin University (Sagamihara, Japan). 10 images of 60 sec exposures were taken in the R filter starting from January 2 on 15:52:26 (UT) about 3 minutes after the trigger and stopped on 16:04:28 (UT). We do not detect the optical afterglow both in the individual images and the stacked image at the location of the X-ray afterglow (Beardmore et al. GCN circ. 22294). The estimated five sigma upper limit is ~16.0 mag using the USNO-B1 catalog.