//////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4429 SUBJECT: GRB060105: Swift detection of a bright long burst DATE: 06/01/05 07:56:10 GMT FROM: David Burrows at PSU/Swift H. Ziaeepour (UCL-MSSL), A. Blustin (UCL-MSSL), D. Burrows (PSU), J. Cummings (GSFC/ORAU), N. Gehrels (GSFC), O. Godet (U. Leicester), J. Kennea (PSU), C. Markwardt (GSFC/UMd), K. Page (U. Leicester), and D. Palmer (LANL) on behalf of the Swift team: At 06:49:28 UT, Swift-BAT triggered and located GRB 060105 (trigger=175942). The spacecraft slewed immediately. The BAT on-board calculated location is RA,Dec 297.474d, +46.362d {19h 49m 54s, +46d 21' 45"} (J2000), with an uncertainty of 3 arcmin (radius, 90% containment, stat+sys). The BAT light curve shows a multi-peaked structure with a total duration of 60 sec, beginning around T-20s. The peak count rate is ~20000 counts/sec (15-350 keV), at ~10 seconds after the trigger. XRT began observing the field at 06:50:55.3 UT, 87 sec after the BAT trigger. Onboard centroiding found a bright fading uncatalogued X-ray source in the field of view at the following coordinates: RA(J2000): 19h 50m 01.1s Dec(J2000): +46d 21' 01.0" We estimate the uncertainty of this position to be 7 arcsec (radius, 90% containment). This uncertainty includes a systematic error of about 5 arcseconds in the on-board calculated positions due to the XRT boresight offset. This position is 87 arcsec from the BAT position above. The initial source flux is 6.8e-9 erg/cm2/sec. We note that the automated GCN notice identified this as a probable cosmic ray. The XRT image at the position given above is definitely a bright celestial source, not a cosmic ray. UVOT took a finding chart exposure of 200 seconds with the V filter starting 91 seconds after the BAT trigger. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. No unambiguous afterglow candidate has been found in the initial data products, although there is a potential low-significance UVOT counterpart on the edge of the XRT error circle, at RA=19h 50m 01s DEC=+46d 20m 56s, with a V magnitude of ~19. The typical 3-sigma upper limit has been about 18th mag. No correction has been made for the expected visual extinction of about 0.6 magnitudes. The XRT position is very close to a bright (B mag ~ 12.8) star. We are currently in the portion of the orbits where the spacecraft does not pass over the Malindi downlink station. Therefore, it will be ~8 hours before we have access to the full data set for the refined analyses. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4430 SUBJECT: GRB060105 : Kiso optical observation DATE: 06/01/05 12:33:38 GMT FROM: Yuji Urata at RIKEN GRB060105 : Kiso optical observation H. Izumiura (NAOJ), H. Mito(Tokyo U.), Y. Urata (RIKEN), K.Y. Huang, W.H. Ip (NCU), Y. Qiu (BAO) on behalf of EAFON report: " We started R band imaging observation for GRB 060105 (Ziaeepour et al. # 4429) using Kiso observatory's 1.05-m Schmidt telescope at 09:39 UT (2.82 hour after the burst). There are no new sources down to the R=20.2 (S/N=3). Since we could not find the UVOT candidate with the limiting magnitude, the source has potential to be an afterglow of GRB 060105. Further analysis is in progress." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4431 SUBJECT: GRB060105, optical observation DATE: 06/01/05 14:56:33 GMT FROM: Shouta Maeno at U.of Miyazaki S.Maeno,E.Sonoda,S.Masuda,Y.Nakamura,M.Yamauchi (University of Miyazaki) "We have observed the field covering the error circle of GRB 060105 (GCN 4429) with the unfiltered CCD camera on the 30-cm telescope at University of Miyazaki. The observation was started 09:13:18 UT on Jan.05. After co-adding a set of 15 images (09:13:18 - 09:31:05 UT) of 30 sec exposures, we have compared with the USNO A2.0 catalog. Preliminary analysis shows there is no new source brighter than 16.1mag." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4432 SUBJECT: GRB060105: Suzaku-XIS and -HXD observation plan DATE: 06/01/05 15:02:18 GMT FROM: Kazutaka Yamaoka at Aoyama Gakuin U Kazuhisa Mitsuda on behalf of Suzaku team We started observation of GRB 060105 (GCN 4429: H. Ziaeepour et al.) at location (RA=19h 50m 01s, DEC=+46d 21' 01", J2000), with the Suzaku narrow field instruments (the XIS and HXD). It started around 12:10 UT, on January 05, 2006, and will continue until 12:00 UT January 06, 2006. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4433 SUBJECT: GRB 060105: XRT refined analysis DATE: 06/01/05 18:51:52 GMT FROM: Olivier Godet at U.of Leicester O. Godet, K. Page, A. Bearmore, J. Osborne (U. Leicester), D. N. Burrows (PSU), D. Grupe (PSU), H. Ziaeepour (UCL-MSSL), P. Boyd (GSFC-UMBC), L. Angelini (GSFC-JHU) report on behalf of the Swift XRT team: We analyzed the first 5 orbits of XRT data from GRB 060105. A 10.2ks photon counting (PC) mode image provides a refined XRT position: RA(J2000) = 19h 50m 00.6s Dec(J2000) = +46d 20' 58.3'' with an uncertainty of 3.2 arcsecs (90% containment). This position is 4.5 arcsecs away from the on-board XRT position quoted in Ziaeepour et al. (GCN 4429) and includes the latest XRT boresight correction. This position is 83 arcseconds from the BAT position (Ziaeepour et al., GCN 4429). The X-ray light curve can be fit with a double broken power-law with an initial decay slope of alpha1 = -1.16+/-0.14, a break at t1-T = 196 + 23/-29s, and a shallower post-break slope of alpha2 = -0.80+/-0.02, followed by another break at t2-T = 3306+/-200s and a steeper decay slope of alpha3 = -2.30+/-0.08. An absorbed power-law fit of the WT data (first orbit) from T+187s to T+1287s gave a photon index of 2.06+/-0.03 and an excess absorption value of (2.4+/-0.2)e21 cm**-2. The error bars are given at a 90% confidence level. The Galactic hydrogen column density in the direction of the burst is 1.8e21 cm**-2. The spectrum of the PC data (4 orbits) can be fit by an absorbed power-law with Gamma=2.17+/-0.16 and excess absorption of (2.8+/-0.8)e21 cm**-2. If the burst continues decaying at the current rate (alpha3) we estimate an XRT count rate of 0.0029 counts/s at T + 24hr, which corresponds to an observed 0.5-10.keV flux of 6.26e-13 ergs cm**-2 s**-1 and an unabsorbed flux of 9.82e-13 ergs cm**-2 s**-1. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4435 SUBJECT: GRB 060105: BAT refined analysis DATE: 06/01/05 20:45:09 GMT FROM: Hans Krimm at NASA-GSFC C. Markwardt (GSFC/UMD), L. Angelini (GSFC/JHU), L. Barbier (GSFC), S. Barthelmy (GSFC), J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC), J. Greiner (MPE), D. Hullinger (UMD), H. Krimm (GSFC/USRA), D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/NRC), G. Sato (ISAS), J. Tueller (GSFC), on behalf of the Swift-BAT team: Using the data set from T-120 to T+300 sec from the recent telemetry downlink, we report further analysis of BAT GRB 060105 (trigger #175942) (Ziaeepour, et al., GCN 4429). The BAT ground- calculated position is (RA,Dec) = 297.488, 46.359 {19h 49m 57.1s, 46d 21' 32.4"} [deg; J2000] +- 0.9 arcmin, (radius, sys+stat, 90% containment). This is 36 arcsec from the BAT onboard position and 52 arcsec from the Swift XRT onboard position (Ziaeepour et al, GCN #4429). The partial coding was 28.5%. The BAT mask-weighted light curve has 3 main peaks, each with multiple sub-peaks, an overall flat-topped shape, and similar spectra. The first is T-22 to T-15 sec, the second from T-3 to T+11 sec, and the third from T+23 to T+36 sec. There is softer, weaker emission in the 15-50 keV band out to at least T+150. T90 (15-350 keV) is (55 +- 5) sec (estimated error including systematics). The power law index of the time-averaged spectrum is 1.11 +- 0.03. The fluence in the 15-150 keV band is (1.82 +- 0.04) x 10^-05 erg/cm2. The 1-sec peak photon flux measured from T+30.42 sec in the 15-150 keV band is (7.5 +- 0.4) ph/cm2/sec. All the quoted errors are at the 90% confidence level. This GRB is among the brightest bursts seen by BAT. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4436 SUBJECT: GRB 060105: Mitsume optical observations DATE: 06/01/05 21:33:51 GMT FROM: Nobuyuki Kawai at Tokyo Tech K. Yanagisawa (OAO/NAOJ), Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of the Mitsume collaboration: "We have observed the field of GRB 060105 (Ziaeepour et al. GCN 4429) with the three-color Mitsume 50 cm telescopes at Okayama and Akeno, Japan starting at 9:14 UT (2.4 hours after the burst). The summary of the observations is following: Telescope bands time (UT) exposure --------- ---------- ---------------- ------------ Okayama g', Rc, Ic 09:14 - 09:41 UT 60 s x 20 Akeno V, Rc, Ic 09:32 - 11:20 UT 30 s x 158 --------- ---------- ---------------- ------------ Comparison with the DSS-2R image does not reveal an OT at the position of the XRT error circle. The 10-sigma upper limit magnitudes for the Okayama images are g': 17.1 Rc: 17.3 Ic: 17.5 The images obtained at Okayama can be viewed at http://bragi.oao.nao.ac.jp/support/telescope/grb50/images/GRB060105A.pdf." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4437 SUBJECT: GRB 060105: Swift/UVOT upper limits DATE: 06/01/05 23:31:06 GMT FROM: Patricia Schady at MSSL/Swift P. Schady (UCL-MSSL/PSU), M. Page (UCL-MSSL), A. Cucchiara (PSU), F. Marshall (GSFC), N. Gehrels (GSFC) on behalf of the Swift/UVOT team report: The Swift/UVOT began observing the field of GRB 060105 at 06:50:59 UT on 2006-01-05, 91 s after the BAT trigger (Ziaeepour et al., GCN 4429). No source was observed in any of the UVOT filters at the XRT position and the potential candidate mentioned in GCN 4429 is most likely contamination from a bright, nearby star. The 3-sigma upper limits in summed images from each of the filters are listed below (not corrected for extinction; E(B-V) = 0.171). Filter T_range(s) Exp(s) 3sigUL(mag) V 91-29544 29453 20.4 B 457-5533 5076 20.1 U 403-23780 23377 20.8 W1 349-22873 22524 20.3 M2 295-30329 30034 20.6 W2 565-28638 28073 21.0 White 511-889 378 19.9 _______________________________________________ Uvot_cal mailing list Uvot_cal@phoenix.astro.psu.edu https://phoenix.astro.psu.edu/mailman/listinfo/uvot_cal //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4438 SUBJECT: GRB 060105: ISAS observations and near IR upper limit DATE: 06/01/06 03:16:15 GMT FROM: Daisuke Yonetoku at Kanazawa U D. Yonetoku, T. Murakami, H. Kodaira, S. Okuno, S. Yoshinari, T. Kidamura (Kanazawa Univ.) and Y. Kobayashi (NAOJ) on behalf of the Kanazawa team report: We have observed the field of GRB 060105 (Ziaeepour et al. GCN #4429) with J, H, Ks-bands using the 1.3m telescope on the roof top of ISAS, Japan. The observation was started at 08:37 UT (1.8 hours after the burst) in poor condition and low elevation. Comparison with the 2MASS catalogue does not reveal any new source within the position of the XRT error circle. The 5-sigma upper limit magnitudes are Ks: 13.8, H: 14.2, J: 15.7, respectively. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4439 SUBJECT: Konus-Wind observation of GRB 060105 DATE: 06/01/06 13:10:21 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and T. Cline on behalf of the Konus-Wind team report: The GRB 060105 (Swift-BAT trigger #175942; Ziaeepour et al., GCN 4429; Markwardt et al., GCN 4435) triggered Konus-Wind at T0=24544.371 s UT (06:49:04.371). The Konus-Wind light curve consists of three main multipeaked pulses with a total duration of ~60 sec. As observed by Konus-Wind the burst had a fluence of 7.86(-0.37,+0.19)x10^-5 erg/cm2 and peak flux on 256 msec time scale 6.55(-0.45,+0.19)x10^-6 erg/cm2/sec (both in the 20 keV - 2 MeV energy range). The time-integrated spectrum of the GRB (from T0 to T0+58.880 sec) is well fitted (in the 20 keV - 2 MeV range) by a power law with exponential cutoff model: dN/dE ~ E^(-alpha) * exp(-E*(2-alpha)/Ep) with alpha = 0.827(-0.044,+0.042) and Ep = 424(-22, +25) keV (chi2 = 63/62dof). It can also be fitted by GRBM (Band) model for which: the low-energy photon index is alpha = -0.790 (-0.052,+0.067), the high energy photon index beta = -2.70(-0.73, +0.35), the break energy E0 = 327 (-46, +40) keV (chi2 = 58/61dof). The spectrum integrated over the most intense part of the GRB (from T0+16.64 to T0+29.184 sec) is well fitted (in the 20 keV - 2 MeV range) by a power law with exponential cutoff model: dN/dE ~ E^(-alpha) * exp(-E*(2-alpha)/Ep) with alpha = 0.571(-0.060,+0.057) and Ep = 549(-31, +34) keV (chi2 = 73/62dof). All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4440 SUBJECT: GRB 060105: MDM Observation DATE: 06/01/06 13:18:06 GMT FROM: Jules Halpern at Columbia U. N. Zimmerman, S. Tyagi, & J. P. Halpern (Columbia U.) report: "Using the MDM 2.4m outfitted with RETROCAM, we have obtained an upper limit on the SDSS r-band magnitude of GRB 060105 as of Jan. 6 02:00 UT, or 19 hours after the burst. The sum of eight 5-minute exposures reveals no new source within the refined XRT error circle (Godet et al,. GCN 4433) to a limit of r = 21.0, as calibrated with Sloan standard stars." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4441 SUBJECT: GRB 060105: Radio observations DATE: 06/01/06 15:40:31 GMT FROM: Dale A. Frail at NRAO Dale A. Frail (NRAO) reports on behalf of a larger collaboration: "We used the Very Large Array to observe the Swift burst GRB060105 (GCN 4435; GCN 4429) at a frequency of 8.46 GHz on 2006 January 6.10 UT. No radio emission is detected within the XRT error circle (GCN 4433) with a peak flux density of 49 +/- 47 uJy. No further observations are planned. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4442 SUBJECT: GRB 060105: pseudo-z from spectral parameters of the prompt emission DATE: 06/01/06 17:02:38 GMT FROM: Jean-Luc Atteia at Lab d Astrophys.,OMP,Toulouse A. Pelangeon & J-L. Atteia (LATT-OMP) report: We have used the spectral parameters of the most intense part of GRB 060105 provided by Golenetskii et al. (GCNC 4439) to compute the spectral pseudo-redshift of this GRB, assuming that the most intense part of the burst contains half of the total fluence. We find a pseudo-redshift pz= 4.0 +/- 1.3 //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4449 SUBJECT: GRB 060105: quick look analysis of the Suzaku/XIS afterglow observation DATE: 06/01/09 01:40:38 GMT FROM: Makoto Tashiro at Saitama U/Swift K. Mitsuda, R. Fujimoto, T. Inui, T. Murakami and the Suzaku GRB-ToO team reports: The Suzaku narrow field instruments: XIS and HXD started observation of GRB060105 from 12:10 UT on 2006-01-05 (Mitsuda et al. GCN 4432), at 5.4 hours after the Swift BAT detection (Ziaeepour et al. GCN 4429). Preliminary analysis shows a fading X-ray source at the reported XRT position (Godet et al. GCN4433). The intensity decreased to 1/3 of the initial at the end of observation, 12:00 UT on 2006-01-06. The averaged flux during the observation is approximately 7x10^-13 erg/s/cm2 (2-10 keV). Detail analysis is in progress. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4606 SUBJECT: GRB060105: refined analysis of the Suzaku observation DATE: 06/01/27 14:52:24 GMT FROM: Kazuhiro Nakazawa at ISAS/JAXA K. Nakazawa (ISAS/JAXA), K. Yamaoka , Y. Nakagawa (AGU), M. Yamauchi, E. Sonoda, S. Maeno (Univ. of Miyazaki), T. Murakami, D. Yonetoku (Kanazawa U.), M. Tashiro, K. Abe, K. Onda (Saitama U.), N. Ishikawa, A. Yoshida (AGU), N. Yamasaki, Y. Terashima, H. Murakami (ISAS/JAXA), K. Torii (Osaka U.), Y. Ichikawa, S. Murasawa, R. Fujimoto (ISAS/JAXA), Tatsuya Inui (Kyoto U.), on behalf of Suzaku GRB ToO team report: We have carried out refined analysis on the data from the Suzaku TOO observation of GRB060105 (Ziaeepour et al. GCN4429). The Suzaku observation started on 2006, January 5 at 12:10 UT, 5 hours 20 minutes after the GRB, and ended on January 6, at 12:00 UT. A good exposure of 35 ks was obtained in total. As reported by Mitsuda et al (GCN4449), the afterglow of GRB060105 is clearly detected in the XIS images and its position is fully consistent with the refined Swift/XRT one (Godet et al., GCN4433). Suzaku XIS spectra ranging 0.5-8 keV are well described with an absorbed power law model. The derived best fit photon index and column density are Gamma = 2.1+/- 0.1 and NH = (3.0 +/- 0.6) x 10^21 cm^-2, respectively. No signature of spectral variability is detected during the observation. The flux fades along the Suzaku observation from (1.9 +/- 0.3) x 10^-12 erg/s/cm2 (T_burst + 5.7-7.0 hours) to (1.5 +/- 0.5) x 10^-13 erg/s/cm2 (T_burst + 26-28 hours) in the 2-10 keV energy band. Decay index was found to be -1.3 +/- 0.2. Note that a possible 10% systematic calibration error is not included in the errors quoted above. These results are generally consistent with those obtained by analyzing the Swift/XRT data. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4754 SUBJECT: GRB060105: optical observations DATE: 06/02/13 15:07:19 GMT FROM: Alexei Pozanenko at IKI, Moscow D. Sharapov (MAO, and NOT La Palma), M. Ibrahimov, (MAO), A. Pozanenko (IKI) and V. Rumyantsev (CrAO) on behalf of larger GRB follow up collaboration report: We observed error box of GRB060105 (Ziaeepour et al., GCN 4429) with 1.5m telescope of Maidanak Astronomical Observatory in R-band on Jan. 06 between (UT) XX and YY. Within refined XRT error circle (Godet et al., GCN 4433) we do not detect new optical objects. Limiting magnitude is based on USNO B1.0 is following: Obs. time, Exp., Mag.(UL), Seeing (UT) (s) Jan. 06 13:35-13:57 7x180 20.8 ~2.3" //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5278 SUBJECT: GRB 060105: Upper limit on Host Galaxy DATE: 06/06/27 18:49:53 GMT FROM: Alexander Kann at TLS Tautenburg D. A. Kann (Thueringer Landessternwarte Tautenburg) and S. Manohar (USC, Los Angeles), report: We observed the field of GRB 060105 (Ziaeepour et al., GCN 4429) with the Tautenburg 1.34m Schmidt telescope under good observing conditions. We obtained 6 x 600 sec images in the Rc filter for a total integration time of 60 minutes. The mean observation time was June 27.9288 UT, which is 172.7 days after the burst. We determine the zero point of the image in comparison with nine unsaturated and isolated stars of the USNOB1.0 catalog. Astrometry is also performed against the USNOB1.0 catalog. At the refined position of the X-ray afterglow (Godet et al., GCN 4433), we do not detect any sources. The 2 sigma limiting magnitude of the image is Rc=23, but the position of the afterglow is affected by the PSF of several nearby bright stars. We set a limiting magnitude of Rc=22.5 for any source at this position. This magnitude is not corrected for the moderate foreground extinction, E(B-V)=0.171. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 5280 SUBJECT: Correction to GCN 5278 & GCN 5279 (GRBs 060105 & 060109) DATE: 06/06/27 19:02:50 GMT FROM: Alexander Kann at TLS Tautenburg D. A. Kann (TLS Tautenburg) reports: The mean observation times of the locations of GRB 060105 (Kann & Manohar, GCN 5278) and GRB 060109 (Kann & Manohar, GCN 5279) should read 26.9X UT, not 27.9X UT. We regret this mistake and thank Petr Kubanek, who also pointed it out.