//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6104 SUBJECT: GRB 070219: Swift detection of a burst DATE: 07/02/19 01:43:52 GMT FROM: Scott Barthelmy at NASA/GSFC T. Sakamoto (NASA/ORAU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), F. E. Marshall (NASA/GSFC), C. Pagani (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL), P. Schady (MSSL-UCL), M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester) and E. Troja (INAF-IASFPA) report on behalf of the Swift Team: At 01:10:16 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 070219 (trigger=261132). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 260.198, +69.364 which is RA(J2000) = 17h 20m 48s Dec(J2000) = +69d 21' 51" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single peak with a duration of about 15 sec. The peak count rate was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began taking data at 01:11:38 UT, 82 seconds after the BAT trigger. From ground-based analysis we find a weak source at RA, Dec (J2000) = 260.190, +69.369 which is RA(J2000) = 17h 20m 45.5s Dec(J2000) = +69d 22' 10.7" with an error radius of 5 arcseconds. This is 21 arcseconds from the BAT position. UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm) filter starting 87 seconds after the BAT trigger. No afterglow candidate has been found in the initial data products at the BAT or XRT position with a white band 3-sigma upper limit of 19.6 mag. The 2.7'x2.7' sub-image covers 25% of the BAT error circle and 100% of the XRT error circle. No correction has been made for the expected extinction corresponding to E(B-V) of 0.035 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6105 SUBJECT: GRB070219 - SDSS Pre-Burst Observations DATE: 07/02/19 01:50:01 GMT FROM: Richard J. Cool at U.of AZ/Steward Obs Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona), David W. Hogg (NYU), Michael R. Blanton (NYU), David J. Schlegel (LBNL), J. Brinkmann (APO), Donald Q. Lamb (Chicago), Donald P. Schneider (PSU), and Daniel E. Vanden Berk (PSU) report: The Sloan Digital Sky Survey (SDSS) imaged the field of burst GRB070219 prior to the burst. As these data should be useful as a pre-burst comparison and for calibrating photometry, we are supplying the images and photometry measurements for this GRB field to the community. Data from the SDSS, including 5 FITS images, 3 JPGS, and 3 files of photometry and astrometry, are being placed at http://mizar.as.arizona.edu/~grb/public/GRB070219 We supply FITS images in each of the 5 SDSS bands of a 8'x8' region centered on the GRB position (ra=260.198 (17:20:47.5), dec=69.3640 (69:21:50.4); Swift-BAT TRIGGER 261132), as well as 3 gri color-composite JPGs (with different stretches). The units in the FITS images are nanomaggies per pixel. A pixel is 0.396 arcsec on a side. A nanomaggie is a flux-density unit equal to 10^-9 of a magnitude 0 source or, to the extent that SDSS is an AB system, 3.631e-6 Jy. The FITS images have WCS astrometric information. In the file GRB070219_sdss.calstar.dat, we report photometry and astrometry of 256 bright stars (r<20.5) within 15' of the burst location. The magnitudes presented in this file are asinh magnitudes as are standard in the SDSS (Lupton 1999, AJ, 118, 1406). Beware that some of these stars are not well-detected in the u-band; use the errors and object flags to monitor data quality. In the files GRB070219_sdss.objects_flux.dat and GRB070219_sdss.objects_magnitudes.dat, we report photometry of 276 objects detected within 6' of the GRB position. We have removed saturated objects and objects with model magnitudes fainter than 23.0 in the r-band. The fluxes listed in GRB070219_sdss.objects_flux.dat are in nanomaggies while the magnitudes listed in GRB070219_sdss.objects_magnitudes.dat are asinh magnitudes. All quantities reported are standard SDSS photometry, meaning that they are very close to AB zeropoints and magnitudes are quoted in asinh magnitudes. Photometric zeropoints are known to about 2% rms. None of the photometry is corrected for dust extinction. The Schlegel, Finkbeiner, and Davis (1998) predictions for this region are A_U=0.178 mag, A_g=0.131 mag, A_r = 0.095 mag, A_i=0.072 mag, and A_z=0.051 mag. There are currently no objects within 6 arcminutes of the GRB position in the SDSS spectroscopic database. SDSS astrometry is generally better than 0.1 arcsecond per coordinate. Users requiring high precision astrometry should take note that the SDSS astrometric system can differ from other systems such as those used in other notices; we have not checked the offsets in this region. More detailed information pertaining to our SDSS GRB releases can be found in our initial data release paper (Cool et al. 2006, PASP 118, 733). See the SDSS DR4 documentation for more details: http://www.sdss.org/dr5. These data have been reduced using a slightly different pipeline than that used for SDSS public data releases. We cannot guarantee that the values here will exactly match those in the data release in which these data are included. In particular, we expect the photometric calibrations to differ by of order 0.01 mag. This note may be cited, but please also cite the SDSS data release paper, Adelman-McCarthy et al. (2006, ApJS, 162, 38), when using the data or referring to the technical documentation. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6106 SUBJECT: GRB 070219: ROTSE-III Optical Limits DATE: 07/02/19 02:33:38 GMT FROM: Heather Swan at U.of Michigan/ROTSE H. Swan (U Mich), J. Aretakis (U Mich) report on behalf of the ROTSE collaboration: ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 070219 (Swift trigger 261132), producing images beginning 35 minutes after the GCN notice time. An automated response took the first image at 01:44:52.6 UT, 2076.5 s after the burst, under twilight conditions. We took 10 5-sec, 10 20-sec and 6 60-sec eposures. These unfiltered images are calibrated relative to USNO A2.0 (R). Comparison to the DSS (second epoch) reveals no new sources within the 3-sigma error circle, for both single images and coadding into sets of 10. Individual images have limiting magnitudes ranging from 15.8-17.0; we set the following specific limits. start UT end UT t_exp(s) mlim t_start-tGRB(s) Coadd? -------------------------------------------------------------------- 01:44:52.6 01:45:52.6 60 16.4 2076.5 N 02:13:52.6 02:14:52.6 60 17.0 3816.5 N 01:51:50.6 02:03:17.4 686 17.8 2494.5 Y //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6107 SUBJECT: GRB 070219: Liverpool Telescope Observations DATE: 07/02/19 03:06:13 GMT FROM: Andrea Melandri at Liverpool John Moores U A. Melandri (Liverpool JMU) on behalf of the Liverpool GRB group reports The 2-m Liverpool Telescope robotically followed up GRB 070219 (Sakamoto et al., GCN 6104, trigger=261132) beginning 53 min after the GRB trigger time (UT:01:10:16). The automatic detection mode (3x10sec) did not identify any new bright object inside the XRT error circle (Sakamoto et al., GCN 6104). Comparison with the USNO B1 for a coadded set of images (for a total exposure time of 300 sec) did not reveal any new object down to a limiting magnitude R~20.2 (between 53-66 minutes after the burst). Further observations are ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6108 SUBJECT: GRB 070219: optical TNG observations DATE: 07/02/19 04:19:40 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo (INAF-OAB), A. Magazzu` (INAF-TNG), Albar G. de Gurtubai (INAF-TNG), L. A. Antonelli (INAF-OAR) report on behalf of the MISTICI and CIBO collaborations: We observed the field of GRB 070219 (Sakamoto et al., GCN 6104) with the Italian TNG telescope sited in La Palma, Canary Islands. Observations were carried out about 2.02 hours after the burst. No object is present inside the XRT error box (Sakamoto et al., GCN 6104) down to a limiting magnitude of R ~ 25 (3sigma level, calibrated against the USNOB1 catalog). We acknowledge the support of the TNG staff. This message can be cited //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6109 SUBJECT: GRB 070219, Swift-BAT refined analysis DATE: 07/02/19 04:50:07 GMT FROM: Takanori Sakamoto at NASA/GSFC GRB 070219, Swift-BAT refined analysis D. Palmer (LANL), L. Barbier (GSFC), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), A. Parsons (GSFC), T. Sakamoto (GSFC/ORAU), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC) on behalf of the Swift-BAT team: Using the data set from T-239.9 to T+499.2 sec from the recent telemetry downlink, we report further analysis of BAT GRB 070219 (trigger #261132) (Sakamoto, et al., GCN Circ. 6104). The BAT ground-calculated position is RA, Dec = 260.219, 69.345 deg which is RA(J2000) = 17h 20m 52.6s Dec(J2000) = 69d 20' 41.4" with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment). The partial coding was 92%. The mask-weighted lightcurve shows a weak FRED-like bump from T-4 to T+20 sec. T90 (15-350 keV) is 17 +- 1 sec (estimated error including systematics). The time-averaged spectrum from T-1.5 to T+17.7 is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.8 +- 0.2. The fluence in the 15-150 keV band is 3.2 +- 0.4 x 10^-07 erg/cm2. The 1-sec peak photon flux measured from T+1.31 sec in the 15-150 keV band is 0.7 +- 0.1 ph/cm2/sec. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6110 SUBJECT: GRB 070219: I-band observations DATE: 07/02/19 11:00:41 GMT FROM: Antonio Deugarte at IAA-CSIC A. de Ugarte Postigo, A. J. Castro-Tirado, J. Gorosabel, M. Jelínek (IAA-CSIC, Granada), P.Rodríguez-Gil and S. López (IAC) on behalf of a larger collaboration, report: "We have imaged the field of GRB 070219 (Sakamoto el al. GCN 6104) with the IAC80 telescope in I-band, starting on Feb 19.28042 UT (5h34m after the burst). No object is detected in the XRT error box down to the POSS2 IR limit." This message can be quoted. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6111 SUBJECT: GRB 070219: Swift/UVOT Upper limits DATE: 07/02/19 14:14:41 GMT FROM: Alice Breeveld at MSSL-UCL A. Breeveld (MSSL/UCL) and T. Sakamoto (NASA/ORAU) report on behalf of the Swift UVOT team: The Swift/UVOT observed the field of GRB 070219 starting 68s after the BAT trigger (Sakamoto et al. 2007, GCN Circ. 6104). We do not find any source, in any of the UVOT observations, inside the XRT error circle. The 3-sigma upper limits for detecting a source inside the XRT error circle in the co-added frames are: Filter T_start T_stop Exp(s) Mag(3-sigma UL) -------------------------------------------------------- V 68 18502 2032 20.3 B 670 6909 432 20.4 U 646 13201 980 20.4 UVW1 622 12659 1160 21.0 UVM2 598 18983 1627 21.5 UVW2 698 17588 1356 21.5 White 87 7114 618 20.7 The values quoted above are not corrected for the expected Galactic extinction corresponding to a reddening of E(B-V) = 0.035 towards the direction of the burst (Schlegel et al. 1998) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6112 SUBJECT: GRB 070219: XRT Refined Analysis DATE: 07/02/19 14:51:03 GMT FROM: Rhaana Starling at U of Leicester R.L.C. Starling (U Leicester), T. Sakamoto (NASA/GSFC), K.L. Page, M.R. Goad and P.A. Evans (U Leicester) report on behalf of the Swift-XRT team: We have analysed the first four orbits (up to 18.8 ks after the BAT trigger) of Swift XRT data for the faint X-ray afterglow of GRB 070219 (Sakamoto et al., GCN 6104). Using ~6 ks of Photon Counting (PC) mode data we find the following astrometrically corrected XRT refined position (by matching the UVOT images with the USNO-B1 catalogue): RA (J2000) = 17h 20m 45.99s Dec(J2000) = +69d 22' 10.6" with an error radius of 3.6 arcseconds (90% confidence). This is 95.2, 21.8 and 3.0 arcseconds away from the BAT refined, BAT initial and XRT initial positions respectively. The lightcurve appears to follow the canonical three-phase decay. It decays with alpha_1~2.2, breaking at T_bk_1~330 s to alpha_2~0.3 and breaking again at T_bk_2~9200 s to a slope of alpha_3~1.5. The PC mode spectrum, summed over all the data collected thus far, is not tightly constrained, but can be fitted with a single power law of photon index Gamma = 2 and a total absorbing column at z = 0 of nH = 1.3E21 cm-2, in excess of the Galactic value of 4.1E20 cm-2. The 0.3-10 keV observed (unabsorbed) flux is 9E-13 (1.2E-12) erg/cm2/s. There are too few counts for a time-resolved spectral analysis, hence any spectral evolution present cannot be measured. If the decay continues with a slope of alpha = 1.5, the predicted count rate at 24 hours post-trigger is 5E-4 cts/s. This corresponds to an observed (unabsorbed) flux of 2E-14 (3E-14) erg/cm2/s. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6113 SUBJECT: GRB070219: MASTER-VWF-Kislovodsk observations DATE: 07/02/19 16:08:05 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, N.Shatskiy, E.Gorbovskoy, A.Belinski, D.Kuvshinov, N.Tyurina, P.Gritsyk Sternberg Astronomical Institute, Moscow Union 'Optic' A. Tlatov, I.Golubov Kislovodsk Solar Station of the Pulkovo observatory "MASTER Very Wide Field Camera located at Kislovodsk Solar Station (http://observ.pereplet.ru, D=70 mm, 420 square degrees, 20'' per pix) has moved to the Swift-BAT trigger 261132 and it has taken a series of 5s exposures starting 76s after the GRB time and 15 s after notice arrivel time at 01-11-30.473 UT under good weather condition. The limiting magnitude is about 11.5m for single exposures. These unfiltered images are calibrated relative to USNO A2.0 (R). There is no OT was found inside Swift error box (T. Sakamoto et al., GCN Circ 6104). T-Tgrb Mean Time Limit Coadd? Note 76s 78.5s 11.0 no slightly moving 81s 106s 12.7 12 81s 331 s 13.5 84 The message can be cited. mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6116 SUBJECT: GRB 070219: Gemini Observations DATE: 07/02/20 09:58:17 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko (Caltech), P. A. Price (IfA/Hawaii), E. Berger (Carnegie), and D. B. Fox (Penn State) report on behalf of a larger collaboration: We have imaged the field of GRB070219 (Sakamoto et al., GCN 6104)) with the Gemini Multi-Object Spectrograph mounted on the Gemini North Telescope. Images consisted of 4 x 180 s exposures in z' and 2 x 180 s exposures in i' at a mean epoch of approximately 14:50 19 February UT (~ 13.7 hr after the burst). Inside the revised XRT error circle (Starling et al., GCN 6112), we see no sources to limiting magnitudues of i' > 23.0, z' > 22.0. Photometric calibration was performed relative to the SDSS fields provided by Cool et al. (GCN 6105)