//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14967 SUBJECT: Fermi394416326: iPTF detection of a possible optical afterglow DATE: 13/07/03 08:24:18 GMT FROM: Leo Singer at CIT/PTF L. P. Singer (Caltech), S. B. Cenko (NASA/GSFC), M. M. Kasliwal (Carnegie Observatories), D. A. Brown (Syracuse), O. Yaron (Weizmann Institute of Science), E. Bellm (Caltech), S. Caudill (Milwaukee), S. Tinyanont (Harvey Mudd), D. Khatami (Pomona), and A. J. Weinstein (Caltech) report on behalf of the intermediate Palomar Transient Factory (iPTF) collaboration: We have imaged 72 deg^2 of the vicinity of the final localization of the Fermi-GBM trigger 394416326 with the Palomar 48 inch Oschin telescope (P48). Images were obtained in the Mould R filter in 2 visits to each of 10 fields. Within the GBM error circle, we detect a bright point source at the position: RA(J2000) = 14h 29m 14.78s DEC(J2000) = +15d 46' 26.4" which is 3.8 degrees away from the center of the final GBM localization (68% confidence radius of 3.99 degrees). At 04:17 UT on 2013 July 2 (4.2 hours after the Fermi-GBM trigger), we measure a magnitude of R = 17.4 for the source, dubbed iPTF13bxl. Nothing was detected at this location in previous P48 images of the field taken on 2011 February 5 to a limiting magnitude of R > 21.1. Automatic follow-up of iPTF13bxl was obtained with the robotic Palomar 60 inch telescope beginning at 4:10 UT on 2013 July 3 (28.1 hours after the burst trigger). At this time we measure a magnitude of r' = 18.7. Assuming the source decays as a single power-law from the time of our P48 to discovery to this time, we infer a decay index of 0.54. We observed iPTF13bxl with the Double Beam Spectrograph on the Palomar 200-inch (P200) on 2013-07-03 04:24:04, 28.3 hours after the burst. The spectrum has a largely featureless blue continuum with no strong, narrow features in emission or absorption between 3800A and 9000A. We triggered target-of-opportunity observations of iPTF13bxl with the Swift satellite, beginning at 00:50 UT on 2013 July 3 (1.03 d after the Fermi-GBM trigger). A total exposure time of 1.4 ks was obtained with the on-board X-Ray Telescope (XRT). A bright source is detected at the location of iPTF13bxl in the XRT. We measure a preliminary count rate of 0.3 ct s^-1 at this time. Assuming a power-law spectrum with a photon index of 2, this corresponds to a 0.3-10.0 keV X-ray flux of ~ 10^-11 erg cm^-2 s^-1. We note that close to iPTF13bxl are two SDSS sources: SDSS J142914.75+154626.0, at a separation of 0.6", a faint source classified as a star with r = 23.01, and SDSS J142914.57+154619.3, at a separation of 7.6", a bright galaxy with a photometric redshift of 0.09 +/- 0.02. Without a secure spectroscopic redshift, we cannot definitively associate this source with the Fermi-GBM GRB. The bright X-ray emission and relatively steep decay in the optical seem to rule out an (unrelated) supernova, but other potential interlopers remain. Follow-up observations are ongoing and encouraged to help identify the nature of this source. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14968 SUBJECT: Fermi394416326: FTN detection DATE: 13/07/03 10:02:32 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi (Ferrara U.), C.G. Mundell, I.A. Steele (LJMU), on behalf of a large collaboration report: On 2013 July 03 (09:03:30 UT) we began observing the field of the possible optical afterglow of Fermi394416326 (Singer GCN Circ. 14967) with the 2-m Faulkes Telescope North in Hawaii. Observations were carried out using the BVRi filters. We clearly detect the optical counterpart discovered by Singer et al. with the following magnitudes Time from GRB Filter Exposure[s] Magnitude (days) ---------------------------------------------------- 1.38 i' 100 18.61 +- 0.07 1.38 R 120 18.46 +- 0.05 ---------------------------------------------------- The calibration was performed using the i' magnitudes of SDSS catalogue field stars and the R magnitudes obtained using the transformations by Jordi et al (2006). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14970 SUBJECT: Fermi GBM trigger 394416326: MASTER early optical limit DATE: 13/07/03 16:24:15 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs H. Levato and C. Saffe Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) C. Mallamaci, C. Lopez and F. Podest Observatorio Astronomico Felix Aguilar (OAFA) E. Gorbovskoy, D. Denisenko, V. Lipunov, V. Kornilov, A. Kuznetsov, D. Kuvshinov, N. Tyurina, N. Shatskiy, P. Balanutsa, D. Zimnukhov, V.V. Chazov Lomonosov Moscow State University, Sternberg Astronomical Institute A. Tlatov, A.V. Parhomenko, D. Dormidontov, V. Sennik Kislovodsk Solar Station of the Pulkovo Observatory K. Ivanov, S. Yazev, N.M. Budnev, O. Gres, O. Chuvalaev, V.A. Poleshchuk Irkutsk State University V. Yurkov, Yu. Sergienko, D. Varda, E. Sinyakov Blagoveschensk Educational State University, Blagoveschensk V. Krushinski, I. Zalozhnich, A. Popov, A. Bourdanov, A. Punanova Ural Federal University MASTER-ICATE robotic very wide field cameras (FOV=2x384 square degrees, D=72mm, f/1.2, 1 pix = 22 arcsec, http://observ.pereplet.ru) located in Argentina (Observatorio Astronomico Felix Aguilar, http://master.sai.msu.ru:8080/) were pointed to the Fermi-GBM trigger 394416326 55 sec after GRB time and 49 sec FERMI trigger Time at 2013-07-02 00:06:18 UT. We haven't found optical transient (Singer et. al. GCN 14967) on single (exp = 5 sec) images with upper limit V<11m and coadded image made of first 58 frames (5 sec exposure without time gap) and total exposure of 290 seconds with upper limit V<12.5m. Our magnitudes are calibrated against V magnitudes from Tycho-2 catalog. This upper limit does not contradict the power law decay with an index of 0.54 inferred by Singer et al. in GCN 14967. The reduction of the whole data set is continuing. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14971 SUBJECT: GRB 130702A / Fermi394416326 : Fermi-LAT detection of a burst DATE: 13/07/03 17:34:28 GMT FROM: Giacomo Vianello at SLAC T. Cheung (NRL), G.Vianello (Stanford), S. Zhu (NASA/GSFC), J. Racusin (NASA/GSFC), V. Connaughton (UAH) and B. Carpenter (NASA/GSFC) report on behalf of the Fermi-LAT team: At 00:05:23.079 UTC on July 02, 2013, Fermi GBM triggered on GRB 130702A / Fermi394416326 (trigger 394416326). The LAT detected high energy emission from this GRB, which was also detected in the optical band by iPTF (Singer et al., GCN 14967) and confirmed by FTN (Guidorzi et al., GCN 14968). The best LAT on-ground location is found to be: RA, DEC = 216.4, 15.8 (J2000), with an error radius of 0.5 deg (90% containment, statistical error only) This position is 4 deg from the best GBM position (RA, Dec = 218.81, +12.25 with a 4 deg radius), and 0.8 deg from the position of the optical afterglow. A preliminary IPN triangulation of the burst using GBM and Konus-Wind data gives an annulus with center RA, DEC = 260.8992, -20.7746 (J2000) of radius 50.85 degrees and a width of (-32.73,+18.42) deg (3 sigma). The center of this annulus is 6.05 deg (0.99 sigma) from the LAT location (Private Communication, with possible IPN refinements using data from distant spacecraft). The best LAT localization for the source was ~75 deg from the LAT boresight at the time of the trigger, i.e., outside the nominal field of view of the LAT (~65 deg), but it entered the FOV at T0+250 s to exit again at T0 + 2200 s. The data from the Fermi LAT in such time interval show a significant increase in the event rate within 10 degree of the source location, with a significance of more than 5 sigmas. This analysis has been carried out with the P7SOURCE_V6 class. More than 5 photons above 100 MeV are observed within 2200 seconds. The highest energy photon is a 1.5 GeV event which is observed 260 seconds after the GBM trigger. The Fermi LAT point of contact for this burst is Giacomo Vianello (giacomov@stanford.edu). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14972 SUBJECT: GRB 130702A / Fermi394416326: Fermi GBM detection DATE: 13/07/03 18:58:21 GMT FROM: Andrew Collazzi at NASA/MSFC/ORAU Andrew C. Collazzi (NASA/ORAU), V. Connaughton (UAH) report on behalf of the Fermi GBM Team: "At 00:05:23.08 UT on 2 July 2013, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 130702A (trigger 394416326 / 130702.004). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 218.8, Dec = +12.25 (J2000 degrees, equivalent to J2000 14h 35m, +12d 15'), with a statistical uncertainty of 4.0 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight is 75 degrees. The GBM trigger is possibly associated with an optical transient reported by Singer et al. (GCN 14697) and Guidorzi et al. (GCN 14698). This event was also detected above 100 MeV by the Fermi LAT (Cheung et al., GCN 14971). The GBM light curve shows a FRED-like burst with a duration (T90) of about 59 s (50-300 keV). The burst has a 1.024-s peak flux of 7.03 +/- 0.86 ph/s-cm^2. The time-averaged spectrum from T0+0.003 to T0+16.384 s is well fit by power-law function with alpha = -1.65 +/- 0.02. The fluence (10-1000 keV) in this time interval is (6.3 +/- 2.0)E-06 erg/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14973 SUBJECT: Fermi GRB 130702A: Swift XRT and UVOT observations DATE: 13/07/03 19:01:40 GMT FROM: Andrea Melandri at INAF-OAB P. D'Avanzo (INAF-OAB), B. Porterfield, D. N. Burrows, M. Siegel (PSU), A. Melandri (INAF-OAB), P. A. Evans (Univ. Leicester) report on behalf of the Swift team: The Fermi GBM and LAT instruments detected GRB 130702A at 00:05:23 UT on July 2, 2013 (Fermi trigger 394416326; Cheung et al. 2013, GCN Circ 14971). Followup by the Palomar Transient Factory (PTF) located a possible optical counterpart, iPTF13bxl (Singer et al. 2013, GCN Circ. 14967). A subsequent TOO observation by Swift located a coincident X- ray counterpart, making this a likely counterpart of GRB 130702A (Singer et al. 2013, GCN Circ 14971). Here we report the results of the analysis of Swift XRT and UVOT data for this object. We have analysed 3.4 ks of XRT data for this object, from 89.1 ks to 95.7 ks after the Fermi/GBM trigger. The data are entirely in Photon Counting (PC) mode. Using 3411 s of PC mode data and 5 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 217.31166, +15.77388 which is equivalent to: RA (J2000): 14h 29m 14.80s Dec(J2000): +15d 46' 26.0" with an uncertainty of 1.5 arcsec (radius, 90% confidence). This position is consistent with the optical counterpart reported by Singer et al. 2013 (GCN Circ. 14967; see also Guidorzi et al. 2013, GCN Circ. 14968). The light curve displays variability consistent with a fading behaviour. More observations are scheduled to confirm whether the source is fading. A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.99 (+/-0.16). The best- fitting absorption column is 6.3 (+3.4, -3.1) x 10^20 cm^-2, in excess of the Galactic value of 1.7 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.6 x 10^-11 (4.2 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 6.3 (+3.4, -3.1) x 10^20 cm^-2 Galactic foreground: 1.7 x 10^20 cm^-2 Excess significance: 2.4 sigma Photon index: 1.99 (+/-0.16) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00032876. The Swift/UVOT began settled observations of the field of GRB 130702A 89111 s after the GBM detection. A source consistent with the P48 position (Singer et al. 2013, GCN Circ. 14967) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 14:29:14.77 = 217.31155 (deg.) Dec (J2000) = +15:46:26.5 = 15.77403 (deg.) with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence). Preliminary detections 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 89232 95967 3414 18.26 +/- 0.04 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B V) = 0.04 in the direction of the burst (Schlegel et al. 1998). This circular is an official product of the Swift team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14974 SUBJECT: IPN localization of GRB 130702A (= Fermi 394416326) DATE: 13/07/03 19:03:54 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team, V. Connaughton, M. S. Briggs, C. Meegan, and V. Pelassa, on behalf of the Fermi GBM team, S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, D. Svinkin, and T. Cline, on behalf of the Konus-Wind team, 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: MESSENGER (GRNS), INTEGRAL (SPI-ACS), Fermi-GBM, and Konus-Wind have detected GRB 130702A (= Fermi 394416326) so far. We have triangulated this burst to an annulus centered at RA, Dec (2000) = 293.0106 degrees, -18.3126 degrees, whose radius is 82.0991 +/- 0.4594 degrees (3 sigma). The distance between the annulus center line and the iPTF optical transient reported by Singer et al. (GCN 14967) is 0.16 degrees, strengthening the association of the transient with the GRB. A map has been posted at ssl.berkeley.edu/ipn3/130702 showing the annulus, the Fermi LAT position (GCN 14971), and the optical transient. This localization may be improved. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14975 SUBJECT: GRB 130702A / Fermi394416326 : Nanshan optical observations DATE: 13/07/03 19:20:27 GMT FROM: Dong Xu at DARK/NBI D. Xu (DARK/NBI), A. Esamdin, L. Ma, X. Zhang (XAO) report: We observed the field of GRB 130702A / Fermi394416326 (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi et al., GCN 14972) using the 1m telescope located at Mt. Nanshan, Xinjiang Astronomical Observatory, China. We obtained 3x600s R-band frames, starting from 17:43:25 UT on 2013-07-03 (i.e., 1.735 days after the Fermi trigger). The optical transient reported in Singer et al. (GCN 14967) is clearly detected in each of the frames. However, it is slightly overlapped with its nearby bright galaxy, SDSS J142914.57+154619.3, due to seeing and technical constraints. The transient has decayed to R~18.9, calibrated with two bright SDSS stars converted to Johnson R. The continuous decay makes it likely the optical counterpart of GRB 130702A / Fermi394416326. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14977 SUBJECT: GRB 130702A: TNG optical observations DATE: 13/07/04 00:29:16 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, A. Melandri (INAF-OAB), G. Andreuzzi, G. Mainella (INAF/FGG) , report on behalf of the CIBO collaboration: We observed the optical counterpart of the Fermi GRB 130702A (Cheung et al. GCN 14971; Collazzi et al. GCN 14972) with the Italian 3.6m TNG telescope located in Canary Islands, equipped with the DOLoRes imager. Observations were carried out starting on 2013 Jul 3.955 UT (1.95 days after the Fermi/GBM trigger). In a single 300 seconds exposures obtained in the SDSS r band we clearly detect the optical afterglow reported by Singer et al. (GCN 14697) with a magnitude of r=19.1 (calibrated against nearby SDSS stars). Further observations are ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14978 SUBJECT: GRB 130702A: NOT optical observations DATE: 13/07/04 01:08:19 GMT FROM: Steve Schulze at U of Iceland S. Schulze (PUC, MCSS), D. Xu (DARK/NBI), D. A. Kann (TLS Tautenburg), D. Malesani (DARK/NBI), S. Geier (NOT, DARK/NBI), P. Jakobsson (U. Iceland) report on behalf of a larger collaboration: We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi et al., GCN 14972) with 2.5m the Nordic Opitcal Telescope (NOT) equipped with ALFOSC. We obtained 1 x 120 s each in the r' and i' bands. Observations started at 23:36:59 UT on July 03 (i.e., 47.53 hrs after the burst). The source reported in Singer et al. (GCN 14967) is clearly detected in both images. It has an r'-band magnitude of 19.13 +/- 0.01 mag and an i' band magnitude of 18.82 +/- 0.01 mag (AB magnitude). The mid-exposure times are 47.5432 and 47.5900 hrs after trigger in r' and i',. The source faded by ~0.4 mag with respect to Singer et al. (GCN 14967). We create a light curve using the Rc/r' data of of Singer et al. (GCN 14967), Guidorzi et al. (GCN 14968) and Xu et al. (GCN 14975), and find a slope of alpha = 0.58, in agreement with that of Singer et al. Compared to all known GRB afterglows, the afterglow of GRB 130702A is among the brightest, of similar brightness as that of GRB130427A at the time of our observation (Xu et al. 2013, arXiv:1305.6832). Calibration was done against SDSS J142915.86+154510.0 and SDSS J142911.60+154535.1 from SDSS DR9. We did not correct for Galactic foreground extinction. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14979 SUBJECT: GRB 130702A: CARMA 3mm detection DATE: 13/07/04 06:15:19 GMT FROM: Daniel Perley at Caltech D. A. Perley (Caltech) and M. Kasliwal (Carnegie) report on behalf of a larger collaboration: We observed the location of the probable optical counterpart of Fermi GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi & Connaughton, GCN 14972) with the Combined Array for Research in Millimeter Astronomy (CARMA) on 2013-07-04 between 00:28:21 and 05:56:31 UT, 2.01-2.24 days after the GBM trigger, at a frequency of 93 GHz (3 mm). Weather conditions were poor initially but improved somewhat over the course of the integration. In a preliminary reduction of the data we detect a millimeter source coincident with the location of the optical counterpart with a flux of approximately ~2 mJy. We thank John Carpenter and the CARMA staff for their support. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14980 SUBJECT: GRB 130702A: RATIR Optical and NIR Observations DATE: 13/07/04 07:13:58 GMT FROM: Nat Butler at Az State U Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), José A. de Diego (UNAM), Leonid Georgiev (UNAM), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report: We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi & Connaughton, GCN 14972) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir from 2013/07 4.16 to 2013/07 4.25 UTC (51.79 to 53.82 hours after the BAT trigger), obtaining a total of 1.42 hours exposure in the r' and i' bands and 0.60 hours exposure in the Z, Y, J, and H bands. At the position of the source from Singer et al. (GCN 14967), in comparison with SDSS DR9 and 2MASS, we obtain the following detections: r' 19.22 +/- 0.01 i' 19.06 +/- 0.02 Z 18.85 +/- 0.03 Y 18.70 +/- 0.03 J 18.72 +/- 0.03 H 18.56 +/- 0.03 These magnitudes are in the AB system and not corrected for Galactic extinction in the direction of the GRB. Further observations are underway. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14981 SUBJECT: GRB 130702A: Continued P60 observations DATE: 13/07/04 08:05:48 GMT FROM: Daniel Perley at Caltech D. A. Perley, L. P. Singer (Caltech), and S. B. Cenko (GSFC) report: We obtained additional observations of the location of the probable afterglow of GRB 130702A with the Palomar 60-inch robotic telescope. A series of repeated imaging sequences were taken in B, g, r, i, and z filters during intermittent clouds. Example photometry from one sequence is as follows: tstart(d) exp(s) filt mag unc 2.20405 120 i = 19.129 +/- 0.05 2.20565 120 r = 19.297 +/- 0.05 2.20728 120 B = 19.635 +/- 0.07 2.20888 120 z = 19.204 +/- 0.16 2.21048 120 g = 19.519 +/- 0.08 Compared to our previous night's P60 observations (Singer et al., GCN 14967) and referenced to the GBM trigger time (Collazzi et al., GCN 14972), the fading is consistent with a power law with decay index of approximately alpha=1.1, steeper than that inferred during the first 24 hours. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14982 SUBJECT: GRB 130702A: further Swift-XRT observations DATE: 13/07/04 09:31:33 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, A. Melandri (INAF-OAB), P. A. Evans (Univ Leicester) report on behalf of the Swift-XRT team: We have analysed 6.2 ks of XRT data for the Fermi GRB 130702A (Cheung et al. GCN 14971; Collazzi et al. GCN 14972), from 89.1 ks to 153.4 ks after the Fermi/GBM trigger. The data are entirely in Photon Counting (PC) mode. We confirm the fading of the X-ray afterglow reported in D'Avanzo et al. (GCN 14973). The light curve can be modelled with a power-law decay with a decay index of alpha=0.57 (+0.21, -0.20). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14983 SUBJECT: GRB 130702A: NOT spectroscopy and redshift of the nearby bright galaxy DATE: 13/07/04 13:10:00 GMT FROM: Giorgos Leloudas at Dark Cosmology Centre G. Leloudas (OKC, Stockholm and DARK/NBI), J. P. U. Fynbo (DARK/NBI), S. Schulze (PUC, MCSS), D. Xu (DARK/NBI), D. Malesani (DARK/NBI), S. Geier (NOT, DARK/NBI), Z. Cano(U. Iceland), P. Jakobsson (U. Iceland) report on behalf of a larger collaboration: We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi et al., GCN 14972) with the Nordic Opitcal Telescope (NOT) equipped with ALFOSC. In addition to our photometric observations (reported in Schulze et al., GCN 14978), we obtained an optical spectrum, with a total exposure of 2 x 1800 s, using Grism #4 and covering the wavelength range 3750 - 9000 AA at a resolution of 17 AA. The slit was oriented to cover both the transient source (also dubbed iPTF13bxl) that has been suggested to be the afterglow of GRB 130702A, and the bright SDSS galaxy located 7.6" South of the source (SDSS J142914.57+154619.3; Singer et al., GCN 14967). The galaxy is found to be at z = 0.145, based on Ca II H & K absorption and emission by [OII] and Halpha. The emission features are weak and we do not detect Hbeta or [OIII]. Overall, and combined with the SDSS colors, this galaxy shows very weak star formation activity. This redshift is consistent with the redshift of the transient source reported by Mulchaey et al. (ATel 5191) and the description given there. The trace of our NOT spectrum at the location of the transient is mostly featureless and we cannot detect the emission lines reported by Mulchaey et al., probably due to a lower S/N. The common redshift suggests that the transient source iPTF13bxl is associated with the galaxy SDSS J142914.57+154619.3. If this transient is indeed the afterglow of GRB 130702A at z = 0.145, it implies an E_iso = (3.0 +- 1.0) * 10^50 erg in the 10-1000 keV (Collazzi et al., GCN 14972). We note that this is an unusual environment for a long GRB: located at a large offset (19.1 kpc in projection) from a relatively passive galaxy. However, we cannot exclude that more sources in the field, including the fainter (r ~ 23 mag) object at 0.6" from the transient (SDSS J142914.75+154626.0; Singer et al., GCN 14967) might be at the same redshift. A possible confirmation of the GRB nature of this transient will be the emergence of an associated supernova. At z = 0.145, a supernova similar to SN 1998bw will peak at R ~ 19.8 mag about 20 days after the GRB, and will be easily detectable. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14984 SUBJECT: GRB 130702A: further TNG observations DATE: 13/07/04 15:44:22 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo (INAF-OAB), V. D'Elia (ASI/ASDC), G. Tagliaferri, A. Melandri (INAF-OAB), D. Malesani (DARK/NBI), M. Della Valle (INAF-OAC), E. Pian (SNS) report on behalf of the CIBO collaboration: We observed the optical counterpart of the Fermi GRB 130702A (Cheung et al. GCN 14971; Collazzi et al. GCN 14972) with the Italian 3.6m TNG telescope located in Canary Islands, equipped with the DOLoRes imager. In addition to what reported in D'Avanzo et al. (GCN 14977), further observations were carried out between Jul 3.955 UT and Jul 4.022 UT (1.95-2.02 days after the Fermi GBM trigger). The optical afterglow is clearly detected in the SDSS g, r, and i bands with the following magnitudes: g=19.3 r=19.1 i=19.0 calibrated against nearby SDSS stars. We also obtained a 2400 seconds spectrum with the LR-B grism, covering the wavelength range 3900-8200 AA with a resolution of R~600. The spectrum has a high S/N and shows a blue continuum nearly featureless. Very faint emission lines can be interpreted as [OII] 3727.5, [OIII] 4959.0/5006.8 and Halpha 6562.8 at a common redshift of 0.145, consistent with what reported by Mulchaey et al. (ATel 5191) for the optical afterglow spectrum and by Leloudas et al. (GCN circ. 14983) for the spectrum of the nearby SDSS galaxy. We acknowledge the TNG staff for excellent support, in particular G. Andreuzzi and G. Mainella. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14985 SUBJECT: GRB130702A: Redshift of Afterglow Candidate iPTF13bxl DATE: 13/07/04 16:09:08 GMT FROM: Mansi M. Kasliwal at Caltech/Carnegie J. Mulchaey (Carnegie), M. M. Kasliwal (Carnegie), I. Arcavi (Weizmann), E. Bellm (Caltech) and D. Kelson (Carnegie) report on behalf of a larger collaboration: We obtained a high SNR low-resolution spectrum of iPTF13bxl (GCN#14967) with IMACS on the 6.5m Magellan telescope at Las Campanas on 2013 July 3.97 covering 3800A-9500A. We also obtained another spectrum with the DBSP spectrograph on the 5m Hale telescope at Palomar at July 4.16. The spectra show a blue continuum with weak H-alpha and O III emission at z=0.145. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14986 SUBJECT: Konus-Wind observation of GRB 130702A DATE: 13/07/04 17:49:17 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team report: The long GRB 130702A (= Fermi 394416326; Optical and X-ray transient discovery: Singer et al., GCN 14967; Fermi-LAT detection: Cheung et al., GCN 14971; Fermi GBM detection: Collazzi & Connaughton, GCN 14972; IPN localization: Huley et al., GCN 14974) was detected by Konus-Wind in the waiting mode. The burst light curve shows a FRED-like pulse with a duration of ~26 s. As observed by Konus-Wind, the burst had a fluence of 6.70(-0.80,+0.82)10^-6 erg/cm2 (in the 20 - 1200 keV energy range). Fitting the K-W 3-channel time-integrated spectrum (from T0(GBM)-2.8 s to T0(GBM)+23.7 s) by a simple power-law model yields a power law index of 1.87 +/- 0.11. Assuming z = 0.145 (Kasliwal et al., GCN 14985; Leloudas et al. GCN 14983) and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, Omega_Lambda = 0.73, the isotropic energy release is E_iso = 6.36(-1.03,+1.34)x10^50 erg in 1 keV to 10 MeV at the GRB rest frame extrapolating the best power-law function fit. All the quoted errors are at the 90% confidence level. The results presented above are preliminary. The K-W light curve of this burst is available at http://www.ioffe.rssi.ru/LEA/GRBs/GRB130702A/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14987 SUBJECT: GRB 130702A: WSRT radio detection DATE: 13/07/05 09:35:55 GMT FROM: Alexander van der Horst at U of Amsterdam A.J. van der Horst (University of Amsterdam) reports on behalf of a large collaboration: "We observed the position of the GRB 130702 afterglow at 4.9 GHz with the Westerbork Synthesis Radio Telescope at July 4 13.55 UT to July 5 01.17 UT, i.e. 2.56 - 3.05 days after the burst (GCN 14972). We detect a radio source with a flux density of 1.23 +/- 0.04 mJy at the position of the optical counterpart (GCN 14967). We would like to thank the WSRT staff for quickly scheduling and obtaining these observations." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14988 SUBJECT: GRB 130702Ð DATE: 13/07/05 14:48:13 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI), A. Volnova (IKI), O. Burhonov (UBAI), I. Molotov (KIAM) report on behalf GRB follow-up collaboration: We observed the field of OT (Singer et al., GCN 14967) of GRB 130702¿ (= Fermi 394416326)(Cheung et al., GCN 14971; Collazzi et al., GCN 14972) with AZT-22 telescope of Maidanak observatory on Jul. 3 and Jul. 4 under good weather conditions and seeing (FWHM) of about 1 arcsec. We clearly detected OT (Singer et al., GCN 14967) in each images of both epochs. A preliminary photometry of combined images is based on the two SDSS stars suggested by Schulze et al. (GCN 14978), i.e. SDSS J142915.86+154510.0 assuming R = 16.03 SDSS J142911.60+154535.2 assuming R = 15.59 T_start T0+ Filter, Exposure, OT (UT) (mid, d) (s) 2013-07-03T17:38:18 1.70828 R 6x600 18.69 +/- 0.03 2013-07-04T16:49:20 2.67427 R 6x300 19.31 +/- 0.04 We note that the fading of a lc assuming a power law between our two epochs is alpha=1.27 which is steeper, than reported in early observations (Perley et al., GCN 14981). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14989 SUBJECT: GRB 130702A (= Fermi 394416326): correction of the GCN #14988 title DATE: 13/07/05 15:08:22 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI) report on behalf larger GRB follow-up collaboration: A title of GCN circular #14988 should be read as "GRB 130702A (= Fermi 394416326): Maidanak optical observations" We apologize for possible inconvenience. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14990 SUBJECT: GRB 130702A: VLA detection DATE: 13/07/05 20:23:22 GMT FROM: Alessandra Corsi at GWU A. Corsi (GWU), D. A. Perley (Caltech), and S. B. Cenko (GSFC) report: We observed the location of iPTF13bxl, the optical counterpart to GRB 130702A (Singer et al., GCN 14967), with the Karl G. Jansky Very Large Array in C-band on 2013-07-04 UT, 2.29 days after the GBM trigger. We detect a radio source at this location with a flux of 1.49 mJy at 5.1 GHz, and 1.60 mJy at 7.1 GHz. The map noise is 0.011 mJy. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14991 SUBJECT: GRB 130702A: Continued UVOT Observations DATE: 13/07/05 23:04:12 GMT FROM: Mike Siegel at PSU/Swift MOC GRB 130702A: Continued UVOT Observations B. Porterfield (PSU), M. Siegel (PSU) and P. D'Avanzo (INAF-OAB) report on behalf of the Swift/UVOT team: Swift reobserved the field of GRB 130702A on July 4 and July 5 2013. We confirm the slow fading of the source first reported by Singer et al. (GCN Circ. 14973) and previously reported in UVOT by D'Avanzo et al. (GCN Circ. 14973). We also note that we detect the transient in all four of UVOT's NUV filters, which is consistent with the low redshift reported by Leloudas et al. (GCN Circ. 14983) and D'Avanzo et al. (GCN Circ. 14984). Preliminary detections using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) are: Filter T_start(s) T_stop(s) Exp(s) Mag u 151366 153361 1962 18.48+-0.05 u 203252 205246 1962 18.97+/-0.07 u 250292 255654 272 19.51+/-0.26 uvw1 249967 255532 629 19.29+/-0.17 uvm2 251591 252014 415 19.67+/-0.28 uvw2 284670 285309 629 19.26+/-0.14 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.04 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14992 SUBJECT: GRB 130702A: Xinglong TNT optical observation DATE: 13/07/07 14:51:36 GMT FROM: L.P. Xin at NAOC L.P. Xin, J. Y. Wei, Y.L. Qiu, J. Wang, J.S. Deng, C. Wu, X. H. Han on behalf of EAFON report: We began to observe the optical counterpart of the Fermi GRB 130702A ( Singer et al. GCN 14967; Collazzi et al. GCN 14972 ) with Xinglong TNT telescope between 14:10:35 and 15:37:22 UT on 5 June, 2013. 15*300 sec R-band images were obtained. The optical counterpart was found with a magnitude of R~19.7 mag, calibrated by USNO-B 1.0 R2 mag, at the mean time of 3.62 days after the burst. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14993 SUBJECT: GRB 130702A: Continued RATIR Optical and NIR Observations DATE: 13/07/07 16:21:05 GMT FROM: Nat Butler at Az State U Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), José A. de Diego (UNAM), Leonid Georgiev (UNAM), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report: We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi & Connaughton, GCN 14972) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir on the nights of 2013/07/06 and 2013/07/07 (4.25 and 5.26 days after the BAT trigger), obtaining a total of 1.4 hours exposure in the r' and i' bands and 0.6 hours exposure in the Z, Y, J, and H bands each night. At the position of the source from Singer et al. (GCN 14967), in comparison with SDSS DR9 and 2MASS, we obtain the following detections: 7/06 7/07 r' 19.86 +/- 0.02 19.94 +/- 0.02 i' 19.89 +/- 0.03 20.02 +/- 0.02 Z 19.68 +/- 0.05 19.76 +/- 0.04 Y 19.46 +/- 0.05 19.69 +/- 0.05 J 19.64 +/- 0.07 19.64 +/- 0.06 H 19.36 +/- 0.08 19.69 +/- 0.08 The source appears to be slowly fading, approximately 0.1 mag/day, or approximately as t^-0.35. This is a significant flattening relative to the bright fluxes we measured 2 days after the GRB (Butler et al.; GCN 14980). These magnitudes are in the AB system and not corrected for Galactic extinction in the direction of the GRB. Further observations are underway. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14994 SUBJECT: GRB130702A: NOT observation - the detection of an emerging supernova DATE: 13/07/08 04:31:28 GMT FROM: Steve Schulze at U of Iceland S. Schulze (PUC, MCSS), G. Leloudas (OKC, Stockholm and DARK/NBI), D. Xu, J. P. U. Fynbo (DARK/NBI), S. Geier (NOT, DARK/NBI) and P. Jakobsson (U Iceland) report on behalf a larger collaboration: We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi et al., GCN 14972) with the 2.5-m Nordic Optical Telescope (NOT) equipped with ALFOSC. We obtained 1 x 150 s in r' and 5 x 60 in i'. Observations started at 23:23:10 UT on July 07 (i.e. 5.97 days after the burst). We measure r' = 20.03 and i' = 20.21 mag. The afterglow became clearly brighter in r'-band with respect to our observation from the night before. Compared to our first observation on 3 July (Schulze et al. GCN 14978), the colour changed from 0.13 to -0.19 mag. This colour evolution is consistent with Butler et al. (GCN 14993), who reported a colour change of -0.08 mag between 4.25 and 5.26 days after the burst. Such a colour evolution is not expected for a decaying optical afterglow but clearly points to an emerging supernova. We obtained an optical low-resolution spectrum with the ALFOSC camera starting at 23:45:33 UT. We used grism #4 that covers the wavelength range from 3750 to 9000 AA. The observation consisted of three individual spectra with a total exposure time of 3x1200 s. The flux-calibrated spectrum presents clear deviations from a power law. In particular, we identify two broad emission features peaking at 4900 and 5600 AA with a local minimum at 5200 AA (all observer frame). Assuming z=0.145 (Mulcaey et al. ATel 5191, GCN 14985; Leloudas et al. GCN 14983; D'Avanzo et al. GCN 14984), the spectrum resembles SN 1998bw at phase 7-8 days past explosion (Patat et al. 2001, ApJ, 555, 900). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14996 SUBJECT: GRB 130702A: Maidanak optical observations DATE: 13/07/09 10:46:20 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI), A. Volnova (IKI), O. Burhonov (UBAI), I. Molotov (KIAM) report on behalf of larger GRB follow-up collaboration: We continue observations of the afterglow (Singer et al., GCN 14967) of GRB 130702A (Cheung et al., GCN 14971; Collazzi et al., GCN 14972) with AZT-22 telescope of Maidanak observatory. A preliminary photometry of combined images is based on two SDSS stars suggested by Schulze et al. (GCN 14978) and used in our previous observations (Pozanenko et al, GCN 14988) T_start T0+ Filter, Exposure, OT (UT) (mid, d) (s) 2013-07-05T16:25:11 3.6592 R 6x600 19.61+/-0.02 2013-07-06T16:20:12 4.6540 R 6x600 19.71+/-0.03 2013-07-07T16:45:34 5.6717 R 6x600 19.83+/-0.04 2013-07-08T16:49:14 6.6759 R 6x300 19.81+/-0.05 The light curve is based on the photometry of this CGN circular and our previous observations (Pozanenko et al, GCN 14988) and can be found at http://grb.rssi.ru/GRB130702A/GRB130702A_MAO_R_lc.png One can see flattening of the lc after 4 days (initially reported by Butler et al., GCN 14993) and possible re-brightening on 6.6 days which can confirm re-brightening of the afterglow (Schulze et al., GCN 14994) and emerging supernova. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14998 SUBJECT: GRB 130702A: P200 Spectroscopic Confirmation of Associated Supernova DATE: 13/07/10 00:28:32 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko (NASA/GSFC), A. Gal-Yam (Weizmann Institute), M. M. Kasliwal (OCIW), D. Stern (JPL), K. Markey, E. Alduena, A. Alduena, and S. Kuo (Walden) report on behalf of a larger collaboration: We have obtained further spectroscopy of the optical afterglow (Singer et al., GCN 14967) of the Fermi-GBM (Collazzi et al., GCN 14972), Fermi-LAT (Cheung et al., GCN 14971), and IPN (Hurley et al., GCN 14974) GRB 130702A. Observations were obtained with the Double Spectrograph mounted on the 5 m Palomar Hale telescope beginning at 5:27 UT on 2013 July 8 (6.2 days after the Fermi GBM trigger) and cover the wavelength range from 3400-8900 A. Compared with our previous optical spectra (Mulchaey et al., GCN 14985), the source shows a significantly redder continuum. Similar to Schulze et al. (GCN 14994), a number of broad features are detected that are reminiscent of canonical GRB-associated supernovae such as SN 2006aj and SN 1998bw. A plot of our most recent spectrum, alongside comparable epochs from SN 2006aj (Modjaz et al., ApJL, 2006, 645, 21) and SN 1998bw (Patat et al., ApJ, 2001, 555, 900), both retrieved from the Weizmann Interactive Supernova Data Repository (WISEREP; http://www.weizmann.ac.il/astrophysics/wiserep/) is available here: http://astro.berkeley.edu/~cenko/public/grb/GRB130702A/GRB130702A_20130708.png //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15000 SUBJECT: GRB 130702A: TNG spectroscopic observations of the emerging supernova DATE: 13/07/10 13:35:24 GMT FROM: Valerio D'Elia at ASDC V. D'Elia (ASI/ASDC, INAF-OAR), P. D'Avanzo (INAF-OAB), D. Fugazza (INAF-OAB), A. Melandri (INAF-OAB), M. Della Valle (INAF-OAC), G. Tagliaferri (INAF-OAB), D. Malesani (DARK/NBI), E. Pian (SNS), L. A. Antonelli, S. Piranomonte (INAF-OAR), A. Harutyunyan, D. Carosati (INAF/TNG) report on behalf of the CIBO collaboration: We continued monitoring the optical counterpart of the Fermi GRB 130702A (Singer et al., GCN 14967, Cheung et al. GCN 14971; Collazzi et al. GCN 14972) with the Italian 3.6m TNG telescope located in the Canary Islands, equipped with the DOLoRes camera. In addition to what reported in D'Avanzo et al. (GCN 14977, GCN 14984), further observations were carried out during the nights of Jul 5 and Jul 9 (4 and 8 days after the Fermi GBM trigger). At a mean t-t0=7.92 days we detect the optical counterpart in the SDSS r band with a magnitude of 19.91 (calibrated against nearby SDSS stars). This value is consistent with our previous epoch obtained 4 days before, confirming the flattening of the optical light curve reported by (Perley et al. GCN 14981, Butler et al. GCN 14993, Schulze et al. GCN 14994, Pozanenko et al. GCN 14996). We also obtained a 2000 seconds spectrum with the LR-B grism, starting at t-t0=7.92 days, covering the wavelength range 3900-8200 AA with a resolution of R~600. With respect to our previous epoch observation which featured a blue, featureless continuum (D'Avanzo et al. GCN 14984), the spectrum is now considerably redder, and shows a number of broad features similar to GRB-associated supernovae. In particular, the shape of the continuum closely resembles the spectrum of SN 1998bw observed at a similar epoch, despite a prominent feature at 4300 AA rest frame, reminiscent of what seen in SN 2006aj (Pian et al. 2006, Nature, 442, 1011). This confirms the emerging of the supernova already reported by Schulze et al. (GCN 14994) and Cenko et al. (GCN 14998). We acknowledge support from the TNG visiting astronomer K. Biazzo. [GCN OPS NOTE(10jul13): Per author's request, DF was added to the author list.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15002 SUBJECT: GMRT radio detection of GRB 130702A DATE: 13/07/11 10:30:07 GMT FROM: Poonam Chandra at TIFR Poonam Chandra (NCRA-TIFR) reports: We carried out Giant Metrewave Radio Telescope (GMRT) observations of GRB 130702A at 1390 and 610 MHz bands on 2013 July 10.54 UT and 10.72 UT, respectively. We detect the radio afterglow of the GRB in both bands. The 1390 MHz band flux density of the afterglow is 792+/-44 uJy and 610 MHz flux density of the afterglow is 457+/-75 uJy. The map resolutions at 1390 and 610 MHz bands are 2.67"x2.26" and 8.91"x5.50", respectively. Further observations are planned. We thank GMRT staff for making these observations possible. -- ********************************************************************** Poonam Chandra Phone: +91 20 2571 9290 Tata Institute of Fundamental Research Email: poonam@ncra.tifr.res.in National Center for Radio Astrophysics Home: ncra.tifr.res.in/~poonam Post Bag 3, Pune University campus Ganeshkhind, Pune 411 008, INDIA //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15003 SUBJECT: GRB 130702A: Maidanak optical observations DATE: 13/07/11 16:11:27 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI), A. Volnova (IKI), O. Burhonov (UBAI), I. Molotov (KIAM) report on behalf of larger GRB follow-up collaboration: We continue observations of the afterglow (Singer et al., GCN 14967) of GRB 130702A (Cheung et al., GCN 14971; Collazzi et al., GCN 14972) with AZT-22 telescope of Maidanak observatory. A preliminary photometry of combined images is based on two SDSS stars suggested by Schulze et al. (GCN 14978) and used in our previous observations (Pozanenko et al, GCNs 14988, 14996) T_start T0+ Filter, Exposure, OT (UT) (mid, d) (s) 2013-07-09T16:50:52 7.6771 R 7x600 19.73+/-0.04 2013-07-10T17:18:05 8.6931 R 6x600 19.64+/-0.03 The light curve can be found at http://grb.rssi.ru/GRB130702A/GRB130702A_MAO_R_lc.png It is clearly visible in the lc a rising SN (Schulze et al., GCN 14994; Cenko et al., GCN 1998; D'Elia et al., GCN 15000). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15009 SUBJECT: GRB 130702A : Xinglong TNT continue optical observation DATE: 13/07/18 09:16:10 GMT FROM: L.P. Xin at NAOC L.P. Xin, J. Y. Wei, Y.L. Qiu, J. Wang, J.S. Deng, C. Wu, X. H. Han on behalf of EAFON report: We continue to observe the optical counterpart of the Fermi GRB 130702A ( Singer et al. GCN 14967; Collazzi et al. GCN 14972 ) with Xinglong TNT telescope at 13:42:16.031 UT on 16 July, 2013 under a bad weather. 6*300 sec R-band images were obtained. The brightness of the optical afterglow was found with a magnitude of R~19.6 +/-0.2 mag, calibrated by USNO-B 1.0 R2 mag of the two stars (Schulze et al. GCN 14978; Pozanenko et al. GCN 15003), at the mean time of 14.57 days after the burst. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15025 SUBJECT: GRB 130702A in the Ep,i - Eiso plane DATE: 13/07/23 13:50:35 GMT FROM: Lorenzo Amati at INAF-IASF/Bologna L. Amati (INAF - IASF Bologna), S. Dichiara, F. Frontera, C. Guidorzi (University of Ferrara), Luca Izzo (ICRANet, Rome), M. Della Valle (INAF-Osservatorio Astronomico di Capodimonte) report: A preliminary analysis of the spectral data of GRB130702A provided by the Fermi/GBM integrated over the whole duration of the event (63.3 s from T0-3.0 to T0 +60.3; detectors n7 and n8) suggests that the spectrum can be fit with a simple power-law with index ~2.1+/-0.1, which is significantly softer than the value obtained by considering only the brightest part of the event (Collazzi & Connaughton GCN 14972; Golenetskii et al. GCN 14986). This result indicates that the spectral peak energy, Ep, is close to the low energy threshold of the instrument or lower than it. After fitting the spectrum with a Band function with alpha fixed at different values and by assuming the redshift of 0.145 (e.g., Leloudas et al. GCN 14983; Mulchaey et al. GCN 14985), we find a 90% upper limit to the cosmological rest-frame peak energy, Ep,i, of ~15-20 keV and and isotropic-equivalent radiated energy, Eiso, of ~(6.5+/-0.10)x10^50 erg (flat FLRW Universe with H0=70 km/s/Mpc and Omega_M = 0.3). Based on these estimates, GRB 130702A is consistent with the Ep,i - Eiso correlation holding for typical long GRBs and lies in the region bridging classical cosmological long GRBs with closer and weaker GRB-SN events like GRB060218/SN2006aj and XRF020903 (see http://www.iasfbo.inaf.it/~amati/grb130702a.pdf). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15243 SUBJECT: GRB 130702A: RTT150 optical observations DATE: 13/09/23 09:59:57 GMT FROM: Rodion Burenin at IKI, Moscow G. Khorunzhev, A. Volnova, A. Pozanenko, R. Burenin, M. Pavlinsky, R. Sunyaev (IKI), I. Bikmaev, N. Sakhibullin (KFU/AST), I. Khamitov, H. Kirbiyik (TUG) report: We observed the afterglow of Fermi GRB 130702A (Singer et al., GCN 14967, Cheung et al., GCN 14971; Collazzi et al., GCN 14972), and their progenitor Supernova SN 2013dx (Schulze et al. GCN 1994; Cenko et al. GCN 14998) with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National Observatory, Turkey) on Aug., 28 starting at UT 18:21:58. We obtained several images with exposure of 300 seconds in R band. A preliminary photometry of the GRB afterglow + SN 2013dx + host galaxy, based on two SDSS stars suggested by Schulze et al. (GCN 14978): T_start T0+ Filter, Exposure, OT (UT) (mid, d) (s) 2013-08-28T18:21:58 57.74046 R 6x300 21.47+/-0.08