GRB 130702A, GRB 130702
GCN Circular 15243
Subject
GRB 130702A: RTT150 optical observations
Date
2013-09-23T09:59:57Z (13 years ago)
From
Rodion Burenin at IKI, Moscow <rodion@hea.iki.rssi.ru>
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
GCN Circular 15025
Subject
GRB 130702A in the Ep,i - Eiso plane
Date
2013-07-23T13:50:35Z (13 years ago)
From
Lorenzo Amati at INAF-IASF/Bologna <amati@iasfbo.inaf.it>
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).
GCN Circular 15009
Subject
GRB 130702A : Xinglong TNT continue optical observation
Date
2013-07-18T09:16:10Z (13 years ago)
From
L.P. Xin at NAOC <xlp@bao.ac.cn>
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.
GCN Circular 15003
Subject
GRB 130702A: Maidanak optical observations
Date
2013-07-11T16:11:27Z (13 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
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).
GCN Circular 15002
Subject
GMRT radio detection of GRB 130702A
Date
2013-07-11T10:30:07Z (13 years ago)
From
Poonam Chandra at TIFR <poonam@ncra.tifr.res.in>
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
GCN Circular 15000
Subject
GRB 130702A: TNG spectroscopic observations of the emerging supernova
Date
2013-07-10T13:35:24Z (13 years ago)
From
Valerio D'Elia at ASDC <delia@asdc.asi.it>
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.]
GCN Circular 14998
Subject
GRB 130702A: P200 Spectroscopic Confirmation of Associated Supernova
Date
2013-07-10T00:28:32Z (13 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
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
GCN Circular 14996
Subject
GRB 130702A: Maidanak optical observations
Date
2013-07-09T10:46:20Z (13 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
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.
GCN Circular 14994
Subject
GRB130702A: NOT observation - the detection of an emerging supernova
Date
2013-07-08T04:31:28Z (13 years ago)
From
Steve Schulze at U of Iceland <sts30@hi.is>
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).
GCN Circular 14993
Subject
GRB 130702A: Continued RATIR Optical and NIR Observations
Date
2013-07-07T16:21:05Z (13 years ago)
Edited On
2024-11-07T20:01:46Z (2 years ago)
From
Nat Butler at Az State U <natbutler@asu.edu>
Edited By
Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
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.
GCN Circular 14992
Subject
GRB 130702A: Xinglong TNT optical observation
Date
2013-07-07T14:51:36Z (13 years ago)
From
L.P. Xin at NAOC <xlp@bao.ac.cn>
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.
GCN Circular 14991
Subject
GRB 130702A: Continued UVOT Observations
Date
2013-07-05T23:04:12Z (13 years ago)
From
Mike Siegel at PSU/Swift MOC <siegel@swift.psu.edu>
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).
GCN Circular 14990
Subject
GRB 130702A: VLA detection
Date
2013-07-05T20:23:22Z (13 years ago)
From
Alessandra Corsi at GWU <corsi@email.gwu.edu>
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.
GCN Circular 14989
Subject
GRB 130702A (= Fermi 394416326): correction of the GCN #14988 title
Date
2013-07-05T15:08:22Z (13 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
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.
GCN Circular 14988
Subject
GRB 130702Ð
Date
2013-07-05T14:48:13Z (13 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
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).
GCN Circular 14987
Subject
GRB 130702A: WSRT radio detection
Date
2013-07-05T09:35:55Z (13 years ago)
From
Alexander van der Horst at U of Amsterdam <A.J.vanderHorst@uva.nl>
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."
GCN Circular 14986
Subject
Konus-Wind observation of GRB 130702A
Date
2013-07-04T17:49:17Z (13 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
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/
GCN Circular 14985
Subject
GRB130702A: Redshift of Afterglow Candidate iPTF13bxl
Date
2013-07-04T16:09:08Z (13 years ago)
From
Mansi M. Kasliwal at Caltech/Carnegie <mansikasliwal@gmail.com>
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.
GCN Circular 14984
Subject
GRB 130702A: further TNG observations
Date
2013-07-04T15:44:22Z (13 years ago)
From
Paolo D'Avanzo at INAF-OAB <paolo.davanzo@brera.inaf.it>
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.
GCN Circular 14983
Subject
GRB 130702A: NOT spectroscopy and redshift of the nearby bright galaxy
Date
2013-07-04T13:10:00Z (13 years ago)
From
Giorgos Leloudas at Dark Cosmology Centre <giorgos@dark-cosmology.dk>
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.
GCN Circular 14982
Subject
GRB 130702A: further Swift-XRT observations
Date
2013-07-04T09:31:33Z (13 years ago)
From
Paolo D'Avanzo at INAF-OAB <paolo.davanzo@brera.inaf.it>
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.
GCN Circular 14981
Subject
GRB 130702A: Continued P60 observations
Date
2013-07-04T08:05:48Z (13 years ago)
From
Daniel Perley at Caltech <dperley@astro.caltech.edu>
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.
GCN Circular 14980
Subject
GRB 130702A: RATIR Optical and NIR Observations
Date
2013-07-04T07:13:58Z (13 years ago)
Edited On
2024-11-07T20:00:12Z (2 years ago)
From
Nat Butler at Az State U <natbutler@asu.edu>
Edited By
Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
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.
GCN Circular 14979
Subject
GRB 130702A: CARMA 3mm detection
Date
2013-07-04T06:15:19Z (13 years ago)
From
Daniel Perley at Caltech <dperley@astro.caltech.edu>
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.
GCN Circular 14978
Subject
GRB 130702A: NOT optical observations
Date
2013-07-04T01:08:19Z (13 years ago)
From
Steve Schulze at U of Iceland <sts30@hi.is>
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.
GCN Circular 14977
Subject
GRB 130702A: TNG optical observations
Date
2013-07-04T00:29:16Z (13 years ago)
From
Paolo D'Avanzo at INAF-OAB <paolo.davanzo@brera.inaf.it>
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.
GCN Circular 14975
Subject
GRB 130702A / Fermi394416326 : Nanshan optical observations
Date
2013-07-03T19:20:27Z (13 years ago)
From
Dong Xu at DARK/NBI <dong.dark@gmail.com>
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.
GCN Circular 14974
Subject
IPN localization of GRB 130702A (= Fermi 394416326)
Date
2013-07-03T19:03:54Z (13 years ago)
From
Kevin Hurley at UCBerkeley/SSL <khurley@ssl.berkeley.edu>
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.
GCN Circular 14973
Subject
Fermi GRB 130702A: Swift XRT and UVOT observations
Date
2013-07-03T19:01:40Z (13 years ago)
From
Andrea Melandri at INAF-OAB <andrea.melandri@brera.inaf.it>
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.
GCN Circular 14972
Subject
GRB 130702A / Fermi394416326: Fermi GBM detection
Date
2013-07-03T18:58:21Z (13 years ago)
From
Andrew Collazzi at NASA/MSFC/ORAU <andrew.collazzi@nasa.gov>
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."
GCN Circular 14971
Subject
GRB 130702A / Fermi394416326 : Fermi-LAT detection of a burst
Date
2013-07-03T17:34:28Z (13 years ago)
From
Giacomo Vianello at SLAC <giacomov@slac.stanford.edu>
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.