GRB 131127B
GCN Circular 15577
Subject
GRB 131127B: Bassano Bresciano Observatory,archival confirmation of iPTF13ecv
Date
2013-12-04T16:29:52Z (12 years ago)
From
Ulisse Quadri at Bassano Bresciano Obs <oabb@ulisse.bs.it>
U.Quadri, L.Strabla and R.Girelli
of the (IAU station 565) Bassano Bresciano
Observatory, Italy (member of ISSP:Italian
Supernovae Search Project) report:
Follow the GCN 15575 (D. Denisenko - Sternberg Astronomical
Institute at Moscow State University), we communicate
that the optical transient iPTF13ecv (Singer et al., GCN
15524) is also present in the POSS1-BLUE plate
on 1953-08-16. with magnitude = 20.1 +/- 0.2
Magnitude were estimated with the USNO-B1 cat.
The image are available at:
http://archive.stsci.edu/cgi-bin/dss_search?v=poss1_blue&r=20+31+48&d=00+59+23&e=J2000&h=15.0&w=15.0&f=gif
The message may be cited.
GCN Circular 15575
Subject
GRB 131127B: archival confirmation of iPTF13ecv as a CV
Date
2013-12-04T15:06:54Z (12 years ago)
From
Denis Denisenko at SAI MSU <d.v.denisenko@gmail.com>
D. Denisenko (Sternberg Astronomical Institute at Moscow State
University) reports:
The position of the optical transient iPTF13ecv (Singer et al., GCN
15524) in the Fermi field of GRB 131127B (von Kienlin, GCN 15528) was
observed in the past with the NEAT project (Teegarden et al., ApJ Vol.
589, pp. L51-L53, 2003). A total of 87 images were obtained on 33
different nights from 1998 July 19 to 2005 Sep. 08. Images can be
downloaded from the SkyMorph website at
http://skyview.gsfc.nasa.gov/skymorph/obs.html The object at the
position of iPTF13ecv was detected in outburst on four last nights,
namely on 2005 Aug. 21, Sep. 01, 07 and 08. It was below the detection
limit (typically 19.5-20.0m) on the other nights.
The following photometry was obtained from the unfiltered NEAT images
using SDSS J203153.05+005858.4 as a reference star with r=16.40:
20050821.372 17.0
20050901.371 18.1
20050908.271 19.3
The coordinates of the object measured from the combination of three
2005-08-21 images are (J2000.0): 20 31 47.76 +00 59 23.8, consistent
to 0.4" with the position reported by Singer et al. and to 1" with
those by Quadri et al. (GCN 15543).
Comparison of NEAT images of the variable object in outburst (2005
Aug. 21, Sep. 01 and 08) and at quiescence is uploaded to
http://master.sai.msu.ru/static/OT/iPTF13ecv-NEAT-2005.jpg (5'x5' FOV
centered at the variable). Reference star is marked on the bottom left
(2005-09-01) panel as 16.4r.
No object is detected at this position on the combination of 26 good
quality NEAT images to the limit ~22.5m. No previous outbursts were
found on 15 DSS plates. Combination of DSS plates and SDSS color image
suggests that the object is fainter than 23m at quiescence. 2005
outburst amplitude about 6 mag and duration of at least about 20 days
are typical for superoutbursts of SU UMa-type dwarf novae.
Thus, the cataclysmic variable nature of iPTF13ecv already determined
spectroscopically by Keck telescopes (Singer et al., GCN 15574) is
independently confirmed by the archival light curve, once again
showing the powerful capabilities of data mining methods.
This message can be cited.
GCN Circular 15574
Subject
GRB 131127B: rejection of optical counterpart candidates
Date
2013-12-04T04:42:30Z (12 years ago)
From
Leo Singer at CIT/PTF <lsinger@caltech.edu>
L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories),
S. B. Cenko (NASA/GSFC), Yi Cao (Caltech), Daniel Perley (Caltech),
and Annalisa De Cia (Weizmann) report on behalf of the intermediate
Palomar Transient Factory (iPTF) collaboration:
We report our continued observations of the optical transient
iPTF13ecv (Singer & Kasliwal, GCN 15524; Xu et al., GCN 15531; Quadri
et al., GCN 15543; Quadri et al., GCN 15558), which was spatially
coincident with the Fermi GBM localization of GRB 131127B (von
Kienlin, GCN 15528) but was well outside the IPN error box
(Golenetskii et al., GCN 15529).
No X-ray source coincident with iPTF13ecv was detected in a 5 ks Swift
XRT observation starting at 2013-11-28 10:10 (0.83 days after the
Fermi-GBM trigger). We calculate a 3 sigma upper limit on the count
rate of < 2.2e-3 cps at this time.
We obtained further optical photometry with the robotic Palomar
60-inch telescope (P60), yielding r=19.0 +/- 0.1 mag at 2013-11-30
03:36.
On 2013-11-29, we obtained a spectrum with the DEIMOS instrument on
the Keck II telescope. The spectrum was blue and featureless from
about 5000 to 8500 angstroms.
On 2013-12-02, we obtained a second spectrum with the LRIS instrument
on Keck I. This spectrum had a blue continuum with prominent Balmer
absorption lines at a redshift of z=0.
Considering the position well outside the IPN localization, the
continued optical detection of iPTF13ecv, its blue optical SED, and
the Balmer absorption lines, we conclude that iPTF13ecv is unrelated
to the GRB trigger and is likely a cataclysmic variable in outburst.
We also note that the other two iPTF candidates reported in GCN
15524, iPTF13ect and iPTF13ecu, are probably due to AGN activity. In
the 6dFGS survey (Jones et al., MNRAS, 355, 747), iPTF13ect displays
a Seyfert I-type spectrum (broad H-alpha and strong [N II] emission
lines) and iPTF13ecu a Seyfert II spectrum (no broad H-alpha
emission, but strong [N II] emission lines).
GCN Circular 15558
Subject
GRB 131127B: Bassano Bresciano Observatory optical observations of iPTF13ecv
Date
2013-12-01T21:25:56Z (12 years ago)
From
Ulisse Quadri at Bassano Bresciano Obs <oabb@ulisse.bs.it>
U.Quadri, L.Strabla and R.Girelli report:
We imaged again the field of iPTF13ecv optical afterglow
candidate of GRB 131127B (Leo Singer: GCN 15524) with
the robotic telescope of (IAU station 565) Bassano
Bresciano Observatory, Italy (member of ISSP:Italian
Supernovae Search Project).
We have observed that the brightness of this object
is not decreased during 5 days after the discovery.
Follow the results of our photometry +/- 0.2 mag:
Date UT Exp R-mag
Middle (s) (rough)
2013 11 28.76209 600 18.77
2013 11 28.76914 600 18.69
2013 11 28.76926 600 18.58
2013 11 28.77644 600 18.89
2013 11 29.75051 600 18.47
2013 12 01.72377 600 18.85
2013 12 01.73159 600 18.85
2013 12 01.74629 600 18.93
Magnitudes were estimated with the USNO-B1 cat.
and are not corrected for galactic dust extinction.
The images are available at:
http://www.osservatoriobassano.org/GRB.asp
The message may be cited.
GCN Circular 15543
Subject
GRB 131127B: Bassano Bresciano Observatory optical observations
Date
2013-11-29T09:49:11Z (12 years ago)
From
Ulisse Quadri at Bassano Bresciano Obs <oabb@ulisse.bs.it>
U.Quadri, L.Strabla and R.Girelli report:
We imaged the fields of GRB 131127B
(von Kienlin, GCN 15528; Singer & Kasliwal,
GCN 15524; Golenetskii et al., GCN 15530) with the robotic
telescope of (IAU station 565) Bassano Bresciano
Observatory, Italy (www.osservatoriobassano.org).
The observations started 27h 55m. after the
Fermi-GBM trigger (Fermi407254341) , with our
schmidt telescope D=320/400 mm F/D=3.1.
Weather conditions were good.
We co-added 3 series of 5 unfiltered exposures
of 120 sec each.
We detected the candidate couterpart of iPTFecv
(Singer et al, GCN 15524) at the following
position (+/- 1 arcsec):
RA (J2000.0) = 20h 31m 47.79s
DEC(J2000.0) = +00d 59m 22.8s
The results of our photometry are:
Date UT Exp R-mag
Middle (s) (rough)
2013 11 28.75862 600 18.84 +/- 0.2
2013 11 28.76579 600 18.85 +/- 0.2
2013 11 28.77297 600 19.08 +/- 0.3
Magnitudes were estimated with the USNO-B1 cat.
and are not corrected for galactic dust extinction.
The images are available at:
http://www.osservatoriobassano.org/GRB.asp
The message may be cited.
GCN Circular 15534
Subject
GRB 131127B: MASTER-Net optical observations
Date
2013-11-28T15:22:44Z (12 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University
E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina,
N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, D.Denisenko,
Sternberg Astronomical Institute, Moscow State University
V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Krushinsky, I.Zalozhnih, A. Popov
Ural Federal University, Yekaterinburg, Kourovka
Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)
Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to the GRB131127.59 73 sec after GRB time at
2013-11-27 14:13:31.093 UT.
Fortunately, the central part (42%) of the IPN error box (Golenetskii et
al., GCN 15529) was covered by first MASTER image (10s exposure).
Unfortunatelly, observations was done at the very high zenit distance (~85
degrees).
We haven`t found optical transient.
The 5-sigma upper limit has been about 14.1 mag
We have 4 images (the one of the tube was under horizont):
Id (image) Coord Pro.type time Exp.time Limit
587443 20h 19m 27.4s -02d 51m 25s Alert 14:13:31 10 14.1
587444 20h 19m 27.3s -02d 51m 31s Alert 14:14:29 30 15.0
587446 20h 19m 27.0s -02d 51m 41s Alert 14:15:52 40 14.8
587448 20h 19m 27.1s -02d 51m 42s Alert 14:17:38 60 15.0
The fist image (FOW = 2x2 degrees) with IPN error box is available at
http://master.sai.msu.ru/static/GRB/grb131127_IPN.jpeg .
The reduction is continued.
The message may be cited.
GCN Circular 15531
Subject
GRB 131127B: Nanshan optical observations
Date
2013-11-28T13:25:05Z (12 years ago)
From
Dong Xu at DARK/NBI <dong.dark@gmail.com>
D. Xu (DARK/NBI), H.-B. Niu, J.-Z. Liu, G.-J. Feng, C.-H. Bai, A.
Esamdin, L. Ma (XAO) report:
We observed the fields of the three afterglow candidates of GRB
131127B (von Kienlin, GCN 15528; Singer & Kasliwal, GCN 15524;
Golenetskii et al., GCN 15530), using the 1m telescope located on Mt.
Nanshan, Xinjiang, China. Observations started at 11:37:34 UT on
2013-11-28, (i.e., 21.42 hr after the Fermi trigger) and a series of
R-band frames were obtained.
The three optical afterglow candidates are clearly detected in their
stacked images.
For the one dubbed iPTF13ecv, we measure its magnitude
m(R)=18.66+/-0.14, calibrated with two nearby SDSS stars and using the
Lupton (2005) transformation. This magnitude is basically consistent
with the value reported in Singer & Kasliwal (GCN 15524), indicating
that its significant fading is ruled out.
For the other two dubbed iPTF13ect and iPTF13ecu, given that they are
very close to the cores of the galaxies and not well resolved in our
images, we are not able to put good constraints on their magnitudes at
the moment.
GCN Circular 15530
Subject
Konus-Wind observation of GRB 131127B
Date
2013-11-28T13:06:06Z (12 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:
The bright, long-duration GRB 131127B
(Fermi GBM detection: von Kienlin, GCN 15528;
IPN triangulation: Golenetskii at al., GCN 15529)
triggered Konus-Wind at T0=51139.678 s UT (14:12:19.678).
The burst light curve shows multiple overlapped pulses
from ~T0-0.5 s to ~T0+20 s.
The emission is seen up to ~12 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB131127_T51139/
As observed by Konus-Wind, the burst
had a fluence of (4.1 � 0.3)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.160 s,
of (1.15 � 0.08)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum (measured from T0 to T0+21.760 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.20 � 0.11,
the high energy photon index beta = -2.51 � 0.19,
the peak energy Ep = 165 � 17 keV,
chi2 = 140/97 dof.
The spectrum near the maximum count rate
(measured from T0 to T0+5.376 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.92 � 0.14,
the high energy photon index beta = -2.43 � 0.19,
the peak energy Ep = 218 � 27 keV,
chi2 = 128/97 dof.
All the quoted values are preliminary.
GCN Circular 15529
Subject
IPN Triangulation of GRB 131127B
Date
2013-11-28T13:02:01Z (12 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline on behalf of the Konus-Wind team,
V. Connaughton, M. S. Briggs, C. Meegan, and V. Pelassa, on behalf of
the Fermi GBM team,
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and
K. Hurley on behalf of the IPN team, report:
The long-duration, intense GRB 131127B (von Kienlin, GCN 15528) has been
observed by Fermi (GBM: trigger 407254341), INTEGRAL (SPI-ACS), and
Konus-Wind, so far, at about 51138 s UT (14:12:18).
We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
---------------------------------------------
RA(2000), deg Dec(2000), deg
---------------------------------------------
Center:
304.839 (20h 19m 21s) -2.830 ( -2d 49' 46")
Corners:
304.599 (20h 18m 24s) -0.050 ( +0d 03' 01")
305.856 (20h 23m 26s) -5.612 ( -5d 36' 45")
305.066 (20h 20m 16s) -5.608 ( -5d 36' 28")
303.808 (20h 15m 14s) -0.033 ( +0d 02' 00")
---------------------------------------------
The error box area is 4.38 sq. deg, and its maximum
dimension is 5.9 deg (the minimum one is 0.77 deg).
The Sun distance was 62 deg.
This box can be improved.
All optical afterglow candidates reported by iPTF (Singer, GCN 15524)
are far outside of the box.
A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB131127_T51139/IPN/
GCN Circular 15528
Subject
GRB 131127B: Fermi GBM detection
Date
2013-11-28T12:53:49Z (12 years ago)
From
Andreas von Kienlin at MPE <azk@mpe.mpg.de>
A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team:
"At 14:12:18.36 UT on 27 November 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 131127B (trigger 407254341 / 131127592).
The on-ground calculated location, using the GBM trigger
data, is RA = 306.1, DEC = -0.8 (J2000 degrees,
equivalent to 20h 24m, -00d 48'), with an uncertainty
of 1.0 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 88 degrees.
This burst was also independently detected by INTEGRAL SPI-ACS.
Three candidates for an optical afterglow were found by iPTF
(Singer et al, GCN 15524) using the GBM on-ground location.
The GBM light curve is multi-peaked with a duration (T90)
of about 18 s (50-300 keV).
The time-averaged spectrum from T0-0.003 s to T0+20.480 s is
best fit by a Band function with Epeak = 181.7 (+7.9/-7.2) keV,
alpha = -1.05 +/- 0.02 , and beta = -2.24 (+0.05/-0.06)
The event fluence (10-1000 keV) in this time interval
is (3.85 +/- 0.03)E-05 erg/cm^2. The 1.024-sec peak photon
flux measured starting from T0+5.824 s in the 10-1000 keV band
is 37.6 +/- 0.5 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."