GRB 140105A
GCN Circular 15688
Subject
GRB 140105A: Fermi GBM detection
Date
2014-01-05T21:39:05Z (11 years ago)
From
Shaolin Xiong at UAH <sx0002@uah.edu>
Shaolin Xiong (UAH) and Valerie Connaughton (UAH)
report on behalf of the Fermi GBM Team:
"At 01:33:01.01 UT on 05 January 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140105A (trigger 410578384 / 140105065).
The on-ground calculated location, using the GBM trigger
data, is RA = 208.22, DEC = 50.17 (J2000 degrees,
equivalent to 13 h 53 m, 50 d 10 '), with an uncertainty
of 6 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 72 degrees.
The optical afterglow candidates reported by iPTF (Singer et al.
GCN 15686) lie within the 1-sigma (statistical and systematic)
uncertainty region surrounding the GBM localization.
The GBM light curve consists of weak pulses
with a duration (T90) of about 0.8 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.64 s is
well fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.98 +/- 0.11 and
the cutoff energy, parameterized as Epeak, is 1200 +/- 500 keV.
The event fluence (10-1000 keV) in this time interval is
(8.7 +/- 0.6)E-7 erg/cm^2. The 64 ms peak photon flux measured
starting from T0 in the 10-1000 keV band is 8.2 +/- 1.2 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 15692
Subject
GRB 140105A/Fermi410578384: MASTER-Net early optical observations
Date
2014-01-06T14:46:32Z (11 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, D.Denisenko, V.Kornilov, D.Kuvshinov, N.Tyurina,
P.Balanutsa, A.Kuznetsov
Sternberg Astronomical Institute, Moscow State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk
K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University
V.Krushinski, I.Zalozhnih, A. Popov
Ural Federal University, 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 Kislovodsk was pointed to the GRB140105.06 60 sec after notice
time and 21 sec after trigger time at 2014-01-05 01:32:39.028 UT. On our
first (10s exposure) set we haven`t found optical transient within our
FOW error-box (ra=13 43 08 dec=+52 55 47) .
The 5-sigma upper limit has been about 16.8 mag.
We have one possible OT candidate iPTF14ae (Singer, Kasliwal and Cenko,
GCN 15686) inside our FOV. But we do not see any OT at this place
brighter than 16.8 unfiltered magnitude.
We have Very Wide Field camera images at this direction (FOV=2x400
square degrees). We have a part of the Error Box at synchronous
images (Shaolin Xiong and Valerie Connaughton, GCN 15688). The reduction
is being continued.
The message may be
cited.
GCN Circular 15694
Subject
GRB 140105A: Swift XRT observations
Date
2014-01-06T22:05:49Z (11 years ago)
From
Dirk Grupe at PSU/Swift-XRT <dxg35@psu.edu>
Dirk Grupe (Swift MOC, PSU) reports on behalf of the
Swift team:
We report on the Swift XRT observations of the field of the
Fermi GBM detected GRB 140105A (Xiong & Connaughton GCN Circ.
15688). We followed three of the four afterglow candidates
reported by Singer et al. (GCN circular 15686). We did not find
an X-ray source in any of these observations. Below is a summary
of the XRT observations:
iPTF14ai: target ID 20338, T-exp=3939s,
Tstart = 2014-01-05 19:46
3sigma ul = 1.5e-3 counts/s
iPTF14ae: target ID 20339, T-exp=3962s
T-start = 2014-01-05 23:01
3sigma ul = 1.53-3 counts/s
Note that the bright source in the XRT image
is the Seyfert 1 galaxy SBS 1343+537.
iPFT14x: target ID 20340, T-exp=3077s
T-start = 2014-01-06 08:56
3sigma ul = 2.8e-3 counts/s
Note that Swift was not able to observe the field of the forth
source, iPTF14ac, because the star tracker did not lock onto the
target and caused Swift to go into a safehold.
This report is an official product of the Swift team.
GCN Circular 15696
Subject
GRB 140105A: continued iPTF observations and rejection of optical candidates
Date
2014-01-07T06:03:23Z (11 years ago)
From
Leo Singer at CIT/PTF <lsinger@caltech.edu>
L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories/Princeton),
S. B. Cenko (NASA/GSFC), E. Bellm (Caltech), and Y. Cao (Caltech) report
on behalf of the intermediate Palomar Transient Factory (iPTF)
collaboration:
We have continued to observe four optical transients (Singer et al.,
GCN 15686) in the Fermi GBM error circle for GRB 140105A (Xiong &
Connaughton, GCN 15688) with the Palomar 48-inch Oschin telescope
(P48), the robotic Palomar 60-inch (P60), and the Palomar 200-inch
(P200) equipped with the Double Beam Spectrograph (DBSP).
At 33 hours after the burst, with the P48 we obtain the following
host-subtracted magnitudes in the Mould R filter:
iPTF14x, R = 20.0
iPTF14ac, R = 20.3
iPTF14ae, R = 20.5
With the P60, at 34 hours after the burst, we obtain the following
magnitude in the SDSS system:
iPTF14ai, r = 20.4
We obtained spectra of all four with the P200. iPTF14x resembles a
Type II supernova. Our spectra for iPTF14ac, iPTF14ae, and iPTF14ai
show a mostly featureless continuum.
The lack of significant optical fading in any of the four candidates
strongly argues against association with the GRB.
GCN Circular 15697
Subject
GRB 140105A: HCT Observations
Date
2014-01-07T12:28:25Z (11 years ago)
From
G.C. Anupama at IIA,Bangalore <gca@iiap.res.in>
V. Bhalerao (IUCAA), Vaidehi S. Paliya (IIA), G. C. Anupama (IIA), and
C. S.
Stalin (IIA) report:
We undertook followup observations of the four optical transients
(Singer et
al., GCN 15686) in the Fermi GBM error circle for GRB 140105A (Xiong &
Connaughton, GCN 15688) with the 2-m Himalayan Chandra Telescope (HCT).
We
obtained two 300s exposures of each field, under non-photometric
conditions.
20 hours after the burst, we obtain the following unsubtracted
magnitudes in
the R band:
iPTF14ae = 20.1 +- 0.1
iPTF11ai = 19.8 +- 0.2
iPTF11x = 19.1 +- 0.3
iPTF11ac is contaminated by a nearby star, and we can only place a limit
that
R > 18.4 mag. We concur with Singer et al. (GCN 15696) that the lack of
fading
rules out these candidates as counterparts to GRB 140105A.
We thank the iPTF team for alerting us about this event.
GCN Circular 15712
Subject
GRB 140105A: MASTER-Net early optical observations and time correction
Date
2014-01-09T17:35:59Z (11 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, D.Denisenko, V.Kornilov, D.Kuvshinov, N.Tyurina,
P.Balanutsa, A.Kuznetsov
Lomonosov Moscow State University, Sternberg Astronomical Institute
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk
K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University
V.Krushinski, I.Zalozhnih, A. Popov
Ural Federal University, 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 VWF robotic very wide field cameras (FOV=2x384 square degrees,
D=72mm, f/1.2, 1 pix = 22 arcsec, http://observ.pereplet.ru) installed on
MASTER-II robotic telescope syncronously covered ~15% part of 3 sigma
FERMI-GBM error box (Xiong et al., GCN 15688). No credible transients have
been found on our images. The 3 sigma unfiltered upper limit is 10.6.
MASTER-II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Kislovodsk was pointed to the GRB140105A 21 sec after notice
time and 45 sec after trigger time at 2014-01-05 01:33:46 UT.
After pointing by FERMI alert we cover 90% of 1-sigma and 70% of 3-sigma
FERMI-GBM error box. We didn't find new object in error box on single and
coadd images. The 3 sigma upper limit on single 5 seconds exposure image
is 10.6 and 12.0 on coadd of 24 images with total exposure 120 seconds.
The positions of all iPTF optical afterglow candidates (Singer et al., GCN
15686) are covered by out cameras since 48 sec. after the trigger but
there are no flares up to 10.6 mag. on their place.
The movie is available here
http://master.sai.msu.ru/static/GRB/GRB140105A/GRB140105A.gif
The map of error box and our FOV is available at
http://master.sai.msu.ru/static/GRB/GRB140105A/GRB140105A_map.png
The pointing time informations in our previous telegram Gorbovskoy et al.
GCN 15692 are not correct. We apologize for this inaccuracy.
The message may be cited.