GRB 140206A
GCN Circular 15835
Subject
GRB140206A: Discovery Channel Telescope Optical Detection
Date
2014-02-14T21:57:28Z (12 years ago)
From
Vicki Toy at UMD <vtoy@astro.umd.edu>
V. Toy (UMD), S.B. Cenko (NASA-GSFC), A. Kutyrev (NASA-GSFC), J. Capone
(UMD), E. Troja (NASA-GSFC), A. Cucchiara (NASA-GSFC), S. Veilleux (UMD),
and S. Gezari (UMD) report on behalf of a larger collaboration:
We observed the field of GRB140206A (Swift trigger 585834, Lien et al., GCN
15784) with the Large Monolithic Imager (LMI) on the recently commissioned
4.3m Discovery Channel Telescope (DCT) at Happy Jack, AZ from 2014/02/13
5:33 to 2014/02/13 6:03 UTC (mean epoch of 6.9 d after the Swift trigger).
A source is clearly detected at the location of the optical afterglow
(Oksanen et al, GCN 15786). Using nearby point sources from SDSS for
calibration, we measure r' = 21.69 +/- 0.07 (AB). This value is not
corrected for Galactic extinction in the direction of the GRB.
We thank the staff of the Discovery Channel Telescope for assistance with
these observations.
GCN Circular 15813
Subject
GRB 140206A: Bassano Bresciano Observatory optical upper limit
Date
2014-02-10T08:51:22Z (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 field of GRB 140206A detected by SWIFT(trigger 585834)
with the robotic telescope of (IAU station 565) Bassano Bresciano
Observatory, Italy (member of ISSP:Italian Supernovae Search Project)
The observations started 85h 35m after the GRB trigger,
with our schmidt telescope D=320/400 mm F/D=3.1.
Weather conditions were good.
We co-added 2 series of 15 exposures of 120 sec each.
We did not found any optical counterpart
in the error box of the XRTcandidate.
(Lien et. al GCN 15784 , Gotz et. al GCN 15784)
Start End Vlim
85h 35m 86h 47m 18.5
Magnitudes were estimated with the USNOB1.0 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 15807
Subject
GRB 140206A: Mondy optical observations
Date
2014-02-08T16:11:34Z (12 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), E. Klunko (ISTP), M. Eselevich (ISTP), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:
We observed the afterglow (Oksanen et al., GCN 15786; Oates et al., GCN
15787) of the Swift/INTEGRAL/Fermi GRB 140206A (Lien et al., GCN 15784;
Gotz et al., GCN 15785, Kienlin et al., GCN 15796) with AZT-33IK
telescope of Sayan observatory (Mondy) starting on Feb. 6 (UT) 14:15.
We clearly detect afterglow in each frame of 60 s exposure. A
preliminary photometry of the afterglow is following:
date Filter UT start Exp,s t-T0,d OT err
2014-02-06 R 14:15:21 120 0.29098 18.73 0.05
2014-02-06 R 14:31:29 60 0.30185 18.59 0.07
2014-02-06 R 15:02:15 60 0.32321 18.61 0.07
2014-02-06 R 18:14:26 60 0.45667 19.01 0.08
2014-02-06 R 18:53:29 60 0.48379 19.29 0.09
The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005)
N SDSS_id R(Lupton)errR
4 J094058.58+664752.4 18.030 0.022
5 J094107.93+664422.0 19.066 0.028
GCN Circular 15806
Subject
GRB 140206A: Liverpool Telescope optical afterglow observations
Date
2014-02-08T09:59:29Z (12 years ago)
From
Drejc Kopac at Math Phys U,Slovenia <drejc.kopac@fmf.uni-lj.si>
D. Kopac, A. Gomboc (U. Ljubljana), C. Guidorzi (U. Ferrara), A.
Melandri (INAF-OAB), I. A. Steele, C. G. Mundell (LJMU), on behalf of a
large collaboration report:
The 2-m Liverpool Telescope automatically observed Swift-INTEGRAL-Fermi
GRB 140206A (Lien et al., GCN 15784; Gotz et al., GCN 15785), starting
at 07:19:30 UT (~2.2 min after the burst trigger).
We clearly detect the fading optical afterglow at the position reported
by Oksanen et al. (GCN 15786). In our first 10 sec frame, we estimate
the magnitude r' = 14.97 +- 0.02 at t_mid = 135 sec since the Swift/BAT
trigger time. The magnitude is calibrated against nearby SDSS stars.
GCN Circular 15805
Subject
GRB 140206A, Swift-BAT refined analysis
Date
2014-02-07T21:56:28Z (12 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
T. Sakamoto (AGU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140206A (trigger #585834)
(Lien, et al., GCN Circ. 15784). The BAT ground-calculated position is
RA, Dec = 145.321, 66.762 deg which is
RA(J2000) = 09h 41m 16.9s
Dec(J2000) = +66d 45' 42.7"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
The mask-weighted light curve shows a multi-peaked structure with roughly three main pulse
durations. The first pulse duration starts at ~T-15 and ends at ~T+25 sec, and consists of
roughly three to four peaks. The second one starts at ~T+50 sec, peaks at ~T+60 sec,
and ends at ~T+90 sec. The third weaker pulse peaks at ~T+210 sec, with a long low-level tail
out to T+400 sec. T90 (15-350 keV) is 93.6 +- 13.8 sec (estimated error including systematics).
The time-averaged spectrum from T-37.2 to T+256.1 sec is best fit by a power law
with an exponential cutoff. This fit gives a photon index 1.04 +- 0.15,
and Epeak of 100.9 +- 14.5 keV (chi squared 52.76 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is 1.6 +- 0.03 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+60.80 sec in the 15-150 keV band is
19.4 +- 0.5 ph/cm2/sec. A fit to a simple power law gives a photon index
of 1.58 +- 0.03 (chi squared 91.21 for 57 d.o.f.). All the quoted errors
are at the 90% confidence level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/585834/BA/
GCN Circular 15803
Subject
GRB 140206A: MITSuME Akeno detection of the optical counterpart
Date
2014-02-07T04:33:05Z (12 years ago)
From
Yoichi Yatsu at Tokyo Tech. <yatsu@hp.phys.titech.ac.jp>
Y. Saito, T. Yoshii, Y. Tachibana, S. Kurita, K. Ito, R. Usui,
K. Ishikawa, T. Tanigawa, Y. Yano, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:
We observed the field of GRB 140206A (A. Y. Lien et al., GCNC 15784) with
the
optical three color (g, Rc, and Ic) CCD cameras mounted on the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.
The observation started on 2014-02-06 15:46:53 UT ( ~8.5 hour after the
burst) and we detected the previously reported afterglow.
The measured magnitudes were listed as follows.
T0+[hour] MID-UT T-EXP[sec] g'
Rc Ic
------------------------------------------------------------
-----------------------------------------
~8.5 17:36:31 199x60 20.74+/-0.14 18.88+/-0.08
18.37+/-0.10
------------------------------------------------------------
-----------------------------------------
(The photon flux were calibrated by SDSS(g') and GSC2.3(Rc, Ic) catalog.)
GCN Circular 15802
Subject
GRB 140206A: TNG redshift confirmation
Date
2014-02-06T22:52:54Z (12 years ago)
From
Valerio D'Elia at ASDC <delia@asdc.asi.it>
V. D'Elia (INAF/OAR & ASI/ASDC), P. D'Avanzo, S. Covino, A. Melandri
(INAF-OAB), S. D. Vergani (CNRS/GEPI), L. Di Fabrizio (INAF/TNG)
report on behalf of the CIBO collaboration:
We report further observations of the field of GRB 140206A (Lien et
al., GCN 15784; Gotz et al., GCN 15785) with the Telescopio Nazionale
Galileo (TNG) equipped with DOLORES.
We obtained a spectrum of the optical source reported in D'Avanzo et
al. (GCN Circ. 15799), with a total exposure of 1800 s, using the
grism LR_B covering the wavelength range 3000 - 8000 AA. The
observation started at 2014-02-06T19:53:07, i.e., ~12.6 hrs after the
GRB.
We detect several absorption lines which we interpret as due to Ly-alpha,
NV, Si II, C II, SiIV, C IV, Al II, AlII and Fe II at a common
redshift of 2.74. In addition, we also detect at the same redshift
fine structure lines from excited levels of SiII and FeII, confirming
that this is the redshift of the GRB host galaxy. Our result is in
perfect agreement with the reported value by Malesani et al. (GCN 15800)
Finally, we also detect a strong intervening Ly-alpha absorber at z~2.32
----------------------------------------------------------------
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GCN Circular 15801
Subject
GRB 140206A: Optical Observations via Virtual Telescope
Date
2014-02-06T22:21:53Z (12 years ago)
From
Gianluca Masi at Bellatrix Astronomical Obs <gianluca@bellatrixobservatory.org>
G. Masi (Ceccano, Italy) and F. Nocentini (Frosinone, Italy) report:
On Feb. 6.9216 2014 UT, we imaged the field around GRB 140206A (Lien et. al GCN
15784 , Gotz et. al GCN 15784) remotely using the the 0.43m-f/6.8 robotic unit
part of the Virtual Telescope robotic facility in Italy.
The source is visible on 300 seconds unfiltered CCD images at the following
coordinates (J2000.0):
R.A. = 09 41 20.23
Decl. +66 45 38.5
We also performed photometry, assuming R-mags from UCAC-4 for the stars in the
field, getting an estimate for the magnitude of 18.9CR).
Observations are ongoing.
This message can be cited
GCN Circular 15800
Subject
GRB 140206A: NOT redshift
Date
2014-02-06T21:52:48Z (12 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani, D. Xu, J. P. U. Fynbo (DARK/NBI), A. de Ugarte Postigo
(IAA/CSIC and DARK/NBI), S. Schulze (PUC and MCSS), A. Finoguenov (U.
Helsinki), P. Jakobsson (U. Iceland), A. Melandri (INAF/OABr), A.
Cucchiara (NASA/GSFC), report on behalf of a larger collaboration:
We observed the field of GRB 140206A (Lien et al., GCN 15784; Gotz et
al., GCN 15785; von Kienlin & Bhat, GCN 15796) with the Nordic Optical
Telescope (NOT) equipped with ALFOSC. Observations started at 19:56 UT
on February 6 (i.e., 12.66 hr after the burst).
We first obtained a 100-s image in R band. We clearly detect the source
reported in Oksanen et al. (GCN 15786). The source has faded to 19.15
+/- 0.10 mag (Vega magnitude), based on nearby USNO stars.
We aso obtained an optical spectrum, with a total exposure of 2 x 1800
s, using grism #4 and a blocking filter covering the wavelength range
3750 - 9000 AA at a resolution of 8.1 AA. The mid exposure time is 13.6
hr after the GRB.
We detect several absorption lines which we interpret as due to Lyalpha,
Si II, C II, C IV, Al II, Fe II at a common redshift of 2.73.
This measurement is not consistent with the predicted theoretical value
by Ruffini et al. (GCN 15794).
We thank Carlos Perez, John Teltin, and Amanda Djupvik (NOT) for
excellent support with the observations.
[GCN OPS NOTE(07feb14): The Troja reference was corrected to the
von Kienlin & & Bhat reference.]
GCN Circular 15799
Subject
GRB 140206A: TNG optical observations
Date
2014-02-06T21:44:59Z (12 years ago)
From
Paolo D'Avanzo at INAF-OAB <paolo.davanzo@brera.inaf.it>
P. D'Avanzo, S. Covino, A. Melandri (INAF/OAB) L. Di Fabrizio (INAF/TNG) report on behalf of the CIBO collaboration:
We observed the field of GRB 140206A (Lien et al., GCN 15784; Gotz et al. GCN 15785) using the DOLORES camera on the 3.6-m TNG Telescope at Canary Islands.
The optical afterglow (Oates & Lien GCN 15787; Yurkov et al. GCN 15788; Xu et al. GCN 15789; Volnova et al. GCN 15792; Oates & Lien GCN 15795; Sonbas et al. GCN 15797) is clearly detected with R = 18.7 +/- 0.1 (calibrated against the USNOB1 catalogue) at t-t0 = 12.52 hours.
Further observations are ongoing.
GCN Circular 15798
Subject
GRB 140206A: Swift-XRT refined Analysis
Date
2014-02-06T20:57:35Z (12 years ago)
From
Alessandro Maselli at INAF/IASF Palermo <maselli@ifc.inaf.it>
A. Maselli (INAF-IASFPA), A. Y. Lien (NASA/GSFC/ORAU) and P. A. Evans
(U. Leicester) report on behalf of the Swift-XRT team:
We have analysed 14 ks of XRT data for GRB 140206A (Lien et al. GCN
Circ. 15784), from 33 s to 30.2 ks after the BAT trigger. The data
comprise 1.2 ks in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN Circ. 15793).
The light curve shows initial flaring activity with two flares peaking
at about 61 s and 223 s after the trigger. The underlying emission can
be modelled with a broken power-law decay: a flat decay with an index
alpha=0.756 (+0.026, -0.028), a break at T+10.7 ks and a late-time
decay with an index 1.31 (+0.15, -0.12).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.762 (+/-0.028). The
best-fitting absorption column is 1.25 (+/-0.07) x 10^21 cm^-2, in
excess of the Galactic value of 4.8 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.95 (+0.08, -0.07)
and a best-fitting absorption column of 1.22 (+0.19, -0.18) x 10^21
cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.8 x 10^-11 (4.9 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.22 (+0.19, -0.18) x 10^21 cm^-2
Galactic foreground: 4.8 x 10^20 cm^-2
Excess significance: 6.6 sigma
Photon index: 1.95 (+0.08, -0.07)
If the light curve continues to decay with a power-law decay index of
1.31, the count rate at T+24 hours will be 0.088 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.3 x
10^-12 (4.3 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00585834.
This circular is an official product of the Swift-XRT team.
GCN Circular 15797
Subject
GRB 140206A: T100 observations
Date
2014-02-06T19:34:14Z (12 years ago)
From
Eda Sonbas at NASA/GSFC <edasonbas@gmail.com>
E. Sonbas (Adiyaman Univ.), T. Guver (Istanbul Univ.), U. Temiz (Cukurova
Univ.), E. Gogus (Sabanci Univ.), M. Kocak (TUG), O. Erece (Akdeniz Univ.),
Z. Eker (Akdeniz Univ.) report on behalf of a larger collaboration
We observed the field of Swift GRB 140206A (Lien et al., GCN#15784) with
the 1.0 meter T100 telescope (Bakirlitepe, TUBITAK National Observatory,
Turkey), starting February, 06, 16:33:24 UT (~ 9.268 hours after the
trigger). Observations were carried out in the R filter under good weather
conditions. The afterglow is clearly detected in 300 s in the R band images
at a position that is consistent with Oksanen et al. GCN#15786 and Oates et
al., GCN#15787
Using USNO-B1 star USNO-B1 1567-0128093 (R.A.=9:41:23.33, Dec=+66:44:32.31)
in the field, the magnitudes of the OT were estimated as follows;
t-t0 (hr) exp.(s) filt mag err (+/-)
9.590 300 R 18.65 0.05
9.689 300 R 18.77 0.06
9.788 300 R 18.75 0.06
10.380 300 R 18.89 0.06
Further observations using the same filter are ongoing.
We are grateful to TUBITAK National Observatory for prompt scheduling the
observations and technical support.
GCN Circular 15796
Subject
GRB 140206A: Fermi GBM detection
Date
2014-02-06T18:29:24Z (12 years ago)
From
Narayana Bhat at U Alabama/Huntsville/GBM <Narayana.Bhat@nasa.gov>
A. von Kienlin (MPE) and P. N. Bhat (UAH)
report on behalf of the Fermi GBM Team:
"At 07:18:15.98 UT on 06 February 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140206A (trigger 413363898 / 140206304),
which was also detected by the Swift (Lien et al. 2014, GCN 15784)
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 123 degrees.
The GBM light curve shows a single pulse
with a duration (T90) of about 27 s (50-300 keV).
The time-averaged spectrum from T0-0.5 s to T0+14.3 s is
best fit by a Band function with Epeak = 120 +/- 6 keV,
alpha = 0.2 +/- 0.1, and beta = -2.4 +/-0.1.
The event fluence (10-1000 keV) in this time interval is
(1.47 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+4.9 s in the 10-1000 keV band
is 17.4 +/- 0.5 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 15795
Subject
GRB 140206A: Swift/UVOT Detection
Date
2014-02-06T18:20:25Z (12 years ago)
From
Samantha Oates at MSSL <sro@mssl.ucl.ac.uk>
S. R. Oates (UCL-MSSL) and A. Y. Lien (NASA/GSFC/ORAU)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 140206A
52 s after the BAT trigger (Lien et al., GCN Circ. 15784).
A source consistent with the XRT position (Osborne et al. GCN Circ. 15793)
and the optical positions reported by Oksanen et al. (GCN 15786) and
Yurkov et al. (GCN 15788) is detected in the initial UVOT exposures. The
lack of detections in the UV filters suggests a redshift ~2 - 3.
The preliminary UVOT position is:
RA (J2000) = 09:41:20.26 = 145.33442 (deg.)
Dec (J2000) = +66:45:38.6 = 66.76072 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).
Preliminary detections and 3-sigma upper limits 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 52 202 147 15.88 +/- 0.02
v 596 616 20 15.75 +/- 0.11
b 522 542 20 16.51 +/- 0.09
u 264 514 246 16.18 +/- 0.04
w1 645 17944 963 >20.9
m2 16137 24450 1607 >21.2
w2 21898 22798 886 >21.0
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.14 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 15794
Subject
GRB 140206A: theoretical prediction of redshift and of supernova occurrence
Date
2014-02-06T18:05:40Z (12 years ago)
From
Remo Rufinni at ICRA <ruffini@icra.it>
R. Ruffini, C.L. Bianco, M. Enderli, M. Kovacevic, M. Muccino, A.V.
Penacchioni, G.B. Pisani, J.A. Rueda, Y. Wang report:
The late Swift/XRT observations of GRB 140206A (1,2) evidences the
fullfillment of the IGC paradigm (3,4). A preliminary overlapping of
its X-ray (0.3-10 keV in rest-frame) luminosity with the one of GRB
090618, namely an IGC prototype (5), gives an estimate of the redshift
of z~0.6 (see Fig. 1 <http://www.icranet.org/images/GCN/GRB140206A.pdf>).
As a consequence, a supernova associated to GRB 140206A is expected to
emerge after 16 days after the trigger.
Continuous monitoring and complementary observations in all possible
wavelengths are encouraged.
References:
(1) Lien et al., GCN 15784
(2) Osborne et al., GCN 15793
(3) Rueda & R. Ruffini, ApJLett, 758, L7 (2012)
(4) Pisani et al., A&A, 552, L5 (2013)
(5) Izzo et al., A&A, 548, L5 (2012)
GCN Circular 15793
Subject
GRB 140206A: Enhanced Swift-XRT position
Date
2014-02-06T16:16:45Z (12 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 2549 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140206A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 145.33452, +66.76101 which is equivalent
to:
RA (J2000): 09h 41m 20.29s
Dec (J2000): +66d 45' 39.6"
with an uncertainty of 1.4 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 15792
Subject
GRB 140206A: ISON-Ussuriysk optical observations
Date
2014-02-06T15:54:46Z (12 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), A. Stepura (UAFO, ISON), A. Matkin (UAFO, ISON), I.
Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB
follow-up collaboration:
We observed the afterglow (Oksanen et al., GCN 15786; Oate et al., GCN
15787) of the Swift and INTEGRAL GRB 140206A (Lien et al., GCN 15784;
Gotz et al., GCN 15785) with VT-50 (0.5m) telescope of
UAFO/ISON-Ussuriysk observatory starting on Feb. 6 (UT) 09:20:05, i.e.
~2 hours after burst trigger. We took unfiltered images of 30s
exposures. In stacked frames we clearly detect afterglow. A
preliminary photometry of the afterglow is following:
T_start T0+ Filter, Exposure, OT, OT_err
(UT) (mid, d) (s)
2014-02-06T09:20:39 0.08783 none 9*30 17.76 0.24
2014-02-06T10:52:26 0.15309 none 19*30 18.06 0.08
The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005)
N SDSS_id R(Lupton)errR
1 J094123.75+664429.9 15.441+/-0.013
2 J094126.54+664410.8 13.837+/-0.014
3 J094131.29+664857.0 13.972+/-0.011
Observations continuing.
The finding chart can be found in
http://grb.rssi.ru/GRB140206A/grb140206A_VT50_fc.png
GCN Circular 15789
Subject
GRB 140206A: Nanshan optical observations
Date
2014-02-06T13:55:07Z (12 years ago)
From
Dong Xu at DARK/NBI <dong.dark@gmail.com>
D. Xu (DARK/NBI), G.-J. Feng, J. Xu, A. Esamdin, L. Ma (XAO) report:
We observed the field of GRB 140206A (Lien et al., GCN 15784; Gotz et
al., GCN 15785) using the 1m telescope located on Mt. Nanshan,
Xinjiang, China. Observations started at 12:30:16 UT on 2014-02-06
(i.e., 5.216 hr after the burst), and a series of R-band frames were
obtained.
The optical afterglow (Oksanen et al., GCN 15786; Oates & Lien, GCN
15787) is clearly detected in each of our frames, and it decayed from
M(R)=18.48+/-0.10 to m(R)=18.64+/-0.10 from 5.40 hr to 5.71 hr
post-burst, calibrated with two nearby SDSS stars. Compared with the
previous measurements in GCNs 15786 & 15788, it shows that so far the
afterglow has been decaying rather slowly and thus spectroscopy may be
doable even for a 2m class telescope in the coming hours.
Further observations are ongoing.
GCN Circular 15788
Subject
GRB 140206A: MASTER OT detection
Date
2014-02-06T11:08:00Z (12 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk
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, A.Sankovich
Sternberg Astronomical Institute, Moscow State University
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
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
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 Blagoveschensk was pointed to the GRB140206A (Lien et. al GCN
15784 , Gotz et. al GCN 15784) 2h 16m (8153 s) after trigger time at
2014-02-06 09:33:13 UT directly after sunset. On our first sets we found
optical transient Oksanen et. al. GCN 15786.
The coordinate is:
RA= 09h 41m 20.21s
DEC= +66d 45m 37.7s
ERROR= 0.5 arcsec
Mag=18.5 +- 0.25m
Our unfiltered magnitude is calibrated by USNO
B1.0 catalog by a parity 0.8R + 0.2B.
The message may be cited.
GCN Circular 15787
Subject
GRB 140206A: Swift/UVOT optical detection
Date
2014-02-06T11:03:15Z (12 years ago)
From
Samantha Oates at MSSL <sro@mssl.ucl.ac.uk>
S. R. Oates (MSSL-UCL) and A. Y. Lien (NASA/GSFC/ORAU) report on behalf
of the Swift/UVOT team:
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 54 seconds after the BAT trigger. There is a candidate afterglow in
the finding chart image:
RA (J2000) 9:41:20.24 = 145.33433
Dec (J2000) +66:45:38.5 = 66.76069
with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence).
This position is consistent with the XRT position (Lien et al., GCN 15784)
and the optical afterglow position reported by Oksanen et al (GCN 15786).
The estimated magnitude is 15.76 with a 1-sigma error of about 0.03.
No correction has been made for the expected extinction corresponding
to E(B-V) of 0.12.
GCN Circular 15786
Subject
GRB140206A - Optical afterglow candidate
Date
2014-02-06T09:42:27Z (12 years ago)
From
Arto Oksanen at Nyrola Obs., Finland <oksanen@nyrola.jklsirius.fi>
A. Oksanen, P. Kehusmaa and C. Harlingten on behalf of Searchlight Observatory Network report:
We detect an afterglow candidate on Rc filtered images taken at 2014-02-06T08:33:09 with
a 40 cm robotic telescope located in New Mexico, USA.
R.A. = 09 41 20 (J2000.0)
Decl = 66 45 38
The position matches with the XRT position given by A. Y. Lien et. al (GCN 15784).
Approximate magnitude R=18, seem to be fading. Observations and analysis is ongoing.
GCN Circular 15785
Subject
GRB140206A: a long GRB detected by INTEGRAL
Date
2014-02-06T08:10:46Z (12 years ago)
From
Diego Gotz at CEA <diego.gotz@cea.fr>
D. Gotz (IASF Milano) S.Mereghetti (IASF-Milano), E.Bozzo, C.Ferrigno, M. Tuerler (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team report:
a long gamma ray burst lasting at least 60 s 0.8 s has been detected by IBAS in the IBIS/ISGRI data at 07:17:26 UT of February 6th.
The refined coordinates (J2000) are:
R.A.= 145.3043 deg
DEC.= +66.7652 deg
with an uncertainty of 0.8 arcmin (90% c.l.). This position is consistent with the Swift/XRT one reported for the same event (Lien et al., GCN 15784).
The burst has been detected at the very beginning of the INTEGRAL orbit, just outside the radiation belts. Therefore the data are polluted by a high particle background, implying a high level of saturation of the IBIS/ISGRI telemetry. Hence no detailed information about the GRB duration can be derived at this stage. A preliminary lower limit on its fluence is 2x10e-6 erg/cmsq in the 20-200 keV energy band.
A plot of the light curve will be posted at http://ibas.iasf-milano.inaf.it/IBAS_Results.html
GCN Circular 15784
Subject
GRB 140206A: Swift detection of a burst
Date
2014-02-06T07:49:38Z (12 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@milkyway.gsfc.nasa.gov>
A. Y. Lien (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), V. D'Elia (ASDC), D. Malesani (DARK/NBI),
A. Maselli (INAF-IASFPA), K. L. Page (U Leicester),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:
At 07:17:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140206A (trigger=585834). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 145.350, +66.750 which is
RA(J2000) = 09h 41m 24s
Dec(J2000) = +66d 45' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows a multi-peaked
structure with a duration of about 80 sec. The peak count rate
was ~19000 counts/sec (15-350 keV), at ~60 sec after the trigger.
The XRT began observing the field at 07:18:04.0 UT, 43.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 145.33438, 66.76074 which
is equivalent to:
RA(J2000) = 09h 41m 20.25s
Dec(J2000) = +66d 45' 38.7"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 44 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. We
cannot determine whether the source is fading at the present time.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 4.79
x 10^20 cm^-2 (Kalberla et al. 2005).
The initial flux in the 2.5 s image was 9.62e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT results are not available at this time.
Burst Advocate for this burst is A. Y. Lien (yarleen AT gmail.com).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)