GRB 140629A
GCN Circular 16477
Subject
GRB 140629A: Swift detection of a burst with an optical counterpart
Date
2014-06-29T14:29:09Z (11 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@milkyway.gsfc.nasa.gov>
A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB),
J. A. Kennea (PSU) and K. L. Page (U Leicester) report on behalf of
the Swift Team:
At 14:17:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140629A (trigger=602884). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 248.982, +41.890 which is
RA(J2000) = 16h 35m 56s
Dec(J2000) = +41d 53' 25"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows an initial rise of the event
starting at ~T-5 sec out to ~T+5 sec, at which point there is a gap in the
TDRSS light curve so nothing can be said at this time for the light curve
past T+5 sec. The peak count rate was ~2000 counts/sec (15-350 keV), at ~0 sec
after the trigger.
The XRT began observing the field at 14:19:04.5 UT, 94.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 248.97675, 41.87702 which
is equivalent to:
RA(J2000) = 16h 35m 54.42s
Dec(J2000) = +41d 52' 37.3"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 48 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. No
spectrum from the promptly downlinked event data is yet available to
determine the column density.
The initial flux in the 2.5 s image was 6.08e-10 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 101 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 16:35:54.46 = 248.97691
DEC(J2000) = +41:52:36.7 = 41.87685
with a 90%-confidence error radius of about 0.74 arc sec. This position is 0.8
arc sec. from the center of the XRT error circle. The estimated magnitude is
14.81 with a 1-sigma error of about 0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01.
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.)
GCN Circular 16478
Subject
GRB 140629A: MASTER OT detection
Date
2014-06-29T15:24:00Z (11 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, M.Pruzhinskaya, V.Kornilov, D.Kuvshinov,
A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov,
V.V.Chazov, D.Denisenko, A.Sankovich
Lomonosov Moscow State University,
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 GRB140629A (Lien et. al GCN
16477) 15 sec after notice time and 33 sec after trigger time at
2014-06-29 14:18:03.188 UT. On our first (10s exposure) set we found
optical transient within SWIFT error-box (ra=16 35 55 dec=+41 53 24
r=0.050000).
The OT coordinates are Ra 16:35:54.41 Dec +41:52:36.53 and magnitude is
15.3 on first images. The OT rises up to 14 mag on following images.
GCN Circular 16479
Subject
GRB 140629A: Enhanced Swift-XRT position
Date
2014-06-29T18:14:23Z (11 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 794 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140629A, 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 = 248.97716, +41.87689 which is equivalent
to:
RA (J2000): 16h 35m 54.52s
Dec (J2000): +41d 52' 36.8"
with an uncertainty of 1.7 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 16480
Subject
GRB 140629A : Xinglong TNT optical observation
Date
2014-06-29T18:19:26Z (11 years ago)
From
L.P. Xin at NAOC <xlp@bao.ac.cn>
L. P. Xin, T. M. Zhang, H. Liu, J. Y. Wei, Y. L. Qiu, J. S. Deng,
J. Wang, H. L. Li, X. H. Han and C. Wu, H. Liu on behalf of EAFON report:
We began to observe GRB 140629A (Lien et al. GCN 16477)
with Xinglong 0.8-m TNT telescope at 14:27:11 (UT) ,
581 sec after the burst. The observations are continued for 1.6 hours.
The optical counterpart reported by (Lien et al. GCN 16477;
Yurkov et al., GCN 16478) was clearly detected in multi-wavelength images.
The brightness of the optical emission is decaying from 14.7mag
to 17.8 mag in R band. The decay slope is estimated to be about 1.2
in our observation epoch.
The message may be cited.
GCN Circular 16481
Subject
GRB 140629A: Swift-BAT refined analysis
Date
2014-06-29T18:26:41Z (11 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
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+622 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140629A (trigger #602884)
(Lien, et al., GCN Circ. 16477). The BAT ground-calculated position is
RA, Dec = 249.017, 41.897 deg, which is
RA(J2000) = 16h 36m 04.1s
Dec(J2000) = +41d 53' 49.6"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 41%.
The mask-weighted light curve shows several overlapping peaks starting
at ~T-8 sec, peaking at ~T+12 sec, and ending at ~T+90 sec.
T90 (15-350 keV) is 42.0 +- 14.3 sec (estimated error including systematics).
The time-averaged spectrum from T-7.53 to T+56.47 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.86 +- 0.11. The fluence in the 15-150 keV band is 2.4 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+12.47 sec in the 15-150 keV band
is 4.2 +- 0.4 ph/cm2/sec. 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/602884/BA/
GCN Circular 16482
Subject
GRB 140629A: RTT150 optical observations
Date
2014-06-29T20:02:26Z (11 years ago)
From
Rodion Burenin at IKI, Moscow <rodion@hea.iki.rssi.ru>
I. Bikmaev (KFU/AST), I. Khamitov (TUG),
E. Irtuganov, N. Sakhibullin (KFU/AST),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
H. Kirbiyik (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)
report:
The field of the optical afterglow of GRB 140629A (Lien et al., GCN
16477, Yurkov et al., GCN 16478) was observed with Russian-Turkish
1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National Observatory,
Turkey) using the TFOSC instrument.
We obtained series of BVRcIc exposures. Start time is June 29, 18:33
UT. The optical transient is clearly detected in each images at
RA,DEC = 16:35:54.44 +41 52 36.7 +/- 0.1 arcsec (J2000).
Using the star at RA,DEC = 16:35:59.9 +41:51:10 (J2000) with USNO-B1
magnitude R1_mag = 16.49 as a reference we estimated the Rc-magnitude
of the afterglow:
Filter exptime T-T0, Mag. +/- Mag.err
(sec) (hour)
Rc 60 4.267 18.00 +/- 0.05
Further OT observations are ongoing at RTT-150.
GCN Circular 16483
Subject
GRB 140629A : Virtual Telescope optical observations
Date
2014-06-29T20:31:34Z (11 years ago)
From
Gianluca Masi at Bellatrix Astronomical Obs <gianluca@bellatrixobservatory.org>
G. Masi, the Virtual Telescope Project - Italy, reports:
I started observations of GRB 140629A (Lien et al. GCN 16477) with the 14"
robotic unit part of the Virtual Telescope at 20:12:00 (UT), 21300 seconds after
the burst.
The optical afterglow reported earlier (Lien et al. GCN 16477; Yurkov et al.,
GCN 16478; Xin et al., GCN 16480) was detected in 300 seconds exposures,
unfiltered. The position of the source is RA: 16h35m54.43s; Decl.: +41d52'36.3"
and the magnitude was estimated to be 18.8, assuming R mags for the reference
stars from UCAC-4
The message may be cited.
GCN Circular 16484
Subject
GRB 140629A: KWFC z-band photometry
Date
2014-06-29T21:41:04Z (11 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
Hiroyuki Maehara (Univ. of Tokyo) reports on behalf of the OISTER collaboration:
We observed the field of GRB 140629A (Lien et al. GCN 16477) with the 1.05-m
Schmidt telescope and KWFC (Sako et al. 2012, Proc. SPIE 8446, 84466L) at
Kiso Observatory in Japan. The observations were made in the Sloan z-band at
2014-06-29 14:30-14:39 (UT; 13-22 min post burst) and 16:30-16:45 (133-148
min post burst).
We detected an uncatalogued fading source at RA=16:35:54.45, DEC=+41:52:36.6
(equinox 2000.0; uncertainty 0".3).$B!!(BPreliminary photometry of the source
is as follows:
obs. date (mid time) t-T0 (days) exp.(sec) filter mag limiting mag
2014-06-29 14:30:30 0.0090 180 sec z 14.89+/-0.02 19.4
14:34:47 0.0120 180 z 15.23+/-0.02 19.4
14:39:05 0.0150 180 z 15.50+/-0.02 19.4
16:30:34 0.0924 180 z 17.68+/-0.06 19.1
16:34:52 0.0954 180 z 18.01+/-0.08 19.1
16:45:18 0.1026 180 z 17.87+/-0.08 18.9
The photometry is based on z-mag of SDSS stars in the observed field.
GCN Circular 16485
Subject
GRB 140629A: NOT optical observations
Date
2014-06-29T22:16:05Z (11 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
Daniele Malesani (DARK/NBI), Nicolaas E. Groeneboom (UiO), Jostein R.
Kristiansen (HiOA), and Pall Jakobsson (Univ. Iceland), report on behalf
of a larger collaboration:
We observed the field of GRB 140629A (Lien et al., GCN 16477) with the
Nordic Optical Telescope (NOT) equipped with the MOSCA imager.
Observations were carried out in the SDSS g, r, i, and z filters. The
afterglow is detected in all filters.
In a 300-s image started at 21:17 UT (7.0 hr after the GRB), the
afterglow has a magnitude r = 19.54 +- 0.02 (AB), calibrated against
several nearby SDSS stars. Calibrated against USNO-B1, the afterglow
coordinates are (J2000):
RA = 16:35:54.45
Dec = +41:52:36.5
with an uncertainty of 0.3". This is in good agreement with the
determinations by UVOT (Lien et al., GCN 16477), MASTER (Yurkov et al.,
GCN 16478), and KWFC (Maehara, GCN 16484).
GCN Circular 16486
Subject
GRB 140629A: T100 observations
Date
2014-06-29T22:56:55Z (11 years ago)
From
Eda Sonbas at NASA/GSFC <edasonbas@gmail.com>
E. Sonbas (Adiyaman Univ.), F. Dolek (Cukurova Univ.), T. Guver (Istanbul
Univ.), , E. Gogus (Sabanci Univ.), O. Erece (Akdeniz Univ.), M. Camurdan,
D. Zengin Camurdan (Ege Univ.), H. Kirbiyik (TUG) report on behalf of a
larger collaboration
We observed the field of Swift GRB 140629A (Lien et al., GCN#16477) with
the 1.0 meter T100 telescope (Bakirlitepe, TUBITAK National Observatory,
Turkey), starting June, 29, 18:42:13 UT (~ 4.412 hours after the trigger).
The afterglow is clearly detected in 300 s in the R band images.
Using USNO-B1 star USNO-B1 1318-0308023 (R.A.=248.99, Dec=+41.85) in the
field, the magnitudes of the OT were estimated as follows;
t-t0 (hr) exp.(s) filt mag err (+/-)
4.412 300 R 18.59 0.03
4.511 300 R 18.61 0.03
We are grateful to TUBITAK National Observatory for prompt scheduling the
observations and technical support.
GCN Circular 16487
Subject
GRB140629A: Kanata/HOWPol optical observation
Date
2014-06-29T23:33:24Z (11 years ago)
From
Koji Kawabata at HASC,Hiroshima U <kawabtkj@hiroshima-u.ac.jp>
K. Takaki, T. Nakaoka, Y. Moritani, K. S. Kawabata (Hiroshima Univ.) report
on behalf of Kanata team:
We performed a series of optical imaging polarimetry for the optical
afterglow of GRB140629A (Yurkov et al., GCN 16478, Xin et. al GCN 16480,
Bikmaev et al., GCN 16482) from 73 sec after the Swift/BAT trigger
(Lien et al., GCN 16477) with HOWPol attached to the 1.5-m Kanata telescope
at Higashi-Hiroshima Observatory, Japan.
Calibrated with USNO-B1 catalogue, our quick-look photometry indicates that
the R-band magnitude of the optical afterglow was 14.0 at the beginning of
our observation, reached its peak brightness of 13.3 mag around 160 sec,
and then smoothly declined. Further analysis is ongoing.
GCN Circular 16488
Subject
GRB 140629A: MITSuME Ishigakijima Optical Observation
Date
2014-06-30T01:11:31Z (11 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda (OAO, NAOJ), H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:
We observed the field of GRB 140629A (Lien et al., GCNC 16477)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.
The observation started on 2014-06-29 14:20:40 UT (~3.2 min after the burst).
We detected the previously reported afterglow (Yurkov et al., GCNC 16478;
Xin et al., GCNC 16480; Bikmaev et al., GCNC 16482; Masi, GCNC 16483;
Maehara, GCNC 16484) in all the three bands.
Photometric results of the OT are listed below.
We used SDSS catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
--------------------------------------------------------------------------
0.00254 14:21:10 60.0 14.37 0.03 13.18 0.03 13.65 0.03
0.21351 19:24:57 540.0 19.47 0.14 18.95 0.09 18.17 0.12
--------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 16489
Subject
GRB 140629A: BTA redshift
Date
2014-06-30T02:08:02Z (11 years ago)
From
Rodion Burenin at IKI, Moscow <rodion@hea.iki.rssi.ru>
A. Moskvitin (SAO-RAS, N. Arkhyz), R. Burenin (IKI, Moscow),
R. Uklein, V. Sokolov (SAO-RAS, N. Arkhyz), R. Sanchez-Ramirez,
J. Gorosabel and A. J. Castro-Tirado (IAA-CSIC, Granada), on behalf of
a larger collaboration, report:
Following the detection of GRB 140629A by Swift (Lien et al. GCNC
16477), we observed the optical counterpart (Lien et al., GCNC 16477,
Yurkov et al. GCNC 16478) with the 6-m BTA (+Scorpio-I) on June 29,
starting 4.1 hours after the event. We obtained 43.6 minutes of
spectral data in the range 4000-9800A and resolution FWHM = 13A. The
optical afterglow spectrum shows prominent absorption lines which we
interpret as AlIII, CIV, CII, FeII, MgII, SiIV at the redshift
z = 2.275 +/- 0.003. We suggest this to be the redshift to GRB
140629A.
GCN Circular 16490
Subject
GRB 140629A: Swift-XRT refined Analysis
Date
2014-06-30T04:29:04Z (11 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), C. Pagani (U.
Leicester), A. Maselli (INAF-IASFPA), A. Melandri (INAF-OAB), B.
Sbarufatti (INAF-OAB/PSU), V. Mangano (PSU), M.C. Stroh (PSU), D.N.
Burrows (PSU) and A.Y. Lien report on behalf of the Swift-XRT team:
We have analysed 10 ks of XRT data for GRB 140629A (Lien et al. GCN
Circ. 16477), from 80 s to 34.9 ks after the BAT trigger. The data
comprise 136 s in Windowed Timing (WT) mode (the first 10 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 Evans et
al. (GCN Circ. 16479).
The late-time light curve (from T0+4.2 ks) can be modelled with a
power-law decay with a decay index of alpha=1.37 (+/-0.09).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.82 (+0.17, -0.16). The
best-fitting absorption column is 4.5 (+3.8, -3.4) x 10^20 cm^-2, in
excess of the Galactic value of 9.3 x 10^19 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.98 (+/-0.10) and a
best-fitting absorption column of 5.2 (+2.2, -2.0) x 10^20 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.3 x 10^-11 (3.7 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 5.2 (+2.2, -2.0) x 10^20 cm^-2
Galactic foreground: 9.3 x 10^19 cm^-2
Excess significance: 3.5 sigma
Photon index: 1.98 (+/-0.10)
If the light curve continues to decay with a power-law decay index of
1.37, the count rate at T+24 hours will be 7.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.4 x
10^-13 (2.8 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00602884.
This circular is an official product of the Swift-XRT team.
GCN Circular 16491
Subject
GRB 140629A: P60 observations
Date
2014-06-30T06:10:50Z (11 years ago)
From
Daniel Perley at Caltech <dperley@astro.caltech.edu>
D. A. Perley (Caltech) and S. B. Cenko (NASA/GSFC) report:
We imaged the location of Swift GRB 140629A (Lien et al., GCN 16477)
with the Palomar 60-inch (P60) robotic telescope on UT 2014-06-30
between 04:10 and 04:44 UT, in the r' filter. We acquired 10 exposures
of 180 seconds each. The optical afterglow (Lien et al., GCN 16477;
Yurkov et al. GCN 16478) is well-detected in the stacked image.
Comparing to SDSS field stars, we measure a magnitude of:
r = 20.91 +/- 0.03 (t_mid = 0.590 days)
Further observations are ongoing.
GCN Circular 16492
Subject
GRB140629A: VATT optical observations
Date
2014-06-30T09:08:08Z (11 years ago)
From
Peter Garnavich at U of Notre Dame <pgarnavi@nd.edu>
P. Garnavich and B. Rose (Notre Dame)
We observed the field of GRB140629A (Lien et al. GCN 16477) with the
Vatican Advanced Technology Telescope and VATT4K CCD camera
on 2014 June 30.2757 (UT). The afterglow is well-detected in two 300s
exposures through a SDSS-r filter.
Calibrating from SDSS stars in the field we estimate the afterglow to be
r=21.08 +/- 0.03 mag at 16.33 hours after the burst.
Combining the brightness reported here and SDSS magnitudes estimated by
Malesani et al. (GCN 16485) and Perley et al. (GCN 16491), the optical power
law decay index is 1.7 between 7 and 16 hours after the burst.
GCN Circular 16493
Subject
GRB 140629A: TNG redshift confirmation
Date
2014-06-30T10:04:17Z (11 years ago)
From
Paolo D'Avanzo at INAF-OAB <paolo.davanzo@brera.inaf.it>
P. D'Avanzo (INAF-OAB), D. Malesani (DARK/NBI), V. D'Elia, L.A. Antonelli (INAF/OAR & ASI/ASDC), G. Tagliaferri (INAF-OAB), S.D. Vergani (CNRS/GEPI), A. Fiorenzano, G. Mainella (INAF/TNG) report on behalf of the CIBO collaboration:
We observed the optical afterglow of GRB 140629A (Lien et al., GCN 16477; Yurkov et al. GCN 16478) on 2014 June 30 with the 3.6m TNG telescope located in the Canary Islands, equipped with the DOLORES operated in both imaging and spectroscopic mode. The observations were carried out under poor weather conditions (clouds and calima).
In a 120 s image started at 01:41:38 UT (~11.4 hr after the GRB), the afterglow has a magnitude r = 20.4 +/- 0.1 (AB), calibrated against nearby SDSS stars.
We also obtained three optical spectra, each one lasting 1200 s, using the grism LR-B covering the wavelength range 3000 - 8000 AA. The observation started at 02:07:21 UT (~11.8 hr after the GRB). Using a preliminary wavelength calibration, in the co-added spectrum we detect several absorption lines which we interpret as due to Ly-alpha, C II (1334), C IV (1548/1550) at a common redshift of 2.29. Our result is in agreement with the redshift reported by Moskvitin et al. (GCN 16489).
GCN Circular 16494
Subject
GRB 140629A: Swift/UVOT Detection
Date
2014-06-30T11:32:49Z (11 years ago)
From
Alice Breeveld at MSSL-UCL <a.breeveld@ucl.ac.uk>
A. A. Breeveld (UCL-MSSL) and A. Y. Lien (GSFC/UMBC) report on behalf of
the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 140629A
101 s after the BAT trigger (Lien et al., GCN Circ. 16477).
A fading source consistent with the XRT position (Evans et al. GCN Circ.
16479) is detected in the initial UVOT exposures. The fact that it is
not seen in uvm2 or uvw2 filters is consistent with the redshift given
by Moskvitin et al., GCN Circ. 16489 and D�Avanzo et al., GCN Circ. 16493.
The preliminary UVOT position is:
RA (J2000) = 16:35:54.42 = 248.97676 (deg.)
Dec (J2000) = +41:52:36.8 = 41.87690 (deg.)
with an estimated uncertainty of 0.42 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 101 251 147 14.78 � 0.02
v 643 663 20 15.29 � 0.09
b 569 589 20 15.70 � 0.06
u 313 563 246 14.89 � 0.03
w1 692 712 19 17.5 � 0.3
m2 667 687 19 >17.5
w2 619 639 19 >18.0
The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.01 in the direction of the
burst (Schlegel et al. 1998).
GCN Circular 16495
Subject
Konus-Wind observation of GRB 140629A
Date
2014-06-30T12:59:28Z (11 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, A. Tsvetkova, A.Lyssenko, and T. Cline
on behalf of the Konus-Wind team, report:
The long GRB 140629A (Swift-BAT trigger #602884: Lien et al., GCN 16477;
Cummings et al., GCN 16481; T0(BAT)=14:17:30 UT)
was detected by Konus-Wind in the waiting mode.
The light curve shows a double-peaked structure which started
~4 s before the BAT trigger and lasted till ~T0(BAT)+22 s.
The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB140629A/
As observed by Konus-Wind, the burst had a fluence of
(3.4 � 0.5)x10^-6 erg/cm2 and a 2.944-s peak energy flux,
measured from ~T0(BAT)+13.450 s, of (4.7 � 0.7)x10^-7 erg/cm2
(both in the 20 - 10000 keV energy range).
Modeling the KW 3-channel time-integrated spectrum
(from T0(BAT)-4.214 s to T0(BAT)+22.282 s) by a power law
with exponential cutoff (CPL) model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.42 � 0.54, and Ep = 86 � 17 keV.
Modelling the 3-channel spectrum near the peak count rate
(from T0(BAT)-13.450 s to T0(BAT)+16.394 s) by
the CPL model yields alpha = -1.50 � 0.23, and Ep = 156 � 52 keV.
Assuming the redshift z=2.275 (Moskvitin et al., GCN 16489;
D'Avanzo et al., GCN 16493)
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, and Omega_Lambda = 0.73,
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is ~4.4x10^52 erg,
the peak luminosity L_iso is ~2.0x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~283 keV.
All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.
GCN Circular 16496
Subject
GRB 140629A: Nishi-Harima NIR Observations
Date
2014-06-30T15:01:06Z (11 years ago)
From
Akira Arai at Nishi-Harima Astro. Obs/U of Hyogo <arai@nhao.jp>
S. Honda, Y. Takagi, A. Arai, K. Morihana (Univ. of Hyogo)
report on behalf of Nayuta team and OISTER collaboration:
We observed the field of GRB 140629A (A. Y. Lien et al., GCN 16477)
with Nishiharima Infrared Camera (NIC) attached to the Nayuta 2-m
telescope at the Nishi-Harima Astronomical Observatory.
The observations were conducted on 2014-06-29 at 14:27-15:32 UT.
We detected the near-infrared afterglow in J, H and Ks bands.
Photometric results of our observations are listed below.
We used 2MASS 16355059+4151367, 16355050+4151433, and 16355992+4151103
as reference stars for photometry.
# MID-UT Tmid-T0 T-EXP J_mag H_mag Ks_mag
-----------------------------------------------------------------------
14:34:02 0.28 600 14.1 +/- 0.2 13.3 +/- 0.1 12.7 +/- 0.2
14:51:34 0.57 600 15.1 +/- 0.2 14.2 +/- 0.1 13.6 +/- 0.2
15:08:16 0.85 600 15.6 +/- 0.2 14.8 +/- 0.1 14.1 +/- 0.2
15:22:49 1.08 480 16.0 +/- 0.2 15.1 +/- 0.1 14.3 +/- 0.2
------------------------------------------------------------------------
Tmid-T0: Elapsed time after the burst (hours)
T-EXP: Total Exposure time (seconds)
--
-------------------------------------------------
Akira Arai,
Nishi-Harima Astronomical Observatory,
University of Hyogo
mail : arai@nhao.jp
-------------------------------------------------
GCN Circular 16498
Subject
GRB 140629A: additional P60 observations
Date
2014-07-01T06:22:11Z (11 years ago)
From
Daniel Perley at Caltech <dperley@astro.caltech.edu>
D. A. Perley (Caltech) and S. B. Cenko (NASA/GSFC) report:
We acquired additional imaging of the afterglow of GRB 140629A (Lien et
al., GCN 16477; Yurkov et al. GCN 16478) with the Palomar 60-inch (P60)
robotic telescope on UT 2014-07-01 between 04:23 and 04:52, acquiring
9x180s exposures in the r' filter. We measure a magnitude of:
r = 22.92 +/- 0.14 (t_mid = 1.598 days)
This indicates a relatively rapid decay index of alpha=1.87 since our
observation the previous night (see also Garnavich and Rose, GCN 16492).
GCN Circular 16499
Subject
GRB 140629A: SAO RAS monitoring
Date
2014-07-01T13:41:18Z (11 years ago)
From
Vladimir Sokolov at SAO RAS <sokolov@sao.ru>
A. Moskvitin (SAO-RAS, N. Arkhyz), R. Burenin (IKI, Moscow),
R. Uklein, V. Sokolov, T. Sokolova (SAO-RAS, N. Arkhyz),
on behalf of a larger collaboration, report:
We performed the photometrical monitoring of the GRB 140629A OT (Lien
et al., GCNC 16477) with two optical telescopes of SAO RAS: the 6-m
BTA (V band) and the 1-m Zeiss-1000 (BVRcIc bands) on the night of
June, 29/30. Observations started 4.1 hours after the Swift trigger.
The optical transient (Lien et al., GCNC 16477; Yurkov et al.,
GCNC 16478; Bikmaev et al., GCNC 16482; Masi, GCNC 16483; Maehara,
GCNC 16484; Malesani et al., GCNC 16485; Sonbas et al., GCNC 16486;
and other teams) is clearly detected in every single image.
On the basis of the same star from USNO-B1 as Bikmaev et al. (GCNC 16482)
with the coordinates R.A., = 16:35:59.9, Decl.= +41:51:10, J2000 and
magnitude R1_mag = 16.49 we made preliminary photometric estimations
of the OT Rc images. The results are as follows:
# Start,UT exp,s R_mag +/- err
====================================
1 19:00:41 180.00 18.02 +/- 0.05
2 19:05:38 180.00 18.20 +/- 0.05
3 19:11:11 180.00 18.45 +/- 0.07
4 19:28:39 300.00 18.25 +/- 0.04
5 20:03:55 300.00 18.53 +/- 0.04
6 20:26:36 300.00 18.58 +/- 0.04
7 20:53:25 300.00 18.87 +/- 0.04
8 22:10:17 300.00 19.00 +/- 0.05
9 22:33:32 300.00 19.11 +/- 0.05
10 22:57:16 300.00 19.00 +/- 0.05
11 23:25:27 300.00 19.31 +/- 0.09
12 23:49:07 300.00 19.38 +/- 0.11
Further analysis and observations go on.
GCN Circular 16500
Subject
GRB 140629A: MASTER-Net preliminary light curve
Date
2014-07-01T15:21:21Z (11 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy (Lomonosov Moscow University)
V. Krushinski (Ural Federal State University)
M. Pruzhinskaya (Lomonosov Moscow University)
P.Balanutsa, A.Kuznetsov, V.V.Chazov, N.Tyurina, D.Denisenko
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University
V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov, A. Gabovich
Blagoveschensk Educational State University, Blagoveschensk
K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University
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)
Three MASTER system telescopes located in Blagoveshchensk, Tunka and
Kislovodsk have observed GRB140629A (Lien et al., GCN 16477) from 33
seconds till ~9 hours after the trigger. MASTER II robotic telescope
(MASTER-Net: http://observ.pereplet.ru) located in Blagoveschensk was
pointed to GRB140629A 15 sec after notice time and 33 sec after
trigger time at 2014-06-29 14:18:03.188 UT and found OT in SWIFT
error-box. MASTER II Tunka was pointed to GRB140629A 78 sec after
trigger time at 2014-06-29 14:18:48.102 UT on the evening twilight sky
(Sun ~5 d. below horizon) with dark sky observations starting ~ 50 min
after trigger time. MASTER II Kislovodsk was pointed to GRB140629A
~3.2 hours after the trigger directly after the Sun set and weather
conditions became suitable.
The preliminary light curve is available here:
http://master.sai.msu.ru/static/GRB/GRB140629A_slope2.png
The optical transient (Lien et al., GCN 16477; Yurkov et al., GCN
16478; Moskvitin et al., GCN 16489; Bikmaev et al., GCN 16482; Masi,
GCN 16483; Maehara, GCN 16484; Malesani et al., GCN 16485; Sonbas et
al., GCN 16486 etc.) has a maximum at ~ 150 sec. after the burst,
reaching 13.8 mag, after which it shows a power law decay. The power
law index (alpha) from 200 to 10000 seconds after the trigger is 1.12
+- 0.1 (F ~ t^-alpha).
There was no polarization more than 3% discovered on afterglow
stage.
GCN Circular 16501
Subject
GRB 140629A: MITSuME Akeno Optical observation
Date
2014-07-02T06:24:29Z (11 years ago)
From
Taketoshi Yoshii at Tokyo Tech <yoshii.t.ac@m.titech.ac.jp>
Y. Yano, T. Yoshii, Y. Saito, Y. Tachibana, H. Ohuchi,
S. Kurita, Y. Ono, T. Fujiwara, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:
We observed the field of GRB 140629A (A. Y. Lien et al., GCN Circular #16477) with the
optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.
The observation started on 2014-06-29 14:23:32 UT (6 min after the burst).
We detected the previously reported optical afterglow of GRB140629A
(V.Yurkov et al., GCN Circular #16478) in the g', Rc and Ic band.
The measured magnitudes are listed below.
T0+[sec] MID-UT T-EXP[sec] g' Rc Ic
----------------------------------------------------------------------------------------------------
362 14:24:02 60.0 15.06+/-0.04 14.25+/-0.03 13.83+/-0.03
11482 17:43:45 600.0 18.77+/-0.23 18.06+/-0.16 17.67+/-0.21
----------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.
GCN Circular 16517
Subject
GRB 140629A, Optical observations
Date
2014-07-04T04:08:29Z (11 years ago)
From
Shashi Bhushan Pandey at ROTSE <shaship@umich.edu>
S. B. Pandey and Brajesh Kumar (ARIES Nainital India,on behalf of larger
Indian GRB collaboration)
We observed the Swift GRB 140629A field (Lien et al., GCNC 16477) using
1.04m ST telescope at ARIES Nainital. Observations were started at 17:40:59
UT on 2014-06-29 (approximately 3.4 h after the burst). Several frames
with an exposure time of 300 s each in R_c and I_c bands were obtained in
good sky conditions.
The optical counterpart of GRB 140629A (Lien et al., GCNC 16477;
Yurkov et al., GCNC 16478; Bikmaev et al., GCNC 16482; Masi, GCNC
16483; ) is clearly detected in each individual frames.
Preliminary photometry is following:
-----------------------------------------------
UT Exp_time Filter Mag
------------------------------------------------
17:40:59 300 s R_c 18.01 +- 0.05
17:56:21 300 s I_c 17.92 +- 0.06
------------------------------------------------
The photometry was performed in comparison to nearby USNO stars.
This massage may be cited
GCN Circular 16518
Subject
GRB 140629A: SAO RAS Rc band photometry
Date
2014-07-04T05:57:05Z (11 years ago)
From
Vladimir Sokolov at SAO RAS <sokolov@sao.ru>
A.S. Moskvitin, V.N. Komarova, T.N. Sokolova, V.V. Sokolov (SAO RAS,
N. Arkhyz), on behalf of a larger collaboration, report:
We observed the GRB 140629A field (Lien et al., GCNC 16477)
with the 1-m SAO RAS telescope Zeiss-1000 on June, 30.
Observations started at 21:21:36 and ended at 23:48:49 UT.
22 x 300 sec. images in the Rc filter were obtained under good weather
conditions.
Unlike the previous night, the OT is not visible in single images,
but is clearly detectable in the stacked image. Based on the same
USNO-B1 star (Moskvitin et al., GCNC 16499; Bikmaev et al., GCNC 16482)
with R1_mag = 16.49, we measured the OT magnitude as R = 22.1 +/- 0.2
on the phase 1.35 days after the trigger.