GRB 140304A
GCN Circular 15914
Subject
GRB 140304A: MASTER OT detecton
Date
2014-03-04T13:33:36Z (11 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, M. Pruzhinskaya, D.Denisenko,
V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute
K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk 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.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 Tunka was pointed to the GRB140304A 84 sec after trigger
time at 2014-03-04 13:23:55.366 UT. On our first (10s exposure) set we
found optical transient within SWIFT error-box (ra=02 02 38
dec=+33 29 24 r=0.050000)
02h 02m 34.13s , +33d 28m 26s.6 mag 16.5
The message may be cited.
GCN Circular 15915
Subject
GRB 140304A: Swift detection of a burst
Date
2014-03-04T13:57:15Z (11 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
P. A. Evans (U Leicester), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), S. T. Holland (STScI),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. H. Siegel (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:
At 13:22:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140304A (trigger=590206). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 30.668, +33.485 which is
RA(J2000) = 02h 02m 40s
Dec(J2000) = +33d 29' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a multi-peaked
structure with a total duration of about 20 sec. The peak count rate
was ~3600 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 13:23:46.2 UT, 75.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 30.6412,
33.4744 which is equivalent to:
RA(J2000) = 02h 02m 33.90s
Dec(J2000) = +33d 28' 27.9"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 89 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.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 5.98
x 10^20 cm^-2 (Kalberla et al. 2005).
The initial flux in the 2.5 s image was 6.28e-10 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 250 seconds with the U filter starting
137 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image processing FAILED
because of no aspect solution. Results from the list of sources generated
on-board are not available at this time. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.08.
This GRB will enter a Moon observing constraint around 20:00 UT and
will not be observable again by Swift until March 6 (Thursday) around
05:30 UT.
Burst Advocate for this burst is P. A. Evans (pae9 AT star.le.ac.uk).
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 15916
Subject
GRB 140304A: Afterglow decay from Nanshan observations
Date
2014-03-04T14:26:19Z (11 years ago)
From
Dong Xu at DARK/NBI <dong.dark@gmail.com>
D. Xu (DARK/NBI), H.-B. Niu, G.-J. Feng, T.-Z. Yang, A. Esamdin, L. Ma
(XAO) report:
We observed the field of GRB 140304A (Evans et al., GCN 15915) using
the 1m telescope located in Nanshan, Xinjiang, China. Observations
started at 13:43:26 UT on 2014-03-04 (i.e., 0.349 hr after the BAT
trigger) and a series of 120s and 500s R-band images were obtained.
In the first 120s R-band image, an optical source is clearly detected
at the MASTER position (Gorbovskoy et al., GCN 15914), which is also
consistent with the Swift/XRT position. We thus think this is the
afterglow of the burst, and it has decayed to R=19.4+/-0.2 mag,
calibrated with nearby SDSS stars.
Observations are ongoing.
GCN Circular 15917
Subject
GRB 140304A: Mondy optical observations
Date
2014-03-04T15:02:59Z (11 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A.Volnova (IKI), A. Pozanenko (IKI), I. Korobtsev (ISTP), E. Klunko
(ISTP), M. Eselevich (ISTP), report on behalf of larger GRB follow-up
collaboration:
We observed the field of GRB 140304A (Evans et al., GCN 15915) with
AZT-33IK telescope of Mondy observatory starting on Mar. 04 (UT)
13:54:10, i.e. ~0.5 hour after burst trigger. In the first images of 60
s exposure we clearly detected afterglow of GRB 140304A reported by
Gorbovskoy et al. (GCN 15914) and Xu et al. (GCN 15916). Preliminary
photometry of the fading afterglow is following:
date UT start t-T0 Exp. Filter OT
(mid, days) (s)
2014-03-04 13:54:10 0.02406 6*60 R 20.29 �� 0.17
The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005):
N SDSS_id R(Lupton) err
J020233.12+332550.3 15.665 0.012
J020219.91+332738.5 14.785 0.012
GCN Circular 15918
Subject
GRB 140304A: Khureltogot optical observations
Date
2014-03-04T15:17:16Z (11 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), N. Tungalag (Research Centre of Astronomy and
Geophysics MAS), S. Schmalz (AIP), V. Voropaev (KIAM), I.Molotov (KIAM),
A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:
We observed the field of the he field of GRB 140304A (Evans et al., GCN
15915) with ORI-40 telescope of Khureltogot observatory starting on
Mar., 04 (UT)13:29:36, i.e., ~7 minutes after the GRB trigger. In the
first unfiltered images of 60 s exposure we clearly detected afterglow
of GRB 140304A reported by Gorbovskoy et al. (GCN 15914), Xu et al.
(GCN 15916), and Volnova et al., (GCN 15917). Preliminary photometry of
the fading afterglow is following:
date UT start t-T0 Exp. Filter OT
(mid, days) (s)
2014-03-04 13:29:36 0.00602 3*60 none 17.5 +/- 0.2
The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005):
N SDSS_id R(Lupton)err
J020233.12+332550.3 15.665 0.012
J020219.91+332738.5 14.785 0.012
GCN Circular 15920
Subject
GRB 140304A: Swift/UVOT Upper Limits
Date
2014-03-04T21:39:55Z (11 years ago)
From
Frank Marshall at GSFC <femarsha@khamseen.gsfc.nasa.gov>
F. E. Marshall (NASA/GSFC) and P. A. Evans (U. Leicester)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 140304A
138 s after the BAT trigger (Evans et al., GCN Circ. 15915).
No optical afterglow consistent with the optical position
(Gorbovskoy et al. GCN Circ. 15914)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
u_FC 138 388 246 >20.4
v 420 1561 165 >19.5
u 138 1519 529 >20.9
w1 469 1495 156 >19.7
m2 570 1470 117 >20.1
w2 396 1546 156 >20.0
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).
In view of the bright (16.5 mag) afterglow reported by
Gorbovskoy et al., it is likely that the GRB has large
intrinsic extinction or is at a redshift greater than
about 3.5.
GCN Circular 15921
Subject
GRB 140304A: NOT observations and redshift estimate
Date
2014-03-04T21:44:36Z (11 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Gorosabel (EHU-UPV,
IAA-CSIC), D. Xu (DARK/NBI), D. Malesani (DARK/NBI), A. Somero (NOT),
B. Milvang-Jensen (DARK/NBI), M.I. Andersen (DARK/NBI), P. Jakobsson
(U. Iceland) and J.P.U. Fynbo (DARK/NBI) report on behalf of a larger collaboration:
We have observed the afterglow of 140304A (Gorbovskoy et al. GCN 15914, Evans et
al. GCN 15915) with the Nordic Optical Telescope (NOT) equipped with ALFOSC.
Observations started at 20:19 UT on March 4 (i.e., 6.95 hr after the burst) in r and g-bands.
The afterglow is clearly detected in r-band at 20.5 mag, but undetected in g-band down to
a 3-sigma limit of 21.5, pointing towards a high-redshift event at z ~ 5 if the Lyman break
is between g and r-band.
Further observations are ongoing.
GCN Circular 15922
Subject
GRB 140304A: 10.4m GTC redshift z = 5.39
Date
2014-03-04T22:01:48Z (11 years ago)
Edited On
2024-11-18T10:04:01Z (7 months ago)
From
Alberto Castro-Tirado at Inst.de Astro. de Andalucia <ajct@iaa.es>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
S. Jeong, R. Sánchez-Ramírez (IAA-CSIC), A. J. Castro-Tirado (IAA-CSIC,
UMA), J. Gorosabel (EHU-UPV, IAA-CSIC), M. Jelinek, J. C. Tello, P.
Ferrero, O. Lara-Gil, R. Cunniffe (IAA-CSIC), D. Pérez-Ramírez (U. Jaén),
S. Guziy (Nikolaev Univ.), J. M. Castro Cerón (ESAC), A. Fernández-Soto
(UV), J. Cepa (IAC), M. A. Rivero and G. Gómez-Velarde (GTC), on behalf of
a larger collaboration, report:
"Following the detection of the optical afterglow (Gorbovskoy et al. GCNC
15914) to GRB 140304A (Evans et al. GCNC 15915), we have obtained an
optical spectrum with the 10.4 m GTC (+OSIRIS) starting aprox. 8.2 hr
postburst, covering the 5700-10000 wavelength range. The continuum is
detected only redwards of aprox. 7750 A, with several absorption metallic
lines (N V, Si II and Si IV amongst others) at a common redshift of z =
5.39 which we propose to be the redshift of GRB 140304A. This is
consistent with the Swift/UVOT upper limits (Marshall et al. GCNC 15920)
and the NOT optical observation (de Ugarte Postigo et al. GCNC 15921)."
[GCN OPS NOTE(04mar14): Per author's request, the "5.XX" was replaced with 5.39.]
GCN Circular 15923
Subject
GRB 140304A: Fermi GBM detection
Date
2014-03-04T22:27:39Z (11 years ago)
From
Peter Jenke at MSFC <peter.a.jenke@nasa.gov>
P. Jenke (UAH) and G. Fitzpatrick (UCD) reports on behalf of the Fermi GBM Team:
"At 13:22:31.48 UT on March 4 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140304A (trigger 415632154/140304577),
which was also detected by Swift (P. A. Evans et al. 2014, GCN 15915).
The GBM on-ground location, using the Fermi GBM trigger
data, is consistent with the Swift/XRT location.
The angle of the burst direction to the Fermi LAT boresight is 80 degrees.
The GBM light curve consists of two main peaks with a
combined duration (T90) of 32 +/- 6 s (50-300 keV).
The time-averaged spectrum from T0-5 s to T0+14 s is
well fit by a power law function with an exponential
high energy cutoff. The power law index is -1.1 +/- 0.1
and the high energy cutoff, parameterized as
EPeak, is 185 +/- 35 keV.
The event fluence (10-1000 keV) in this time interval is
(2.6 +/- 0.2)E-06 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+7.2 s in the 10-1000 keV band
is 2.5 +/- 0.3 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 15924
Subject
GRB 140304A: Redshift from the NOT
Date
2014-03-05T00:41:12Z (11 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. Xu (DARK/NBI),
J. Gorosabel (EHU-UPV, IAA-CSIC), D. Malesani (DARK/NBI),
B. Milvang-Jensen (DARK/NBI), M.I. Andersen (DARK/NBI),
P. Jakobsson (U. Iceland), J.P.U. Fynbo (DARK/NBI), and
A. Somero (Tuorla Obs.) report on behalf of a larger collaboration:
Following the photometry reported in GCN 15921, we have performed spectroscopy
of GRB 140304A (Gorbovskoy et al. GCN 15914, Evans et al. GCN 15915) with the
Nordic Optical Telescope (NOT) equipped with ALFOSC. The observation began at
21:20 UT (7.97 hr after the burst) and consisted of a single 1500 s exposure
covering the range between 3200 and 9100 A.
We detect continuum emission with a deep absorption consistent with a
DLA at a redshift of 5.28+/-0.02, as well as emission down to ~5800 A, which
is consistent with the Ly-limit at a similar redshift. Despite the lack of metal
features identified in our spectrum, a redshift of z=5.39 as reported by
Jeong et al. (GCN 15922) is inconsistent with our data.
GCN Circular 15925
Subject
GRB 140304A: Enhanced Swift-XRT position
Date
2014-03-05T00:43:34Z (11 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.
Using 3335 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 140304A, 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 = 30.64267, +33.47384 which is equivalent
to:
RA (J2000): 02h 02m 34.24s
Dec (J2000): +33d 28' 25.8"
with an uncertainty of 1.6 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 15926
Subject
GRB 140304A: Swift-XRT refined Analysis
Date
2014-03-05T02:57:04Z (11 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
K.L. Page (U. Leicester), C. Pagani (U. Leicester), A. Maselli
(INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU),
J.A. Kennea (PSU), V. Mangano (PSU), M.C. Stroh (PSU), A.P. Beardmore
(U. Leicester) and P.A. Evans report on behalf of the Swift-XRT team:
We have analysed 6.4 ks of XRT data for GRB 140304A (Evans et al. GCN
Circ. 15915), from 81 s to 23.1 ks after the BAT trigger. The data
comprise 42 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Beardmore et al. (GCN Circ. 15925). The late-time light curve (from
T0+5.2 ks) is consistent with a constant source of mean count rate
1.1e+00 ct/sec. A power-law fit gives an index of 0.2 (+/-0.7).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.00 (+0.15, -0.14). The
best-fitting absorption column is 9.8 (+3.4, -3.1) x 10^20 cm^-2, in
excess of the Galactic value of 6.0 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 (4.6 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 9.8 (+3.4, -3.1) x 10^20 cm^-2
Galactic foreground: 6.0 x 10^20 cm^-2
Excess significance: 2.0 sigma
Photon index: 2.00 (+0.15, -0.14)
If the light curve continues to decay with a power-law decay index of
0.2, the count rate at T+24 hours will be 0.024 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.7 x
10^-13 (1.1 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/00590206.
This circular is an official product of the Swift-XRT team.
GCN Circular 15927
Subject
GRB 140304A: Swift-BAT refined analysis
Date
2014-03-05T04:14:02Z (11 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
P. A. Evans (U Leicester), 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-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140304A (trigger #590206)
(Evans, et al., GCN Circ. 15915). The BAT ground-calculated position is
RA, Dec = 30.653, 33.480 deg, which is
RA(J2000) = 02h 02m 36.8s
Dec(J2000) = +33d 28' 47.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 74%.
The mask-weighted light curve shows several overlapping peaks starting
at ~T-10 sec, peaking at ~T+10 sec, and ending at ~T+30 sec.
T90 (15-350 keV) is 15.6 +- 1.9 sec (estimated error including systematics).
The time-averaged spectrum from T-3.94 to T+15.77 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.29 +- 0.08. The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+10.22 sec in the 15-150 keV band
is 1.7 +- 0.2 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/590206/BA/
GCN Circular 15928
Subject
GRB 140304A: RATIR g-band Dropout
Date
2014-03-05T04:59:08Z (11 years ago)
Edited On
2024-11-07T18:57:53Z (7 months ago)
From
Nat Butler at UC berkeley <natxbutler@gmail.com>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@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
(ORAU/GSFC), 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 140304A (Evans, et al., GCN 15915) 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 2014/03 5.12 to 2014/03 5.16 UTC (13.50 to
14.40 hours after the BAT trigger), obtaining a total of 0.26 hours
exposure in the g and r bands, 0.53 hours exposure in the i band, and 0.30
hours exposure in the Z, Y, J, and H bands.
For a source within the Swift-XRT error circle (Evans, et al., GCN 15925),
in comparison with the SDSS DR9 and 2MASS, we obtain the following
detections and 3-sigma upper limit:
g > 23.07
r 21.78 +/- 0.13
i 20.66 +/- 0.06
Z 19.45 +/- 0.05
Y 19.19 +/- 0.06
J 19.11 +/- 0.07
H 18.71 +/- 0.08
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.
Using the procedure outlined in Littlejohns et al. 2013 (arXiv:1312.3967),
we derive a photometric redshift z_phot = 5.45 (-0.2,+0.1; 90% confidence).
This photometric redshift is consistent with the one reported by de
Ugarte-Postigo et al. (GCN 15921) and the spectroscopic redshift
determinations by Jeong et al. (GCN 15922) and de Ugarte-Postigo et al.
(GCN 15924).
We thank the staff of the Observatorio Astronómico Nacional in San Pedro
Mártir.
GCN Circular 15930
Subject
GRB 140304A: VLA Detection
Date
2014-03-05T17:10:53Z (11 years ago)
From
Tanmoy Laskar at Harvard U <tanmoylaskar@gmail.com>
T. Laskar, A. Zauderer, and E. Berger (Harvard) report:
"We observed the position of GRB 140304A (Evans et al; GCN 15915) with
the VLA beginning on 2014 May 5.01 UT (0.45 days after the burst). At a
mean frequency of 6 GHz, we detect a radio source with a preliminary flux
density of ~ 0.05 mJy at
RA = 02:02:34.173 +/- 0.001
Dec = 33:28:26.01 +/- 0.02
consistent with the enhanced Swft/XRT position (Beardmore et al.; GCN
15925) and the optical position (Gorbovskoy et al.; GCN 15914). Follow-up
observations are planned."
GCN Circular 15931
Subject
GRB 140304A: CARMA 3mm detection
Date
2014-03-05T17:28:20Z (11 years ago)
From
Ashley Zauderer at CfA <bevinashley@gmail.com>
B. A. Zauderer, T. Laskar, and E. Berger (Harvard) report on behalf of the
CARMA Key Project "A Millimeter View of the Transient Universe":
"We observed the position of GRB 140304A (Evans et al., GCN 15915)
with the Combined Array for Research in Millimeter Astronomy (CARMA)
beginning
2014 Mar 5.01 UT (10.8 hours post-burst) at a mean frequency of ~85 GHz.
We detect a radio source with a flux of ~0.5 mJy consistent with the
enhanced Swift-XRT
position (Beardmore et al., GCN 15925), the optical afterglow
localization (Gorbovskoy et al.,
GCN 15914), and our VLA 5.8 GHz position (Laskar et al., GCN 15930).
Follow-up observations are in progress.
We thank the CARMA staff and observers, Shaye Storm and Robin Dong,
for their support of these rapid-response observations."
GCN Circular 15932
Subject
GRB 140304A: MASTER OT light curve
Date
2014-03-05T18:41:37Z (11 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, M. Pruzhinskaya, D.Denisenko, V.Kornilov, N.Tyurina,
P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute
K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk 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.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 Tunka was pointed to the GRB140304A (Evans et. al GCN 15915)
26 sec after notice time and 77 sec after trigger
time at 2014-03-04 13:23:49 UT. We detect OT (Gorbovskoy et. al GCN
15914) in two polarization bands during ~1 h while the source was brighter
than our upper limit.
The preliminary photometry result available in table 1 and here
http://master.sai.msu.ru/static/GRB/grb140304A.png .
Table 1. Preliminary early GRB140304A observations.
T_start(JD) T_trig-T_mid Exptime Mag1 Mag2 Coadd
2456721.05834 82 10 16.8 16.2 -
2456721.05931 172 30 17.2 16.9 -
2456721.06073 294 50 18.0 17.6 -
2456721.06142 358 120 18.1 17.6 2
2456721.06211 413 70 18.3 18.0 -
2456721.06724 894 580 18.5 18.5 4
2456721.08121 2070 1080 19.6 19.0 6
2456721.09812 3526 1080 19.9 19.4 6
Mag1 and Mag2 - Magnitude in two perpendicular polarizations.
The power low index alpha is 0.77+-0.05 (F ~ t-apha).
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Blagoveschensk was pointed to the GRB140304A 5 sec after
notice time and 46 sec after trigger time at 2014-03-04 13:23:17 UT.
The observations on this site made on bad weather conditions and on high
zenith distance. The 5-sigma upper limit On our first (10s exposure) image
has been about 13.0 mag.
The message may be cited.
GCN Circular 15936
Subject
GRB 140304A: 10.4m GTC refined redshift z = 5.283
Date
2014-03-06T16:12:38Z (11 years ago)
From
Alberto Castro-Tirado at Inst.de Astro. de Andalucia <ajct@iaa.es>
S. Jeong, R. S�nchez-Ram�rez (IAA-CSIC), J. Gorosabel (EHU-UPV,
IAA-CSIC) and A. J. Castro-Tirado (IAA-CSIC, UMA), on behalf of a larger
collaboration, report:
�Once the calibration data have been available we have reduced again the
optical spectrum taken with the 10.4 m GTC (+OSIRIS) starting aprox. 8.2
hr postburst. At the host galaxy location for GRB 140304A, we find a
damped Ly-alpha system with log N(H) ~ 21.6 and z = 5.283. We also get
the same redshift from its metal lines that we interpret as SII, SiII,
SiII*, CII, CII*, SiIV and FeII. This value supersedes the preliminary
measurement given in GCNC 15922 (Jeong et al.) and is consistent the one
reported in GCNC 15924 (de Ugarte Postigo et al.).�
GCN Circular 15937
Subject
GRB 140304A: Continued RATIR Optical and NIR Observations
Date
2014-03-06T16:57:05Z (11 years ago)
Edited On
2024-11-07T18:49:43Z (7 months ago)
From
Nat Butler at Az State U <natbutler@asu.edu>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@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
(ORAU/GSFC), 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 140304A (Evans, et al., GCN 15915) 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 2014/03 6.12 to 2014/03 6.14 UTC (37.55 to
38.08 hours after the BAT trigger), obtaining a total of 0.36 hours
exposure in the r and i bands and 0.15 hours exposure in the Z,
Y, J, and H bands.
For a source within the Swift-XRT error circle, in comparison with the SDSS
DR9 and 2MASS, we obtain the following detection and upper limits (3-sigma):
r > 22.77
i > 22.60
Z 20.88 +/- 0.20
Y > 20.96
J > 20.65
H > 20.31
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In the Z-band, the source has
faded as a powerlaw t^(-1.3) relative to our observations conducted last
night (Butler et al., GCN 15928).
We thank the staff of the Observatorio Astronómico Nacional in San Pedro
Mártir.
GCN Circular 15942
Subject
GRB 140304A: Suzaku WAM observation of the prompt emission
Date
2014-03-10T07:14:31Z (11 years ago)
From
Kazutaka Yamaoka at Nagoya U <yamaoka@stelab.nagoya-u.ac.jp>
W. Iwakiri (RIKEN), M. Tashiro, Y. Terada, T. Yasuda, Y. Ishida, H. Ueno,
S. Sugimoto, S. Koyama, S. Takeda, T. Nagayoshi (Saitama U.),
M. Yamauchi, N. Ohmori, M. Akiyama, R. Kinoshita (Univ. of Miyazaki),
M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa
(Hiroshima U.), K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.),
Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Hanabata (ICRR),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:
The long GRB 140304A (Swift/BAT trigger #590206 ; Evans et al., GCN
15915; Fermi-GBM detection: Jenke and Fitzpatrick, GCN 15923) was
detected by the the Suzaku Wide-band All-sky Monitor (WAM) which covers
an energy range of 50 keV - 5 MeV at 13:22:33 UT (=T0).
The observed light curve shows a multi-peaked structure lasting from
T0-3 s to T0+11 s with a duration (T90) of about 12 seconds. The fluence
in 100 - 1000 keV was 1.69 (+0.32/-0.34) x10^-6 erg/cm^2.
The 1-s peak flux measured from T0-1 s was 0.48 (+0.28, -0.23)
photons/cm^2/s in the same energy range.
Preliminary result shows that the time-averaged spectrum from T0-3 s to
T0+11 s is well fitted by a single power-law with a photon index of 2.09
(+0.66/-0.38) (chi^2/d.o.f = 12.3/14).
All the quoted errors are at statistical 90% confidence level, in which
the systematic uncertainties are not included.
The light curves with 1-sec time resolution for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html