GRB 100414A
GCN Circular 10698
Subject
GRB 100414A : EVLA Radio Detection
Date
2010-04-28T16:10:57Z (15 years ago)
From
Dale A. Frail at NRAO <dfrail@nrao.edu>
Dale A. Frail (NRAO), Poonam Chandra (RMC), S. Bradley Cenko
(Berkeley) and Fiona Harrison (Caltech) report on behalf of a larger
collaboration:
"We used the Expanded Very Large Array (EVLA) to observe the field of
view towards the Fermi GBM/LAT burst GRB 100414A (GCN 10594, 10595,
10649) on April 27.18 UT at a center frequency of 8.46 GHz. We detect
the radio afterglow with flux density of 397 � 15 microJy at the
position of the optical afterglow detected by GROND (GCN 10607).
Further observations are planned.
The EVLA is still undergoing active commissioning and we caution that
these results should be considered preliminary. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc."
GCN Circular 10697
Subject
GRB 100414A : WSRT Radio Detection
Date
2010-04-28T14:58:30Z (15 years ago)
From
Atish Kamble at U. of Amsterdam <A.P.Kamble@uva.nl>
A.P. Kamble (U of Amsterdam), A.J. van der Horst (NASA/MSFC/ORAU),
R.A.M.J. Wijers, E. Rol (U of Amsterdam), C. Kouveliotou (NASA/MSFC)
and K. Wiersema (U of Leicester) report on behalf of a larger
collaboration :
"We observed the field of Fermi GBM/LAT burst GRB 100414A (GCN 10594,
10595, 10649) using the Westerbork Synthesis Radio Telescope at 4.8 GHz
from April 27, 16.0 UT to April 28, 04.0 UT, i.e. 13.57 to 14.1 days
after the burst. We detect the radio afterglow with flux density
of 420 +/- 38 microJy at the position of the optical afterglow
detected by GROND (GCN 10607).
We would like to thank the WSRT staff for rapidly scheduling and
obtaining these observations."
GCN Circular 10649
Subject
GRB 100414A: Radio Afterglow Detection with the Expanded VLA
Date
2010-04-22T17:44:55Z (16 years ago)
From
Poonam Chandra at Royal Mil. College Canada <Poonam.Chandra@rmc.ca>
Poonam Chandra (RMC), Dale A. Frail (NRAO), S. Bradley Cenko (Berkeley)
and Fiona Harrison (Caltech) report on behalf of a larger collaboration:
We used the Expanded Very Large Array (EVLA) to observe the
Fermi burst GRB 100414A (Takahashi et al, GCN 10594 Foley GCN 10595)
on 2010 Apr 19 UT Within the revised XRT error circle (Goad et al
GCN 10605).
We detect the GRB afterglow with a flux density of 406 +/- 22 uJy.
The EVLA is undergoing active commissioning and as such these results
should be considered preliminary=2E Further observations are planned.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities Inc.
[GCN OPS NOTE(22apr10): Per author's request, the "13A" in the
Subject line was changed to "14A".]
GCN Circular 10641
Subject
GRB 100414A: CFHT optical observations
Date
2010-04-21T10:17:20Z (16 years ago)
From
Yuji Urata at Nat. Central U. <urata@astro.ncu.edu.tw>
Y. Urata (NCU) and K.Y Huang (ASIAA) on behalf of EAFON report;
"We observed the location of the GRB100414A optical afterglow
(Cucchiara et al. 10608) with CFHT on the night of April 19 (5.2 day
after the trigger) and 20 (6.2 day). The g', r' and i' band images
show the afterglow clearly. We estimate preliminary magnitudes of
r'=22.46+/-0.05 (5.19 day) and r'=22.84+/-0.05 (6.17 day) against the
SDSS field stars. Combined with the photometric results reported by
Filgas et al (10607) and Cucchiara (10606), the optical afterglow
light curves are well described by a simple power law decay with the
temporal index about 2.5."
GCN Circular 10632
Subject
GRB 100414A: Confirmation of the X-ray afterglow
Date
2010-04-20T10:06:01Z (16 years ago)
From
Kim Page at U.of Leicester <kpa@star.le.ac.uk>
K.L. Page (U. Leicester) and J.K. Cannizzo (NASA/UMBC) report on behalf of the
Swift-XRT team:
A second Swift-XRT observation of the Fermi-detected GRB 100414A (GCN
Circs 10594 and 10595) was performed on 2001-04-19, 5.7 days after the
trigger. The source reported by Page et al. (GCN Circs 10601, 10605) is no
longer detected, with a 3-sigma upper limit on the count rate of 4.5x10^-3
count s^-1 (corresponding to an observed flux of 2.5x10^-13 erg cm^-2
s^-1). This non-detection sets a lower limit on the decay slope of alpha >
1.5.
With this fading, we can confirm that this source is the X-ray afterglow of GRB
100414A.
This circular is an official product of the Swift-XRT team.
GCN Circular 10618
Subject
GRB100414A: SAO RAS optical observations
Date
2010-04-19T07:34:18Z (16 years ago)
From
Vladimir Sokolov at SAO RAS <sokolov@sao.ru>
A. Moskvitin, T. Fatkhullin, V. Sokolov (SAO RAS Niznijh Arkhyz, Russia),
on behalf of a larger colaboration, report:
We observed an OT (Cucchiara & Fox, GCN Circ. 10606, 10608;
Filgas, Kruehler & Greiner, GCN Circ. 10607; Landsman & Cannizzo,
GCN Circ. 10609) of GRB 100414A with the Zeiss-1000 telescope
of SAO RAS, Russia. Observations started 87.31 hours after
the Fermi LAT and GBM triggers (Takahashi et al., GCN Circ. 10594;
Foley, GCN Circ. 10595). We obtained 12 x 300 sec images both in Rc
and V bands with the airmass 1.2-1.7 under good weather conditions.
Calibration was carried out with 8 SDSS nearby stars, whose magnitudes
were transformed according to formulae from
http://www.sdss.org/dr5/algorithms/sdssUBVRITransform.html (Lupon 2005).
Rc = 21.40 +/- 0.09 (17:39:01 -- 19:05:27 UT, mean epoch = April, 17.765),
V = 21.75 +/- 0.08 (19:08:49 -- 20:31:05 UT, mean epoch = April, 17.826).
These magnitudes are not corrected for the expected Galactic extinction
reported in Landsman & Cannizzo, GCN Circ. 10609.
This message may be cited.
GCN Circular 10610
Subject
GRB 100414A: Suzaku WAM observation of the prompt emission
Date
2010-04-17T19:42:41Z (16 years ago)
From
Kazutaka Yamaoka at Aoyama Gakuin U <yamaoka@phys.aoyama.ac.jp>
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.),
K. Yamaoka (Aoyama Gakuin U.), S. Sugita (Nagoya U),
Y. Terada, M. Tashiro, S. Hong, A. Endo, K. Onda, T. Sugasahara, W. Iwakiri
(Saitama U.), M. Ohno, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, M. Suzuki, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji,
E. Sonoda, K. Kono, H. Hayashi, K. Noda, Y. Nishioka, M. Yamauchi
(Univ. of Miyazaki), N. Vasquez (Tokyo Tech.), Y. Urata, H. M. Lin, P. Tsai
(NCU), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:
The bright long, Fermi-LAT GRB 100414A (Takahashi et al., GCN 10594;
Fermi/GBM trigger #292904423 / 100414097; Foley, GCN 10595) triggered the
Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range
of 50 keV - 5 MeV at 02:20:22.879 UT (=T0).
The observed light curve shows a multi-peaked structure starting at T0-1.5 s,
ending at T0+24.5 s with a duration (T90) of about 22 seconds.
The fluence in 100 - 1000 keV was 4.88(-0.36, +0.13)x10-5 erg/cm^2.
The 1-s peak flux measured from T0+22.5 s was 6.13(-0.79, +0.40)
photons/cm^2/s in the same energy range.
Preliminary result shows that the time-averaged spectrum from
T0-1.5 s to T0+24.5 s is well fitted by a GRB Band model as follows.
the low-energy photon index alpha: -0.56(-0.29, +0.37),
the high-energy photon index beta: -3.05(-0.53, +0.30),
and the peak energy Epeak: 612(-53, +55) keV (chi^2/d.o.f = 34/23).
Due to the brightness of this burst, a 3% systematic error was
added for low energy channels. In addition, there might be
some calibration uncertainties in these spectral parameters
because GRB photons came to the WAM detector by passing through the
large Ne dewar of the X-ray micro-calorimeter (XRS).
All the errors are quoted at 90% confidence level.
The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html
GCN Circular 10609
Subject
GRB 100414A: Swift/UVOT Observations
Date
2010-04-17T15:56:44Z (16 years ago)
From
Wayne Landsman at GSFC/SSAI <wayne.b.landsman@nasa.gov>
W. Landsman (GSFC) and J. Cannizzo (GSFC) report on behalf of the
Swift/UVOT team:
The Swift/UVOT began observations of the field of GRB 100414A 40.4 hours
after the Fermi LAT and GBM-detected trigger (Takahashi et al. GCN Circ.
10594, Foley et al., GCN Circ. 10595). We detect the source reported
by Cucchiara & Fox (GCN Circ. 10606, 10608) and Filgas et al. (GCN Circ.
10607) Combining our white observations into exposures beginning at
40.4 and 53.2 hours, we find evidence for source fading.
Filter T_start (hr) Exp(s) Mag Err
White 40.38 765 20.54 +/- 0.10
White 53.20 3531 20.86 +/- 0.06
These observations are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V)=0.03 mag
in the direction of the burst (Schlegel et al. 1998). The photometry
is on the UVOT photometric system described in Poole et al.(2008, MNRAS,
383,627).
GCN Circular 10608
Subject
GRB 100414A: Gemini-N observation (correction)
Date
2010-04-17T14:40:20Z (16 years ago)
From
Antonino Cucchiara at PSU <cucchiara@astro.psu.edu>
A. Cucchiara (PSU) reports on behalf of a larger collaboration:
"We noted a typo in the coordinate reported in GCN 10606.
The correct position of the GRB 100414A optical transient
in our Gemini-N image is:
RA: 12:48:26.96
Dec: +08:41:34.91
We thank W. Landsman for pointing this out to us and we
apologize for any confusion this may have caused."
GCN Circular 10607
Subject
GRB 100414A: GROND Detection of the Optical Afterglow
Date
2010-04-17T09:53:25Z (16 years ago)
From
Thomas Kruehler at MPE/MPI <kruehler@mpe.mpg.de>
Robert Filgas, Thomas Kruehler and Jochen Greiner (all MPE Garching)
report on behalf of the GROND team:
We observed the field of GRB 100414A (Fermi GBM/LAT trigger
292904423/100414.097; Takahashi et al., GCN #10594, Foley, GCN #10595)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2 m MPI/ESO telescope at La Silla Observatory (Chile).
Observations started at 03:11 UT on April 17, 73 hours after the GRB
trigger, and were performed through thick cloud coverage.
We detect the optical afterglow reported by Cucchiara & Fox (GCN #10606)
in the optical bands. To reiterate the position, we measure
RA (J2000.0) = 12 h 48 m 26.93 s
DEC (J2000.0) = +08d 41' 34.4"
with an uncertainty of 0.5" in each coordinate against SDSS astrometry
and inside the enhanced XRT error circle reported by Page et al. (GCN
#10605).
Based on 4 min of total exposure, we estimate preliminary magnitudes
(all in AB system) of
g' = 21.3 +- 0.1 mag,
r' = 20.9 +- 0.1 mag
Given magnitudes are calibrated against SDSS field stars and are not
corrected for the expected Galactic foreground extinction corresponding
to a reddening of E_(B-V)=0.03 mag in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 10606
Subject
GRB 100414A: Gemini-N candidate and redshift
Date
2010-04-17T08:16:49Z (16 years ago)
From
Antonino Cucchiara at PSU <cucchiara@astro.psu.edu>
A. Cucchiara and D. B. Fox (PSU) report on behalf of
a larger collaboration:
"Starting on 2010 April 17.26 UT we used the GMOS spectrograph
on the Gemini North 8-m telescope to observe the field of the
Fermi-LAT GRB 100414A (Takahashi et al. GCN 10594).
In our 5 min i'-band observation we detected a bright source
inside the refined XRT error circle (Page et al., GCN 10605)
at the following coordinate:
RA: 12:48:29.96
Dec: +8:41:34.91
with 0.5" uncertainty in both directions.
Using two USNO-B1 stars we obtain i' = 20.37 +- 0.03 mag for this
object.
A sequence of 2x1200s spectra were also obtained with the same
instrument, covering a spectral range of 4000-8000A.
A series of metal absorption features were identified (FeII2374,
FeII2383,FeII2587,MnII2594, FeII2600, MgII2796,2803,MgI2853) at
the common redshift of z= 1.368.
We therefore suggest this as the redshift of GRB 100414A.
Further observations are planned.
We thank the Gemini staff for performing this observation,
in particular A. Fritz."
GCN Circular 10605
Subject
GRB 100414A: Enhanced Swift-XRT position of candidate afterglow
Date
2010-04-17T07:37:24Z (16 years ago)
From
Kim Page at U.of Leicester <kpa@star.le.ac.uk>
K.L. Page, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the
Swift-XRT team:
Using 3686 s of XRT Photon Counting mode data and 3 UVOT images, 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 =
192.11266, 8.69309 which is equivalent to:
RA (J2000): 12 48 27.04
Dec (J2000): +08 41 35.1
with an uncertainty of 2.0 arcsec (radius, 90% confidence).
This position may be improved as more data are received. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
Please note that we still cannot confirm that this source is fading.
This circular is an official product of the Swift-XRT team.
GCN Circular 10603
Subject
GRB 100414A: Palomar Transient Factory Observations
Date
2010-04-16T22:06:46Z (16 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. B. Cenko (UC Berkeley), A. Rau (MPE Garching), E. O. Ofek (Caltech),
P. E. Nugent (LBNL), J. Greiner (MPE Garching), and S. R. Kulkarni
(Caltech) report on behalf of a larger collaboration:
We have imaged the Fermi-LAT localization of GRB 100414A (Takahashi et
al., GCN 10594; Foley, GCN 10595) with the automated Palomar 48 inch
Schmidt telescope as part of the Palomar Transient Factory (PTF; Law et
al, PASP, 1395; Rau et al, PASP 121, 1334) survey. A 60 s R-band image
was obtained beginning at 7:53 UT on 15 April 2010 (~ 29.5 hours after the
burst trigger), followed approximately an hour later by another 60 s image
of the identical field.
Digital subtraction with respect to a stacked pre-explosion P48 reference
image reveals no afterglow candidate to a limiting magnitude of R > 21.0
mag within the 90% LAT localization region (Takahashi et al., GCN 10594).
We note, however, that our imaging does not cover the location of the
potential XRT afterglow candidate identified by Page et al. (GCN 10601).
GCN Circular 10601
Subject
GRB 100414A: Swift-XRT detection of a possible X-ray afterglow
Date
2010-04-16T20:02:44Z (16 years ago)
From
Kim Page at U.of Leicester <kpa@star.le.ac.uk>
K.L. Page (U. Leicester), J. L. Racusin (NASA/GSFC), J.A. Kennea (PSU) and
J.K. Cannizzo (NASA/UMBC) report on behalf of the Swift-XRT team:
Following a Target of Opportunity request, Swift started observing the
field of the Fermi GBM- and LAT-detected GRB 100414A about 48 hours after
the trigger (GCN Circs. 10594, 10595). In 1.4 ks of data there is an
uncatalogued source detected within the XRT field of view, at a position
of RA, Dec = 192.11199, 8.69172, which is equivalent to
RA (J2000): 12 48 26.88
Dec (J2000): +08 41 30.2
with an uncertainty of 3.8 arcsec (radius, 90% containment).
The source is at a count rate of 0.022 +/- 0.004 count s^-1 (0.3-10 keV),
corresponding to an observed flux of ~1.31x10^-12 erg cm^-2 s^-1; however,
with the limited data collected so far, it is not possible to determine
whether this source is fading.
GCN Circular 10599
Subject
GRB 100414A: IPN Localization
Date
2010-04-15T22:05:36Z (16 years ago)
From
Valerie Connaughton at MSFC <valerie@nasa.gov>
S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin and T. Cline on behalf of the Konus-Wind
team,
K. Yamaoka, M. Ohno, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada,
T. Murakami, K. Makishima, and Y. Hanabata on behalf of the Suzaku-WAM
team,
V. Connaughton, M.S. Briggs and C.A. Meegan on behalf of the Fermi
GBM team,
and K. Hurley
report:
The long GRB 100414A, seen by Fermi/LAT (Takahashi et al., GCN 10594)
Fermi/GBM (Foley, GCN 10595), and Konus-Wind (Golenetskii et al., GCN
10597) was also detected by Suzaku WAM so far.
Triangulation gives a Konus-WAM annulus centered at RA(2000)=223.490
(14h 53m 58s) Dec(2000)=-18.645 (-18d 38' 42"), whose
radius is 41.329 � 0.588 deg (3 sigma);
and a Konus-GBM annulus centered at RA(2000)=223.527 (14h 54m 06s)
Dec(2000)=-18.436 (-18d 26' 09"), whose radius is 41.123 � 0.262 deg
(3 sigma). These annuli are parallel and cannot be used to
define a small error box. The Konus-GBM annulus is entirely contained
within the the Konus-WAM annulus in the region around the Fermi/LAT
localization.
The center of the LAT position (RA,Dec,Err = 191.59, 8.57, 0.18 deg)
is 0.377 deg from the center line of the annulus.
A figure of the triangulated localization can be seen at:
http://gammaray.nsstc.nasa.gov/gbm/science/ipn_plots/GRB100414A_IPN.png
This localization may be refined with the arrival of data from more
distant spacecraft.
Swift is following up this localization using information from the IPN
triangulation and further processing from the Fermi LAT team.
GCN Circular 10598
Subject
Konus-Wind observation of GRB 100414A (correction to GCN 10597)
Date
2010-04-15T13:26:42Z (16 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
D. Frederiks, on behalf of Konus-Wind team, report:
The correct designation of the burst reported in the GCN 10597
is GRB 100414A (not GRB 100414B).
GCN Circular 10595
Subject
GRB 100414A: Fermi GBM detection
Date
2010-04-14T23:06:12Z (16 years ago)
From
Suzanne Foley at MPE <sfoley@mpe.mpg.de>
S. Foley (MPE) reports on behalf of the Fermi GBM Team:
"At 02:20:21.99 UT on 14 April 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 100414A (trigger 292904423 / 100414097).
The Fermi Observatory executed a maneuver following this trigger and
tracked the burst location for the next 5 hours, subject to
Earth-angle constraints.
The on-ground calculated location, using the GBM trigger
data, is RA = 184.51, DEC = 9.65 (J2000 degrees,
equivalent to 12 h 18 m, 09 d 39 '), with an uncertainty
of 1.0 degree (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 65 degrees.
The GBM light curve consists of one main pulse
with a duration (T90) of about 26.4 (+/-1.6) s (50-300 keV).
The time-averaged spectrum from T0+2.3 s to T0+28.9 s is
well fit by a power law function with an exponential
high energy cutoff. The power law index is -0.58 (+/- 0.01) and
the cutoff energy, parameterized as Epeak, is 627.6 (+12.5/-12.1)
keV (CSTAT 1075.2 for 480 d.o.f.).
The event fluence (8-1000 keV) in this time interval is
(1.29 +/- 0.02)E-4 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+22.8 s in the 8-1000 keV band
is 18.22 +/- 0.24 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 10594
Subject
GRB100414A: Fermi LAT detection
Date
2010-04-14T22:23:42Z (16 years ago)
From
Nicola Omodei at INFN(Pisa)/GLAST <nicola.omodei@pi.infn.it>
Hiromitsu Takahashi (Hiroshima Univ.), Masanori Ohno (ISAS/JAXA), Nicola Omodei (Stanford Univ.) report on behalf of the Fermi Large Area Telescope collaboration
At 02:20:21 UT on 14th April 2010, the Fermi Large Area Telescope (LAT) detected gamma rays from the long GRB 100414A, which was triggered and located by the Fermi Gamma-ray Burst Monitor (GBM) (trigger 292904423/100414.097).
At the time of the trigger the GRB was approximately at 70 degrees with respect to the LAT boresight which is close the edge of the LAT field of view.
The GBM trigger caused an Autonomous Repoint Request, and the spacecraft moved to point at the GBM location.
The data from the Fermi LAT show significantly detected emission from a transient point source as late as 300 seconds after the GBM trigger.
The best LAT on-ground localization is found to be RA,Dec= 191.59, 8.57; (12:46:21.60, 08:34:12.0, J2000) with a 90% containment radius of 0.18 deg (statistical; 68% containment radius: 0.14 deg, preliminary systematic error is less than 0.1 deg).
More than 20 photons above 100 MeV are observed within 300 seconds, and the highest energy photon coincident with the GRB position is a 4 GeV event which is observed 40 seconds after the GBM trigger.
Further analysis is ongoing.
The point of contact for this burst is Hiromitsu Takahashi
(hirotaka@hep01.hepl.hiroshima-u.ac.jp)
The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV.
It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.