GRB 100614A
GCN Circular 10967
Subject
GRB 100614A: 10.4-m GTC deep-optical limit
Date
2010-07-23T15:00:20Z (16 years ago)
From
Sergey Guziy at IAA CSIC <gss@iaa.es>
S. Guziy, M. Jel��nek, J. Gorosabel (IAA-CSIC Granada), P. Kub��nek (U.
Valencia), A. de Ugarte Postigo (INAF-OAB), D. P��rez-Ram��rez (U, Ja��n),
G. G��mez (GTC La Palma) and A. J. Castro-Tirado (IAA-CSIC), on behalf of
a larger collaboration, report:
"We observed the field of GRB 100614A (G.Stratta et al., GCN #10837)
in ugriz bands with the 10.4-m Gran Telescopio Canarias (GTC)
at the Observatorio del Roque de los Muchachos on the island of La Palma.
Observations started at 01:55 UT on 2010 June 15th, 4.3 h after the GRB
trigger. Images were obtained at an average seeing of 0."6 and an
average airmass of 1.1 with the OSIRIS instrument (Cepa et al. 2010,
HSA5,conf.) and a total integration time of 180-s for each band. We do
not detect any source within the Swift-XRT error circle reported by
Osborne et al. (GCN #10849) with the following 3-sigma limiting magnitudes
(Vega
system):
u > 25.2,
g > 27.1,
r > 26.4,
i > 25.9,
z > 24.9.
The given limits were obtained by observation of standard stars and
compared with
the SSDS catalog and are not corrected for the Galactic foreground
extinction."
This message can be quoted.
GCN Circular 10893
Subject
GRB 100614A: CrAO optical limit
Date
2010-06-26T19:55:21Z (16 years ago)
From
Vasilij Rumjantsev at CrAO <rum@crao.crimea.ua>
D. Shakhovskoy, V. Rumyantsev (CrAO), A. Pozanenko (IKI) report on behalf
of larger GRB follow-up collaboration:
We observed the field of the Swift GRB 100614A (Stratta et al. GCN 10837)
with AZT-11 telescope of CrAO between (UT) June, 15 19:18 -- 20:19.
We do not detect any source in enhanced XRT error circle (Osborne et al.,
GCN 10849).
The photometry based on USNO-B1.0 star 1392-0274963 (RA(J2000) = 17:34:02.22
Dec(J2000)= +49:14:58.3 ) assuming R=17.73 is following:
T0+ Filter, Exposure, mag. UL
(mid, d) (s)
0.9236 R 20x180 > 21.9
GCN Circular 10862
Subject
GRB 100614A: Gemini/NIRI Observations
Date
2010-06-16T17:22:59Z (16 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. B. Cenko, D. A. Perley (UC Berkeley), N. R. Tanvir (U. Leicester), A.
J. Levan (U. Warwick), J. S. Bloom, B. E. Cobb (UC Berkeley), K. Wiersema
(U. Leicester) report on behalf of a larger collaboration:
We have imaged the field of GRB100614A (Stratta et al., GCN 10837) with
the Gemini Near InfraRed Imager on the 8-m Gemini North telescope.
Observations were obtained in the Y, J, and K filters beginning at 7:05 UT
on 15 June 2010 (~ 9.5 hours after the burst).
We find no sources inside the revised XRT error circle (Osborne et al.,
GCN 10849) to limiting magnitudes of J > 22.7, K > 21.6 (Vega mags,
calibrated with respect to 2MASS). The lack of optical/NIR detections at
other facilities (Mundell and Steele, GCN 10838; Jelinek et al., GCN
10839; Levan et al., GCN 10840; Gorbovskoy et al., GCN 10853, Malesani et
al., GCN 10854, Holland and Stratta, GCN 10857), coupled with the moderate
excess column inferred from the XRT spectrum (Margutti et al., GCN 10846),
suggest a highly extinguished optical/NIR afterglow.
GCN Circular 10855
Subject
GRB 100614A: Swift/UVOT Upper Limits
Date
2010-06-15T19:20:53Z (16 years ago)
From
Stephen Holland at USRA/NASA/GSFC/SSC <Stephen.T.Holland@nasa.gov>
S. T. Holland (CRESST/GSFC/USRA) and
G. Stratta (ASDC)
report on the behalf of the Swift UVOT team:
The Swift/UVOT observed the field of GRB 100614A starting 123 s
after the BAT trigger (Stratta, et al., 2010, GCN Circ. 10837).
Settled observations started at 139 s. No white observations were
taken due to the presence of the bright A0 star HD 159607 (V = 7.4)
located 11.5 arcmin from the XRT source. We do not find any new
source, relative to the DSS, USNO-B1.0, or 2MASS at the position of
the XRT afterglow (Osborne, et al. 2010, GCN Circ. 10849).
Preliminary 3-sigma upper limits for detecting a source in the u-band
finding chart, and in the co-added images, using a 2.5 arcsecond
radius circular aperture, are
Filter T_start T_stop Exp(s) Mag
--------------------------------------------
u (fc) 139 339 246 >21.0
v 445 12,065 1218 >21.4
b 395 7165 549 >21.8
u 139 6960 897 >21.7
uvw1 494 13,145 675 >21.2
uvm2 770 12,970 1102 >21.4
uvw2 421 7365 484 >21.1
--------------------------------------------
The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight corresponding to a
reddening of E_{B-V} = 0.03 mag (Schlegel, et al., 1998, ApJS, 500,
525). All photometry is on the UVOT photometry system described in
Poole et al. (2008, MNRAS, 383, 627).
GCN Circular 10854
Subject
GRB 100614A: NOT optical upper limits
Date
2010-06-15T16:34:46Z (16 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI), D. Xu (Weizmann Inst.), T. Pursimo (NOT), P.
Jakobsson (Univ. Iceland), report on behalf of a larger collaboration:
We observed the field of GRB 100614A (Stratta et al., GCN 10837) with
the NOT equipped with ALFOSC. Observations were carried out in the R, I,
and z filters, with mean times 54, 79, and 107 minutes after the GRB
trigger, respectively.
We do not detect any source within the refined XRT error circle (Osborne
et al., GCN 10849) in any of our images. The limiting magnitudes are R >
24.0, I > 22.8 calibrated against the USNO-B1 catalog (calibration of
the z-band data is not presently feasible). Our findings are in
agreement with non-detections reported by other groups (Mundell &
Steele, GCN 10838; Jelinek et al., GCN 10839; Levan et al., GCN 10840;
Gorbovskoy et al., GCN 10853).
We acknowledge prompt reaction and careful assistence of the NOT staff.
GCN Circular 10853
Subject
GRB 100614A: MASTER-Net optical alert observations
Date
2010-06-15T14:22:59Z (16 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov, D.Zimnukhov,
M. Kornilov
Sternberg Astronomical Institute, Moscow State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk
V.Krushinski, I.Zalozhnich, T.Kopytova, A. Popov
Ural State University, Kourovka
K.Ivanov, S.Yazev, N.M.Budnev, E.Konstantinov, V.Lenok, O.Gres,
O.Chuvalaev
Irkutsk State University
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located near Kislovodsk was pointed to the GRB 100614A (Stratta et al.,
GCN 10837) 26 s after notice time and 7 min 59 s after GRB time in two
polarizations at 2010-06-14 21:46:25 UT.
We have a number images with 180-s exposition.
We haven't found optical transient within Swift-XRT error-box.
The 3-sigma unfiltred upper limit has been about 20.9 mag on 34
coadded images (21:46:25 - 22:42:05 UT).
The message may be cited.
mailto: lipunov@sai.msu.ru
GCN Circular 10852
Subject
GRB 100614A: Swift-BAT refined analysis
Date
2010-06-15T13:59:10Z (16 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), M. Stamatikos (GSFC/ORAU),
G. Stratta (ASDC), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 100614A (trigger #424716)
(Stratta, et al., GCN Circ. 10837). The BAT ground-calculated position is
RA, Dec = 263.534, 49.232 deg which is
RA(J2000) = 17h 34m 08.2s
Dec(J2000) = +49d 13' 56.4"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 56%.
The mask-weighted light curve shows a relatively smooth peak starting
at ~T-10 sec, peaking around T+50 sec, and ending at ~T+275 sec.
T90 (15-350 keV) is 225 +- 55 sec (estimated error including systematics).
The time-averaged spectrum from T-9.0 to T+282.0 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.88 +- 0.15. The fluence in the 15-150 keV band is 2.7 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+31.00 sec in the 15-150 keV band
is 0.7 +- 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/424716/BA/
GCN Circular 10849
Subject
GRB 100614A: Enhanced Swift-XRT position
Date
2010-06-15T11:50:36Z (16 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.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 3444 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 100614A, 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 = 263.49923, +49.23434 which is equivalent
to:
RA (J2000): 17h 33m 59.82s
Dec (J2000): +49d 14' 03.6"
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 10846
Subject
GRB 100614A: Swift-XRT refined analysis
Date
2010-06-15T10:01:56Z (16 years ago)
From
Raffaella Margutti at U. di Milano Bicocca <raffaella.margutti@brera.inaf.it>
R. Margutti, B. Sbarufatti (INAF-OAB) and G. Stratta (ASDC) report on
behalf of the Swift-XRT team:
We have analysed 1.4 ks of XRT data for GRB 100614A (Stratta et al. GCN
Circ. 10837), from 136 s to 1.6 ks after the BAT trigger. The data
comprise 319 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The light curve can be modelled with an initial
power-law decay with an index of alpha=1.79 (+/-0.11) followed by a break
around T+300 s to an alpha of 2.51 (+0.12, -0.10). X-ray flaring activity
is detected in the first 300 s of observation.
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.84 (+/-0.05). The best-fitting
absorption column is 1.80 (+/-0.15) x 10^21 cm^-2, in excess of the
Galactic value of 2.2 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode
spectrum has a photon index of 1.92 (+0.21, -0.20) and a best-fitting
absorption column of 1.0 (+/-0.5) x 10^21 cm^-2. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum
is 4.1 x 10^-11 (5.1 x 10^-11) erg cm^-2 count^-1.
If the light curve continues to decay with a power-law decay index of
2.51, the count rate at T+24 hours will be 1.3 x 10^-5 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.2 x 10^-16
(6.5 x 10^-16) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00424716.
This circular is an official product of the Swift-XRT team.
GCN Circular 10840
Subject
GRB 100614A: WHT I-band observations
Date
2010-06-15T01:32:15Z (16 years ago)
From
Andrew Levan at U.of Leicester <A.J.Levan@warwick.ac.uk>
A.J. Levan (U. Warwick), N.R. Tanvir (U. Leicester) and P. Groot
(Nijmegen) report for a larger collaboration:
"We obtained imaging of GRB 100614A (Stratta et al. GCN 10837) with
the 4.2m William Herschel Telescope (WHT). Observations began at
22:38 UT, approximately 1.0 hours after the burst. A total of 1200s
integration was obtained in the I-band. Within the refined XRT
position we do not locate any obvious sources to a preliminary
limiting magnitude of I>24."
GCN Circular 10839
Subject
GRB 100614A: BOOTES-2/TELMA optical observations
Date
2010-06-14T23:16:03Z (16 years ago)
From
Alberto Castro-Tirado at Inst.de Astro. de Andalucia <ajct@iaa.es>
M. Jelinek, A. J. Castro-Tirado (IAA-CSIC Granada), P. Kubanek (IAA-CSIC
and IPL-UV) and A. de Ugarte Postigo (OAB), on behalf of a larger
collaboration, report:
"The TELMA 0.6m robotic telescope at the BOOTES-2 astronomical station
in South Spain has responded to GRB 100614A 18s after the GCN notice
(and about 6.9 min after the onset of the GRB). The co-add of 36 images
(3-s each, unfiltered) obtained through cirrusses provides a R = 18
limiting magnitude at the position of the X-ray atterglow (Stratta et
al. GCNC 10837)."
This message can be quoted.
GCN Circular 10838
Subject
GRB 100614A: Liverpool Telescope Observations
Date
2010-06-14T23:07:02Z (16 years ago)
From
Carole Mundell at ARI, JMU,Liverpool <cgm@astro.livjm.ac.uk>
C.G. Mundell and I.A. Steele (Liverpool JMU) report on behalf of a larger
collaboration:
"The 2-m Liverpool Telescope robotically followed up GRB100614A
(SWIFT trigger 424716; Stratta et al. GCN10837) 17.07 min after the GRB
trigger time. Initial analysis shows no optical counterpart is detected in
the XRT error circle to the following limiting magnitudes (wrt USNOB1):
Time from trigger Filter Limiting Mag
----------------- ------- ------------
29 mins R > 21 mag
31 mins i' > 21 mag
We note also that no counterpart is detected in z'-band images.
Observations and analysis are ongoing.
This message may be cited"
GCN Circular 10837
Subject
GRB 100614A: Swift detection of a burst
Date
2010-06-14T22:09:01Z (16 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
G. Stratta (ASDC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU), V. D'Elia (ASDC),
J. M. Gelbord (PSU), C. Gronwall (PSU),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
W.B Landsman (GSFC), J. Mao (INAF-OAB), F. E. Marshall (NASA/GSFC),
J. P. Osborne (U Leicester), T. Sakamoto (NASA/UMBC),
C. J. Saxton (UCL-MSSL), B. Sbarufatti (INAF-OAB/IASFPA),
M. Stamatikos (OSU/NASA/GSFC), T. N. Ukwatta (GSFC/GWU) and
L. Vetere (PSU) report on behalf of the Swift Team:
At 21:38:26 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100614A (trigger=424716). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 263.519, +49.227, which is
RA(J2000) = 17h 34m 05s
Dec(J2000) = +49d 13' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). As is typical for image triggers, the TDRSS
lightcurve does not show anything significant.
The XRT began observing the field at 21:40:39.1 UT, 133.0 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
263.4992, 49.2347 which is equivalent to:
RA(J2000) = 17h 33m 59.81s
Dec(J2000) = +49d 14' 05.1"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). 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 in excess of the Galactic value (2.2e+20
cm^-2, Kalberla et al. 2005), with an excess column of 1.3
(+1.11/-1.03) x 10^21 cm^-2 (90% confidence).
The initial flux in the 0.1 s image was 4.41e-08 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of nominal 250 seconds with the U filter
starting 873 seconds after the BAT trigger. No white observations were taken
because there is a V = 7.4 star in the UVOT field of view. The UVOT image covers
100% of the XRT error circle. No credible afterglow candidate has been found in
the initial data products to an estimated magnitude limit of u > 19.2. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.03 mag.
Burst Advocate for this burst is G. Stratta (giulia.stratta AT asdc.asi.it).
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.)