- GCN Circular #15864
K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,
I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,
S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks, D. Svinkin, and
T. Cline on behalf of the Konus-Wind team,
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro,
Y. Terada, T. Murakami, and K. Makishima, on behalf of the Suzaku WAM
team, and
V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein,
on behalf of the Fermi GBM team, report:
The extremely bright long 140219A has been observed by Fermi/GBM
(trigger 414531995), INTEGRAL (SPI-ACS), Suzaku (WAM), Mars Odyssey
(HEND) and MESSENGER (GRNS), so far, at about 71192 s UT (19:46:32).
We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
---------------------------------------------
idx RA(2000),deg Dec(2000),deg
---------------------------------------------
Center:
156.44 7.46
Corners:
1 157.06 10.06
2 156.56 7.30
3 155.51 4.70
4 156.31 7.66
---------------------------------------------
The error box area is 0.644 sq. deg, and its maximum dimension is 5.57
deg (the minimum one is 0.36 deg).
This box can be improved.
A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140219_T71192/IPN/
- GCN Circular #15865
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a series of observations, tiled on the sky, of the
IPN GRB 140219A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00024
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the IPN event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.
Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; and 2009, MNRAS, 397, 1177).
This circular is an official product of the Swift-XRT team.
- GCN Circular #15866
Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:
=93At 19:46:32.24 UT on February 19 2014, the Fermi Gamma-Ray Burst Monit=
or
triggered and located an extremely bright long GRB 140219A (trigger 41453=
1995/140219824),
which was also detected by INTEGRAL (SPI-ACS), Suzaku (WAM), Mars Odyssey=
(HEND) and
MESSENGER (GRNS) (Holland et al., GCN 15825). The GBM on-ground location =
is consistent=20
with IPN error box.
The GRB position was occulted by the Earth during the brightest period of=
emission and=20
only the weaker tail emission was observed by GBM. Using the available da=
ta we find that=20
the GBM light curve consists of a multiple-peak structure with a duration=
of about 80 s
(50-300 keV). The time-averaged spectrum from T0-2 s to T0+78 s is well f=
it with
a power law function with an exponential high energy cutoff, which is pa=
rameterized
as Epeak =3D 194 +/- 61 keV, alpha =3D -1.3 +/- 0.1. The event fluence (=
10-1000 keV)
in this time interval is (4.9 +/- 0.6)E-06 erg/cm^2. The 1.0-sec peak pho=
ton flux
measured starting from T0-0.9 s in the 10-1000 keV band is 3.2 +/- 0.2 ph=
/s/cm^2.
The spectral analysis results presented above are preliminary; final resu=
lts will
be published in the GBM GRB Catalog."
- GCN Circular #15867
S. Guiriec (GSFC/CRESST/UMD), J. Racusin (GSFC), G. Vianello (Stanford)
and E. Bissaldi (University & INFN Trieste),
report on behalf of the Fermi-LAT team:
At 19:46:32.2 on February 19, 2014, Fermi LAT detected high-energy emission
from GRB 140219A, which was also detected by Fermi-GBM (trigger 414531995
- Zhang et al., GCN 15866) and located by IPN (Hurley et al., GCN 15864).
GRB 140219A was not observable by LAT until ~T0+500 s due to
Earth occultation and it remained in the LAT field of view from ~T0+500 s
until T0+2300 s.
An analysis of the LAT data over a period covering ~T0+500 s to ~T0+2300 s
reveals a marginal detection with a TS of about 25 using the center of
the IPN error box.
The best LAT on-ground location is RA, Dec 158.2, 7.2 (J2000). The 90%
containment region (statistical error only) is asymmetrical with a width of
2.75 deg
and a height of 1.65 deg compatible with the IPN contour
(see http://fermigrb.stanford.edu/GRB140219A_tsmap.jpg).
The highest energy photon with a probability of being associated with
the GRB > 90% is a 1.6 GeV photon at T0+1350 s.
The Fermi LAT point of contact for this burst is Sylvain Guiriec
(sylvain.guiriec@nasa.gov).
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.
- GCN Circular #15870
S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:
The long-duration, exceptionally bright and hard GRB 140219A (localized=20
by IPN: Hurley et al., GCN 15864; GBM detection: Zhang, GCN 15866; LAT=20
detection: Guiriec et al., GCN 15867) triggered Konus-Wind at=20
T0=3D71162.611 s UT (19:46:02.611).
The burst light curve shows an extremely bright multi-peaked pulse with=20
a duration of ~2.5 s followed by a less intense multi-peaked emission=20
episodes until ~T0+26 s and a very weak tail until ~T0+35 s.
The emission is seen up to ~18 MeV.
As observed by Konus-Wind, the burst had a fluence of (1.14 =B1=20
0.02)x10^-3 erg/cm2, and a 16-ms peak flux, measured from T0+0.240 s,
of (1.44 =B1 0.12)x10^-3 erg/cm2/s (both in the 20 keV - 10 MeV energy ra=
nge).
The time-integrated spectrum (measured from T0 to T0+38.912 s)
is best fit (in the 26 keV - 18 MeV range)
by a GRB (Band) model with the following model parameters:
the low-energy photon index alpha =3D -1.07 =B1 0.01,
the high energy photon index beta =3D -3.26(-0.88,+0.38),
the peak energy Ep =3D 2777 =B1 70 keV,
chi2 =3D 112.7/96 dof.
The spectrum of the main pulse (measured from T0 to T0+2.304 s)
is best fit (in the 26 keV - 18 MeV range)
by a GRB (Band) model with the following model parameters:
the low-energy photon index alpha =3D -0.65 =B1 0.04,
the high energy photon index beta =3D -3.28(-0.89,+0.39),
the peak energy Ep =3D 3363 =B1 141 keV,
chi2 =3D 47.9/77 dof.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140219_T71162/
All the quoted errors are at the 90% confidence level.
All the quoted results are preliminary.
The derived peak flux and Epeak are the highest ever measured for GRBs=20
with Konus-Wind during almost 20 years of its continuous observations:
the peak flux is ~50% higher than the previous record holder, GRB=20
110918A, with the measured peak flux of ~0.9x10^-3 erg/cm2/s (Frederiks=20
et al. ApJ, 779, 151 (2013)).
Follow-up observations are strongly encouraged.
- GCN Circular #15871
E. Gorbovskoy, V. Lipunov, 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 VWF robotic very wide field cameras (FOV=2x384 square degrees,
D=72mm, f/1.2, 1 pix = 22 arcsec) installed on MASTER-II robotic
telescope in Tunka covered full IPN error box (Hurley et. al. GCN15864)
for very short time before and after the trigger.
Fortunatelly we have set of 26 continous 5 seconds exposure images since
19:43:16 to 19:45:21 UT i.e. since 196 s to 71 s before the trigger and
set of continous 5 seconds exposure images since 19:47:01 to 19:58:31 UT
i.e. 3 sec after Notice Time and 29 s after the trigger.
We haven`t found credible optical transient with 3-sigma upper limit
10.5m on single and about 12.0 m on coadd (20 x 5 sec = 100 sec) images.
The Very Wide Field Cameras observation schedule with respect to GRB light
curve (S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin et al., GCN
15870) is available at
http://master.sai.msu.ru/static/GRB/GRB140219A_schedule.png
The first images movie available here
http://master.sai.msu.ru/static/GRB/GRB140219A_IPN_single.gif
The coadd images move available here
http://master.sai.msu.ru/static/GRB/GRB140219A_IPN_coadd1.gif
http://master.sai.msu.ru/static/GRB/GRB140219A_IPN_coadd2.gif
The same MASTER VWF robotic very wide field cameras installed on
MASTER-II robotic telescope in Blagoveschensk also made the observations
of IPN error box after the trigger. However the upper limit on them on
1.5m worse than in Tunka due to adverse weather conditions.
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to the GRB140219A 78 sec after trigger
time at 2014-02-19 19:47:50.943 UT by FERMI GBM trigger N414531995 in two
polarizations. On our first (10s exposure) set we haven`t found optical
transient within 4 sq. degree center part of FERMI-GBM first error-box
(ra=10 11 55 dec=+12 14 00 radius = 32, Zhang et. al. GCN 15866) .
The 5-sigma upper limit has been about 15.1 mag.
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Blagoveschensk was pointed to the GRB140219A 30 sec after
notice time and 57 sec after trigger time at 2014-02-19 19:47:29.9 UT by
FERMI GBM trigger .414531995 in two polarizations. On our first (10s
exposure) set we haven`t found optical transient within 4 sq. degree
center part of FERMI-GBM first error-box (ra=10 11 55 dec=+12 14 00
radius = 32 ).
The 5-sigma upper limit has been about 14.9 mag.
After IPN notice (Hurley et. al. GCN15864) we cover full IPN and LAT
(Guiriec et. al GCN 15867) error boxes in survey mode using 3 fields on
two MASTER II telescope in Tunka and Blagoveschensk. The first images was
obtained 18h 22m after trigger time at 2014-02-20 14:08:49 with upper
limit 19.5 m in Tunka and 18.0 m in Blagoveschensk. We also haven`t found
credible optical transient up to 20.5 m here.
The obseravtions argue that GRB 140219A is extremely dark GRB with low
Optical to Gamma Emission Ratio:
F_opt/F_gamma <~ 1 : 130 000
On the figure
( http://master.sai.msu.ru/static/GRB/GRB140219A_schedule.png )
you can find the Gamma-Optic diagramm for the prompt
fluence of GRBs observed by MASTER (Gorbovskoy et. al Astronomy Reports,
Volume 57, Issue 4, pp.233-286).
The message may be cited.
- GCN Circular #15872
V. Mangano (PSU), P. A. Evans (U. Leicester), F. E. Marshall (NASA/GSFC)
report on behalf of the Swift Team:
Swift-XRT has observed the central part of the error region of the
IPN GRB 140219A in a series of observations tiled on the sky.
The total exposure time is 5.9 ks spread over 3 fields;
the maximum exposure within the sky observed was 3.9 ks.
The observations started 70.3 ks after the IPN trigger.
Within these data there are 2 objects which are not catalogued in
X-rays. At the present time we cannot be sure which, if either,
of these is the afterglow.
Source details:
Source 1
RA: 156.49768 = 10h 25m 59.44s (J2000)
Dec: 7.52128 = +07d 31' 16.6" (J2000)
Err: 10.0 (radius, 90% confidence)
Exposure time: 2.2 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_1.php
Source 2
RA: 156.44031 = 10h 25m 45.67s (J2000)
Dec: 7.96378 = +07d 57' 49.6" (J2000)
Err: 10.0 (radius, 90% confidence)
Exposure time: 1.5 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_2.php
UVOT observed both of the XRT source regions.
In the region for XRT Source 1, UVOT finds a bright
optical source that we identify with the star
SDSS J102559.46+073114.1.
UVOT finds no optical counterpart to XRT Source 2
in a 803-second exposure with the white filter
starting 82.3 ks after the trigger.
The preliminary 3-sigma upper limit
using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)
is 21.7 mag. No correction has been made
for Galactic extinction due to the reddening of
E(B-V) of 0.03 in the direction of the source
(Schlegel et al. 1998).
This circular is an official product of the Swift team.
- GCN Circular #15873
D. Xu (DARK/NBI), D.-M. Wei, H.-B. Zhao, Y. Xia (PMO), C.-H. Bai, X.
Zhang, H.-B. Niu, A. Esamdin, L. Ma (XAO), Y. Osorio (NOT) report on
behalf of a large collaboration:
We observed the whole IPN field and its surrounding region of GRB
140219A (Hurley et al., GCN 15864). The first epoch was done at ~15:40
UT on 2014-02-20 using the 1m telescope located at Xuyi, Jiangsu,
China, equipped with a 3x3 deg^2 CCD camera. The second epoch was done
at ~17:50 UT on 2014-02-20 using the 1m telescope located at Nanshan,
Xinjiang, China, equipped with a 1.2x1.2 deg^2 CCD camera. For both
epochs, a series of R-band 120s exposures were obtained.
The depths of the images of the two epochs are largely comparable and
it has R~19 mag. Within the IPN field, we found two relatively bright
sources, but they can be ruled out to be an afterglow by cross
checking the Xuyi, Nanshan, and DSS images. A third epoch was done at
the 2.5m Nordic Optical Telescope (NOT) and the NOT images confirm the
above ruling-out. Therefore, assuming GRB 140219A is a conventional
cosmological burst happening within the IPN field, its afterglow would
be fainter than R~19 mag at T~20 hrs post-burst, which is a possible
case according to previous GRB follow-ups. Inspection of some
surrounding region of the IPN field also leads to no credible
afterglow candidate detection.
For the reported two Swift/XRT sources in the central part of the IPN
field (Mangano et al., GCN 15872), S2 is not present in the Xuyi and
Nanshan images as well, while S1 is a known source.
- GCN Circular #15875
V. Mangano (PSU) and P. A. Evans (U. Leicester)
report on behalf of the Switf-XRT team
Swift-XRT has observed the error circle of the IPN GRB 140219A in a
series of observations tiled on the sky. The total exposure time is 9.9
ks spread over 5 fields; the maximum exposure within the sky observed
was 3.9 ks. The observations started 70.3 ks after the IPN trigger.
Within these data we detect a fading, uncatalogued X-ray source at RA,
Dec= 156.02772, 6.49399 which is equivalent to:
RA (J2000.0) = 10h 24m 6.65s
Dec (J2000.0) = +06d 29' 38.4"
with an uncertainty of 7.9 arcsec (radius, 90% confidence). The
exposure at this location was 3.0 ks.
This previously uncatalogued source is fading, and we thus consider it
the likely GRB afterglow.
The results of the automatic processing for this source are available
athttp://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_5.php
This circular is an official product of the Swift-XRT team.
- GCN Circular #15876
A. Pozanenko (IKI), E. Klunko (ISTP), A.Volnova (IKI), M. Eselevich
(ISTP), report on behalf of larger GRB follow-up collaboration:
We observed the field of XRT afterglow candidate (Mangano et al., GCN
15875) of the GRB 140219A (Hurley et al., GCN 15864, Zhang GCN 15866,
Guiriec et al.,GCN 15867, Golenetskii et al. GCN 15870) with AZT-33IK
telescope of Mondy observatory starting on Feb. 22 (UT) 14:45. We
obtained 60 images in R-filter. In the initial images within XRT error
circle (Mangano et al., GCN 15875) we detected two objects which are
present in SDSS DR9. One of them is a galaxy (SDSS 3015-301-3-0280-0458)
and other one is a star (SDSS 3015-301-3-0280-0457). No new objects were
detected. Upper limit of the initial image of 60-s exposure is R=20.8.
A finding chart can be found in
http://grb.rssi.ru/GRB140219A/GRB140219A_XRT_5_fc.png
- GCN Circular #15878
L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories/Princeton),
and S. B. Cenko (NASA/GSFC) report on behalf of the intermediate Palomar
Transient Factory (iPTF) collaboration:
We have searched for optical counterparts of GRB 140219A using the Palomar
48-inch Oschin telescope (P48). We observed 9 fields covering an area of
67.8 deg2 intersecting the Fermi GBM 1-sigma contour (Fermi trigger
414531995, Zhang et al., GCN 15866) and a preliminary MESSENGER-Suzaku IPN
annulus (K. Hurley, personal communication) that was available when the
GBM localization was first observable from Palomar. We observed all 9
fields for several epochs, with the first epoch extending from 7.0 to 8.1
hours after the burst. Sifting through candidate variable sources using
image subtraction and standard iPTF vetting procedures, we found no
compelling optical afterglow candidates to an average limiting magnitude
of r=21.1 mag.
About 80% of the published IPN error box (Hurley et al., GCN 15864) was
contained in these 9 fields, with most of the remaining 20% falling on a
disabled CCD on the P48. To fill the gap in the IPN error box, we observed
two additional fields starting 33.7 hours after the burst. The deepest
epoch of observations of these two fields had a limiting magnitude of
r=20.7 mag. Since we lacked reference images for these two offset fields,
we performed a catalog comparison search, examining any source that was
detected in our two deepest epochs but was not coincident with a stellar
object in SDSS. Of 342 sources meeting this criterion, all were known
galaxies and none were compelling optical afterglow candidates.
XRT source 1
(http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_1.php, Mangano
et al., GCN 15872) is contained in our nine early fields, and we associate
a coincident optical detection with the star SDSS J102559.46+073114.1.
XRT source 2
(http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_2.php, Mangano
et al., GCN 15872) is contained in our two late fields, and we detect no
coincident optical source to a limiting magnitude of r=20.5 mag at 35.7
hours after the burst.
XRT source 4
(http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_4.php) is
contained in our nine early fields, and we find no coincident optical
source to a limiting magnitude of r=20.2 mag at 8.1 hours after the burst.
XRT source 5
(http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_5.php, Mangano
et al., GCN 15875), the most plausible afterglow candidate due to its
observed fading, is also contained in our two late fields. We detect two
optical sources within the XRT error circle: the star SDSS
J102406.41+062937.6, and the galaxy SDSS J102406.58+062945.7. These were
also the sources detected by Pozanenko et al. (GCN 15876). For the star,
we report r=20.0+/-0.1, which is about 0.5 mag brighter than the value
given by SDSS DR10. We find no additional sources inside the XRT error
circle to a limiting magnitude of r=21.0.
The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi414531995.pdf
shows the footprints of the nine early P48 fields in relation to the Fermi
GBM 1-, 2-, and 3-sigma statistical+systematic contours (black) and the
IPN INTEGRAL-MESSENGER and WAM-HEND annuli (blue). The INTEGRAL-MESSENGER
annulus is comparable to the initial MESSENGER-Suzaku localization on
which we based these observations.
The diagram
http://www.its.caltech.edu/~lsinger/iptf/Fermi414531995_inset_1.pdf shows
the early P48 fields in relation to a six-sided IPN polygon and the XRT
candidates.
The diagram
http://www.its.caltech.edu/~lsinger/iptf/Fermi414531995_inset_2.pdf shows
the late P48 fields.
- GCN Circular #15879
V. Lipunov, M. Pruzhinskaya, E. Gorbovskoy, 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)
We refined our reduction of images started 18h 22m after trigger time
(Gorbovskoy et al., GCN 15871). We found the 3-sigma OT on several (at
least 4) best unfiltered images with limit ~ 20 mag inside XRT error box
(Mangano and Evans, GCN 15875) at automatic position:
2014-02-20 14:08:50.873 10h 24m 06.46s , +06d 29m 40s.8
with 2 arcsec error (2 arcsec = 1 pix).
The unfiltered magnitude is about 19.
Fortunately we have archive images of this area at the same telescope
with slightly better limit(MASTER II, Tunka,2011-02-06 16:34:55
180) without any optical source. The OT is brighter at least 1 magnitude
at 18.5 hours after trigger.
The OT position does not coincide with SDSS J102406.58+062945.7 galaxy
(Singer, iPTF GCN 15878, source XRT 5), closer to SDSS star
J102406.41+062937.6 .
The detection and reference images are available at
http://master.sai.msu.ru/static/GRB/GRB140219A_OT.png
We do not see any OT at alert Very Wide Field images at this place
(Gorbovskoy et al., GCN 15871).
The message may be cited.
- GCN Circular #15880
P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:
Further analysis of the XRT afterglow candidate of GRB 140219A (GCN
Circ. 15875) reveals that the light curve of this object had been
contaminated by the presence of a nearby, bright, catalogued X-ray
source. Refined analysis of the previously-announced afterglow candidate
reveals it to be approximately constant, with a count rate of ~5e-3
ct/sec, thus it is probably not the afterglow.
This circular is an official product of the Swift-XRT team.
- GCN Circular #15881
V. Lipunov, M. Pruzhinskaya, E. Gorbovskoy, 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)
We present the reduction of the best coadded image started 2014-02-20
14:42:07, i.e. 18.92 hour after trigger time with total
exposition 3960 s (Gorbovskoy et al., GCN 15871) with unfiltered 21.0 mag
limit.
We found the optical source inside XRT-5 error box (Mangano
and Evans, GCN 15875) at automatic position:
T_start = 2014-02-20 14:42:07.5 (T_start-T_trig = 18.92 h)
T_mid = 2014-02-20 16:14:23.7 (T_start-T_mid = 20.45 h)
T_fin = 2014-02-20 17:46:40.0 (T_start-T_fin = 22.01 h)
RA 10h 24m 06.45s
Dec +6d 29m 37.86s
(156.021889 6.420445)
with 0.7 arcsec error.
Unfiltered magnitude:
Mag = 19.7+/-0.3
This source coincides with SDSS J102406.41+062937.6 star.
This star must be visible at archive image of this area at the same
telescope (MASTER II, Tunka,2011-02-06 16:34:55 180, Lipunov et all., GCN
15879) on 4 sigma level. The absence of the SDSS J102406.41+062937.6 star
confirms its brightening ~0.7 mag.
But the absence of the X-ray variation of XRT-5 source (P.F. Evans,
GCN15880) argues that brightening may be usual variable star and does not
connect with GRB 140219A.
All our limits published earlier are still valid (GCN 15871, GCN 15879 )
The coadded image is available at
http://observ.pereplet.ru/images/10240645+062937.jpg
The message may be cited.
- GCN Circular #15882
M. Serino (RIKEN), S. Ueno, H. Tomida, S. Nakahira, M. Kimura,
M. Ishikawa, Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki,
M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN),
N. Kawai, R. Usui, T. Yoshii, Y. Tachibana (Tokyo Tech),
A. Yoshida, T. Sakamoto, Y. Nakano, Y. Kawakubo, H. Ohtsuki (AGU),
H. Tsunemi, M. Sasaki (Osaka U.), H. Negoro, M. Nakajima,
K. Fukushima, T. Onodera, K. Suzuki (Nihon U.),
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.),
Y. Tsuboi, M. Higa (Chuo U.), M. Yamauchi, K. Yoshidome,
Y. Ogawa, H. Yamada (Miyazaki U.), K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:
The MAXI/GSC detected a rapid increase of the count rate in
all six working counters at 2014-02-19T19:45:58.15 UT.
The time is consistent with GRB 140219A
(Hurley et al., GCN 15864; Zhang, GCN 15866; Guiriec et al., GCN 15867;
Golenetskii et al., GCN 15870).
The IPN postion of GRB 140219A was not in the field of view of any of the
MAXI Gas Slit Cameras, implying that the detected counts are produced by the
hard X-rays that penetrated the Ti counter walls with Pb shiled, or the phosphor
bronze collimator with Al housing of GSC, or by the Compton-scattered electrons
induced by the gamma-rays. It suggests that this GRB was exceptionally bright
and hard.
The light curve shows an intense spike with a duration of ~0.2 s followed by
a bright emission until T0+~2.5 s. A weak emission lasts until T0+~20 s.
The peak count rate is ~2000 c/s per counter (GSC_3).
The MAXI/GSC light curve of this GRB is available at
http://maxi.riken.jp/news/en/?p=1101 .
There was no significant excess flux in the transits before and after the
GRB at UT 19:40 and 21:13 with an upper limit of 20 mCrab (4-10 keV, 1 sigma)
for each.
- GCN Circular #15885
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 extremely bright and long-duration GRB 140219A
(localized by IPN: Hurley et al., GCN 15864;
Fermi-GBM detection: Zhang, GCN 15866; Fermi-LAT detection: Guiriec et
al., GCN 15867; Konus-Wind detection: Golenetskii et al., GCN15870;
MAXI/GSC detection: Serino et al., GCN15882) triggered the Suzaku
Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 19:45:57.754 UT (=3DT0).
The observed light curve shows a strong multi-peaked structure lasting from
T0 s to T0+3 s, followed by a weaker multi-peaked emissions
seen up to T0+27 s with a total duration (T90) of about 17 seconds.=E3=80
=80
The fluence in 100 - 1000 keV was 1.73 (+0.06,-0.08)x10^-5 erg/cm^2. The
1-s
peak flux measured from T0+1.5 s was 83.6 (+6.5,-6.4) photons/cm^2/s in
the same energy range.
Preliminary result shows that the time-averaged spectrum from
T0 s to T0+27 s is fitted by a GRB Band model as follows.
the low-energy photon index alpha: -1.00 (+0.06,-0.11),
the high-energy photon index beta: -2.68 (+0.08,-0.11),
and the peak energy Epeak: 1930(+176,-79) keV (chi^2/d.o.f =3D 71.9/47).
There might be some calibration uncertainties in spectral parameters
since the GRB photons came through the X-ray micro-calorimeter (XRS) dewar.
All the quoted errors are 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 #15890
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 possible XRT afterglow candidate (Mangano et
al., GCN 15875) of the GRB 140219A (Hurley et al., GCN 15864, Zhang GCN
15866, Guiriec et al.,GCN 15867, Golenetskii et al. GCN 15870, Serino et
al. GCN 15882) with AZT-33IK telescope of Mondy observatory on Feb. 22
(UT) 14:45-15:45 (Pozanenko et al., GCN 15876) and Feb. 27 (UT)
15:18-16:18. We obtained several images with exposure of 60 seconds in
R-filter during each observational set. In the stacked images within XRT
error circle (Mangano et al., GCN 15875) we clearly detect two objects
which are present in SDSS plates and SDSS DR9. One of them is a galaxy
(refereed below as G5), SDSS J102406.58+062945.8, and other one is a
star (X5), SDSS J102406.41+062937.6, both objects mentioned earlier
(Pozanenko et al., GCN 15876, Singer et al., GCN 15878).
No new objects were detected.
The photometry of the two sources is following:
date UT start t-T0 Exp. Filter G5 X5
(mid, days) (s)
2014-02-22 14:45:44 2.81197 51*60 R 20.77+/-0.12 19.74+/-0.05
2014-02-27 15:18:29 7.81388 60*60 R 20.51+/-0.09 19.59+/-0.06
The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005):
N SDSS_id R(Lupton) err
1 J102410.32+062923.9 17.391 0.017
2 J102410.04+062943.6 18.163 0.023
3 J102404.63+062938.7 18.962 0.025
The known star X5 is ~0.5m brighter than assumed R mag from SDSS DR9,
i.e. R = 20.24 +/- 0.06, in accordance with Singer et al. (GCN 15878).
We also may suspect, that known galaxy G5 might be brighter in our
second epoch (Feb. 27) than on first epoch (Feb. 22). We encourage
further observation of the galaxy G5 to confirm re-brightening, and if
so the galaxy might be a host of GRB 140219A.
Also we report a redshift of G5 galaxy z= 0.12 +/- 0.12 obtained
photometrically using SDSS DR9 catalog.
- GCN Circular #16067
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. Hanabata (ICRR), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:
The quoted fluence in GCN 15885 was incorrect.
The correct value is 1.73 (+0.06,-0.08)x10^-4 erg/cm^2
in the 100-1000 keV range.
We apologize for any inconvenience.
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