- GCN/BACODINE POSITION NOTICE
TITLE: GCN/INTEGRAL NOTICE
NOTICE_DATE: Thu 02 Jul 09 10:41:05 UT
NOTICE_TYPE: INTEGRAL Wakeup
TRIGGER_NUM: 5896, Sub_Num: 0
GRB_RA: 175.8866d {+11h 43m 33s} (J2000),
176.0091d {+11h 44m 02s} (current),
175.2417d {+11h 40m 58s} (1950)
GRB_DEC: +11.4937d {+11d 29' 37"} (J2000),
+11.4409d {+11d 26' 27"} (current),
+11.7712d {+11d 46' 16"} (1950)
GRB_ERROR: 3.23 [arcmin, radius, statistical only]
GRB_INTEN: 8.39 [sigma]
GRB_TIME: 38449.57 SOD {10:40:49.57} UT
GRB_DATE: 15014 TJD; 183 DOY; 09/07/02
SC_RA: 182.51 [deg] (J2000)
SC_DEC: 9.22 [deg] (J2000)
SUN_POSTN: 101.62d {+06h 46m 28s} +23.01d {+23d 00' 28"}
SUN_DIST: 71.32 [deg] Sun_angle= -5.0 [hr] (East of Sun)
MOON_POSTN: 221.89d {+14h 47m 34s} -21.49d {-21d 29' 39"}
MOON_DIST: 55.79 [deg]
GAL_COORDS: 254.09, 67.67 [deg] galactic lon,lat of the burst
ECL_COORDS: 171.63, 8.91 [deg] ecliptic lon,lat of the burst
COMMENTS: INTEGRAL GRB Coordinates.
COMMENTS: Possibly real GRB event
- red DSS finding chart
ps-file
- GCN NOTICE
TITLE: GCN/INTEGRAL NOTICE
NOTICE_DATE: Thu 02 Jul 09 12:25:09 UT
NOTICE_TYPE: INTEGRAL Offline
TRIGGER_NUM: 5896, Sub_Num: 1
GRB_RA: 175.8882d {+11h 43m 33s} (J2000),
176.0107d {+11h 44m 03s} (current),
175.2433d {+11h 40m 58s} (1950)
GRB_DEC: +11.5006d {+11d 30' 02"} (J2000),
+11.4478d {+11d 26' 52"} (current),
+11.7781d {+11d 46' 41"} (1950)
GRB_ERROR: 2.50 [arcmin, radius, statistical only]
GRB_INTEN: 8.39 [sigma]
GRB_TIME: 38449.57 SOD {10:40:49.57} UT
GRB_DATE: 15014 TJD; 183 DOY; 09/07/02
SC_RA: 182.51 [deg] (J2000)
SC_DEC: 9.22 [deg] (J2000)
SUN_POSTN: 101.69d {+06h 46m 46s} +23.00d {+23d 00' 08"}
SUN_DIST: 71.25 [deg] Sun_angle= -5.0 [hr] (East of Sun)
MOON_POSTN: 222.81d {+14h 51m 15s} -21.73d {-21d 44' 04"}
MOON_DIST: 56.65 [deg]
GAL_COORDS: 254.08, 67.68 [deg] galactic lon,lat of the burst
ECL_COORDS: 171.63, 8.92 [deg] ecliptic lon,lat of the burst
COMMENTS: INTEGRAL GRB Coordinates.
COMMENTS: refined_coordinates_after_offline_analysis
- GCN Circular #9603
A. Paizis (IASF-Milano), D.Gotz (CEA-Saclay), S.Mereghetti, (IASF-
Milano), Wakiko Ishibashi, C. Ferrigno, M. Beck (ISDC, Versoix), and
J. Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team
report:
A long gamma ray burst with a soft spectrum, and without any
detectable signal above 40 keV has been detected by IBAS in the IBIS/
ISGRI data at 10:40:37 U.T. on July 2nd. Its duration is about 10 s
and its refined coordinates (J2000) are:
R.A.: 175.888 [degrees]
DEC.: +11.501 [degrees]
with an uncertainty of 2.5 arcmin (90% c.l.).
A preliminary analysis gives a peak flux in the 20-200 keV range of
about 0.15 ph/cmsq/s (1 s integration time) and a fluence over the same
energy range of about 1.5e-7 erg/cmsq.
A plot of the light curve will be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html
This message can be cited.
- GCN Circular #9604
B. Sbarufatti, V. Mangano (INAF-IASFPA), report on behalf of the Swift-
XRT team:
Swift began observation of the XRF detected by INTEGRAL (Paizis, et
al., GCN Circ. 9603) on 2009 July 2 at 14:15 UT, 3.5 hours after the
trigger. In the XRT field of view we detect a single faint,
uncatalogued source inside the IBIS/ISGRI error circle with a 5.5
sigma significance. The XRT position obtained using a 6ks Photon
Counting mode exposure is RA, Dec =
175.89800, 11.50219 which is equivalent to:
RA (J2000): 11 43 35.5
Dec (J2000): +11 30 07.9
with an uncertainty of 4.9 arcsec (radius, 90% confidence). This is
0.6 arcmin away from the INTEGRAL IBIS/ISGRI position. The count-rate
is (6.8+/-1.2)E-3 counts/s, for a total of 40 observed photons from
the source. With the current amount of data we are unable to see if
the source is fading.
This is an official product of the Swift XRT team.
- GCN Circular #9605
P. D'Avanzo (Univ. Bicocca/INAF-OAB), S. Campana, S. Covino (INAF-OAB),
E. Bozzo (ISDC) and L. Stella (INAF-OAR) report, on behalf of a larger
collaboration:
We observed the field of XRF 090702 (Paizis et al., GCN 9603) with the
ESO-VLT equipped with the FORS2 camera in imaging mode. In a first
series of R-band images (6 minutes of total exposure time) carried out
on Jul 2.9965, we do not see any optical counterpart inside the XRT
error circle (Sbarufatti & Mangano, GCN 9604) down to a limiting
magnitude of R > 24.2 (3sigma limit, calibrated against USNOB1 catalogue).
We note that the GRB position is about 10 deg from the Virgo Cluster.
We aknowledge the Paranal staff for their support, in particular C.
Ledoux and K. O'Brien.
- GCN Circular #9607
S. R. Oates (MSSL-UCL) and D. M. Palmer (LANL) report on behalf of the
Swift/UVOT team:
The Swift/UVOT began observing the field of INTEGRAL GRB 090702,
3.5hrs after the
INTEGRAL trigger (Paizis et al., GCN 9603). We do not detect any
source at the
Swift XRT position (Sbarufatti et al. GCN 9604).
The 3-sigma upper limits for the finding chart exposure is:
Filter T_start(s) T_stop(s) Exp(s) Mag (3-sigma upper limit)
-------------------------------------------------------------
white 14080 20350 971 > 22.72
v 14646 20964 1126 > 21.20
b 13516 25451 1753 > 22.37
u 12951 24855 1796 > 21.89
-------------------------------------------------------------
The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight of E_(B-V) = 0.039 mag.
All photometry is on the UVOT photometric system described in Poole et
al. (2008, MNRAS, 383, 627).
- GCN Circular #9609
Sbarufatti B., Mangano V. (INAF-IASFPA) report on behalf of the Swift
Team:
We have analyzed the Swift-XRT data of XRF 090702 (Paizis, et al., GCN
Circ. 9603) comprising 6 ks in Photon Counting (PC) mode from T+16.5
ks to T+25.4 ks.
The best position for the X-ray afterglow is the XRT UVOT-enhanced
position:
RA, Dec = 175.89704, +11.50161 which is equivalent to:
RA (J2000): 11h 43m 35.29s
Dec (J2000): +11d 30' 05.8"
with an uncertainty of 5.0 arcsec (radius, 90% confidence).
The light-curve consists of two data points at the level of some 1E-3
counts/s, and shows evidence of a fading behaviour. A power-law
extrapolation of the available data indicates a count-rate of 9.4E-5
counts/s at T+48 h.
The average spectrum was fitted using Cash statistics with an absorbed
power-law model. The absorbing column NH was fixed at the Galactic
value of 3.5E20 cm^-2, the photon index is 1.9+/-0.4. The observed
(unabsorbed) flux is 2.8(3.0)E-13 ergs cm^-2 s^-1. The C-statistic is
29.3 with 32 bins. The count-rate to flux conversion factor is 4.4E-11.
All quoted errors are at 90% confidence level.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020106
This circular is an official product of the Swift-XRT team.
- GCN Circular #9614
A. Meshcheryakov (IKI), I. Khamitov (TUG), R. Burenin, M. Pavlinsky,
R. Sunyaev (IKI), Z. Eker (TUG), U. Kiziloglu (METU),
E. Gogus (Sabanci Uni.), I. Bikmaev, N. Sakhibullin (KSU/AST)
report:
We observed the field of XRF 090702 detected with IBIS/INTEGRAL (Paizis
et al., GC N 9603;) with Russian-Turkish 1.5-m telescope (RTT150,
Bakirlitepe, TUBITAK National Observatory, Turkey), starting at 02 Jul,
18:54 UT, i.e. 8.2h after the burst.
We made 2x600s exposures in SDSS r filter. In the combined image we do
not detect any sources inside the XRT/SWIFT error circle (Sbarufatti &
Mangano, GCN 9604). Using SDSS catalog for photometric calibration, we
estimate 3-sigma upper limit for any optical counterpart as m_r > 22.4.
- GCN Circular #9917
J. Haislip, D. Reichart, L. Cominsky, K. McLin, T. Graves, G. Spear, K.
Ivarsen, M. Schubel, A. LaCluyze, A. Foster, J. Moore, A. Oza, J. Styblova,
A. Trotter, J. A. Crain, and M. Nysewander report:
Skynet observed the INTEGRAL/IBAS localization of GRB 090702 (Paizis et
al., GCN 9603) with the 14" GORT telescope at Hume Observatory in
California beginning 18.2 hours after the the trigger in I.
We do not detect the afterglow (Sbarufatti & Mangano, GCN 9607). Stacking
only images that increase the limiting magnitude yields:
mean 1-sig. 1-sig.
time 3-sig. sys. stat.
since lim. cal. cal. cal.
trig. tel. exp. fil. mag. stars* unc. unc.
(h) (# x s) (mag) (mag)
<
18.2 GORT 2 x 80 I 17.7 32 SDSS 7 0.051 0.007
* Transformed using Jester et al., 2005, ApJ, 130, 873.
Previous IAU Circulars 