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ATEL # 2196; C. Baldovin (ISDC), E. Kuulkers (ESA/ESAC, Spain), C. Ferrigno (ISDC/IAAT), E. Bozzo (ISDC), J. Chenevez, S. Brandt (National Space Institute, Denmark), V. Beckmann (APC, France), A. Bird (Southampton, UK), A. Domingo (LAEFF/INTA, Spain), K. Ebisawa (ISAS, Japan), P. Jonker (SRON, The Netherlands), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (GSFC, USA), T.Oosterbroek (ESA/ESTEC, The Netherlands), A. Paizis (INAF-IASF, Italy), D. Risquez (LAEFF/INTA, Spain), C. Sanchez-Fernandez (ESA/ESAC, Spain), S. Shaw (Southampton, UK), R. Wijnands (UvA, The Netherlands)
on 13 Sep 2009; 18:10 UT
Distributed as an Instant Email Notice (Request for Observations)
Password Certification: Nami Mowlavi (Nami.Mowlavi@obs.unige.ch)
Subjects: X-ray, Gamma Ray, Request for Observations, Transients
Referred to by ATEL #: 2197
During the latest observations of the Galactic Bulge monitoring (see ATel #438), carried out between 2009-09-12 03:21:34 and 2009-09-12 05:27:22 (UTC), INTEGRAL discovered a new bright hard X-ray source, which we designate IGRJ17511-3057.
The source is detected in the INTEGRAL/IBIS mosaic image with a significance of 14 sigma in the 20-40 keV energy band, and 7 sigma in the 40-80 keV energy band. The corresponding count rates in these bands are 4.2+/0.3 cts/s (28 mCrab) and 1.8+/-0.3 cts/s (25 mCrab), respectively. The source is also detected in the JEM-X mosaic in the three energy bands 3-7 keV, 7-11 keV, and 11-20 keV. The source flux is ~20 mCrab and the detection significance is 3 sigma in all bands.
The best determined source position is RA: 267.811 DEC: -30.954 (J2000), with a 90% error radius of 2.0 arcmin.
The combined IBIS/ISGRI and JEM-X spectrum in the 3-100 keV energy range is well described by a single power-law with photon index 2.0+/-0.2. The source flux is 5.7e-10 erg/cm2/s in the 3-20 keV energy band and 4.8e-10 erg/cm2/s in the 20-100 keV energy band.
We did not find any previously known X-ray source in the Simbad database within the INTEGRAL error circle. A Swift follow-up has already been requested. We encourage multi-wavelength observations.