Bat X-ray survey I. Methodology and X-ray identification

M. Ajello, J. Greiner, G. Kanbach, A. Rau, A. W. Strong, J. A. Kennea

Research output: Contribution to journalArticlepeer-review

49 Scopus citations

Abstract

We applied the maximum likelihood (ML) method, as an image reconstruction algorithm, to the BAT X-Ray Survey (BXS). This method was specifically designed to preserve the full statistical information in the data and to avoid mosaicking of many exposures with different pointing directions, thus reducing systematic errors when co-adding images. We reconstructed, in the 14-170 keV energy band, the image of a 90 × 90 deg2 sky region, centered on (R.A., decl.) = (105°, -25°), which BAT surveyed with an exposure time of ∼1 Ms (in 2005 November). The best sensitivity in our image is ∼0.85 mcrab or 2.0 × 10-11 ergs cm-2. We detect 49 hard X-ray sources above the 4.5 σ level; of these, only 12 were previously known as hard X-ray sources (>15 keV). Swift XRT observations allowed us to firmly identify the counterparts for 15 objects, while 2 objects have Einstein IPC counterparts (Harris et al. 1990); in addition to those, we found a likely counterpart for 13 objects by correlating our sample with the ROSATAll-Sky Survey Bright Source Catalog (Voges et al. 1999). Seven objects remain unidentified. Analysis of the noise properties of our image shows that ∼75% of the area is surveyed to a flux limit of ∼1 mcrab. This study shows that the coupling of the ML method to the most sensitive, all-sky surveying, hard X-ray instrument, BAT, is able to probe for the first time the hard X-ray sky to the millicrab flux level. The successful application of this method to BAT demonstrates that it could also be applied with advantage to similar instruments such as INTEGRAL IBIS.

Original languageEnglish (US)
Pages (from-to)102-115
Number of pages14
JournalAstrophysical Journal
Volume678
Issue number1
DOIs
StatePublished - May 1 2008

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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