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The Palermo Swift-BAT Hard X-Ray Catalogue*

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The Palermo Swift-BAT Hard X-Ray Catalogue* A&A 510, A48 (2010) Astronomy DOI: 10.1051/0004-6361/200811184 & c ESO 2010 Astrophysics The Palermo Swift-BAT hard X-ray catalogue II. Results after 39 months of sky survey G. Cusumano1,V.LaParola1, A. Segreto1, V. Mangano1,C.Ferrigno1,2,3, A. Maselli1,P.Romano1,T.Mineo1, B. Sbarufatti1, S. Campana4, G. Chincarini5,4,P.Giommi6,N.Masetti7, A. Moretti4, and G. Tagliaferri4 1 INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, via U. La Malfa 153, 90146 Palermo, Italy e-mail: [email protected] 2 Institut für Astronomie und Astrophysik Tübingen (IAAT), Germany 3 ISDC Data Centre for Astrophysics, Chemin d’Écogia 16, 1290 Versoix, Switzerland 4 INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate, Italy 5 Università degli studi di Milano-Bicocca, Dipartimento di Fisica, Piazza delle Scienze 3, 20126 Milan, Italy 6 ASI Science Data Center, via Galileo Galilei, 00044 Frascati, Italy 7 INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy Received 17 October 2008 / Accepted 23 June 2009 ABSTRACT Aims. We present the Palermo Swift-BAT hard X-ray catalogue obtained from the analysis of data acquired during the first 39 months of the Swift mission. Methods. We developed a dedicated software to perform the data reduction, mosaicking, and source detection of the BAT survey data. We analyzed the BAT dataset in three energy bands (14−150 keV, 14−30 keV, 14−70 keV), obtaining a list of 962 detections above a significance threshold of 4.8 standard deviations. The identification of the source counterparts was pursued using three strategies: cross-correlation with published hard X-ray catalogues, analysis of field observations of soft X-ray instruments, and cross-correlation with SIMBAD databases. Results. The survey covers 90% of the sky down to a flux limit of 2.5 × 10−11 erg cm−2 s−1 and 50% of the sky down to a flux limit of 1.8 × 10−11 erg cm−2 s−1 in the 14−150 keV band. We derived a catalogue of 754 identified sources, of which ∼69% are extragalactic, ∼27% are Galactic objects, and ∼4% are already known X-ray or gamma ray emitters, whose nature has yet to be determined. The integrated flux of the extragalactic sample is ∼1% of the cosmic X-ray background in the 14−150 keV range. Key words. X-rays: general – catalogs – surveys 1. Introduction Wood et al. 1984). Later, sky images for energies greater than 10 keV were produced using coded mask detectors (e.g., The study of Galactic and extragalactic sources at energies Fenimore & Cannon 1978; Skinner et al. 1987a): in these de- greater than 10 keV is fundamental to both the investigation of tectors the entrance window of the telescope is partially masked non thermal emission processes and to the study of source pop- and the “shadows” of the cosmic sources are projected onto a ulations that are not detectable in the soft X-ray energy band position-sensitive detector. Dedicated algorithms are then used because their emission is strongly absorbed by a thick column to reconstruct the position and intensity of the sources in the of gas or dust. Another major aim of deep and sensitive surveys ff field of view and, therefore, reproduce the image of the ob- in the hard X-ray domain is to resolve the di use X-ray back- served sky. In the last two decades, space observatories equipped ground (CXB) and identify which class of sources represents the with this type of telescopes have surveyed the sky reporting most significant contribution: while the CXB at energies lower − detections of numerous sources emitting in the hard X-ray do- than 10 keV has been almost entirely resolved (80 90%, Moretti main: Spacelab/XRT (Skinner et al. 1987b), MIR/KVANT/TTM et al. 2003; Worsley et al. 2005, 2006; Brandt & Hasinger 2005), / ∼ (Sunyaev et al. 1991), GRANAT ART-P (Pavlinsky et al. 1992, only 1.5% of the CXB at higher energies can be associated with 1994), GRANAT/SIGMA (Cordier et al. 1991; Sunyaev et al. resolved sources (Ajello et al. 2008b). 1991), and BeppoSAX/WFC (Jager et al. 1997). Today, the IBIS- Until now, the observation of the hard X-ray sky has not ISGRI camera (Ubertini et al. 2003; Lebrun et al. 2003)onthe been performed with imaging grazing incidence telescopes be- INTEGRAL observatory (Winkler et al. 2003) with its field of cause the reflectivity above 10 keV rapidly declines because of view of 8◦ × 8◦ (fully coded) is carrying out a hard X-ray sur- the steep decrease in the critical angle with energy. The first vey focussing mostly on the Galactic plane in the 20−150 keV surveys in the hard X-ray domain were performed with detec- energy band with a sensitivity higher than previous observato- tors equipped with collimator-limited field of view: UHURU − − ries. The main results of this survey and the relevant source cata- (2 20 keV; Forman et al. 1978) and HEAO1 (0.2 keV 10 MeV; logues are reported in several papers (e.g. Bird et al. 2004, 2006, Table 2 is also available in electronic form at the CDS via anony- 2007; Bassani et al. 2006; Krivonos et al. 2007, 2005; Sazonov mous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via et al. 2007; Churazov et al. 2007). http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/510/A48 Article published by EDP Sciences Page 1 of 20 A&A 510, A48 (2010) The Burst Alert Telescope (BAT; Barthelmy et al. 2005) on- the spacescraft attitude was unstable (i.e., with a significant vari- board the Swift observatory (Gehrels et al. 2004), because of its ation in the pointing coordinates). The resulting dataset was pre- large field of view (100◦ × 60◦ half coded) and large detector analyzed (see Sect. 4), to produce preliminary Detector Plane area (a factor of 2 greater than ISGRI), offers the opportunity Images (DPI, obtained integrating the DPH along the spectral to significantly increase the number of detections contributing dimension) from where the bright sources (S/N > 8) and back- to the luminosity of the sky in the hard X-rays allowing a sub- ground were subtracted; very noisy DPHs, i.e., with a standard stantial improvement of our knowledge of the AGN and of the deviation significantly larger than the average value where sub- cosmic hard X-ray background. The first results on the BAT sur- tracted. The list of bright sources detected in each DPH was vey have been presented in Markwardt et al. (2005), Ajello et al. used to identify and discard the files suffering from inaccurate (2008a,b), and Tueller et al. (2008). The latter presents a cata- position reconstruction. After cross-correlating the position of logue of sources detected in the first 9 months of the BAT survey these sources with the ISGRI catalogue, the GRB positions, data, identifying 154 extragalactic sources (129 at |b| > 15◦). and the newly discovered Swift sources documented in literature To take full advantage of the BAT survey archive, we devel- (Markwardt et al. 2005; Ajello et al. 2008a; Tueller et al. 2008), oped the dedicated software BatImager (Segreto et al. 2010), we discarded the files where: which is independent from the software developed by the Swift- – the bright sources in the BAT field of view are detected more BAT team1. In this paper, we present the results obtained from than 10 arcmin from their counterpart position (because of a the analysis of 39 months of BAT sky survey. The paper is orga- star tracker loss of lock); nized as follows: in Sect. 2, we describe the BAT telescope; in – the reconstructed image of at least one bright source has Sect. 3, we describe the data set and screening criteria; in Sect. 4, a strongly elongated shape (maybe due to an unrecognized we present a brief description of the code used for the analysis slew). and illustrate our analysis strategy. In Sect. 5, we describe the survey properties. The catalogue construction and the results are After the screening based on these criteria, the usable archive reported in Sect. 6. The last section summarizes our results. The has a total nominal exposure time of 72.7 Ms, corresponding spectral properties of our extragalactic sample will be discussed to 91.2% of the total survey exposure time during the period in a forthcoming paper (La Parola et al. 2010, in preparation). under investigation. The cosmology adopted in this work assumes H0 = −1 −1 = Ω = . Λ = . 70 km s Mpc , k 0, m 0 3, and 0 0 7. Quoted 4. Methodology errors are at 1σ confidence level, unless stated otherwise. To perform a systematic and efficient search for new hard X-ray sources, we developed the BatImager, a dedicated software 2. The BAT telescope that produces an all-sky mosaic directly from a list of BAT data The BAT, one of the three instruments onboard the Swift ob- files. A complete and detailed description of the software and its servatory, is a coded aperture imaging camera consisting of performance is presented in Segreto et al. (2010). Here we report a 5200 cm2 array of 4 × 4mm2 CdZnTe elements mounted on a only the details of the procedure which are relevant to this work. plane 1 m behind a 2.7 m2 coded aperture mask of 5 × 5mm2 el- ements distributed with a pseudo-random pattern. The telescope, 4.1. The code which operates in the 14−150 keV energy range, has a large field of view (1.4 steradian half coded), and a point spread function The BatImager integrates each single DPH in a selected energy (PSF) of 17 arcmin, and is devoted mainly to the monitoring of a range, producing the corresponding DPI.
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