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The Deep X-ray Radio Blazar Survey (DXRBS). II. New Identifications | | H. Landt
; P. Padovani
; E. Perlman
; P. Giommi
; H. Bignall
; A. Tzioumis
; | | Date: |
15 Dec 2000 | | Journal: | Mon.Not.Roy.Astron.Soc. 323 (2001) 757 | | Subject: | astro-ph | | Affiliation: | 1,2), P. Padovani (1,3), E. Perlman (1,4), P. Giommi , H. Bignall , A. Tzioumis ( STScI, Hamburg Observatory, Germany, ESA, UMBC, BeppoSAX/SDC, ASI, Italy, Univ. of Adelaide, Australia, ATNF, Australia | | Abstract: | We have searched the archived, pointed ROSAT Position Sensitive Proportional Counter data for blazars by correlating the WGACAT X-ray database with several publicly available radio catalogs, restricting our candidate list to serendipitous X-ray sources with a flat radio spectrum (alpha_r <= 0.70). This makes up the Deep X-ray Radio Blazar Survey (DXRBS). Here we present new identifications and spectra for 106 sources, including 86 radio-loud quasars, 11 BL Lacertae objects, and 9 narrow-line radio galaxies. Together with our previously published objects and already known sources, our sample now contains 298 identified objects: 234 radio-loud quasars (181 flat-spectrum quasars: FSRQ [alpha_r <= 0.50] and 53 steep-spectrum quasars: SSRQ), 36 BL Lacs, and 28 narrow-line radio galaxies. Redshift information is available for 96% of these. Thus our selection technique is ~ 90% efficient at finding radio-loud quasars and BL Lacs. Reaching 5 GHz radio fluxes ~ 50 mJy and 0.1-2.0 keV X-ray fluxes a few x 10^-14 erg/cm^2/s, DXRBS is the faintest and largest flat-spectrum radio sample with nearly complete (~ 85%) identification. We review the properties of the DXRBS blazar sample, including redshift distribution and coverage of the X-ray-radio power plane for quasars and BL Lacs. Additionally, we touch upon the expanded multiwavelength view of blazars provided by DXRBS. By sampling for the first time the faint end of the radio and X-ray luminosity functions, this sample will allow us to investigate the blazar phenomenon and the validity of unified schemes down to relatively low powers. | | Source: | arXiv, astro-ph/0012356 | | Services: | Forum | Review | PDF | Favorites | |
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