AGN and QSOs in the eROSITA All-Sky Survey

作者：Kolodzig Alexander^*; Gilfanov Marat; Sunyaev Rashid; Sazonov Sergey; Brusa Marcella

来源：ASTRONOMY %26 ASTROPHYSICS, 2013, 558: A89.

DOI：10.1051/0004-6361/201220880

• surveys
• X-rays: general
• X-rays: galaxies
• quasars: general
• galaxies: luminosity function, mass function
• galaxies: active

Context. The main element of the observing program of the Spectrum-Roentgen-Gamma orbital observatory is a four-year all-sky survey, in the course of which the entire sky will be scanned eight times. %26lt;br%26gt;Aims. We analyze the statistical properties of active galactic nuclei (AGN) and quasars/quasi-stellar objects (QSOs) that are expected to be detected in the course of the eROSITA all-sky survey (eRASS). %26lt;br%26gt;Methods. According to the currently planned survey strategy and based on the parameters of the Galactic and extragalactic X-ray background as well as on the results of the recent calculations of the eROSITA instrumental background, we computed a sensitivity map of the eRASS. Using the best available redshift-dependent AGN X-ray luminosity XLF), we computed various characteristics of the eRASS AGN sample, such as their luminosity- and redshift distributions, and the brightness distributions of their optical counterparts. %26lt;br%26gt;Results. After four years of the survey, a sky-average sensitivity of about 1 x 10(-14) erg s(-1) cm(-2) will be achieved in the 0.5-2.0 keV band. With this sensitivity, eROSITA is expected to detect about 3 million AGN on the extragalactic sky (| b| %26gt; 10 degrees). The median redshift of the eRASS AGN will be z approximate to 1 with approximately 40% of the objects in the z = 1-2 redshift range. About 10(4) -10(5) AGN are predicted beyond redshift z = 3 and about 2000-30 000 AGN beyond redshift z = 4, the exact numbers depend on the poorly known behavior of the AGN XLF in the high-redshift and high-luminosity regimes. Of the detected AGN, the brightest 10% will be detected with more than approximate to 38 counts per point-spread-half-energy width), while the faintest 10% will have fewer than approximate to 9 counts. The optical counterparts of approximately 95% of the AGN will be brighter than I-AB = 22.5mag. The planned scanning strategy will allow one to search for transient events on a timescale of half a year and a few hours with a 0.5-2.0 keV sensitivity of 10(-14) to approximate to 2 x 10(-13) erg s(-1) cm(-2), respectively.

• 出版日期2013-10