2013A&A...558A..89K


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:55:32

2013A&A...558A..89K - Astronomy and Astrophysics, volume 558A, 89-89 (2013/10-1)

AGN and QSOs in the eROSITA All-Sky Survey. I. Statistical properties.

KOLODZIG A., GILFANOV M., SUNYAEV R., SAZONOV S. and BRUSA M.

Abstract (from CDS):

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. 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). 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 function (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. After four years of the survey, a sky-average sensitivity of about 1x10–14erg/s/cm2 will be achieved in the 0.5-2.0keV band. With this sensitivity, eROSITA is expected to detect about 3 million AGN on the extragalactic sky (|b|>10°). The median redshift of the eRASS AGN will be z≃1 with approximately 40% of the objects in the z=1-2 redshift range. About 104-105 AGN are predicted beyond redshift z=3 and about 2000-30000 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 ≃38 counts per point-spread-function (half-energy width), while the faintest 10% will have fewer than ≃9 counts. The optical counterparts of approximately 95% of the AGN will be brighter than IAB=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 0.5-2.0keV sensitivity of ≃2x10–14 to ≃2x10–13erg/s/cm2, respectively.

Abstract Copyright:

Journal keyword(s): surveys - X-rays: general - X-rays: galaxies - quasars: general - galaxies: luminosity function, mass function - galaxies: active

Simbad objects: 5

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Number of rows : 5

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME Chandra Deep Field-South reg 03 32 28.0 -27 48 30           ~ 1812 1
2 NAME COSMOS Field reg 10 00 28.60 +02 12 21.0           ~ 2069 0
3 NAME Lockman Hole reg 10 45 00.0 +58 00 00           ~ 748 0
4 NAME NOAO Deep Wide Field reg 14 32 05.75 +34 16 47.5           ~ 324 0
5 NAME Local Bubble ISM ~ ~           ~ 693 0

    Equat.    Gal    SGal    Ecl

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2020.07.10-02:55:32

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