XMMCTY2AGN - XMM-COSMOS X-Ray Selected Type-2 AGN

Overview

This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10¹⁰ solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M_U, absolute magnitude M_V, absolute magnitude M_J (Johnson-Kron-Cousin system), and the morphological class.

Catalog Bibcode

2011A&A...534A.110L

References

The bolometric output and host-galaxy properties of obscured AGN in the
XMM-COSMOS survey.
    Lusso E., Comastri A., Vignali C., Zamorani G., Treister E., Sanders D.,
    Bolzonella M., Bongiorno A., Brusa M., Civano F., Gilli R., Mainieri V.,
    Nair P., Aller M., Carollo M., Koekemoer A.M., Merloni A., Trump J.R.
    <Astron. Astrophys. 534, A110 (2011)>
    =2011A&A...534A.110L        (SIMBAD/NED BibCode)

Provenance

This table was created by the HEASARC in October 2011 based on CDS table J/A+A/534/A110 file table1.dat. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018.

HEASARC Implementation

The HEASARC has added the positions of these X-ray sources and their XMM-Newton source names by matching the source numbers given in this table with those in Brusa et al. (2010, ApJ, 716, 348, the XMMCOSMOID table in HEASARC Browse). The HEASARC has also made the following changes to the data values:

(1) Values of 0.00 for the bolometric correction k_bol parameter (called hardxray_bc in this version) have been set to nulls: there were 15 such cases;

(2) The corresponding values of the (logarithm of the) bolometric luminosity for these 15 cases haves also been set to null values: in the original table, these had (unphysically large) values in the range 56 to 83.

Parameters

Source_Number
The XMM-COSMOS identification (XID) Number for the source, from Cappelluti et al. (2009, A&A, 497, 635).

Alt_Name
The name for the X-ray source using the naming convention recommended by the Dictionary of Nomenclature of Celestial Objects for XMM-COSMOS sources, viz. the 'XMMC' prefix and the source (XID) number, e.g., 'XMMC 5094'.

Name
The name of the X-ray source in the form 'XMMU JHHMMSS.s+DDMMSS' where the prefix is the usual one for XMM-Newton sources and the remainder of the field is the J2000.0 equatorial coordinates truncated to 0.1 seconds of time in RA and to 1 arcsecond in Declination.

RA
The Right Ascension of the source in the selected equinox. This was given in J2000.0 equatorial coordinates in decimal degrees to a precision of 10-5 degrees in the original Brusa et al. (2010, ApJ, 716, 348) table.

Dec
The Declination of the source in the selected equinox. This was given in J2000.0 equatorial coordinates in decimal degrees to a precision of 10-5 degrees in the original Brusa et al. (2010, ApJ, 716, 348) table.

LII
The Galactic Longitude of the source.

BII
The Galactic Latitude of the source.

Redshift
The spectroscopic redshift of the source. The origin of the redshifts for these sources is given in Footnote 2 in the Section 2 of the reference paper.

Log_Lx
The logarithm of the intrinsic X-Ray luminosity of the source in the hard X-ray (2 - 10 keV) energy band, in erg s^-1.

Log_L_Bol
The logarithm of the nuclear bolometric luminosity of the source, in erg s^-1. The method used to estimate this parameter is discussed in Section 6 of the reference paper.

Hardxray_Bc
The hard-X-ray bolometric correction, k_bol, of the source, defined as the ratio of the bolometric and hard X-ray luminosities.

Log_Stellar_Mass
The logarithm of the stellar mass of the associated galaxy, in solar masses.

SFR
The star formation rate of the associated galaxy, in solar masses per year.

Abs_Umag
The absolute U magnitude of the associated galaxy.

Abs_Vmag
The absolute V magnitude of the associated galaxy.

Abs_Jmag
The absolute J magnitude of the associated galaxy.

Morph_Class
The morphological classification of the associated galaxy (Type-2 AGN host), coded from 0 to 99 as follows:

               0 = elliptical
               1 = S0
               2 = bulge-dominated
               3 = intermediate-bulge
               4 = disk-dominated
               5 = irregular
               6 = compact/irregular
               7 = compact
               8 = unresolved/compact
               9 = blended
              10 = bulge-dominated/close-companion
              11 = intermediate-bulge/close-companion
              12 = S0/close-companion
              23 = possible mergers
              99 = no classification

Contact Person

Questions regarding the XMMCTY2AGN database table can be addressed to the HEASARC Help Desk.

Page Author: Browse Software Development Team
Last Modified: Monday, 16-Sep-2024 17:37:09 EDT