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17551. XMM/CDFS AGN intrinsic absorption
ID:
ivo://CDS.VizieR/J/A+A/459/693
Title:
XMM/CDFS AGN intrinsic absorption
Short Name:
J/A+A/459/693
Date:
21 Oct 2021
Publisher:
CDS
Description:
We combine bright XMM-Newton data with the Chandra Deep Field South observations to explore the behavior of the intrinsic AGN absorption, as a function of redshift and luminosity. Our sample consists of 359 sources selected in the hard 2-8keV band, spanning the flux range 6x10^-16^-3x10^-13^erg/cm^2^/s with a high rate of spectroscopic or photometric redshift completeness (100 and 85 per cent respectively for the Chandra and XMM-Newton data). We derive the column density values using X-ray spectral fits. We find that the fraction of obscured AGN falls with increasing luminosity in agreement with previous findings. The fraction of obscured AGN shows an apparent increase at high redshifts (z>2). Simulations show that this effect can most probably be attributed to the fact that at high redshifts the column densities are overestimated.
17552. XMM/CFDS catalogue
ID:
ivo://CDS.VizieR/J/MNRAS/350/785
Title:
XMM/CFDS catalogue
Short Name:
J/MNRAS/350/785
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the X-ray source catalogues for the XMM surveys of the 3-h and 14-h (also known as the Groth Strip) Canada-France Redshift Survey fields (0.5-10keV flux range ~2x10^-15^-10^-13^erg/cm^2^/s). We use a subset of the XMM sources, which have Chandra positions, to determine the best method of obtaining optical identifications of sources with only XMM positions. We find optical identifications for 79 per cent of the XMM sources for which there are deep optical images. The sources without optical identifications are likely to be optically fainter and have higher redshifts than the sources with identifications. We have estimated 'photometric redshifts' for the identified sources, calibrating our method using ~200 galaxies in the fields with spectroscopic redshifts. We find that the redshift distribution has a strong peak at z~0.7.
17553. XMM/Chandra study of IC 10
ID:
ivo://CDS.VizieR/J/MNRAS/362/1065
Title:
XMM/Chandra study of IC 10
Short Name:
J/MNRAS/362/1065
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. A list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field is provided; a substantial fraction of them are likely stellar objects in the Milky Way due to the low Galactic latitude location of IC 10.
17554. XMM Clusters of galaxies in COSMOS field
ID:
ivo://CDS.VizieR/J/ApJS/172/182
Title:
XMM Clusters of galaxies in COSMOS field
Short Name:
J/ApJS/172/182
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the results of a search for galaxy clusters in the first 36 XMM-Newton pointings on the Cosmic Evolution Survey (COSMOS) field. We reach a depth for a total cluster flux in the 0.5-2keV band of 3x10^-15^ergs/cm^2^/s, having one of the widest XMM-Newton contiguous raster surveys, covering an area of 2.1deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. Verification of the cluster candidates is done based on a galaxy concentration analysis in redshift slices of thickness 0.1-0.2 in redshift, using the multiband photometric catalog of the COSMOS field and restricting the search to z<1.3 and i_AB_<25. We identify 72 clusters and derive their properties based on the X-ray cluster scaling relations. A statistical description of the survey in terms of the cumulative log(N>S)-logS distribution compares well with previous results, although yielding a somewhat higher number of clusters at similar fluxes. The X-ray luminosity function of COSMOS clusters matches well the results of nearby surveys, providing a comparably tight constraint on the faint-end slope of alpha=1.93+/-0.04. For the probed luminosity range of (8x10^42^)-(2x10^44^)ergs/s, our survey is in agreement with and adds significantly to the existing data on the cluster luminosity function at high redshifts and implies no substantial evolution at these luminosities to z=1.3.
17555. XMM-COSMOS Catalog of Optical/IR Counterparts
ID:
ivo://nasa.heasarc/xmmcosmoid
Title:
XMM-COSMOS Catalog of Optical/IR Counterparts
Short Name:
XMMCOSMOID
Date:
14 Feb 2025
Publisher:
NASA/GSFC HEASARC
Description:
This table contains the final optical identifications of the medium-depth (~60 ks), contiguous (2 degree&lt;sup&gt;2&lt;/sup&gt;) XMM-Newton survey of the COSMOS field. XMM-Newton has detected ~1800 X-ray sources down to limiting fluxes of ~5 x 10&lt;sup&gt;-16&lt;/sup&gt;, ~3 x 10&lt;sup&gt;-15&lt;/sup&gt;, and ~7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV, 2-10 keV, and 5-10 keV bands, respectively (~1 x 10&lt;sup&gt;-15&lt;/sup&gt;, ~6 x 10&lt;sup&gt;-15&lt;/sup&gt;, and ~1 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;, in the three bands, respectively, over 50% of the area). The work is complemented by an extensive collection of multi-wavelength data from 24 microns to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for &gt;~50% of the sample, and high-quality photometric redshifts for the rest. The XMM-Newton and multi-wavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%) have MIPS 24 um detections. Thanks to the redshift completeness (almost 100%) the authors were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of log L&lt;sub&gt;X&lt;/sub&gt; &gt; 44.5 active galactic nuclei (AGNs) is at z ~ 2. Spectroscopically identified obscured and unobscured AGNs, as well as normal and star-forming galaxies, present well-defined optical and infrared properties. The authors devised a robust method to identify a sample of ~150 high-redshift (z &gt; 1), obscured AGN candidates for which optical spectroscopy is not available. They were able to determine that the fraction of the obscured AGN population at the highest (L&lt;sub&gt;X&lt;/sub&gt; &gt; 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) X-ray luminosity is ~15%-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. The authors studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO (source number 2028), caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations. This table was created by the HEASARC in July 2010 based on the electronic version of Table 2 from the paper which was obtained from the Astrophysical Journal web site. &lt;p&gt; The HEASARC has made some changes to this material in order to make it more compliant with CDS/IAU Nomenclature and HEASARC table standards: &lt;p&gt; (i) The original naming convention suggested by the authors used a prefix of &#39;XMMC_&#39; and the J2000.0 RA and Dec position in decimal degrees to 10&lt;sup&gt;-5&lt;/sup&gt; degrees precision, e.g., XMMC_150.10515+1.98082&#39;; the HEASARC has replaced these names by alternative new ones (in the alt_name parameter) of the form &#39;XMMU JHHMMSS.s+DDMMSS&#39; 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; &lt;p&gt; (ii) We have used for the alt_name parameter the naming convention recommended by the Dictionary of Nomenclature of Celestial Objects for XMM-COSMOS sources, viz. the &quot;XMMC&#39; prefix and the source (XID) number, e.g., &quot;XMMC 2028&#39;. This is a service provided by NASA HEASARC .
17556. XMM-COSMOS Catalog of X-Ray Selected Type 1 AGN
ID:
ivo://nasa.heasarc/xmmcosmagn
Title:
XMM-COSMOS Catalog of X-Ray Selected Type 1 AGN
Short Name:
XMMCOSMAGN
Date:
14 Feb 2025
Publisher:
NASA/GSFC HEASARC
Description:
This table contains the results from a study of the X-ray to optical properties of a sample of 545 X-ray selected Type 1 AGN, from the XMM-Newton Cosmic Evolution (XMM-COSMOS) survey, over a wide range of redshifts (0.04 &lt; z &lt; 4.25) and X-ray luminosities (40.6 &lt;= log(L&lt;sub&gt;2-10keV&lt;/sub&gt;) &lt;= 45.3). About 60% of them are spectroscopically identified Type 1 AGN, while the others have a reliable photometric redshift and are classified as Type 1 AGN on the basis of their multi-band Spectral Energy Distributions (SEDs). In the reference, the authors discuss the relationship between UV and X-ray luminosity, as parametrized by the X-ray to optical-UX alpha&lt;sub&gt;ox&lt;/sub&gt; spectral slope, and its dependence on redshift and luminosity. Herein optical and X-ray properties for 545 Type 1 AGN in XMM-COSMOS are presented. For each source, X-ray ID, spectroscopic redshift, photometric redshift, upper error on the photometric redshift, lower error on the photometric redshift, logarithm of the monochromatic luminosity at 2500 Angstroms, logarithm of the monochromatic luminosity at 2 keV, alpha&lt;sub&gt;ox&lt;/sub&gt;, logarithm of the 2-10 keV luminosity, logarithm of the bolometric luminosity in solar units, bolometric correction, photometric classification, logarithm of the Eddington ratio, logarithm of the black hole mass in solar masses, and a flag for the 2-10 keV detection (flag = 1 [343 entries] means a detection in the 2-10 keV band, while flag = 0 is for 2-10 keV upper limits) are given. This table was created by the HEASARC in May 2010 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/512/A34"&gt;CDS catalog J/A+A/512/A34&lt;/a&gt; file table2.dat. This is a service provided by NASA HEASARC .
17557. XMM-COSMOS Type 1 AGNs
ID:
ivo://CDS.VizieR/J/A+A/512/A34
Title:
XMM-COSMOS Type 1 AGNs
Short Name:
J/A+A/512/A34
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a study of the X-ray to optical properties of a sample of 545 X-ray selected Type 1 AGN, from the XMM-COSMOS survey, over a wide range of redshifts (0.04<z<4.25) and X-ray luminosities (40.6<=LogL[2-10]keV<=45.3). About 60% of them are spectroscopically identified Type 1 AGN, while the others have a reliable photometric redshift and are classified as Type 1 AGN on the basis of their multi-band Spectral Energy Distributions. We discuss the relationship between UV and X-ray luminosity, as parameterized by the alpha_ox_ spectral slope, and its dependence on redshift and luminosity.
17558. XMM-COSMOS X-Ray Selected Type-2 AGN
ID:
ivo://nasa.heasarc/xmmcty2agn
Title:
XMM-COSMOS X-Ray Selected Type-2 AGN
Short Name:
XMMCTY2AGN
Date:
14 Feb 2025
Publisher:
NASA/GSFC HEASARC
Description:
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 10&lt;sup&gt;10&lt;/sup&gt; 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&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class. 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&#39;s implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
17559. XMM count-rates in M 55 and NGC 3201
ID:
ivo://CDS.VizieR/J/A+A/445/155
Title:
XMM count-rates in M 55 and NGC 3201
Short Name:
J/A+A/445/155
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have observed two low concentration Galactic globular clusters with the X-ray observatory XMM-Newton. We detect 47 faint X-ray sources in the direction of M 55 and 62 in the field of view of NGC 3201. Using the statistical LogN-LogS relationship of extragalactic sources derived from XMM-Newton Lockman Hole observations, to estimate the background source population, we estimate that very few of the sources (1.5+/-1.0) in the field of view of M 55 actually belong to the cluster. These sources are located in the centre of the cluster as we expect if the cluster has undergone mass segregation. NGC 3201 has approximately 15 related sources, which are centrally located but are not constrained to lie within the half mass radius. The sources belonging to this cluster can lie up to 5 core radii from the centre of the cluster which could imply that this cluster has been perturbed. Using X-ray (and optical, in the case of M 55 ) colours, spectral and timing analysis (where possible) and comparing these observations to previous X-ray observations, we find evidence for sources in each cluster that could be cataclysmic variables, active binaries, millisecond pulsars and possible evidence for a quiescent low mass X-ray binary with a neutron star primary, even though we do not expect any such objects in either of the clusters, due to their low central concentrations. The majority of the other sources are background sources, such as AGN.
17560. 4XMM-DR9-HECATE-based ULX catalogue
ID:
ivo://CDS.VizieR/J/A+A/659/A188
Title:
4XMM-DR9-HECATE-based ULX catalogue
Short Name:
J/A+A/659/A188
Date:
25 Mar 2022 09:09:32
Publisher:
CDS
Description:
Ultraluminous X-ray sources (LX>1x10^39^erg/s, ULXs) are excellent probes for extreme accretion physics, star formation history in galaxies, and intermediate-mass black holes searches. As the sample size of X-ray data from modern observatories such as XMM-Newton and Chandra increases, producing extensive catalogues of ULXs and studying their collective properties has become both a possibility and a priority. Our aim is to build a clean updated ULX catalogue based on one of the most recent XMM-Newton X-ray serendipitous survey data releases, 4XMM-DR9, and the most recent and exhaustive catalogue of nearby galaxies, HECATE. We performed a preliminary population study to test if the properties of the expanded XMM-Newton ULX population are consistent with previous findings. We performed positional cross-matches between XMM-Newton sources and HECATE objects to identify host galaxies, and we used distance and luminosity arguments to identify ULX candidates. We flagged interlopers by finding known counterparts in external catalogues and databases such as Gaia DR2 SSDS, Pan-STARRS1, the NASA/IPAC Extragalactic Database, and SIMBAD. Source, galaxy and variability parameters from 4XMM-DR9, HECATE, and 4XMM-DR9s were used to study the spectral, abundances and variability properties of the ULX sample. We identify 779 ULX candidates, 94 of which hold LX>5x10^40^erg/s. Spiral galaxies are more likely to host ULXs. For early spiral galaxies the number of ULX candidates per star-forming rate is consistent with previous studies, while a significant ULX population in elliptical and lenticular galaxies also exists. Candidates hosted by late-type galaxies tend to present harder spectra and to undergo more extreme inter-observation variability than those hosted by early-type galaxies. Approximately 30 candidates with LX>1x10^41^erg/s are also identified, constituting the most interesting candidates for intermediate-mass black hole searches. We have built the largest ULX catalogue to date. Our results on the spectral and abundance properties of ULXs confirm the findings made by previous studies based on XMM-Newton and Chandra data, while our population-scale study on variability properties is unprecedented. Our study, however, provides limited insight into the properties of the brightest ULX candidates due to the small sample size. The expected growth of X-ray catalogues and potential future follow-ups will aid in drawing a clearer picture.

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