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2261. XMM-OM Serendipitous Source Survey Catalogue (XMM-SUSS5.0)
ID:
ivo://CDS.VizieR/II/370
Title:
XMM-OM Serendipitous Source Survey Catalogue (XMM-SUSS5.0)
Short Name:
II/370
Date:
03 Dec 2021 13:12:28
Publisher:
CDS
Description:
SUSS5.0 is a new 2020 release of the XMM OM Serendipitous Ultraviolet Source Survey catalogue. his release is largely an increment of the previous XMM-OM-SUSS4.1 release but includes flagging of sources affected by a patch of reduced sensitivity near the centre of the OM field of view. The catalogue was compiled for the Optical Monitor instrument on board the ESA XMM Newton observatory. This version, the 5th release of the catalogue, spans the period of observations from XMM-Newton revolution 34 (February 2000) to revolution 3704 (February 2020). A detailed description of the Catalogue can be found at https://www.ucl.ac.uk/mssl/research-projects/2018/dec/xmm-newton. A refereed paper on the first version can be found in Page M.J. et al. (2012MNRAS.426..903P). In addition to covering a larger observation period, this fifth release includes flagging of sources affected by a patch of reduced sensitivity near the boresight, caused by erroneously V-filter exposures during an observation of Jupiter in July 2017 (revolution 3224). All data have been fully processed at the European Space Astronomy Centre (ESAC, Madrid, Spain) using the XMM Science Analysis Software (SAS) system version 18.0. The number of observations (OBSIDs) included in the catalogue is 10,628. The total number of entries in this release is 8,863,922. They correspond to 5,965,434 sources, of which 1,120,754 have multiple entries in the source table, corresponding to different observations. The Catalogue is a FITS file consisting of two tables (please note that users wishing to use the TOPCAT tool to manipulate the catalogue, need to select the table format option, "FITS" to load the catalogue). The first one (SRCLIST) contains the sources, with positional and photometric data (count rate, magnitude and flux) and quality flags for each measurement.
2262. XMM-OM Serendipitous Source Survey Catalogue (XMM-SUSS4.1)
ID:
ivo://CDS.VizieR/II/356
Title:
XMM-OM Serendipitous Source Survey Catalogue (XMM-SUSS4.1)
Short Name:
II/356
Date:
21 Oct 2021
Publisher:
CDS
Description:
SUSS4.1 is a new 2018 release of the XMM OM Serendipitous Ultraviolet Source Survey catalogue. This new release corrects some inconsistencies between IAUNAME and SRCNUM found in the previous release (OM SUSS4). The catalogue was compiled for the Optical Monitor instrument on board the ESA XMM Newton observatory. This version, the 4th release of the catalogue, spans the period of observations from 2000 to July 2017. A detailed description of the Catalogue can be found at https://www.ucl.ac.uk/mssl/research-projects/2018/dec/xmm-newton. A refereed paper on the first version can be found in Page M.J. et al. (2012MNRAS.426..903P). In addition to covering a larger observation period, the fourth release differs from the previous one in the implementation of a new time dependent sensitivity degradation correction. As in the previous release, sources detected on stacked images are properly flagged. All data have been fully processed at the European Space Astronomy Centre (ESAC, Madrid, Spain) by using the XMM Science Analysis Software (SAS) system version 17.0. The number of observations (OBSIDs) included in the catalogue is 9,749. The total number of entries in this release is 8,176,156. They correspond to 5,503,765 sources, of which 1,035,453 have multiple entries in the source table, corresponding to different observations. The Catalogue consists of two tables. The first one (SRCLIST) contains the sources, with positional and photometric data (count rate, magnitude and flux) and quality flags for each measurement. In the second table (SUMMARY) we give a summary of the observations from which the sources have been detected and measured.
2263. XMM-OM Serendipitous Source Survey Catalogue (XMM-SUSS2.1)
ID:
ivo://CDS.VizieR/II/340
Title:
XMM-OM Serendipitous Source Survey Catalogue (XMM-SUSS2.1)
Short Name:
II/340
Date:
21 Oct 2021
Publisher:
CDS
Description:
The second release of the XMM OM Serendipitous Source Survey Catalogue (XMM-SUSS2) was produced by processing the XMM-Newton Optical Monitor (OM) data obtained from the beginning of the mission (2000) until the end of 2012. The latest release, XMM-SUSS2.1, now includes an extra year of data to the end of 2013. The data processing was performed at the European Space Astronomy Centre (ESAC, Spain) and at Mullard Space Science Laboratory (MSSL UCL, U.K.) by using the XMM Science Analysis Software system (SAS) version 14.0. In addition to covering a larger observation period, this release differs from the first release (XMM-SUSS) by inclusion of all the OM observations (not only those containing UV filters) and by performing source detection on stacked images, thus facilitating the detection of fainter sources. The number of observations (OBSIDs) included in the catalogue is 7,170. The total number of entries included in the catalogue is 6,246,432. They correspond to 4,329,363 sources, of which 831,582 have multiple entries in the source table, corresponding to different observations.
2264. XMM Optical Monitor Survey of TMC
ID:
ivo://CDS.VizieR/J/A+A/468/379
Title:
XMM Optical Monitor Survey of TMC
Short Name:
J/A+A/468/379
Date:
21 Oct 2021
Publisher:
CDS
Description:
The Optical Monitor (OM) on-board XMM-Newton obtained optical/ultraviolet data for the XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST), simultaneously with the X-ray detectors. With the XEST OM data, we study the optical and ultraviolet properties of TMC members, and to perform correlative studies between the X-ray and OM light curves. In particular, we aim to determine whether accretion plays a significant role in the optical/ultraviolet and X-ray emissions. The Neupert effect in stellar flares is also investigated. Coordinates, average count rates and magnitudes were extracted from OM images, together with light curves with low time resolution (a few kiloseconds). For a few sources, OM FAST mode data were also available, and we extracted OM light curves with high time resolution. The OM data were correlated with Two Micron All Sky Survey (2MASS) data and with the XEST catalogue in the X-rays. The XEST OM catalogue contains 2,148 entries of which 1,893 have 2MASS counterparts. However, only 98 entries have X-ray counterparts, of which 51 are known TMC members and 12 additional are TMC candidates. The OM data indicate that accreting stars are statistically brighter in the U band than non-accreting stars after correction for extinction, and have U-band excesses, most likely due to accretion. The OM emission of accreting stars is variable, probably due to accretion spots, but it does not correlate with the X-ray light curve, suggesting that accretion does not contribute significantly to the X-ray emission of most accreting stars. In some cases, flares were detected in both X-ray and OM light curves and followed a Neupert effect pattern, in which the optical/ultraviolet emission precedes the X-ray emission of a flare, whereas the X-ray flux is proportional to the integral of the optical flux.
2265. 3XMM/SDSS Stripe 82 Galaxy Cluster Survey. I.
ID:
ivo://CDS.VizieR/J/A+A/594/A32
Title:
3XMM/SDSS Stripe 82 Galaxy Cluster Survey. I.
Short Name:
J/A+A/594/A32
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a galaxy cluster survey based on XMM-Newton observations that are located in Stripe 82 of the Sloan Digital Sky Survey (SDSS). The survey covers an area of 11.25deg^2^. The X-ray cluster candidates were selected as serendipitously extended detected sources from the third XMM-Newton serendipitous source catalogue (3XMM-DR5). A cross-correlation of the candidate list that comprises 94 objects with recently published X-ray and optically selected cluster catalogues provided optical confirmations and redshift estimates for about half of the candidate sample. We present a catalogue of X-ray cluster candidates previously known in X-ray and/or optical bands from the matched catalogues or NED. The catalogue consists of 54 systems with redshift measurements in the range of 0.05-1.19 with a median of 0.36. Of these, 45 clusters have spectroscopic confirmations as stated in the matched catalogues. We spectroscopically confirmed another 6 clusters from the available spectroscopic redshifts in the SDSS-DR12. The cluster catalogue includes 17 newly X-ray discovered clusters, while the remainder were detected in previous XMM-Newton and/or ROSAT cluster surveys. Based on the available redshifts and fluxes given in the 3XMM-DR5 catalogue, we estimated the X-ray luminosities and masses for the cluster sample. We also present the list of the remaining X-ray cluster candidates (40 objects) that have no redshift information yet in the literature. Of these candidates, 25 sources are considered as distant cluster candidates beyond a redshift of 0.6. We also searched for galaxy cluster mergers in our cluster sample and found two strong candidates for newly discovered cluster mergers at redshifts of 0.11 and 0.26. The X-ray and optical properties of these systems are presented.
2266. XMM serendipitous survey AXIS X-ray source counts
ID:
ivo://CDS.VizieR/J/A+A/469/27
Title:
XMM serendipitous survey AXIS X-ray source counts
Short Name:
J/A+A/469/27
Date:
21 Oct 2021
Publisher:
CDS
Description:
Recent results have revised upwards the total X-ray background (XRB) intensity below 10keV, therefore an accurate determination of the source counts is needed. There are also contradictory results on the clustering of X-ray selected sources. We have studied the X-ray source counts in four energy bands: soft (0.5-2keV), hard (2-10keV), XID (0.5-4.5keV) and ultra-hard (4.5-7.5keV) in order to evaluate the contribution of sources at different fluxes to the X-ray background. We have also studied the angular clustering of X-ray sources in those bands. AXIS (An XMM International Survey) is a survey of 36 high Galactic latitude XMM observations covering 4.8deg^2^ in the Northern sky and containing 1433 serendipitous X-ray sources detected with 5-sigma significance. This survey has similar depth to the XMM catalogues and therefore serves as a pathfinder to explore their possibilities. We have combined this survey with shallower and deeper surveys, and fitted the source counts with a Maximum Likelihood technique. Using only AXIS sources we have studied the angular correlation using a novel robust technique. Our source counts results are compatible with most previous samples in the soft, XID, ultra-hard and hard bands. We have improved on previous results in the hard band. The fractions of the XRB resolved in the surveys used in this work are 87%, 85%, 60% and 25% in the soft, hard, XID and ultra-hard bands, respectively. Extrapolation of our source counts to zero flux is not sufficient to saturate the XRB intensity. Only galaxies and/or absorbed AGN could contribute the remaining unresolved XRB intensity. Our results are compatible, within the errors, with recent revisions of the XRB intensity in the soft and hard bands. The maximum fractional contribution to the XRB comes from fluxes within about a decade of the break in the source counts (~10^-14^cgs), reaching ~50% of the total in the soft and hard bands. Angular clustering (widely distributed over the sky and not confined to a few deep fields) is detected at 99-99.9% significance in the soft and XID bands, with no detection in the hard and ultra-hard band (probably due to the smaller number of sources). We cannot confirm the detection of significantly stronger clustering in the hard-spectrum hard sources. Medium depth surveys such as AXIS are essential to determine the evolution of the X-ray emission in the Universe below 10keV.
2267. XMM survey of soft background. III. Galactic halo
ID:
ivo://CDS.VizieR/J/ApJ/773/92
Title:
XMM survey of soft background. III. Galactic halo
Short Name:
J/ApJ/773/92
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present measurements of the Galactic halo's X-ray emission for 110 XMM-Newton sight lines selected to minimize contamination from solar wind charge exchange emission. We detect emission from few million degree gas on ~4/5 of our sight lines. The temperature is fairly uniform (median = 2.22x10^6^K, interquartile range = 0.63x10^6^K), while the emission measure and intrinsic 0.5-2.0keV surface brightness vary by over an order of magnitude (~(0.4-7)x10^-3^cm^-6^pc and ~(0.5-7)x10^-12^erg/cm2/s deg^-2^, respectively, with median detections of 1.9x10^-3^cm^-6^pc and 1.5x10^-12^erg/cm2/s deg^-2^, respectively). The high-latitude sky contains a patchy distribution of few million degree gas. This gas exhibits a general increase in emission measure toward the inner Galaxy in the southern Galactic hemisphere. However, there is no tendency for our observed emission measures to decrease with increasing Galactic latitude, contrary to what is expected for a disk-like halo morphology. The measured temperatures, brightnesses, and spatial distributions of the gas can be used to place constraints on models for the dominant heating sources of the halo. We provide some discussion of such heating sources, but defer comparisons between the observations and detailed models to a later paper.
2268. XQ-100. X-shooter quasar spectra
ID:
ivo://CDS.VizieR/J/MNRAS/462/3285
Title:
XQ-100. X-shooter quasar spectra
Short Name:
J/MNRAS/462/3285
Date:
21 Oct 2021
Publisher:
CDS
Description:
We statistically study the physical properties of a sample of narrow absorption line (NAL) systems looking for empirical evidences to distinguish between intrinsic and intervening NALs without taking into account any a priori definition or velocity cut-off. We analyse the spectra of 100 quasars with 3.5<z_em_<4.5, observed with X-shooter/Very Large Telescope in the context of the XQ-100 Legacy Survey. We detect an ~8{sigma} excess in the CIV number density within 10000km/s of the quasar emission redshift with respect to the random occurrence of NALs. This excess does not show a dependence on the quasar bolometric luminosity and it is not due to the redshift evolution of NALs. It extends far beyond the standard 5000km/s cut-off traditionally defined for associated absorption lines. We propose to modify this definition, extending the threshold to 10000km/s when weak absorbers (equivalent width <0.2{AA}) are also considered. We infer NV is the ion that better traces the effects of the quasar ionization field, offering the best statistical tool to identify intrinsic systems. Following this criterion, we estimate that the fraction of quasars in our sample hosting an intrinsic NAL system is 33 per cent. Lastly, we compare the properties of the material along the quasar line of sight, derived from our sample, with results based on close quasar pairs investigating the transverse direction. We find a deficiency of cool gas (traced by C II) along the line of sight connected to the quasar host galaxy, in contrast with what is observed in the transverse direction.
2269. X-ray AGN from RASS and SDSS
ID:
ivo://CDS.VizieR/J/AJ/126/2209
Title:
X-ray AGN from RASS and SDSS
Short Name:
J/AJ/126/2209
Date:
21 Oct 2021
Publisher:
CDS
Description:
We describe the initial results of a new program aimed to ultimately yield ~10^4^ fully characterized X-ray source identifications - a sample about an order of magnitude larger than earlier efforts. The technique is detailed and employs X-ray data from the ROSAT All-Sky Survey (RASS, Cat. <IX/10>, <IX/29>) and optical imaging and spectroscopic follow-up from the Sloan Digital Sky Survey (SDSS, <J/AJ/123/567>); these two surveys prove to be serendipitously very well matched in sensitivity. As part of the SDSS software pipelines, optical objects in the SDSS photometric catalogs are automatically positionally cross-correlated with RASS X-ray sources. Then priorities for follow-on SDSS optical spectra of candidate counterparts are automatically assigned using an algorithm based on the known ratios of fX/fopt for various classes of X-ray emitters at typical RASS fluxes of 10^-13^ergs/cm^2^/s. SDSS photometric parameters for optical morphology, magnitude, and colors, plus FIRST radio information, serve as proxies for object class.
2270. X-ray emission of RASS Abell clusters
ID:
ivo://CDS.VizieR/J/AJ/126/2740
Title:
X-ray emission of RASS Abell clusters
Short Name:
J/AJ/126/2740
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present an analysis of the X-ray emission for a complete sample of 288 Abell clusters spanning the redshift range 0.016<=z<=0.09 from the ROSAT All-Sky Survey. This sample is based on our 20cm VLA survey of nearby Abell clusters. We find an X-ray detection rate of 83%. We report cluster X-ray fluxes and luminosities and two different flux ratios indicative of the concentration and extent of the emission. We examine correlations between the X-ray luminosity, Abell richness, and Bautz-Morgan and Rood-Sastry cluster morphologies. We find a strong correlation between LX and cluster richness coupled with a dependence on the optical morphological type. These results are consistent with the observed scatter between X-ray luminosity and temperature and a large fraction of cooling flows. For each cluster field, we also report the positions, peak X-ray fluxes, and flux ratios of all X-ray peaks above 3{sigma} significance within a box of 2x2(h_75_)^-1^Mpc centered on Abell's position.

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