We present an analysis of the X-ray properties of the Magellanic-type galaxy NGC 55 based on two contiguous XMM-Newton observations. We detect a total of 137 X-ray sources in the field of view, down to a flux of ~5x10^-15^erg/cm^2^/s (0.3-6keV), 42 of which are located within the optical confines of the galaxy. On the basis of X-ray colour classification and after correcting for background objects, we conclude that our source sample includes ~20 X-ray binaries (XRBs), five supernova remnants and seven very soft sources (including two good candidate supersoft sources) associated with NGC 55. We also detect an X-ray source coincident with a previously identified globular cluster in NGC 55.
The following tables describe the results of a survey for X-ray (0.3-3 keV) sources in the young (30Myr) NGC 2547 open cluster using the XMM-Newton EPIC instrument. Table 1 lists the details of X-ray sources which are correlated with optical cluster members. Table 2 catalogues the cross-identifications with optical catalogues for the sources in Table 1 and derives their X-ray luminosities and X-ray to bolometric flux ratios. Table 3 lists the X-ray properties of sources which are uncorrelated with cluster members. Table 7 lists the correlations between cluster members detected by XMM-Newton and those detected 7 years earlier by the ROSAT HRI instrument, along with the X-ray luminosities and flux ratios as determined by the HRI.
Galactic globular clusters harbour binary systems that are detected as faint X-ray sources. These close binaries are thought to play an important role in the stability of the clusters by liberating energy and delaying the inevitable core collapse of globular clusters. The inventory of close binaries and their identification is therefore essential. We present XMM-Newton observations of two Galactic globular clusters: NGC 2808 and NGC 4372. We use X-ray spectral and variability analysis combined with ultra-violet observations made with the XMM-Newton optical monitor and published data from the Hubble Space Telescope to identify sources associated with the clusters. We compare the results of our observations with estimates from population synthesis models.
We present the characteristics of the X-ray variability of stars in the cluster NGC 2516 as derived from XMM-Newton/EPIC/pn data. The X-ray variations on short (hours), medium (months), and long (years) time scales have been explored. We detected 303 distinct X-ray sources by analysing six EPIC/pn observations; 194 of them are members of the cluster. Stars of all spectral types, from the early-types to the late-M dwarfs, were detected.
We present the results of an XMM-Newton observation of the young (~2-4Myr) cluster around the hot star sigma Orionis. In a previous paper (Sanz-Forcada et al., 2004A&A...421..715S) we presented the analysis of the RGS spectrum of the central hot star; here we discuss the results of the analysis of the full EPIC field. We have detected 175 X-ray sources, 88 of which have been identified with cluster members, including very low-mass stars down to the substellar limit. We detected eleven new possible candidate members from the 2MASS (Cat. <II/246>) catalogue.
The Lockman Hole represents the sky area of lowest Galactic line-of-sight columns density. It was observed by the XMM-Newton X-ray observatory in 18 pointings performed between April 2000 and December 2002. The total exposure time spent on the field was 1.16Ms (EPIC pn detector; EPIC MOS detector: 1.30 Ms). The effective exposure after removal of times of high particle background is 637ks (EPIC pn detector; EPIC MOS detector: 765ks). The catalogue lists positions, count rates, fluxes, hardness ratios, and partial optical classifications of 409 X-ray point sources detected in the central 0.196{deg}2 of the field down to a detection likelihood threshold of 10 (3.9sigma). The analysis was performed using the XMM-Newton SAS data analysis package version 6.0.
X-rays are a powerful probe of activity in early stages of star formation. They allow us to identify young stars even after they have lost the IR signatures of circumstellar disks and provide constraints on their distance. Here, we report on XMM-Newton observations that detect 121 young stellar objects (YSOs) in two fields between L1641S and {kappa} Ori. These observations extend the Survey of Orion A with XMM and Spitzer (SOXS). The YSOs are contained in a ring of gas and dust apparent at millimeter wavelengths, and in far-IR and near-IR surveys. The X-ray luminosity function of the YSOs detected in the two fields indicates a distance of 250-280pc, much closer than the Orion A cloud and similar to distance estimates of {kappa} Ori. We propose that the ring is a 5-8pc diameter shell that has been swept up by {kappa} Ori. This ring contains several groups of stars detected by Spitzer and WISE including one surrounding the Herbig Ae/Be stars V1818 Ori. In this interpretation, the {kappa} Ori ring is one of several shells swept up by massive stars within the Orion Eridanus Superbubble and is unrelated to the southern portion of OrionA/L1641S.
The XMM-Newton X-ray observatory has performed repeated observations of the CDFS in 33 epochs (2001-2010) through the XMM-CDFS Deep Survey. During the X-ray observations, XMM-OM targeted the central 17x17arcmin^2^ region of the X-ray field of view, providing simultaneous optical/UV coverage of the CDFS. The resulting set of data can be taken into account to build an XMM-OM catalogue of the CDFS, filling the UV spectral coverage between the optical surveys and GALEX observations. We present the UV catalogue of the XMM-CDFS Deep Survey. Its main purpose is to provide complementary UV average photometric measurements of known optical/UV sources in the CDFS, taking advantage of the unique characteristics of the survey. The data reduction is intended also to improve the standard source detection on individual observations, by cataloguing faint sources through the stacking of their exposure images. We reprocessed the XMM-OM data of the survey and we stacked the exposures from consecutive observations using the standard SAS tools to process the data obtained during single observations. Average measurements of detections with SAS good quality flags from individual observations and from stacked images have been joined to compile the catalogue. Sources have been validated through the cross-identification within the EIS and COMBO-17 surveys. Photometric data of 1129 CDFS sources are provided into the catalogue, and optical/UV/X-ray photometric and spectroscopic information from other surveys are also included. The stacking extends the detection limits by ~1 mag in the three UV bands, contributing 30% of the catalogued UV sources. The comparison with the available measurements in similar spectral bands confirms the validity of the XMM-OM calibration. The combined COMBO-17/X-ray classification of the "intermediate" sources (e.g. optically diluted and/or X-ray absorbed AGN) is also discussed.
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.
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.
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