The XMM-Newton observatory is a cornerstone mission of the European Space Agency (ESA) Horizon 2000 program. This spacecraft, the largest ever flown by ESA for a scientific program, was launched on December 10, 1999, carrying a payload funded by ESA member states and the USA (NASA). The scientific payload comprises three CCD imaging cameras (European Photon Imaging Cameras, EPIC), sensitive in the 0.1-15 keV band, and two Reflecting Grating Spectrometers (RGS), sensitive in the 0.3-2.1 keV band, and characterized by a resolving power E/{Delta}E = 100 to 800. The X-ray instruments are complemented by an Optical Monitor, sensitive in the 150-650nm band, which allows simultaneous multiwavelength monitoring of celestial sources. The XMM-Newton observational program is determined on the bases of the proposals sent in response to Announcement of Opportunities, and selected by peer review panels. The XMM-Newton Science Archive (XSA) contains all the science data of all the performed observations. Its user interface (http:xmm.vilspa.esa.es/xsa) allows a user to retrieve them after the 1-year proprietary period has expired. Calibration observations are normally not covered by proprietary rights; their data being therefore public. Target of Opportunity and Discretionary Time observations have a 6-months proprietary period. For each archived observation, the XSA stores Observation Data Files (ODF) and Pipeline Processing System (PPS) products, if available, as well as the XMM-Newton EPIC serendipitous catalogue, the OM source catalogue and the Slew Survey Source Catalogue (see the catalogues documentation at http://xmm.esac.esa.int/xsa). The ODF comprises raw telemetry files, reformatted in FITS format, and contains uncalibrated information. The PPS products are a collection of top-level, validated scientific and cross-correlation products, routinely generated by the Science Survey Center, University of Leicester, UK (http://xmmssc-www.star.le.ac.uk). The content of the XSA is updated daily. The latest version of all the scientific data is made available through its interface. Systematic reprocessing of all the XMM-Newton telemetry is periodically carried on during the mission. The last bulk reprocessing was performed in 2007. The XMM-Newton observation log lists all the science observations included in the XSA. This log gives observation details and provides links to quick-look scientific products, to documents describing XMM-Newton science and calibration data, and to the SAS (Science Analysis System), a specific software package designed to reduce and analyze XMM-Newton data. Additional links in the log allows a user to start a retrieval session for the data of an observation, whenever not protected by proprietary rights. XMM-Newton HelpDesk: http://xmm.esac.esa.int/external/xmm_user_support/helpdesk.shtml
We present an XMM-Newton observation of the massive edge-on Sb galaxy NGC 2613. We discover that this galaxy contains a deeply embedded active nucleus with a 0.3-10keV luminosity of 3.3x10^40^erg/s and a line-of-sight absorption column of 1.2x10^23^cm^-2^. Within the 25mag arcsec-2 optical B-band isophote of the galaxy, we detect an additional four sources with an accumulated luminosity of 4.3x10^39^erg/s. The bulk of the unresolved X-ray emission spatially follows the near-infrared (NIR) K-band surface brightness distribution; the luminosity ratio LX/LK~8x10^-4^ is consistent with that inferred from galactic discrete sources. This X-ray-NIR association and the compatibility of the X-ray spectral fit with the expected spectrum of a population of discrete sources suggest that low-mass X-ray binaries (LMXBs) are the most likely emitters of the unresolved emission in the disc region.
We observed the main core F of the rho Ophiuchi cloud, an active star-forming region located at d~140pc, using XMM-Newton with an exposure of 33ks on February 19, 2001. We detect 87 X-ray sources within the 30' diameter field-of-view of the EPIC imaging detector array with significance above 4.4 sigma. We cross-correlate the positions of XMM-Newton X-ray sources with previous X-ray, infrared (IR), and optical catalogs.
The NGC 1333 star forming region was observed with the European Photon Imaging Cameras (EPIC) on board XMM-Newton on 27/28 February 2002. The observation covered a period of about 14 hours and has a total MOS-equivalent exposure time of 235 ksec. In addition to 46 bright X-ray sources revealed by source detection routines, weak X-ray emission at the positions of 40 X-ray sources detected originally in a recent Chandra observation of NGC 1333 was also detected.
Using the XMM-Newton observatory, we have observed the giant H II region N11 of the LMC. The field includes three OB associations LH9, LH9, and LH13. Our XMM observations included parallel observations with the OM camera that provided us with unique UV and optical photometry of more than 6000 sources. In this paper we present the photometrical data for these sources as well as their cross-identifications with several catalogues.
We report on a 30ks XMM-Newton observation of the central region of the Cha I star forming cloud. The field includes a substantial fraction of the known pre-main-sequence population of Cha I South, including all thirteen known very-low mass H{alpha} emitters. We detect two bona-fide brown dwarfs (spectral types M 7.5 and M 8) and seven H{alpha} emitting objects near the hydrogen burning mass limit, including six of seven earlier detections by ROSAT.
Following the advent of increasingly sensitive X-ray observatories, deep observations of early-type stars became possible. However, the results for only a few objects or clusters have until now been reported and there has been no large survey comparable to that based upon the ROSAT All-Sky Survey (RASS). A limited survey of X-ray sources, consisting of all public XMM observations (2XMMi) and slew survey data (XMMSL1), is now available. The X-ray counterparts to hot, massive stars have been searched for in these catalogs. About 300 OB stars were detected with XMM. Half of them were bright enough for a spectral analysis to be possible, and we make available the detailed spectral properties that were derived. The X-ray spectra of O stars are represented well by low (< 1 keV) temperature components and seem to indicate that an absorption column is present in addition to the interstellar contribution. The X-ray fluxes are well correlated with the bolometric fluxes, with a scatter comparable to that of the RASS studies and thus larger than found previously with XMM for some individual clusters. These results contrast with those of B stars that exhibit a large scatter in the L<sub>X</sub> - L<sub>bol</sub> relation, no additional absorption being found, and the fits indicate a plasma at higher temperatures. Variability (either within one exposure or between multiple exposures) was also investigated whenever possible: short-term variations are far more rare than long-term ones (the former affects a few percent of the sample, while the latter concerns between one third and two thirds of the sources). This is a catalog of X-ray emitters amongst early-type stars following a correlation between the Reed (2003, AJ, 125, 2531) Catalog of galactic OB Stars and the 2XMMi Catalog (Watson et al. 2009, A&A, 493, 339). See the reference paper for more details. This table was created by the HEASARC in November 2009 based on CDS table J/A+A/506/1055 file table1.dat. This is a service provided by NASA HEASARC .
The Optical Monitor Catalog of serendipitous sources (OMCat) contains entries for every source detected in the publicly available XMM-Newton Optical Monitor (OM) images taken in the imaging mode. Since the OM records data simultaneously with the X-ray telescopes on XMM-Newton, it typically produces images in one or more near-UV/optical bands for every pointing of the observatory. As of the beginning of 2014, the data in the public archive covered roughly 0.5% of the sky in 3425 fields. The OMCat is not dominated by sources previously undetected at other wavelengths; the bulk of objects have optical counterparts. However, the OMCat can be used to extend optical or X-ray spectral energy distributions for known objects into the ultraviolet, to study at higher angular resolution objects detected with GALEX, or to find high-Galactic-latitude objects of interest for UV spectroscopy. Differences between the current OMCat and the previous version of the OMCat (which was designated as XMMOMOBJ) are improved coordinates, improved quality flags, and a reduced number of spurious sources. The OM reduction was done with the standard ESAS software, with post-processing to apply the coordinate corrections in a more consistent manner. There is a major change in the way the data are represented in the table. In the previous XMMOMOBJ table a separate row was generated for each filter. In the current XMMOMCAT table each observation of each object generates only a single row regardless of how many filters were used. Unused filters have nulls while filters where the object is not detected have nulls for the detection parameters but a non-zero value for exposure. The table includes information for each filter and averaged information for the object as a whole. Only filters in which the object was detected are used in the averages. The parameters in this table comprise two sets: parameters describing the detection overall including id's and mean values, and values specific to the individual bands. There are three possible situations for the band data: (1) If there was no exposure in that band, then all fields for that band will be null. (2) If there was some exposure in the band but the object was not detected in that band, then the exposure field will give the actual exposure, but all of the other fields for that band will be null. (3) If the object was detected, then all of the fields for the band should be filled in. The filters included are V, B, U, UVW1, UVM2, UVW2 and white (i.e., unfiltered). The original table (formerly known as XMMOMOBJ) was created by the HEASARC in March 2008, based on a table supplied by the authors. The XMMOMCAT version was generated and ingested in February 2014 using a program which concatenated the objects detected in processing each observation. This is a service provided by NASA HEASARC .
XMM-Newton Optical Monitor Chandra Deep Field-South UV Catalog
Short Name:
XMMOMCDFS
Date:
14 Feb 2025
Publisher:
NASA/GSFC HEASARC
Description:
The XMM-Newton X-ray observatory has performed repeated observations of the Chandra Deep Field-South (CDFS) in 33 epochs (2001 - 2010) through the XMM-CDFS Deep Survey (Comastri et al. 2011, A&A, 526, L9). During the X-ray observations, the XMM-Newton Optical Monitor (XMM-OM) targeted the central 17 x 17 arcmin<sup>2</sup> 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 catalog of the CDFS, filling the UV spectral coverage between the optical surveys and GALEX observations. This table contains the UV catalog 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. The authors reprocessed the XMM-OM data of the survey and 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 ESO Imaging Survey (EIS: Arnouts et al. 2001, A&A, 379, 740) and COMBO-17 (Wolf et al. 2004, A&A, 421, 913; 2008, A&A, 492, 933) surveys. Photometric data of 1129 CDFS sources are provided in the main catalog, 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 in the reference paper. This table was created by the HEASARC in June 2015 based on the union of <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/217/4/">CDS Catalog J/ApJS/217/4/</a> files omcdfst7.dat (the 1,129 sources in the main catalog) and omcdfst8.dat (the 44 sources in the supplementary catalog). This is a service provided by NASA HEASARC .
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