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92 results for “XMM-Newton”
XMM-Newton Slew Survey Clean Source Catalog, v3.0
This table contains the 'clean' sample of sources from the third catalog of X-ray sources found in slew data taken by the European Space Agency's XMM-Newton Observatory, XMMSL3 or XMMSLEW, Version 3.0. It has been created by the XMM-Newton Survey Science Center (SSC) on behalf of ESA, building on previous work carried out by the XMM-Newton SOC. The core <a href="/W3Browse/xmm-newton/xmmslewful.html">XMMSL3</a> catalog contains detections drawn from 3120 XMM-Newton pn slew observations, covering an energy interval from 0.2 keV to 12 keV. These observations were made between 2000 August 26 and 2023 August 11. All slew observations are public. A full discussion of the differences between XMMSL3 and XMMSL2 is given in Section 12 of the <a href="http://xmmssc.irap.omp.eu/Catalogue/XMMSL3/XMMSL3_Catalogue_User_Guide.html">XMMSL3 Users Guide</a>. This database table was first created by the HEASARC in August 2007 based on the FITS version of XMMSL1D1 (v1.1) of the XMM Slew Catalog. The current version was ingested in February 2025 and is based on the FITS version of XMMSL3 (v3.0) of the XMM Slew Catalog obtained from the following URLs: <a href="http://xmmssc.irap.omp.eu/Catalogue/XMMSL3/xmmsl3_v1.0.fits">http://xmmssc.irap.omp.eu/Catalogue/XMMSL3/xmmsl3_v1.0.fits</a> (the total sample). This catalog contains only the entries from that FITS file which have VAL_FLAG = 'CLEAN SAMPLE'. <p> The HEASARC has endeavored to retain the same parameter names as in the ESA version, but some names have been changed so as to conform to the standard HEASARC parameter naming conventions, e.g., all error parameter names which ended in "_err" in the ESA version end in "_error" in this HEASARC version. For other parameters which have had their names changed, their original ESA names are listed in square brackets in their descriptions below. This is a service provided by NASA HEASARC .
XMM-Newton OB Stars Catalog
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 .
Lynds 1641 and iota Ori Region XMM-Newton X-Ray Point Source Catalog
This table contains results from an XMM-Newton and Spitzer survey of the part of the Orion A cloud south of the Orion Nebula, the 'Survey of Orion A with XMM-Newton and Spitzer (SOXS)'. The goal of SOXS is to detect the relatively bright X-ray sources in the Orion A cloud and complete the census of more evolved YSOs in this region. These stars represent a sample of cloud members chosen with minimal a priori bias toward their IR properties. This XMM-Newton survey includes the Lynds 1641 (L1641) dark cloud, a region of the Orion A cloud with very few massive stars and hence a relatively low ambient UV flux, and the region around the O9 III star iota Orionis. In addition to proprietary data, the authors used archival XMM data of the Orion Nebula Cluster (ONC) to extend their analysis to a major fraction of the Orion A cloud. They have detected 1060 X-ray sources with more than 4.5-sigma significance in L1641 and the iota Ori region. About 94% of the sources have Two Micron All Sky Survey (2MASS) and Spitzer counterparts, 204 and 23 being Class II and Class I or protostar objects, respectively. In addition, the authors have identified 489 X-ray sources as counterparts to Class III candidates, given they are bright in X-rays and appear as normal photospheres at mid-IR wavelengths. The remaining 205 X-ray sources are likely distant active galactic nuclei (AGN) or other galactic sources not related to Orion A. The authors find that Class III candidates appear more concentrated in two main clusters in L1641. The first cluster of Class III stars is found toward the northern part of L1641, concentrated around iota Ori. The stars in this cluster are more evolved than those in the Orion Nebula. The authors estimate a distance of 300-320 pc for this cluster showing that it is in the foreground of the Orion A cloud. Another cluster rich in Class III stars is located in L1641 South and appears to be a slightly older cluster embedded in the Orion A cloud. Furthermore, other evolved Class III stars are found north of the ONC toward NGC 1977. The SOXS survey is composed of seven specifically proposed ~ 50 ks XMM-Newton fields, south of the ONC, to which the authors added four archival fields in the same region. The archival fields are centered on iota Orionis, V380 Ori, and V883 Ori, respectively (see Fig. 1 and Table 1 of the reference paper for more details of the X-ray observations). This HEASARC table contains the contents of Table 2 (1060 X-ray detected sources in the fields S1 - S10 listed in Table 1 of the reference paper), Table 3 (best-fit spectral parameters for the 232 brightest of these X-ray sources) and Table 4 (list of 1041 IR counterparts to the X-ray sources) from the reference paper. Some X-ray sources have no identified counterparts (16 of them in fact lie outside of the FOV of the Spitzer observations), most have a single counterpart, and a small number have 2 or even 3 IR counterparts within the 5 arcseconds matching radius used. For X-ray sources with more than 1 IR counterpart, we have added entries for the additional counterparts (71 in total), repeating the X-ray information in such cases. Thus, this HEASARC table contains 1131 (1060 + 71) entries corresponding to the 1060 X-ray source detections. To make its contents easier to visualize, the HEASARC has added a a parameter ir_match which lists the counterpart number for the entry: If there is no identified IR counterpart, ir_match is set to 0, for the first listed IR counterpart to 1, for the second and third, to 2 and 3, respectively. Thus, if the user wants to reduce the table back to a pure list of X-ray sources and their primary IR counterparts, they should search the table selecting ir_match < 2. This table was created by the HEASARC in August 2013 based on the electronic versions of Tables 2 and 3 from the original reference paper (2013ApJ...768...99P) and Table 4 from the erratum (2013ApJ...773...80P), which were all obtained from the ApJ web site. This is a service provided by NASA HEASARC .
XMM-Newton Slew Survey Full Source Catalog, v3.0
This table contains the 'total' sample of sources from the third catalog of X-ray sources found in slew data taken by the European Space Agency's XMM-Newton Observatory, XMMSL3 or XMMSLEW, Version 3.0. It has been created by the XMM-Newton Survey Science Center (SSC) on behalf of ESA, building on previous work carried out by the XMM-Newton SOC. It is an incremental version of the XMMSL2 catalog but contains 50% more observations than the previous version, including 8.5 additional years of data, using modified software and slightly revised screening methodology and therefore has been given a major version increment. It contains 1006 more observations for a total of 3120 observations and 68,383 more detections (for a total of 140,735 detections) than the preceding XMMSL2 catalog, which was made public in March 2017. This release of XMMSL3 contains detections drawn from 3120 XMM-Newton pn slew observations, covering an energy interval from 0.2 keV to 12 keV. These observations were made between 2000 August 26 and 2023 August 11. All slew observations are public. A full discussion of the differences between XMMSL3 and XMMSL2 is given in Section 12 of the <a href="http://xmmssc.irap.omp.eu/Catalogue/XMMSL3/XMMSL3_Catalogue_User_Guide.html">XMMSL3 Users Guide</a>. This database table was first created by the HEASARC in August 2007 based on the FITS version of XMMSL1D1 (v1.1) of the XMM Slew Catalog. The current version was ingested in February 2025 and is based on the FITS version of XMMSL3 (v3.0) of the XMM Slew Catalog obtained from the following URLs: <a href="http://xmmssc.irap.omp.eu/Catalogue/XMMSL3/xmmsl3_v1.0.fits">http://xmmssc.irap.omp.eu/Catalogue/XMMSL3/xmmsl3_v1.0.fits</a> (the total sample). <p> The HEASARC has endeavored to retain the same parameter names as in the ESA version, but some names have been changed so as to conform to the standard HEASARC parameter naming conventions, e.g., all error parameter names which ended in "_err" in the ESA version end in "_error" in this HEASARC version. For other parameters which have had their names changed, their original ESA names are listed in square brackets in their descriptions below. This is a service provided by NASA HEASARC .
XMM-Newton Deep Survey in the CDF-S 2-10 keV Source Catalog
Nuclear obscuration plays a key role in the initial phases of AGN growth, yet not many highly obscured AGN are currently known beyond the local Universe, and their search is an active topic of research. The XMM-Newton survey in the Chandra Deep Field South (XMM-CDFS) aims at detecting and studying the spectral properties of a significant number of obscured and Compton-thick (N<sub>H</sub> >= 10<sup>24</sup> cm<sup>-2</sup>) AGN. The large effective area of XMM-Newton in the 2-10 and 5-10 keV bands, coupled with a 3.45-Ms nominal exposure time (2.82 and 2.45 Ms after lightcurve cleaning for MOS and PN respectively), allows the authors to build clean samples in both bands, and makes the XMM-CDFS the deepest XMM-Newton survey currently published in the 5-10 keV band. The large multi-wavelength and spectroscopic coverage of the CDFS area allows for an immediate and abundant scientific return. In this paper, the authors present the data reduction of the XMM-CDFS observations, the method for source detection in the 2-10 and 5-10 keV bands, and the resulting catalogs. A number of 339 and 137 sources are listed in the above bands with flux limits of 6.6 x 10<sup>-16</sup> and 9.5 x 10<sup>-16</sup> erg/s/cm<sup>2</sup>, respectively. The flux limits at 50% of the maximum sky coverage are 1.8 x 10<sup>-15</sup> and 4.0 x 10<sup>-15</sup> erg/s/cm<sup>2</sup>, respectively. The catalogs have been cross-correlated with the Chandra ones: 315 and 130 identifications have been found with a likelihood-ratio method, respectively. 15 new sources, previously undetected by Chandra, have been found; 5 of them lie in the 4-Ms area. Redshifts, either spectroscopic or photometric, are available for ~92% of the sources. The number counts in both bands are presented and compared to other works. The survey coverage has been calculated with the help of two extensive sets of simulations, one set per band. The simulations have been produced with a newly-developed simulator, written with the aim of the most careful reproduction of the background spatial properties. For this reason, the authors present a detailed decomposition of the XMM-Newton background into its components: cosmic, particle, and residual soft protons. The three components have different spatial distributions. The importance of these three components depends on the band and on the camera; the particle background is the most important one (80-90% of the background counts), followed by the soft protons (4-20%). X-ray sources were detected in the 3-Ms XMM-Newton observations of the Chandra Deep Field South. Source detection was done in two steps, first using the PWXDetect software, and then using emldetect. 339 Sources detected by both programs are presented in the main tables, while 74 sources only detected by PWXDetect are presented in the supplementary tables. The 2-10 and 5-10 keV bands were analyzed separately. This HEASARC table contains the main sample of 339 sources detected in the 2-10 keV band in the XMM-CDFS survey. (The table of 5-10 keV XMM-CDFS sources is also available at the HEASARC as the XMMCDFS510 table). This table does not include the 74 supplementary sources which were detected only with PWXDetect. These supplementary sources were on average detected at low significance; many of them were on the borders of the FOV; and a few were in crowded fields where EMLDetect had trouble separating the different PSF components. Nevertheless, 4 of these sources were bright enough that a spectrum could be extracted. This table was created by the HEASARC in September 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/555/A42">CDS Catalog J/A+A/555/A42</a> files main210.dat and notes210.dat. This is a service provided by NASA HEASARC .
XMM-Newton Bright Serendipitous Survey
We present here the XMM-Newton Bright Serendipitous Survey, composed of two flux-limited samples: the XMM-Newton Bright Source Sample (BSS, hereafter) and the XMM-Newton "Hard" Bright Source Sample (HBSS, hereafter). The selection criteria for these two sample, 0.5 - 4.5 keV count rate >= 0.01 ct/s (BSS) and 4.5 - 7.5 keV count rate >= 0.002 ct/s (HBSS), correspond to a flux limit of f<sub>X</sub> ~ 7 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s in the 0.5 - 4.5 keV and 4.5 - 7.5 keV energy bands, respectively, for sources with power-law spectra with energy spectral indices between 0.7 and 0.8. This table contains the basic data on a complete sample of 400 X-ray sources (389 of them belong to the BSS, 67 to the HBSS, with 56 X-ray sources in common) derived from the analysis of 237 suitable XMM-Newton fields (211 for the HBSS). At the flux limit of the survey, it covers a survey area of 28.10 (25.17 for the HBSS) square degrees. The extragalactic number-flux relationships (in the 0.5 - 4.5 keV and in the 4.5 - 7.5 keV energy bands) are in good agreement with previous and new results making the authors confident in the correctness of the data selection and their analysis. This table was created by the HEASARC in October 2006 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/428/383">CDS Catalog J/A+A/428/383</a> (the merger of files table3.dat and table4.dat). This is a service provided by NASA HEASARC .
Lockman Hole XMM-Newton X-Ray Point Source Catalog
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 1.16 Ms (EPIC pn detector; EPIC MOS detector: 1.30 Ms). The effective exposure after removal of times of high particle background is 637 ks (EPIC pn detector; EPIC MOS detector: 765 ks). The catalog lists positions, count rates, fluxes, hardness ratios, and partial optical classifications of 409 X-ray point sources detected in the central 0.196 square degrees of the field down to a detection likelihood threshold in the full energy band of 10 (3.9 sigma), up to 4 of which may be spurious according to the authors' Monte Carlo simulations. The analysis was performed using the XMM-Newton SAS data analysis package version 6.0. This table was created by the HEASARC in May 2008 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/479/283">CDS Catalog J/A+A/479/283</a> file table3.dat. This is a service provided by NASA HEASARC .
M 31 XMM-Newton Spectral Survey X-Ray Point Source Catalog
This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L<sub>X</sub> interval 37.0 <~ log L<sub>X</sub> erg s<sup>-1</sup> <~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L<sub>X</sub> ~1.4 x 10<sup>36</sup> erg s<sup>-1</sup>, the observed population is statistically dominated by the point source population of M 31. This table was created by the HEASARC in October 2009 based on the electronic version of Table A1 from the reference paper which was obtained from the CDS (their catalog J/A+A/495/733 file tablea1.dat. This is a service provided by NASA HEASARC .
XMM-Newton Survey Science Center Survey of the Galactic Plane
Many different classes of X-ray sources contribute to the Galactic landscape at high energies. Although the nature of the most luminous X-ray emitters is now fairly well understood, the population of low-to-medium X-ray luminosity (L<sub>X</sub> = 10<sup>27</sup> - 10<sup>34</sup> erg/s) sources remains much less studied, our knowledge being mostly based on the observation of local members. The advent of wide-field and high-sensitivity X-ray telescopes such as XMM-Newton now offers the opportunity to observe this low-to-medium L<sub>X</sub> population at large distances. This study reports the results of a Galactic plane survey conducted by the XMM-Newton Survey Science Centre (SSC). Beyond its astrophysical goals, this survey aims at gathering a representative sample of identified X-ray sources at low latitude that can be used later on to statistically identify the rest of the serendipitous sources discovered in the Milky Way. The survey is based on 26 XMM-Newton observations, obtained at |b| < 20 degrees, distributed over a large range in Galactic longitudes and covering a summed area of 4 deg<sup>2</sup>. The flux limit of this survey is 2 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s in the soft (0.5 - 2 keV) band and 1 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s in the hard (2 - 1 2keV) band. A total of 1319 individual X-ray sources have been detected. Using optical follow-up observations supplemented by cross-correlation with a large range of multi-wavelength archival catalogs, the authors identify 316 X-ray sources. This constitutes the largest group of spectroscopically identified low-latitude X-ray sources at this flux level. The majority of the identified X-ray sources are active coronae with spectral types in the range A to M at maximum distances of ~1 kpc. The number of identified active stars increases towards late spectral types, reaching a maximum at K. Using infrared colors, the authors classify 18% of the stars as giants. The observed distributions of F<sub>X</sub>/F<sub>V</sub>, X-ray and infrared colors indicates that their sample is dominated by a young (100 Myr) to intermediate (600 Myr) age population with a small contribution of close main-sequence or evolved binaries. The authors find other interesting objects such as cataclysmic variables (d ~ 0.6 - 2 kpc), low-luminosity high-mass stars (likely belonging to the class of Gamma-Cas-like systems, d ~ 1.5 - 7 kpc), T Tauri and Herbig-Ae stars. A handful of extragalactic sources located in the highest Galactic latitude fields could be optically identified. For the 20 fields observed with the EPIC pn camera, the authors have constructed log N(>S) - log S curves in the soft and hard bands. In the soft band, the majority of the sources are positively identified with active coronae and the fraction of stars increases by about one order of magnitude from b = 60 degrees to b = 0 degrees at an X-ray flux of 2 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s. The hard band is dominated by extragalactic sources, but there is a small contribution from a hard Galactic population formed by CVs, HMXB candidates or Gamma-Cas-like systems and by some active coronal stars that are also detected in the soft band. At b = 0 degrees, the surface density of hard sources brighter than 1 x 10<sup>-13</sup> erg/cm<sup>2</sup>/s steeply increases by one order of magnitude from l = 20 degrees to the Galactic center region (l = 0.9 degrees). This HEASARC table contains 739 X-ray sources detected in the 26 different fields observed in this study and listed in Tables 8 - 33, inclusive, of the reference paper. These 739 sources have the best XMM quality, i.e. the summary flag sum_flag which contains information about flags set automatically and manually for a given source is zero, meaning that there are no negative flags for the source detection, have either a 2MASS, USNO, GSC, or SDSS counterpart, whatever the probability of identification is, or have some information via SIMBAD or the authors own imaging or spectroscopic observations. For each X-ray source, its X-ray parameters are summarized, listing the pn count rates, and information on optical and infrared counterparts is provided. The properties of the 26 target fields are given in Table 1 of the reference paper, along with the breakdown of source classes in each field. This table was created by the HEASARC in May 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/553/A12">CDS Catalog J/A+A/553/A12</a>, the 26 files table8.dat to table33.dat, inclusive. This is a service provided by NASA HEASARC .
NGC 2264 XMM-Newton X-Ray Point Source Catalog
This table contains (some of) the results from an X-ray imaging survey of the young cluster NGC 2264, carried out with the European Photon Imaging Cameras (EPIC) on board the XMM-Newton spacecraft. XMM-Newton EPIC observations were made separately of the northern and southern portions of NGC 2264 on 2001 March 20 and 2002 March 17 - 18, respectively. Details concerning the two pointings are summarized in Table 1 of the reference paper. The nominal integration time was 42 ks for both observations. The three EPIC cameras were operated in full window mode. To prevent contamination of the X-ray images by the XUV and EUV emission of the optically and UV-bright sources in the field of view, the thick filter was used, which imposes a strong cut-off in the response at the lower energies. The X-ray data are merged with extant optical and near-infrared photometry, spectral classifications, H-alpha emission strengths, and rotation periods to examine the interrelationships between coronal and chromospheric activity, rotation, stellar mass, and internal structure for a statistically significant sample of pre-main-sequence stars. Out of the 316 distinct point-like sources that were detected at >= 3-sigma levels in one or more of six EPIC images, a total of 300 distinct X-ray sources can be identified with optical or near-infrared counterparts. The sources are concentrated within three regions of the cluster: in the vicinity of S Mon, within the large emission/reflection nebulosity southwest of S Mon, and along the broad ridge of molecular gas that extends from the Cone Nebula to the NGC 2264 IRS 2 field. From the extinction-corrected color-magnitude diagram of the cluster, ages and masses for the optically identified X-ray sources are derived. A median age of ~ 2.5 Myr and an apparent age dispersion of ~ 5 Myr are suggested by pre-main-sequence evolutionary models. The X-ray luminosity of the detected sources appears well-correlated with bolometric luminosity, although there is considerable scatter in the relationship. Stellar mass contributes significantly to this dispersion, while isochronal age and rotation do not. X-ray luminosity and mass are well correlated such that L<sub>X</sub> ~ (M/M<sub>solar</sub>)<sup>1.5</sup>, which is similar to the relationship found within the younger Orion Nebula Cluster. No strong evidence is found for a correlation between E(H-K), the near-infrared color excess, and the fractional X-ray luminosity, which suggests that optically thick dust disks have little direct influence on the observed X-ray activity levels. Among the X-ray-detected weak-line T Tauri stars, the fractional X-ray luminosity, L<sub>X</sub>/L<sub>bol</sub>, is moderately well correlated with the fractional H-alpha luminosity, L<sub>H(alpha)</sub>/L<sub>bol</sub>, but only at the 2-sigma level of significance. The cumulative distribution functions for the X-ray luminosities of the X-ray-detected classical and weak-line T Tauri stars within the cluster are comparable, assuming the demarcation between the two classes is at an H-alpha equivalent width of 10 Angstroms. However, if the non-detections in X-rays for the entire sample of H-alpha emitters known within the cluster are taken into account, then the cumulative distribution functions of these two groups are clearly different, such that classical T Tauri stars are underdetected by at least a factor of 2 relative to the weak-line T Tauri stars. Examining a small subsample of X-ray-detected stars that are probable accretors based on the presence of strong H-alpha emission and near-infrared excess, the authors conclude that definitive non-accretors are ~ 1.6 times more X-ray luminous than their accreting counterparts. In agreement with earlier published findings for the Orion Nebula Cluster, the authors find a slight positive correlation (valid at the 2-sigma confidence level) between L<sub>X</sub>/L<sub>bol</sub> and the rotation period in NGC 2264 stars. The lack of a strong anti-correlation between X-ray activity and rotation period in the stellar population of NGC 2264 suggests that either the deeply convective T Tauri stars are rotationally saturated or that the physical mechanism responsible for generating magnetic fields in pre-main-sequence stars is distinct from the one that operates in evolved main-sequence stars. This table was created by the HEASARC in September 2007 based on the electronic version of Table 2 from the reference paper which was obtained from the electronic AJ site. This is a service provided by NASA HEASARC .
XMM-Newton COSMOS X-Ray Point Source Catalog
This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg<sup>2</sup> of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg<sup>2</sup>. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml > 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s, ~9.3 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s and ~1.3 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s over 90% of the area (1.92 deg<sup>2</sup>) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively. This table was created by the HEASARC in April 2009 based on the electronic version of Table 3 from the paper which was obtained from the CDS (their catalog J/A+A/497/635 file catalog.dat). It was last updated in May 2010 to correct the source number for XMMU J100100.7+015947 to be XMMC 129, as indicated by SIMBAD. This is a service provided by NASA HEASARC .
X-ray models from "An XMM-Newton spectral survey of 12 µm selected galaxies - I. X-ray data"
<p>Copied table models that used to be hosted at http://astro.ic.ac.uk/mbrightman/home</p> <p>from publication: https://ui.adsabs.harvard.edu/abs/2011MNRAS.413.1206B</p>
ScienceDex guides
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
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International Brain Laboratory public data
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OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.