- ID:
- ivo://nasa.heasarc/xmmao
- Title:
- XMM-Newton Accepted Targets
- Short Name:
- XMMAO
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table contains the current target list of the X-ray Multi-Mirror Newton (XMM-Newton) mission including those in (i) the routine calibration plan, (ii) the Guaranteed Time Observation (GTO) program, (iii) the triggered target candidates or ToOs accepted for the First through the Twentieth-Fourth Announcements of Opportunity (AO-1 through AO-24) programs, (iv) the AO-1 through AO-24 Guest Observer (GO) program targets with priority A or B, (v) the AO-1 through AO-19 GO program targets with priority C which have been observed, (vi) the AO-20 through AO-24 GO program targets with priority C, and (vii) the targets granted by agreement of the ESA Director of Science and the National Space Agency of Japan, following the loss of the original Astro-E spacecraft. For complete and authoritative information on the XMM-Newton mission, policies, and data archive, refer to the web pages of the European Space Agency's (ESA's) XMM-Newton Science Operations Center at <a href="http://xmm.esac.esa.int/">http://xmm.esac.esa.int/</a> and of NASA's XMM-Newton Guest Observer Facility at <a href="http://heasarc.gsfc.nasa.gov/docs/xmm/xmmgof.html">http://heasarc.gsfc.nasa.gov/docs/xmm/xmmgof.html</a> Notice that all priority C targets from AOs 1 through 19 which were never observed by XMM-Newton (and hence have expired) have been removed from this table. To check which targets have either already been observed by XMM-Newton or are on the short-term schedule to be observed in the next few weeks, users should examine the <a href="/db-perl/W3Browse/w3table.pl?tablehead=name%3Dxmmmaster&Action=More+Options">XMMMASTER</a> table which is also contained in Browse. To find out which targets are currently scheduled to be observed in the next three months, the user should check the XMM-Newton Advanced Plan at <a href="http://xmm.esac.esa.int/external/xmm_sched/advance_plan.shtml">http://xmm.esac.esa.int/external/xmm_sched/advance_plan.shtml</a> While abstracts are available for most proposals, there are a number of targets for which the HEASARC lacks the corresponding abstracts: e.g., the abstracts for AO-2 Guest Observer targets which have non-US PIs are not available. This database table was last updated by the HEASARC in December 2024, when AO-24's accepted targets were added. <p> AO-23's accepted targets were added in November 2023. <p> AO-22's accepted targets were added in November 2022. <p> AO-21's accepted targets were added and AO-19's unobserved priority C targets were removed in December 2021. <p> AO-20's accepted targets were added and AO-18's unobserved priority C targets were removed in December 2020. <p> AO-19's accepted targets were added and AO-17's unobserved priority C targets were removed in April 2020. <p> In June 2019, many duplicate entries were removed. <p> AO-18's accepted targets were added and AO-16's unobserved priority C targets were removed in November 2018. <p> AO-17's accepted targets were added and AO-15's unobserved priority C targets were removed in November 2017. <p> AO-16's accepted targets were added and AO-14's unobserved priority C targets were removed in December 2016. <p> AO-15's accepted targets were added and AO-13's unobserved priority C targets were removed in December 2015. <p> In August 2015, proposal titles were added. <p> AO-14's accepted targets were added and AO-12's unobserved priority C targets were removed in December 2014. <p> AO-13's accepted targets were added and AO-11's unobserved priority C targets were removed in December 2013. <p> AO-12's accepted targets were added and AO-10's unobserved priority C targets were removed in December 2012. <p> AO-11's accepted targets were added and AO-9's unobserved priority C targets were removed in December 2011. <p> AO-10's accepted targets were added and AO-8's unobserved priority C targets were removed in December 2010. <p> AO-9's accepted targets were added and AO-7's unobserved priority C targets were removed in January 2010. <p> AO-8's accepted targets were added and AO-6's unobserved priority C targets were removed in December 2008. <p> AO-7's accepted targets were added and AO-5's unobserved priority C targets were removed in January 2008. <p> AO-6's accepted targets were added in January 2007, and, in November 2006, an effort was made to remove most of the unobserved priority C targets from previous AOs. This is a service provided by NASA HEASARC .
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- ID:
- ivo://nasa.heasarc/xmmbss
- Title:
- XMM-Newton Bright Serendipitous Survey
- Short Name:
- XMMBSS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 .
- ID:
- ivo://nasa.heasarc/xmmbssagn
- Title:
- XMM-Newton Bright Serendipitous Survey: AGN X-Ray Spectral Properties
- Short Name:
- XMMBSSAGN
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- X-ray surveys are a key instrument in the study of active galactic nuclei (AGN). Thanks to their penetrating ability, X-rays are able to map the innermost regions close to the central super massive black hole (SMBH) as well as to detect and characterize its emission up to high redshift. This table contains results from a detailed X-ray spectral analysis of the AGN belonging to the XMM-Newton Bright Serendipitous Survey (XBS, the HEASARC Browse XMMBSS table, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/IX/41">CDS Cat. IX/41</a>). The XBS is composed of two flux-limited samples selected in the complementary 0.5 to 4.5 and 4.5 to 7.5 keV energy bands and comprising more than 300 AGN up to redshift ~2.4. The authors have performed an X-ray analysis following two different approaches: by analyzing individually each AGN X-ray spectrum and by constructing average spectra for different AGN types. From the individual analysis, the authors find that there seems to be an anticorrelation between the spectral index and the sources' hard X-ray luminosity, such that the average photon index for the higher luminosity sources (>10<sup>44</sup> erg s<sup>-1</sup>) is significantly (>2 sigma) flatter than the average for the lower luminosity sources. They also find that the intrinsic column density distribution agrees with AGN unified schemes, although a number of exceptions are found (3% of the whole sample), which are much more common among optically classified type 2 AGN. The authors also find that the so-called "soft-excess", apart from the intrinsic absorption, constitutes the principal deviation from a power-law shape in AGN X-ray spectra and it clearly displays different characteristics, and likely a different origin, for unabsorbed and absorbed AGN. Regarding the shape of the average spectra, they find that it is best reproduced by a combination of an unabsorbed (absorbed) power law, a narrow Fe K-alpha emission line and a small (large) amount of reflection for unabsorbed (absorbed) sources. This table was created by the HEASARC in November 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/530/A42">CDS Catalog J/A+A/530/A42</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/xmmcfrsoid
- Title:
- XMM-Newton/Canada-France Redshift Survey Fields Optical Identifications
- Short Name:
- XMM/CFRSID
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the proposed identifications for all the good optical ID candidates (true probability value P' that the object is not associated of < 0.15) corresponding to the X-ray sources from the XMM-Newton surveys of the 3 and 14 hours Right Ascension (hereafter 3-h and 14-h, respectively) fields from the Canada-France Redshift Survey. (These fields are also known as the Groth Strip). The X-ray sources cover the 0.5 - 10 keV flux range from ~2 x 10<sup>-15</sup> - 10<sup>-13</sup> erg/cm<sup>2</sup>/s. The authors have used a subset of the XMM-Newton sources, which have Chandra positions, to determine the best method of obtaining optical identifications of sources with only XMM-Newton positions. They found optical identifications for 79% of the XMM-Newton sources for which there were deep optical images. The sources without optical identifications are likely to be optically fainter and have higher redshifts than the sources with identifications. The authors have estimated 'photometric redshifts' for the identified sources, calibrating their method using ~200 galaxies in the fields with spectroscopic redshifts. They find that the redshift distribution has a strong peak at z ~ 0.7. This table was created by the HEASARC in July 2005 based on the combination of CDS table J/MNRAS/350/785/tablea34.dat (the merged Tables A3 and A4 from the published paper) and CDS table J/MNRAS/350/785/tablea56.dat (the merged Tables A5 and A6 from the published paper). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/xmmcfrscat
- Title:
- XMM-Newton/Canada-France Redshift Survey Fields X-Ray Sources
- Short Name:
- XMM/CFRS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the X-ray source catalogs for the XMM-Newton surveys of the 3 and 14 hours Right Ascension (hereafter 3-h and 14-h, respectively) fields from the Canada-France Redshift Survey. (These fields are also known as the Groth Strip). The X-ray sources cover the 0.5-10 keV flux range from ~2 x 10<sup>-15</sup> - 10<sup>-13</sup> erg/cm<sup>2</sup>/s. The authors have used a subset of the XMM-Newton sources, which have Chandra positions, to determine the best method of obtaining optical identifications of sources with only XMM-Newton positions. They have found optical identifications for 79% of the XMM-Newton sources for which there were deep optical images. The sources without optical identifications are likely to be optically fainter and have higher redshifts than the sources with identifications. The authors have estimated 'photometric redshifts' for the identified sources, calibrating their method using ~200 galaxies in the fields with spectroscopic redshifts. They find that the redshift distribution has a strong peak at z~0.7. This table was created by the HEASARC in July 2005 based on CDS table J/MNRAS/350/785/tablea12.dat (the merged Tables A1 and A2 from the published paper). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/cfhtlsgxmm
- Title:
- XMM-Newton CFHTLS W1 Field Galaxy Groups Catalog
- Short Name:
- CFHTLSGXMM
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a catalog of 128 X-ray galaxy groups, covering a redshift (z) range 0.04 < z <1.23, selected in the ~ 3 deg<sup>2</sup> part of the CFHTLS W1 field overlapping XMM-Newton observations performed under the XMM-LSS project. The authors carry out a statistical study of the redshift evolution out to redshift 1 of the magnitude gap between the first and the second brightest cluster galaxies of a well defined mass-selected group sample. They find that the slope of the relation between the fraction of groups and the magnitude gap steepens with redshift, indicating a larger fraction of fossil groups at lower redshifts. They also find that 22.2% +/- 6% of their groups at z <= 0.6 are fossil groups. The authors compare their results with the predictions of three semi-analytic models based on the Millennium simulation. The intercept of the relation between the magnitude of the brightest galaxy and the value of magnitude gap becomes brighter with increasing redshift. This trend is steeper than the model predictions which the authors attribute to the younger stellar age of the observed brightest cluster galaxies. This trend argues in favor of stronger evolution of the feedback from active galactic nuclei at z < 1 compared to the models. The slope of the relation between the magnitude of the brightest cluster galaxy and the value of the gap does not evolve with redshift and is well reproduced by the models, indicating that the tidal galaxy stripping, put forward as an explanation of the occurrence of the magnitude gap, is both a dominant mechanism and sufficiently well modeled. In this study, the authors analyzed the XMM-Newton observations of the CFHTLS wide (W1) field as a part of the XMM-LSS survey (Pierre et al., 2007, MNRAS, 382, 279). The details of the observations and the data reduction are presented in Bielby et al. (2010, A&A, 523, A66). The authors concentrate on the low-z counterparts of the X-ray sources and use all XMM-Newton observations performed until 2009, covering an area of 2.276 x 2.276 square degrees. The CFHTLS wide observations were carried out in the period between 2003 and 2008, covering an effective survey area of ~ 154 square degrees. The optical images and data of the CFHTLS were obtained with the MegaPrime instrument mounted on the CFHT in the five filters u*, g', r', i' and z'. This table was created by the HEASARC in December 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/566/A140">CDS catalog J/A+A/566/A140</a> file table1.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/xcs
- Title:
- XMM-Newton Cluster Survey Catalog, DR1 Version
- Short Name:
- XCS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The XMM Cluster Survey (XCS) is a serendipitous search for galaxy clusters using all publicly available data in the XMM-Newton Science Archive. Its main aims are to measure cosmological parameters and trace the evolution of X-ray scaling relations. In their paper, the authors present the first data release from the XMM Cluster Survey (XCS-DR1). This consists of 503 optically confirmed, serendipitously detected, X-ray clusters. Of these clusters, 256 are new to the literature and 357 are new X-ray discoveries. They present 463 clusters with a redshift estimate (0.06 < z < 1.46), including 261 clusters with spectroscopic redshifts. The remainder have photometric redshifts. In addition, the authors have measured X-ray temperatures (kT<sub>X</sub>) for 401 clusters (0.4 < kT<sub>X</sub> < 14.7 keV). This table was created by the HEASARC in May 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/423/1024">CDS Catalog J/MNRAS/423/1024</a> file xcsdr1.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/xmmcphotz
- Title:
- XMM-Newton COSMOS (XMM-COSMOS) Survey Photometric Redshift Catalog
- Short Name:
- XMMCPHOTZ
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- In their paper, the authors release accurate photometric redshifts for 1692 counterparts to Chandra sources in the central square degree of the Cosmic Evolution Survey (COSMOS) field. The availability of a large training set of spectroscopic redshifts that extends to faint magnitudes enabled photometric redshifts comparable to the highest quality results presently available for normal galaxies. The authors demonstrate that morphologically extended, faint X-ray sources without optical variability are more accurately described by a library of normal galaxies (corrected for emission lines) than by active galactic nucleus (AGN) dominated templates, even if these sources have AGNlike X-ray luminosities. Preselecting the library on the bases of the source properties allowed them to reach an accuracy sigma[Delta-z/(1+Z<sub>spec</sub>)] ~ 0.015 with a fraction of outliers of 5.8% for the entire Chandra-COSMOS sample. These Chandra sources are not contained in this table but are available in the HEASARC table CCOSMPHOTZ). In addition, in this study the authors released revised photometric redshifts for the 1735 optical counterparts of the XMM-detected sources over the entire 2 deg<sup>2</sup> of COSMOS, and these are the sources listed in the present table. For 248 sources, their updated photometric redshift differs from the previous release by Delta-z > 0.2. These changes are predominantly due to the inclusion of newly available deep H-band^ photometry (H<sub>AB</sub> = 24 mag). The authors illustrate once again the importance of a spectroscopic training sample and how an assumption about the nature of a source together, with the number and the depth of the available bands, influences the accuracy of the photometric redshifts determined for AGN. These considerations should be kept in mind when defining the observational strategies of upcoming large surveys targeting AGNs, such as eROSITA at X-ray energies and the Australian Square Kilometre Array Pathfinder Evolutionary Map of the Universe in the radio band. This table contains the photometric redshifts and related quantities for 1735 XMM-Newton sources over the entire 2 square degrees of the COSMOS field. Notice that in the original as-published paper no positional information was provided. The HEASARC has assumed that the source numbers used in the present catalog are in the same source numbering scheme as used by Cappelluti et al. (2009, A&A, 497, 635, the XMM-Newton Wide-Field Survey in the COSMOS Field Point-like X-ray Source Catalog, available at the HEASARC as the XMMCOSMOS table) and thus obtained the positions and (position-based) names corresponding to these X-ray sources from the latter. This table was created by the HEASARC in November 2011 based on an electronic version of Table 5 from the reference paper which was obtained from the ApJ website. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/xmmcosmos
- Title:
- XMM-Newton COSMOS X-Ray Point Source Catalog
- Short Name:
- XMMCOSMOS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 .
- ID:
- ivo://nasa.heasarc/xmmcdfs510
- Title:
- XMM-Newton Deep Survey in the CDF-S 5-10 keV Source Catalog
- Short Name:
- XMMCDFS510
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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. 137 Sources detected in the 5-10 keV band by both programs are presented in the main table, while 61 5-10 keV sources only detected by PWXDetect are presented in the supplementary table. The 2-10 and 5-10 keV bands were analyzed separately. This HEASARC table contains the main sample of 137 sources detected in the 5-10 keV band in the XMM-CDFS survey. (The table of 2-10 keV XMM-CDFS sources is also available at the HEASARC as the XMMCDFS210 table.) This table does not include the 61 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 main510.dat and notes510.dat. This is a service provided by NASA HEASARC .
