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XMM-Newton Accepted Targets
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
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XTEProposalInfo&Abstracts
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The XTEAO database table contains the official observing program for the Rossi X-Ray Timing Explorer (RXTE) satellite. This list contains the targets recommended by the review panels for the various Cycles of Guest Observer (GO) proposals up to and including Cycle 15. Notice that not all entries in this list will actually be observed, since it includes observations of Targets of Opportunity (ToOs) which may never be triggered. Also note that multiple pointings at a particular target are permitted. This database table was updated by the HEASARC periodically, based on information provided by the RXTE Guest Observer Facility (GOF). This is a service provided by NASA HEASARC .
NGC 2264 XMM-Newton X-Ray Point Source Catalog
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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 LX ~ (M/Msolar)1.5, 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, LX/Lbol, is moderately well correlated with the fractional H-alpha luminosity, LH(alpha)/Lbol, 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 LX/Lbol and the rotation period in NGC 2264 stars. The lack of a strong
XMM-Newton Galactic Plane Survey - XGPS
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This table contains the first results from the XMM-Newton Galactic Plane Survey (XGPS). In the first phase of the program, 22 pointings were used to cover a region of approximately 3 square degrees between 19 and 22 degrees in Galactic Longitude and +/-0.6 degrees in Galactic Latitude. In total, over 400 point X-ray sources have been resolved at >=5-sigma significance, down to a flux limit of ~2 x 10-14 erg/s/cm2 (2-10 keV). The sources exhibit a very wide range of spectral hardness, with interstellar absorption identified as a major influence. The source populations detected in the soft (0.4 - 2 keV) band and hard (2 - 6 keV) band show surprisingly little overlap. The majority of the soft sources appear to be associated with relatively nearby stars with active stelaar coronae, judging from their high coincidence with bright stellar counterparts. The combination of the XGPS measurements in the hard X-ray band with the results from earlier surveys carried out by ASCA and Chandra reveals the form of the low-latitude X-ray source counts over 4 decades of flux. It appears that extragalactic sources dominate below ~10-13 erg/s/cm2 (2-10 keV), with a predominantly Galactic source population present above this flux threshold. The nature of the faint Galactic population observed by XMM-Newton remains uncertain, although cataclysmic variables and RS CVn systems may contribute substantially. This table was created by the HEASARC in February 2005 based on CDS Catalog J/MNRAS/351/31/tablea1.dat. This is a service provided by NASA HEASARC .
XMM-Newton Optical Monitor SUSS Catalog, v6.1: Observation IDs
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The 2023 release of the XMM OM Serendipitous Ultraviolet Source Survey (XMM-SUSS6.1) Catalog, a catalog of optical/UV sources detected by the Optical Monitor (OM) on-board the European Space Agency's (ESA's) XMM-Newton observatory, spans the period of observations from 2000 to November 2022. The data processing was performed at the European Space Astronomy Centre (ESAC, Madrid, Spain) using the XMM Science Analysis Software system (SAS) versions 18 and 19. In addition to covering a larger observation period, this sixth release reflects a change in philosophy with regard to the origin of the incorporated data. In previous releases, the data were generated via a bespoke processing of the OM Observation Data Files (ODFs) while in this new release, the catalog has been guided by the XMM user community and the authors have sought to harmonize the contents of the catalog with those of the OM data in the XMM-Newton Science Archive (XSA), which derive from the standard XMM-Newton pipeline processing system. While the bespoke processing and pipeline systems are fundamentally very similar, they are not identical and the differences lead to some differences in the output. The number of observations (OBSIDs) included in the catalog is 12,057. This table (XMMOMSUOB) contains the list of these observations and their characteristics, giving for each observation the filters used, the exposure time for each filter, the number of sources detected in each filter and the detection magnitude limit for each filter. The total number of entries in this release is 9,920,390. They correspond to 6,659,554 unique sources, of which 1,225,117 have multiple entries in the source table, corresponding to different observations. This list of sources is available at the HEASARC as the XMMOMSUSS table. The documentation on the first release of this catalog is available at http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/Summary.shtml. This HEASARC database table contains the sixth release of the XMM-OM SUSS catalog, XMM-SUSS6.1, released by ESA in October 2023, obtained from the XMM-Newton Science Archive (http://xmm.esac.esa.int/xsa), and ingested into the HEASARC database in October 2023. It is also available at the HEASARC as the gzipped FITS file https://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/XMM-OM-SUSS6-1.1.fits.gz. This is a service provided by NASA HEASARC .
XMM-Newton Optical Monitor Serendipitous UV Source Survey Catalog, v6.1
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The 2023 release of the XMM OM Serendipitous Ultraviolet Source Survey (XMM-SUSS6.1) Catalog, a catalog of optical/UV sources detected by the Optical Monitor (OM) on-board the European Space Agency's (ESA's) XMM-Newton observatory, spans the period of observations from 2000 to November 2022. The data processing was performed at the European Space Astronomy Centre (ESAC, Madrid, Spain) using the XMM Science Analysis Software system (SAS) versions 18 and 19. In addition to covering a larger observation period, this sixth release reflects a change in philosophy with regard to the origin of the incorporated data. In previous releases, the data were generated via a bespoke processing of the OM Observation Data Files (ODFs) while in this new release, the catalog has been guided by the XMM user community and the authors have sought to harmonize the contents of the catalog with those of the OM data in the XMM-Newton Science Archive (XSA), which derive from the standard XMM-Newton pipeline processing system. While the bespoke processing and pipeline systems are fundamentally very similar, they are not identical and the differences lead to some differences in the output. The number of observations (OBSIDs) included in the catalog is 12,057. The total number of entries in this release is 9,920,390. They correspond to 6,659,554 unique sources, of which 1,225,117 have multiple entries in the source table, corresponding to different observations. For each entry, positional and photometric data (count rate, magnitude and flux) and quality flags for each measurement are provided. The description of the previous release of the catalog can be found in Page M.J. et al. (2012, MNRAS, 426, 903). U, B, V, UVW2, UVM2 and UVW1 refer to the filter bandpasses defined in the Source Properties: Filter Set section of the MSSL documentation for this catalog: http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/SourcePropertiesFilters.shtml. There is a second, related table which gives a summary of the observations from which the XMM-SUSS6.1 sources listed in this table have been detected and measured. That summary table is available at the HEASARC as the XMMOMSUOB table. This HEASARC database table contains the sixth release of the XMM-OM SUSS catalog, XMM-SUSS6.1, released by ESA in October 2023, obtained from the XMM-Newton Science Archive (http://xmm.esac.esa.int/xsa), and ingested into the HEASARC database in October 2023. It is also available at the HEASARC as the gzipped FITS file https://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/XMM-OM-SUSS6-1.1.fits.gz. This is a service provided by NASA HEASARC .
Chandra Observations
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This database table contains all of the observations made by the Chandra X-Ray Observatory (CXO, formerly known as the Advanced X-ray Astrophysics Facility or AXAF) as part of the Performance Verification and Calibration (PVC) phase and also contains all of the subsequent Cycles' Guaranteed Time Observers (GTO) and General Observer (GO) targets, and any Director's Discretionary Time (DDT) targets that have been observed. It also includes scheduled and as-yet-not-scheduled targets. The HEASARC updates this database table on a twice-weekly basis by querying the database table at the Chandra X-Ray Center (CXC) website, as discussed in the Provenance section. For observations whose status is 'archived', data products can be retrieved from the HEASARC's mirror of the CXC's Chandra Data Archive (CDA). The CXC should be acknowledged as the source of Chandra data. The PVC phase was during the first few months of the CXO mission; some of the calibration observations that are for monitoring purposes will be performed in later mission cycles. All calibration data (entries with Type = CAL in this database) are placed immediately into the CXO public data archive at the Chandra X-Ray Observatory Center (CXC); please see the Web page at http://asc.harvard.edu/ for more information on the CXC data archive). GTO observations during Cycle 1 or any subsequent Cycle will probably occupy 100% of months 3-4, 30% of months 5-22, and 15% of the available time for the remainder of the mission. Guaranteed Time Observers will have the same proprietary data rights as General Observers (i.e., their data will be placed in the public CXC archive 12 months after they have received the data in usable form). For detailed information on the Chandra Observatory and datasets see:
 http://cxc.harvard.edu/ for general Chandra information http://cxc.harvard.edu/cda/ for the Chandra Data Archive http://cxc.harvard.edu/cal/ for calibration information http://cxc.harvard.edu/caldb/ for the calibration database http://cxc.harvard.edu/ciao/ for data analysis http://cxc.harvard.edu/ciao/download/ for analysis software http://cxc.harvard.edu/ciao/threads/ for analysis threads http://cda.harvard.edu/chaser/ for WebChaSeR 
The HEASARC updates this database table on a twice-weekly basis based on information obtained from the Chandra Data Archive at the CXC website. This is a service provided by NASA HEASARC .
XMM-Newton 2XMMi-DR3 Selected Source Detections Catalog
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The authors have carried out a classification of 4,330 X-ray sources in the 2XMMi-DR3 catalog. The sources were selected under the requirement of being a point source with multiple XMM-Newton observations and at least one detection with a signal-to-noise ratio larger than 20. For about one-third of the sources, the authors are able to obtain reliable source types from the literature. They mostly correspond to various types of stars (611), active galactic nuclei (AGNs, 753), and compact object systems (138) containing white dwarfs, neutron stars, and stellar-mass black holes. The authors find that about 99% of stars can be separated from other source types based on their low X-ray-to-IR flux ratios and frequent X-ray flares. AGNs have remarkably similar X-ray spectra, with the power-law photon index centered around 1.91 +/- 0.31, and their 0.2-4.5 keV flux long-term variation factors have a median of 1.48, with 98.5% being less than 10. In contrast, 70% of compact object systems can be very soft or hard, highly variable in X-rays, and/or have very large X-ray-to-IR flux ratios, separating them from AGNs. Using these results, the authors derive a source type classification scheme to classify the other sources and find 644 candidate stars, 1,376 candidate AGNs, and 202 candidate compact object systems, whose false identification probabilities are estimated to be about 1%, 3%, and 18%, respectively. There are still 320 sources associated with nearby galaxies and 151 in the Galactic plane, which the authors expect to be mostly compact object systems or background AGNs. There are also 100 candidate ultraluminous X-ray sources. They are found to be much less variable than other accreting compact objects. This table contains the list of 19,637 detections of the 4,330 unique X-ray sources which comprise the authors' sample. The list of 4,330 unique X-ray sources and their classifications is also available as the HEASARC XMMSSCLWBS table. This table was created by the HEASARC in October 2012 based on an electronic version of Table 3 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
XRISM Master Catalog
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The X-Ray Imaging and Spectroscopy Mission (XRISM) is an international mission led by Institute of Space and Astronautical Science (ISAS) of Japan Aerospace Exploration Agency (JAXA). XRISM was launched on 2023 September 6 (UT) into a near-circular orbit with an apogee of ~575 km, an inclination of ~31 degrees, and an orbital period of about 96 minutes. During the performance verification (PV) phase, targets selected by the XRISM science team are being observed. Subsequently, it will become a general observatory with annual call for proposals open to all astronomers. XRISM has two co-aligned instruments that are used concurrently: Resolve, a soft X-ray spectrometer, and Xtend, a wide field-of-view imager. Resolve uses an X-ray microcalorimeter with ~5 eV spectral resolution withs a 3x3 arcmin field of view. It is currently operating with the Gate Valve closed, which limits its effective bandpass to 1.7-12 keV. Xtend is an X-ray CCD instrument with a 38 x 38 arcmin2 field of view. This table contains a list of observations that have taken place as well as those that have been accepted and planned. The latter includes pre-approved targets for TOO observations and priority C targets whose observations are not guaranteed. This database table is based on information supplied by the XRISM Science Data Center at NASA/GSFC. It is updated automatically on a regular basis. This is a service provided by NASA HEASARC .
XMM-Newton Slew Survey Full Source Catalog, v3.0
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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 XMMSL3 Users Guide. 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: http://xmmssc.irap.omp.eu/Catalogue/XMMSL3/xmmsl3_v1.0.fits (the total sample).

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 .

Marano Field XMM-Newton X-Ray Source Optical Counterparts
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This table contains some of the results from a medium deep XMM-Newton survey of the Marano Field and optical follow-up observations. The mosaicked XMM-Newton pointings in this optical quasar survey field cover 0.6 deg2 with a total of 120 ks good observation time. 328 X-ray sources were detected in total with detection likelihoods ML >= 5. The X-ray fluxes are in the range fX = (0.16 - 54) x 10-14 erg cm-2 s-1 (0.2 - 10 keV). The turnover flux of this sample is fX ~ 5 x 10-15 erg/cm2/s in this same energy band. With VLT FORS1 and FORS2 spectroscopy 96 new X-ray counterparts have been classified. The central 0.28 deg2 region, where detailed optical follow-up observations were performed, contains ~ 170 X-ray sources (detection likelihood ML > 10), out of which 48 had already been detected by ROSAT. In this region 23 out of 29 optically selected quasars have been recovered. With a total of 110 classifications in their core sample, the authors have reached a completeness of ~65%. About one-third of the XMM-Newton sources are classified as type II AGN with redshifts mostly below 1.0. Furthermore, five high redshift type II AGN (2.2 <= z <= 2.8) have been detected. This table contains the list of the 195 optical counterparts for 172 of the XMM-Newton X-ray sources given in Table 8 of the reference paper. It does not contain the full list of 328 X-ray sources given in Table A1 of the reference paper, nor the lists of marginal X-ray sources given in Appendix B of the reference paper. This table was created by the HEASARC in May 2007 based on CDS catalog J/A+A/466/41 file table8.dat. This is a service provided by NASA HEASARC .