- ID:
- ivo://nasa.heasarc/roshri
- Title:
- ROSAT Results Archive Sources for the HRI
- Short Name:
- ROSAT/HRI
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ROSHRI data table contains a list of sources detected by the Standard Analysis Software System (SASS) in reprocessed, public HRI datasets. In addition to the parameters returned by SASS (like position, count rate, signal-to-noise, etc.) each source in the table has associated with it a set of source and sequence "flags." These flags are provided by the ROSAT data centers in the US, Germany and the UK to help the user of the ROSHRI database table quickly judge the reliability of a given source. The ROSHRI table excludes sources that meet the following parameter criteria: false_det = 'T' or deferred = 'T' or not_checked = 'T' or un_unique ='T'. See the documentation below for descriptions of these parameters. These data have been screened by ROSAT data centers in the US, Germany, and the UK as a step in the production of the ROSAT Results Archive. The RRA contains extracted source and associated products with an indication of reliability for the primary parameters. This database table was last updated in August 2001. More information about the ROSAT Results Archive for HRI sources can be obtained at the following web pages: <pre> <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html</a> <a href="http://hea-www.harvard.edu/rosat/rra.html">http://hea-www.harvard.edu/rosat/rra.html</a> <a href="http://www.aip.de/groups/xray/rosat/rra.html">http://www.aip.de/groups/xray/rosat/rra.html</a> <a href="http://ledas-www.star.le.ac.uk/rra">http://ledas-www.star.le.ac.uk/rra</a> </pre> This is a service provided by NASA HEASARC .
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- ID:
- ivo://nasa.heasarc/rospspc
- Title:
- ROSAT Results Archive Sources for the PSPC
- Short Name:
- ROSAT/PSPC
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ROSPSPC database table contains a list of sources detected by the Standard Analysis Software System (SASS) in public, unfiltered, pointed PSPC datasets. In addition to the parameters returned by SASS (like position, count rate, likelihood, etc.) each source in the table has associated with it a set of source and sequence "flags." These flags are provided by the ROSAT data centers in the US, Germany and the UK to help the user of the ROSPSPC database table quickly judge the reliability of a given source. The ROSPSPC table excludes sources that meet the following parameter criteria: false_det = 'T' or deferred = 'T' or not_checked = 'T'. See the documentation below for descriptions of these parameters. The catalog consists of all primary source parameters from the automated detection algorithm employed by the SASS. In addition each observation has been quality checked, both by automatic algorithms and by detailed visual inspection. The results of this quality checking are contained as a set of logical-value flags for a set of principal source parameters. If a source parameter is suspect, the associated flag is set to "TRUE"; parameters with no obvious problems maintain the default, "FALSE", value. This database table was last updated in August 2001. More information about the ROSAT Results Archive for PSPC sources can be obtained at the following web pages: <pre> <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html</a> <a href="http://hea-www.harvard.edu/rosat/rra.html">http://hea-www.harvard.edu/rosat/rra.html</a> <a href="http://www.aip.de/groups/xray/rosat/rra.html">http://www.aip.de/groups/xray/rosat/rra.html</a> <a href="http://ledas-www.star.le.ac.uk/rra">http://ledas-www.star.le.ac.uk/rra</a> </pre> This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/rospspcf
- Title:
- ROSAT Results Archive Sources for the PSPC with Filter
- Short Name:
- ROSPSPCF
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table is derived from the Second ROSAT Source Catalog of Pointed Observations with the ROSAT PSPC (Roentgen Satellite Position-Sensitive Proportional Counter) Observed Using the Boron Filter, or the 2RXF Catalog. 2XRF contains arcsecond positions and count rates for 2,526 detected sources from 258 ROSAT PSPC Filter observations covering 0.15% of the sky, including 704 high-confidence detections and 20 obvious sources which were not detected by SASS. The complete version of the list of detections (the HEASARC's <a href="/W3Browse/rosat/rospspcftot.html">ROSPSPCFTOT</a>) table contains 2,526 entries, whereas the short 'high-confidence' version contained in this present table has 704 detection. The ROSPSPCF table excludes sources that meet the following parameter criteria: false_det = 'f' or deferred = 'D' or not_checked = 'n'. See the documentation below for descriptions of these parameters. The catalog consists of all primary source parameters from the automated detection algorithm employed by the SASS. In addition each observation has been quality checked, both by automatic algorithms and by detailed visual inspection. The results of this quality checking are contained as a set of logical-value flags for a set of principal source parameters. If a source parameter is suspect, the associated flag is set to a corresponding alphabetical value; parameters with no obvious problems maintain the default, '.', value. The Second ROSAT Pointed PSPC Filter Source Catalog includes missing sources, i.e. obvious sources which were not detected by the SASS source detection software but which could be easily detected by visual inspection. Missed sources are marked by negative values of their source identification number, i.e. the parameter 'MPLSX_ID' has a negative value for these sources. The only tabulated quantities for these visually identified missed sources are source positions; other quantities (like count rates, hardness ratios, etc.) are not available. These data have been screened by ROSAT data centers in the US, Germany, and the UK as a step in the production of the ROSAT Results Archive. The RRA contains extracted source and associated products with an indication of reliability for the primary parameters. More information about the ROSAT mission and the SASS can be obtained from the ROSAT User Handbook, available at <pre> <a href="http://heasarc.gsfc.nasa.gov/docs/rosat/rosdocs.html">http://heasarc.gsfc.nasa.gov/docs/rosat/rosdocs.html</a> </pre> This table was created by the HEASARC in May 2012 based on the file rospspcfcat-short.txt obtained from the MPE ROSAT Results Archive site (which is no longer available, unfortunately). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/orionxray
- Title:
- ROSAT Survey of the Orion Nebula
- Short Name:
- HRI/Orion
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This catalog presents some of the results from 3 deep ROSAT High Resolution Imager (HRI) observations of the Orion Nebula star-forming region. The fields covered by the X-ray images contain over 1500 catalogued stars in a roughly 0.8 square degree region centered on the Trapezium. In all, 389 distinct X-ray sources were detected, at least two-thirds of which were associated with a single proper-motion cluster member. X-ray emission was detected from stars of all spectral types, from the massive O- and B-type components of the Trapezium to the coolest, low-mass pre-main-sequence (PMS) stars. In the research paper in which these data were presented (Gagne et al. 1995), the authors focussed primarily on X-ray emission from the late-type PMS stars. Of the ~100 late-type cluster members with measured spectral types, approximately three-fourths were detected; the authors derived X-ray luminosity upper limits for the remaining stars. They found that coronal X-ray emission appeared to turn on at around a spectral type of F6, with the upper envelope of activity increasing with decreasing effective temperature. The current database is a concatenation of Tables 2 and 3 from Gagne et al. (1995) which list the 389 distinct X-ray sources and their candidate optical counterparts. A detection criterion of 3 sigma was used, i.e., a sigal-to-noise ratio criterion of 3. 324 of the X-ray sources have a single candidate optical counterpart, 50 of the X-ray sources (listed in Table 3 of the original paper) have multiple candidates for the optical counterparts, and the remainder have no optical counterparts. Notice that Table 6 of Gagne et al. (1995) which presents a compilation of optical and X-ray data for a sub-group of the Orion stars for which data on the spectral types and the spectroscopic rotational velocities or the photometric rotational periods are available is not part of this database. This database was created at the HEASARC in December 1997 based on a computer-readable version of Tables 2 and 3 of Gagne et al. (1995) that was obtained from the CDS (their catalog J/ApJ/445/280). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ros13hrcxo
- Title:
- ROSAT/XMM-Newton 13-hour Field Chandra X-Ray Source Catalog
- Short Name:
- ROS13HRCXO
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains some of the results from a Chandra ACIS-I survey of a high-latitude region at RA, Dec = 13 hours, +38 degrees which was earlier observed with ROSAT and which had recently been observed by XMM-Newton for 200 ks. XMM-Newton was expected to provide good-quality X-ray spectra for over 200 sources with fluxes around the knee of the log N /log S distribution, which are responsible for the bulk of the X-ray background. The main aim of the Chandra observations was to provide arcsecond, or better, positions, and hence reliable identifications, for the XMM-Newton sources. The ACIS-I observations were arranged in a mosaic of four 30-ks pointings, covering almost all of the 15-arcminute radius XMM-Newton/ROSAT field. 214 Chandra sources were detected above a Cash likelihood statistic of 25, which approximates to a 5-sigma significance, to a limiting flux of ~ 1.3 x 10<sup>-15</sup>erg/cm<sup>2</sup>/s (0.5 - 7 keV). Optical counterparts were derived from a Subaru SuprimeCam image reaching to R ~ 27. The very large majority of the Chandra sources have an optical counterpart, with the distribution peaking at 23 < R < 24, although 14 have no counterpart to R = 27. The fraction of X-ray sources with no identification brighter than R = 27 is similar to that found in deeper Chandra surveys. The majority of the identifications are with galaxies. As found in other Chandra surveys, there is a very wide range of optical magnitudes for a given X-ray flux, implying a range of emission mechanisms, and many sources have high L<sub>X</sub>/L<sub>opt</sub> ratios, implying absorption at moderate redshift. Comparison with the earlier ROSAT survey shows that the accuracy of the ROSAT positions agrees very well with the predictions from simulations by McHardy et al. and that the large majority of the identifications were correct. This table was created by the HEASARC in July 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/342/802">CDS Catalog J/MNRAS/342/802</a> files table2.dat and table5.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ros13hrvla
- Title:
- ROSAT/XMM-Newton 13-hr Deep Field VLA 20-cm Source Catalog
- Short Name:
- ROS13HRVLA
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- In order to determine the relationship between the faint X-ray and faint radio source populations, and hence to help understand the X-ray and radio emission mechanisms in those faint source populations, the authors have made a deep 1.4-GHz Very Large Array radio survey of the 13<sup>h</sup> 34<sup>m</sup> 37<sup>s</sup>, +37<sup>o</sup> 54' 44" (J2000) ROSAT/XMM-Newton X-ray Survey Area (McHardy et al. 1998, MNRAS, 295, 641; Loaring et al. 2005, MNRAS, 362, 1371: the catalog of XMM-Newton sources from the latter paper is available at the HEASARC as the ROS13HRXMM table). From a combined VLA data set of 10 hours of B-configuration data and 14 hours of A-configuration data, maps with 3.35-arcsec resolution and a noise limit of 7.5 microJansky (µJy) were constructed. A complete sample of 449 sources was detected within a 30-arcmin diameter region above a 4-sigma detection limit of 30 uJy, at the map center, making this one of the deepest radio surveys at this frequency. The differential source count shows a significant upturn at sub-milliJansky flux densities, similar to that seen in other deep surveys at 1.4 GHz (e.g. the Phoenix survey, Hopkins et al. 2003, AJ, 125, 465: available at the HEASARC as the PDS1P4GHZ table), but larger than that seen in the Hubble Deep Field (HDF) which may have been selected to be underdense. This upturn is well modeled by the emergence of a population of medium-redshift star-forming galaxies which dominate at faint flux densities. The brighter source counts are well modeled by active galactic nuclei. This HEASARC table contains the catalog of 449 radio sources in a region of 30-arcmin diameter centered on the ROSAT/XMM 13-hours field which were detected at 1.4 GHz (20 cm) above a detection threshold of 4 sigma, equivalent to 30 uJy at the phase center. This table was created by the HEASARC in July 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/352/131">CDS Catalog J/MNRAS/352/131</a> file table a1.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/rosatxuv
- Title:
- ROSAT XUV Pointed Phase
- Short Name:
- ROSAT/REP
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- We present a catalogue of XUV sources from observations by the Wide Field Camera (WFC) on ROSAT during the pointed phase. The ROSAT WFC is a telescope sensitive in the extreme UV range (17-210eV) which observes in parallel with the ROSAT X-Ray Telescope (XRT). The 5916 pointed observations processed are from the calibration and verification phase in June 1990 and from the period 9 Feb. 1991 to 15 July 1994. The catalogue contains 1022 independent source detections which correspond to 328 individual sources, many of which have been observed repeatedly. Each observation was done with one of four filters S1, S2, P1 and P2. Of the 328 sources 113 are new sources (they are not listed in the "2RE" catalogue) and 274 have been identified with optical counterparts. The catalogue contains coordinates, observed count rates, normalized source count rates and the proposed optical counterpart with its spectral class. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/rosettecxo
- Title:
- Rosette Molecular Cloud Chandra X-Ray Point Source Catalog
- Short Name:
- ROSETTECXO
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The authors of this study have explored the young stellar populations in the Rosette Molecular Cloud (RMC) region with high spatial resolution X-ray images from the Chandra X-ray Observatory, which are effective in locating weak-lined T Tauri stars as well as disk-bearing young stars. A total of 395 X-ray point sources are detected, 299 of which (76%) have an optical or near-infrared (NIR) counterpart identified from deep FLAMINGOS images. From X-ray and mass sensitivity limits, the authors infer a total population of ~1700 young stars in the survey region. Based on smoothed stellar surface density maps, they investigate the spatial distribution of the X-ray sources and define three distinctive structures and substructures within them. Structures B and C are associated with previously known embedded IR clusters, while structure A is a new X-ray-identified unobscured cluster. A high-mass protostar RMCX 89 = IRAS 06306+0437 and its associated sparse cluster are studied. The different subregions are not coeval but do not show a simple spatial-age pattern. Disk fractions vary between subregions and are generally <~ 20% of the total stellar population inferred from the X-ray survey. The data are consistent with speculations that triggered star formation around the H II region is present in the RMC, but do not support a simple sequential triggering process through the cloud interior. While a significant fraction of young stars are located in a distributed population throughout the RMC region, it is not clear if they originated in clustered environments. This HEASARC table contains the 348 primary sources listed in Table 1 of the reference paper, as well as the 47 tentative sources listed in Table 2 (the latter having a likelihood > 10<sup>-3</sup> of being a spurious background fluctuation based on Poisson statistics), to make a total of 395 X-ray sources. The information on optical and infrared counterparts to these X-ray sources which was provided in Table 4 of the reference paper has also been included herein. In order to allow users to clearly identify these 2 samples, the HEASARC has created a parameter source_sample which is set to 'P' for the Table 1 primary sources and to 'T' for the Table 2 tentative sources. This HEASARC table also contains the X-ray spectroscopic information derived for 158 sources which have photometric significance (the snr parameter) >= 2.0 which was presented in Table 3 of the reference paper. All spectral fits used the "wabs(apec)" model in XSPEC and assumed 0.3 * Z_Sun abundances. The quoted emission measures and X-ray luminosities assume a distance to the Rosette molecular cloud of 1.4 kpc. This table was created by the HEASARC in July 2009 based on the merger of electronic versions of tables 1, 2, 3 and 4 from the above reference which were obtained from the ApJ web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/roxa
- Title:
- ROXA (Radio-Optical-X-ray at ASDC) Blazars Catalog
- Short Name:
- ROXA
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Although blazars are a small fraction of the overall AGN population, they are expected to be the dominant population of extragalactic sources in the hard X-ray and gamma-ray bands and have been shown to be the largest contaminant of CMB fluctuation maps. So far the number of known blazars is of the order of several hundreds, but the forthcoming AGILE, GLAST and Planck space observatories will detect several thousand of objects of this type. In preparation for these missions it is necessary to identify new samples of blazars to study their multi-frequency characteristics and statistical properties. The authors have compiled a sample of objects with blazar-like properties via a cross-correlation between large radio (NVSS, ATCAPMN) and X-ray surveys (RASS) using the SDSS-DR4 and 2dF survey data to spectroscopically identify their candidates and test the validity of the selection method. They present the Radio-Optical-X-ray catalog built at ASDC (ROXA), a list of 816 objects among which 510 are confirmed blazars. Only 19% of the candidates turned out to be certainly non-blazars, demonstrating the high efficiency of our selection method. This catalog includes 173 new blazar identifications, or about 10% of all presently known blazars. The relatively high flux threshold in the X-ray energy band (given by the RASS survey) preferentially selects objects with high F_X/F_r ratio, leading to the discovery of new High Energy Peaked BL Lac (HBLs). This catalog therefore includes many new potential targets for GeV-TeV observations. The selection method consisted of three steps: 1) a first cross-correlation between radio and X-ray surveys (the NRAO VLA Sky Survey, ATCAPMN (ATCA catalogue of compact PMN sources) and ROSAT All Sky Survey; 2) for each radio/X-ray match, optical magnitudes were retrieved from the Guide Star Catalog; 3) for all radio/optical/X-ray matches the authors calculated the X-ray to optical (alpha_ox) and radio to optical (alpha_ro) spectral slopes and took only sources with alpha_ox and alpha_ro values within the blazar area. For each object, redshift, B and G magnitudes, radio fluxes at 1.4 GHz and at 5 GHz, X-ray flux, F_X/F_r ratio, X-ray luminosity, radio luminosity, Ca H&K break and classification are given. This table was created by the HEASARC in November 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/472/699">CDS catalog J/A+A/472/699</a> file catalog.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/sacy
- Title:
- SACY (Search for Associations Containing Young Stars) Catalog
- Short Name:
- SACY
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The SACY (Search for Associations Containing Young Stars) Catalog contains the results from a high-resolution optical spectroscopic survey aimed to search for nearby young associations and young stars among optical counterparts of ROSAT All-Sky Survey X-ray sources in the Southern Hemisphere. 1953 late-type (B-V>=0.6), potentially young, optical counterparts were selected out of a total of 9574 1RXS sources for follow-up observations. At least one high-resolution spectrum was obtained for each of 1511 targets. This paper is the first in a series presenting the results of the SACY survey in which the sample of X-ray selected stars and the supporting optical observations are described. The SACY sample is defined by Hipparcos (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/239">CDS Cat. <I/239></a>) and Tycho-2 (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/259">CDS Cat. <I/259></a>) stars within an error radius of 2.6 times the positional error of the ROSAT All-Sky Bright Source Catalogue (1RXS, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/IX/10">CDS Cat. <IX/10></a>). The used cut-off (B-V=0.6), corresponding approximately to a G0 dwarf, is near the hottest stars where the strength of the LiI line can be used as an youth indicator. All Hipparcos stars having M_v < 2.0 have been excluded. The northern boundary limits of the survey are given in Table 1 of the reference paper. In addition to the 1511 stars observed at least once, 115 stars with data taken from the literature have been added in order to complement the sample. In addition to these 1626 stars in the SACY sample (sources with source number prefixes of 'S'), entries for 165 other observed stars (sources with source number prefixes of 'O') are also included in this table. Most of the spectroscopic observations (~70%) were performed with the FEROS spectrograph at the 1.5m/ESO telescope at La Silla between January 1999 and September 2002 (ON-ESO agreement and ESO program identification 67.C-0123). Two more runs (ESO program identifications 072.C-0393 and 077.C-0138) were carried out at the 2.2m/ESO telescope. Another set of data (~30%) was collected at the coude spectrograph attached to 1.60m telescope at the Observatorio rio do Pico dos Dias (OPD), LNA, Brazil. Some spectra are a re-analysis of the ones taken for the PDS program. A few observations were collected using the CORALIE attached to the Swiss Euler Telescope at La Silla. UBV(RI)c photometry for part of the sample was obtained using FOTRAP at the 0.60m Zeiss telescope of the OPD. When a star was not observed photometrically by the authors, they tried to obtain some useful photometric data from the Hipparcos and Tycho Catalogues or in the available literature in the SIMBAD. For multiple stars, magnitudes and colors were corrected in order to take into account the presence of the companion(s). This table was created by the HEASARC in March 2007 based on the CDS table J/A+A/460/695, files table3.dat and table4.dat This is a service provided by NASA HEASARC .
