- ID:
- ivo://nasa.heasarc/ppm
- Title:
- Positions and Proper Motions Catalog
- Short Name:
- PPM
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The PPM database is the Catalog of Positions and Proper Motions. It combines the two catalogs for PPM North and PPM South, the Bright Stars Supplement to PPM, and the 90,000 Stars Supplement to the PPM. The PPM North list gives positions and proper motions of 181731 stars north of -2.5 degrees declination. PPM South gives positions and proper motions of 197179 stars south of about -2.5 degrees declination. The star density of PPM South is slightly higher than that of its northern counterpart and the accuracy of the present-epoch positions is roughly twice that in the north. A number of bright stars are missing from the PPM and PPM South Star Catalogs. The Bright Stars Supplement included here makes the PPM catalogs complete down to V=7.5 mag. For this purpose it adds all missing stars brighter than V=7.6 mag that could be found in published star lists. Their total number is 321. Only 5 of them are brighter than V=3.5 Since its appearance in 1966, the SAO Catalogue has been the primary source for stellar positions and proper motions. Typical values for the rms errors are 1 arcsec in the positions at epoch 1990, and 1.5 arcsec/century in the proper motions. The corresponding figures for the AGK3 Catalog in the northern hemisphere are 0.45 arcsec and 0.9 arcsec/century. Common to both of these catalogues is the fact that proper motions are derived from two observational epochs only, and that positions are nominally in the B1950/FK4 coordinate system. The PPM Star Catalogue (Roeser and Bastian, 1991, Bastian et al., 1993; for a short description see Roeser and Bastian, 1993) effectively replaced these catalogues by providing more precise astrometric data for more stars on the J2000/FK5 coordinate system. Compared to the SAO Catalogue the improvement in precision is about a factor of 3 on the northern and a factor of 6 to 10 on the southern hemisphere. In addition, the number of stars is increased by about 50 percent. Typical values for the rms errors on the northern hemisphere are 0.27 arcsec in the positions at epoch 1990, and 0.42 arcsec/century in the proper motions. On the southern hemisphere PPM is much better, the corresponding figures being 0.11 arcsec and 0.30 arcsec/century. The improvement over the SAO Catalogue was made possible by the advent of new big catalogues of position measurements and by the inclusion of the century-old Astrographic Catalogue (AC) into the derivation of proper motions. The AC contains roughly four million stars that are not included in PPM. For most of them no precise modern-epoch position measurements exist. Thus it is not yet possible to derive proper motions with PPM quality for all AC stars. But among the 4 million there is a subset of some 100,000 CPC-2 stars that are not included in PPM. These stars constitute the 90,000 Stars Supplement to PPM, and can be identified from their PPM Number having a value between 700001 and 789676. This database was updated by the HEASARC in October 1999 based on ADC/CDS catalogs I/146 (PPM - North), I/193 (PPM - South), I/206 (Bright Stars Supplement to PPM), and I/208 (90,000 Stars Supplement to PPM). This is a service provided by NASA HEASARC .
Number of results to display per page
Search Results
- ID:
- ivo://nasa.heasarc/ppmxlbmd
- Title:
- PPM-XL Bright M Dwarfs Catalog
- Short Name:
- PPMXLBMD
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Using the Position and Proper Motion Extended-L (PPMXL) catalog, the authors have used optical and near-infrared color cuts together with a reduced proper motion cut to find bright M dwarfs for future exoplanet transit studies. PPMXL's low proper-motion uncertainties allow them to probe down to smaller proper motions than previous similar studies. The authors have combined unique objects found with this method to that of previous work to produce 8,479 K < 9th magnitude M dwarfs. Low-resolution spectroscopy was obtained of a sample of the objects found using this selection method to gain statistics on their spectral type and physical properties. Results show a spectral-type range of K7 to M4V. This catalog is the most complete collection of K < 9 M dwarfs currently available and is made available herein. The PPMXL catalog (Roeser et al. 2010) represents a combination of the USNO-B1.0 and Two Micron All-Sky Survey (2MASS) catalogs mapped on to the International Celestial Reference Frame (ICRF), which allows proper motions to be described in a quasi-absolute manner as opposed to relative. PPMXL now provides low uncertainties for both the proper motion and position for many of the objects within the two catalogs. Typical uncertainties for proper motions are 4 - 10 mas/yr. The NIR JHK magnitudes from 2MASS and the optical BVRI magnitudes from USNO-B1.0 also provide very useful color information about the objects and are used during the sample selection process. In this work, the authors classified 4,054 M dwarfs with magnitudes of K < 9 from the PPMXL catalog. By probing down to lower proper motions, this work has produced 1,193 new bright M dwarf candidates that were not included in previous catalogs. By combining these objects with M dwarfs from Lepine & Gaidos (2011, AJ, 142, 138) the authors obtained a final catalog with 8,479 K < 9 late K and M dwarfs suitable for future exoplanet transit studies. This table was created by the HEASARC in February 2015 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/435/2161">CDS Catalog J/MNRAS/435/2161</a> file table3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/pgc2003
- Title:
- Principal Galaxy Catalog (PGC) 2003
- Short Name:
- PGC
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec<sup>2</sup>, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, <a href="http://leda.univ-lyon1.fr/">http://leda.univ-lyon1.fr/</a>. This table was created by the HEASARC in July 2004 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/237">CDS catalog VII/237</a> file pgc.dat.gz. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/pspc2
- Title:
- PSPC summed pointed observations, 2 degree cutoff, Intensity
- Short Name:
- PSPC2
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ROSAT PSPC surveys were generated by <i> SkyView </i> as mosaics from publically available PSPC observations. The surveys include all data available through March 1, 1997. This includes the vast majority of ROSAT PSPC observations. Filter observations and observations taken during the verification phase in 1991 were not included in either set. The details of the generation of the surveys are discussed in a <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> companion document</a>. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two. <p> The smaller cut-offs allow users to distinguish point sources in fields where a bright source may have been towards the edge of one observation and near the center of another. In these cases the source appears fuzzy due to the poor resolution of ROSAT near the edge of the field of view. This comes at the cost of a substantial reduction in the fraction of the sky covered. Counts and exposure maps are included for users who may need this information (<i>e.g.</i>, to do statistical analysis). <p> The global organization of the surveys is similar to the IRAS survey. Each map covers an area of 2.5&#176;;x2.5&#176;; with a minimum overlap of 0.25&#176;;. To cover the entire sky would require over 10,000 maps. However due to lack of coverage only approximately 4000-6000 maps are actually populated. Users asking for reqions where there is no ROSAT coverage may get a blank region returned. <p> Detailed information regarding the creation of the ROSAT suveys can be found in the <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> ROSAT PSPC Generation Document</a>. Provenance: Observational data from NASA Goddard Space Flight Center, mosaicking of images done by <i>SkyView</i>.. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/pspc0.6int
- Title:
- PSPC summed pointed observations, 0.6 degree cutoff, Intensity
- Short Name:
- PSPC0.6Int
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ROSAT PSPC surveys were generated by <i> SkyView </i> as mosaics from publically available PSPC observations. The surveys include all data available through March 1, 1997. This includes the vast majority of ROSAT PSPC observations. Filter observations and observations taken during the verification phase in 1991 were not included in either set. The details of the generation of the surveys are discussed in a <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> companion document</a>. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two. <p> The smaller cut-offs allow users to distinguish point sources in fields where a bright source may have been towards the edge of one observation and near the center of another. In these cases the source appears fuzzy due to the poor resolution of ROSAT near the edge of the field of view. This comes at the cost of a substantial reduction in the fraction of the sky covered. Counts and exposure maps are included for users who may need this information (<i>e.g.</i>, to do statistical analysis). <p> The global organization of the surveys is similar to the IRAS survey. Each map covers an area of 2.5&#176;;x2.5&#176;; with a minimum overlap of 0.25&#176;;. To cover the entire sky would require over 10,000 maps. However due to lack of coverage only approximately 4000-6000 maps are actually populated. Users asking for reqions where there is no ROSAT coverage may get a blank region returned. <p> Detailed information regarding the creation of the ROSAT suveys can be found in the <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> ROSAT PSPC Generation Document</a>. Provenance: Observational data from NASA Goddard Space Flight Center, mosaicking of images done by <i>SkyView</i>.. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/pspc1
- Title:
- PSPC summed pointed observations, 1 degree cutoff, Intensity
- Short Name:
- PSPC1
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The ROSAT PSPC surveys were generated by <i> SkyView </i> as mosaics from publically available PSPC observations. The surveys include all data available through March 1, 1997. This includes the vast majority of ROSAT PSPC observations. Filter observations and observations taken during the verification phase in 1991 were not included in either set. The details of the generation of the surveys are discussed in a <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> companion document</a>. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two. <p> The smaller cut-offs allow users to distinguish point sources in fields where a bright source may have been towards the edge of one observation and near the center of another. In these cases the source appears fuzzy due to the poor resolution of ROSAT near the edge of the field of view. This comes at the cost of a substantial reduction in the fraction of the sky covered. Counts and exposure maps are included for users who may need this information (<i>e.g.</i>, to do statistical analysis). <p> The global organization of the surveys is similar to the IRAS survey. Each map covers an area of 2.5&#176;;x2.5&#176;; with a minimum overlap of 0.25&#176;;. To cover the entire sky would require over 10,000 maps. However due to lack of coverage only approximately 4000-6000 maps are actually populated. Users asking for reqions where there is no ROSAT coverage may get a blank region returned. <p> Detailed information regarding the creation of the ROSAT suveys can be found in the <a href="https://skyview.gsfc.nasa.gov/help/pspc_generation.html"> ROSAT PSPC Generation Document</a>. Provenance: Observational data from NASA Goddard Space Flight Center, mosaicking of images done by <i>SkyView</i>.. This is a service of NASA HEASARC.
727. Pulsar Catalog
- ID:
- ivo://nasa.heasarc/pulsar
- Title:
- Pulsar Catalog
- Short Name:
- Taylor
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database is based on the 1995 May 3 electronic version of the Taylor et al. Pulsar Catalog and contains data on 706 pulsars, i.e., it contains 25% more entries than the version published by Taylor et al. in 1993 ApJS. The HEASARC obtained this electronic version from the Princeton University FTP site. This is a service provided by NASA HEASARC .
728. PVO Gamma-Ray Bursts
- ID:
- ivo://nasa.heasarc/pvogrb
- Title:
- PVO Gamma-Ray Bursts
- Short Name:
- PVOGRB
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This catalog gives information on the triggered events detected by the PVO instrument from 1978-09-14 to 1988-07-21. The table was taken from the Ph.D. thesis of Kuan-Wen Chuang (UC-Riverside, 1990). The data originates from the Ph.D. thesis of Kuan-Wen Chuang (UC-Riverside, 1990). The current version of this database table was created by the HEASARC in August 2002, replacing the previous version (named PVOTRIG) in which the times were somewhat inaccurate. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ecdfsrssam
- Title:
- Radio-Selected Extended Chandra Deep Field South Source Catalog
- Short Name:
- ECDFSRSSAM
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- In order to trace the instantaneous star formation rate (SFR) at high redshift, and thus help in understanding the relation between the different emission mechanisms related to star formation, the authors have combined the recent 4-Ms Chandra X-ray data and the deep Very Large Array radio data in the Extended Chandra Deep Field-South (E-CDF-S) region. They find 268 sources detected both in the X-ray and radio bands. The availability of redshifts for ~ 95% of the sources in their sample allows them to derive reliable luminosity estimates and the intrinsic properties from X-ray analysis for the majority of the objects. The present table lists the X-ray properties and redshifts of these 268 radio-selected sources. In the E-CDF-S area, the authors have two sets of X-ray data obtained with Chandra. The most important is a 4-Ms exposure observation resulting from the co-addition of 54 individual Chandra ACIS-I exposures from 1999 October to 2010 July, with centers spaced within a few arcseconds of RA = 03:32:28.80, Dec = -27:48:23 (J2000). The authors use the data from the new VLA program which provides deep, high-resolution 1.4-GHz imaging across the full E-CDF-S, consisting of a six-pointing mosaic of 240 h spanning 48 d of individual 5-h observations (Miller et al., 2008, ApJS, 179, 114). The E-CDF-S area has been targeted by a large number of spectroscopic surveys. For the X-ray sources, the authors use the spectroscopic redshifts published in Xue et al. (2011, ApJS, 195, 10). This table was created by the HEASARC in May 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/420/2190">CDS Catalog J/MNRAS/420/2190</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/rssgrbag
- Title:
- Radio-Selected Gamma-Ray Burst Afterglow Catalog
- Short Name:
- RSSGRBAG
- Date:
- 21 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a catalog of radio afterglow observations of gamma-ray bursts (GRBs) over a 14 year period from 1997 to 2011. This sample of 304 afterglows consists of 2,995 flux density measurements (including upper limits) at frequencies between 0.6 GHz and 660 GHz, with the majority of data taken in the 8.5-GHz frequency band (1,539 measurements). The authors use this dataset to carry out a statistical analysis of the radio-selected sample. The detection rate of radio afterglows stayed unchanged almost at 31% before and after the launch of the Swift satellite. The canonical long-duration GRB radio light curve at 8.5 GHz peaks at three to six days in the source rest frame, with a median peak luminosity of 10<sup>31</sup> erg/s/Hz. The peak radio luminosities for short-hard bursts, X-ray flashes, and the supernova-GRB classes are an order of magnitude or more fainter than this value. There are clear relationships between the detectability of a radio afterglow and the fluence or energy of a GRB, and the X-ray or optical brightness of the afterglow. However, the authors find few significant correlations between these same GRB and afterglow properties and the peak radio flux density. In their paper, they also produce synthetic light curves at centimeter and millimeter bands using a range of blast wave and microphysics parameters derived from multi-wavelength afterglow modeling, and use them to compare with the radio sample. Finding agreement, the authors extrapolate this behavior to predict the centimeter and millimeter behavior of GRBs which will observed by the Expanded Very Large Array and the Atacama Large Millimeter Array. The compiled sample consists of 304 GRBs observed with radio telescopes between 1997 January and 2011 January, along with the 2011 April 28 Fermi burst, GRB 110428A. The sample consists of a total of 2,995 flux density measurements taken in the frequency range from 0.6 to 660 GHz and spanning a time range from 0.026 to 1,339 days. Most of the afterglows (270 in total) in this sample were observed as part of VLA radio afterglow programs, whereas 15 bursts were observed by the Expanded VLA (EVLA), and 19 southern bursts with the Australia Telescope Compact Array (ATCA). This catalog describes the radio, optical and X-ray afterglow detections (see Section 2.2 of the reference paper): out of the 304 bursts, 123 bursts were observed in the pre-Swift epoch from 1997 until 2004. The remaining 181 bursts were observed between 2005 and 2011 April (the post-Swift epoch). Out of the 95 radio-detected afterglows (see Section 2.2 of the reference paper), 63 had radio lightcurves (i.e., three or more detections in a single radio band), whereas 32 bursts had less than three detections. For the GRBs for which the light curves were available, the authors determined the peak flux density and the time of the peak in the VLA frequency bands (i.e., 1.4 GHz, 4.9 GHz, 8.5 GHz, 15 GHz, and 22.5 GHz bands) by fitting the data with forward shock formula of the form (Frail 2005, IAU Coll. 192, p. 451) given in equation (1) of the reference paper. This formula may not accurately represent the full complexity of the radio lightcurve evolution. However, it is good enough to determine the approximate values for the peak flux density F<sub>m</sub> and the time of the peak t<sub>m</sub>. See the discussion in Section 3.5 of the reference paper for more details and some caveats. For the remaining bursts, the flux density values were taken directly from the data, and hence do not have the best-fit errors for the peak flux, peak time and rest-frame peak time parameters F<sub>m</sub>, t<sub>m</sub> and t<sub>m</sub>/(1+z), respectively. This table was created by the HEASARC in November 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/746/156">CDS catalog J/ApJ/746/156</a> files table1.dat and table4.dat. This is a service provided by NASA HEASARC .
