- ID:
- ivo://nasa.heasarc/m31stars2
- Title:
- MIT/Amsterdam M 31 Survey
- Short Name:
- M31Stars/deep
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The MIT/Amsterdam M 31 Survey, or the Extended Magnier et al. Catalog of Objects in the Field of M 31, is based on deep BVRI CCD photometry that was performed on a 1 square degree region of M 31. The observations were made between September 12 and September 27 1990, using the McGraw-Hill 1.3m telescope at the Michigan-Dartmouth-MIT (MDM) observatory at Kitt Peak. The catalogue has typical completeness limits of 20.7 (Bmag), 21.7 (Vmag), 20.2 (Rmag) and 20.5 (Imag), although there is a large region in the inner disk for which the completeness limits are substantially deeper: 22.3 (Bmag), 22.2 (Vmag), 22.2 (Rmag), and 20.9 (Imag). The photometric accuracy is about 2% at Vmag = 19. The final astrometric calibrations take into account the systematic error discovered in the Berkhuijsen et al. (1988, A&AS, 76, 65) catalog by Magnier et al. (1993, A&A, 272, 695). They are in the J2000 system and are eventually tied to the HST Guide Star Catalog. The final photometric calibrations are tied via the NGC 206 region to photometry taken at the Michigan-Dartmouth-MIT (MDM) 1.3m in September and October 1993. These are tied to the Landolt (1992, AJ, 104, 340) system of standard stars, and are in the Johnson-Kron-Cousins system (BVRcIc). This version of the MIT/Amsterdam M31 Survey Catalog was created at the HEASARC in March 1999 based on the CDS/ADC Catalogue II/208. The HEASARC revised this version in February 2001. This is a service provided by NASA HEASARC .
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- ID:
- ivo://nasa.heasarc/m31rbcgc
- Title:
- M 31 Revised Bologna Clusters and Candidates Catalog (Version 5)
- Short Name:
- M31RBCGC
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Revised Bologna Catalogue of M 31 globular clusters and candidates (RBC, V.5, August 2012) lists all the confirmed globular clusters (GCs), all the known candidates GCs, and also all the objects that were identified as candidate GCs in the past and were subsequently recognized not to be genuine clusters, each entry being properly classified (GC, candidate GC, foreground star, background galaxy, HII region, etc.). The latter entries are maintained in the catalog to avoid re-discoveries of objects that may look like M 31 GCs and have been already classified as non-GCs. Please take into account the classification flag(s) when you use the RBC. Please acknowledge the use of this catalog. The proper reference is: Galleti S., Federici L., Bellazzini M., Fusi Pecci F., Macrina S. "2MASS NIR photometry for 693 candidate globular clusters in M 31 and the Revised Bologna Catalogue (V.1.0)", Astron.&Astrophys., 2004, 416, 917 (2004A&A...416..917G) This table was created by the HEASARC in November 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/V/143">CDS Catalog V/143</a> file rbc5.dat, Version 5 of the Revised Bologna Catalogue of M 31 globular clusters and candidates. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/nuvbemdcat
- Title:
- Near-UV Detected Bright Early-M Dwarf Star Catalog
- Short Name:
- NUVBEMDCAT
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Planets orbiting within the close-in habitable zones of M dwarf stars will be exposed to elevated high-energy radiation driven by strong magnetohydrodynamic dynamos during stellar youth. Near-ultraviolet (NUV) irradiation can erode and alter the chemistry of planetary atmospheres, and a quantitative description of the evolution of NUV emission from M dwarfs is needed when modeling these effects. The authors investigated the NUV luminosity evolution of early M-type dwarfs by cross-correlating the Lepine & Gaidos (LG11: 2011, AJ, 142, 138) catalog of bright M dwarfs (available at the HEASARC as the MDWARFASC table) with the Galaxy Evolution Explorer (GALEX) catalog of NUV (1771-2831 Angstrom) sources. Of the 4,805 sources with GALEX counterparts, 797 have NUV emission significantly (> 2.5 sigma) in excess of an empirical basal level. The authors inspected these candidate active stars using visible-wavelength spectra, high-resolution adaptive optics imaging, time-series photometry, and literature searches to identify cases where the elevated NUV emission is due to unresolved background sources or stellar companions; they estimated the overall occurrence of these "false positives" (FPs) as ~ 16%. The authors constructed an NUV luminosity function that accounted for FPs, detection biases of the source catalogs, and GALEX upper limits. They found the NUV luminosity function to be inconsistent with predictions from a constant star-formation rate and simplified age-activity relation defined by a two-parameter power law. This table was created by the HEASARC in March 2015 based on an electronic versions of Table 4 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/newmdwarfs
- Title:
- New M Dwarfs in the Solar Neighborhood
- Short Name:
- NEWMDWARFS
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the results from a spectroscopic study of 1080 nearby active M dwarfs, selected by correlating the Two Micron All Sky Survey (2MASS) and ROSAT catalogs at galactic latitudes greater than 15 degrees above or below the Galactic Plane and using a matching radius of 20 arcseconds, as well as color cuts (J-H < 0.75, H-K > 0.15 and 0.8 < J-K < 1.1) designed to select M dwarfs. The authors have derived the spectral types and estimated distances for all of their stars. The spectral types range between K5 and M6. Nearly half of the stars lie within 50 pc. The authors have measured the equivalent width of the H-alpha emission line. Their targets show an increase in chromospheric activity from early to mid-spectral types, with a peak in activity around M5. Using the count rate and hardness ratios obtained from the ROSAT catalog,the authors have derived the stellar X-ray luminosities. Their stars display a "saturation-type" relation between the chromospheric and coronal activity. The relation is such that log L<sub>X</sub>/L<sub>bol</sub> remains "saturated" at a value of approximately -3 for varying H-alpha equivalent width. The authors have found 568 matches in the USNO-B catalog and have derived the tangential velocities v<sub>tan</sub> for these stars. There is a slight trend of decreasing chromospheric activity with age, such that the stars with higher v<sub>tan</sub> values have lower H-alpha equivalent widths. The coronal emission, however, remains saturated at a value of log L<sub>X</sub>/L<sub>bol</sub> ~ -3 for varying tangential velocities, suggesting that the coronal activity remains saturated with age. The authors do not find any break in the saturation-type relation at the spectral type at which stars become fully convective (~M3.5). Most of the stars in their sample show more coronal emission than the dMe stars in the Hyades and Praesepe clusters and have v<sub>tan</sub> < 40 km s<sup>-1</sup>, suggesting that they belong to a young population. This table was created by the HEASARC in March 2010 based on the (corrected) electronic version of Table 1 from the reference paper which was obtained from the Astronomical Journal web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/openclust
- Title:
- New Optically Visible Open Clusters and Candidates Catalog
- Short Name:
- OpenCluster
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/92">CDS Cat. VII/92</a>, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret & M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, <a href="http://www.univie.ac.at/webda/">http://www.univie.ac.at/webda/</a>). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects (almost 1,000) relative to the Lynga Catalog. In total, 99.7% of the objects have estimates of their apparent diameters, and 74.5% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 54.7% have their mean proper motions listed, 25% their mean radial velocities, and 24.2% have both information simultaneously. Acknowledgments: Extensive use has been made by the authors of the SIMBAD and WEBDA databases. This project is supported by FAPESP (grant number 03/12813-4) and CAPES (CAPES-GRICES grant number 040/2008). This database table was originally created by the HEASARC in September 2002 based on the CDS version of the catalog. In March 2006, the HEASARC updated the table to use instead the following file obtained from the authors' web site: <a href="http://www.astro.iag.usp.br/ocdb/file/clusters.txt">http://www.astro.iag.usp.br/ocdb/file/clusters.txt</a>. In August 2017, the HEASARC reverted to using the CDS version of this catalog, available as the file clusters.dat at <a href="http://cdsarc.u-strasbg.fr/ftp/cats/B/ocl/">http://cdsarc.u-strasbg.fr/ftp/cats/B/ocl/</a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/ngc6530oid
- Title:
- NGC 6530 Chandra Point Source Optical/IR Identifications Catalog
- Short Name:
- NGC6530OID
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The authors have obtained astrometry and BVI photometry, down to a V magnitude of ~22, of the very young open cluster NGC 6530, from observations taken with the Wide Field Imager (WFI) camera at the MPG/ESO 2.2m Telescope. They have positionally matched their optical catalog with the list of X-ray sources found in a Chandra-ACIS observation of this cluster (Damiani et al. 2004, ApJ, 608, 781: available in Browse both via links from this table and also as the NGC6530CXO table), finding a total of 828 stars in common, 90% of which are pre-main sequence stars in NGC 6530. The data used in this work come from the combination of optical BVI images taken with the WFI camera made on 27-28 July 2000, a 60 ks Chandra ACIS X-ray observation, and public near-infrared data from the All-Sky Catalog of Point Sources of the Two Micron All Sky Survey (2MASS, CDS Cat. <II/24>). The total number of optical sources falling in the Chandra FOV is 8956, while the Damiani et al. (2004, ApJ, 608, 781) Catalog contains 884 X-ray sources, who concluded that at least 90% of the X-ray sources are very probable cluster members. To cross-correlate the X-ray and optical catalogs, the authors used a matching distance of < 4 sigmaX, where sigmaX is the the X-ray positional error, or 1.5", whichever is smaller, after a systematic shift between the X-ray and WFI positions of 0.2" in RA and -0.26" in Dec had been included. This resulted in a number of multiple identifications, among which 4 turned into unique identifications when a reduced distance of 1.5" was used. This finally resulted in 721 single, 44 double, and 3 triple identifications in the optical catalog; in addition, one X-ray source has 4 optical identifications, and another has 6 optical identifications. The total number of X-ray sources with WFI counterparts is therefore 770; of them, only 15 X-ray identified stars come from the Sung et al. (2000, AJ, 120, 333) Catalog and are not in the WFI Catalog. The total number of optical sources with an X-ray counterpart is 828. The agreement between X-ray and WFI optical positions is excellent in most cases, with offsets below 1". This database table was created by the HEASARC in February 2007, based on CDS table J/A+A/430/941/table5.dat This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/nltt
- Title:
- NLTTCatalog&FirstSupplement
- Short Name:
- NLTT
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This catalog (Luyten 1979, 1980) is a collection of stars on more than 800 Palomar Proper Motion Survey plates found to have relative annual proper motions exceeding 0.18 arcsec. The motions have been determined by Luyten and his coworkers by either hand blinking and measuring or with the automated- computerized scanner and measuring machine built by Control Data Corporation and located at the University of Minnesota. The new catalog replaces the LTT Catalogues (Luyten 1957, 1961, 1962), wherein stars in the Bruce Proper Motion Survey discovered to have motions exceeding 0.2 arcsec had been compiled. For further information on the NLTT Catalogue itself, including discussions of positional errors, estimation of magnitudes, star designations used in the catalog, completeness, and accuracy of the measured motions, the introduction to the published NLTT (see Volume I) should be consulted. The First Supplement to the NLTT Catalogue (Luyten and Hughes 1980) is the result of continued plate analysis and measurements during printing of the NLTT. The Supplement contains data for 398 stars having motions larger than 0.179 arcsec annually. Duplicate entries were removed from the HEASARC implementation of this catalog in June 2019. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/oriysoir
- Title:
- Orion Nebula YSO IR Properties
- Short Name:
- ORIYSOIR
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The origin and evolution of the X-ray emission in very young stellar objects (YSOs) are not yet well understood because it is very hard to observe YSOs in the protostellar phase. Using COUP data, the authors studied in their reference paper the X-ray properties of stars in the Orion Nebula Cluster (ONC) in different evolutionary classes: luminosities, hydrogen column densities N<sub>H</sub>, effective plasma temperatures, and time variability were compared to understand if the interaction between the circumstellar material and the central object can influence the X-ray emission. They have assembled the deepest and most complete photometric catalog of objects in the ONC region from the UV to 8 microns (um) using data from the HST Treasury Program; deep and almost simultaneous UBVI and JHK images taken, respectively, with WFI at ESO 2.2m and ISPI at CTIO 4m telescopes; and Spitzer IRAC imaging. They selected high-probability candidate Class 0-I protostars, a sample of "bona fide" Class II stars, and a set of Class III stars with IR emission consistent with normal photospheres. Their principal result is that Class 0-Ia objects are significantly less luminous in X-rays, in both the total and hard bands, than the more evolved Class II stars with mass larger than 0.5M_{sun}_; the latter show X-ray luminosities similar to those of Class 0-Ib stars. This table contains the JHK and IRAC data, as well as the protostar classifications, for 398 ONC YSOs. This online catalog was created by the HEASARC in October 2010 based on the machine-readable versions of Tables 2, 3, 4 and 5 from the reference paper which were obtained from the CDS (their catalog J/ApJ/677/401). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/dncvobcat
- Title:
- Outburst Catalog of Dwarf Novae-type and Other Cataclysmic Variables
- Short Name:
- DNCVOBCAT
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This outburst catalog contains a wide variety of observational properties for 722 dwarf nova-type (DN) cataclysmic variables (CVs) and 309 CVs of other types from the Catalina Real-time Transient Survey (CRTS). In particular, it includes the apparent outburst and quiescent V-band magnitudes, duty cycles, limits on the recurrence time, upper- and lower-limits on the distance and absolute quiescent magnitudes, color information, orbital parameters, and X-ray counterparts. These properties were determined by means of a classification script presented in the reference paper. The DNs in the catalog show a correlation between the outburst duty cycle and the orbital period (and outburst recurrence time), as well as between the quiescent absolute magnitude and the orbital period (and duty cycle). This is the largest sample of dwarf nova properties collected to date (2016). Besides serving as a useful reference for individual systems and a means of selecting objects for targeted studies, it will prove valuable for statistical studies that aim to shed light on the formation and evolution of cataclysmic variables. The CRTS identifies transients in the data from the Catalina Sky Survey (Larson et al. 1998, BAAS, 30, 1037; 2003, BAAS, 35, 982), a photometric survey that searches for Potentially Hazardous Asteroids and Near Earth Objects. Three sub-surveys constitute the Catalina Sky Survey, namely the original CSS (Catalina Schmidt Survey), the MLS (Mt Lemmon Survey) based in Arizona, and the SSS (Siding Spring Survey) in Australia, which ended on 2014 July 5. The field of view and typical limiting magnitude for each survey (at ~30 s integrations) are 8.2 degrees and V~19.5 mag for the CSS, 1.1 degrees and V~21.5 mag for the MLS, and 4 degrees and V~19 mag for the SSS. Together, these surveys cover 30, 000 deg<sup>2</sup> between -70 and +70 degrees Declination (see Drake et al. 2014, MNRAS, 441, 1186 for more details). The entire zone within 15 Degrees of the Galactic Plane is avoided due to overcrowding, as are the Magellanic Clouds. The properties of the cataclysmic variables in this catalog are derived from the long-term optical light curves from the CRTS, as well as magnitudes, fluxes and orbital parameters from the SDSS, 2MASS, UKIDSS, ROSAT, Chandra, XMM and WISE catalogs, and from the Catalog of Cataclysmic Binaries, Low-Mass X-Ray Binaries and Related Objects (RKCat: Ritter and Kolb 2003, A&A, 404, 301, available at the HEASARC as the RITTERCV, RITTERLMXB and RITTERRBIN tables). This table was created by the HEASARC in October 2017 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/456/4441">CDS catalog J/MNRAS/456/4441</a> file catalog.dat. . This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/pg
- Title:
- Palomar-Green Catalog of UV-Excess Stellar Objects
- Short Name:
- PG
- Date:
- 10 May 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Palomar-Green Catalog of UV-Excess Stellar Objects provides positions (the original_ra and original_dec parameters) accurate to about 8 arcsec in each coordinate, photographic B-magnitudes accurate to 0.29 mag, spectral types, some cross-references, and photoelectric broad-band, multichannel, and Stroemgren colors when available. Of the 1874 objects in the catalog as published in 1986 (1878 in this version), 1715 comprise a statistically complete sample covering 10714 square degrees from 266 fields taken on the Palomar 18-inch Schmidt telescope. Limiting magnitudes vary from field to field, ranging from 15.49 to 16.67. The overall completeness is estimated to be 84%, but that figure and the relative contributions of magnitude, color, and accidental errors vary depending on the magnitude and color distribution of the spectroscopic subsample. The dominant population in this catalog is that of the hot, hydrogen-atmosphere subdwarfs, the sdB stars, which comprise nearly 40 per cent of the sample. The hot white dwarfs of spectral types DA, DB, and DO account for 21, 2.8, and 1.0 per cent of the sample, respectively, while cooler DC or DZ white dwarfs add another 1.2 per cent. Cataclysmic variables and composite-spectrum binaries account for 5 per cent, although many other spectra dominated by a hot star showed evidence for a cool companion at red wavelengths. Planetary nebulae central stars account for another 0.5 per cent. Extragalactic objects comprise about 9 per cent of the complete sample, with QSOs representing 5.4 per cent. Only 0.3 per cent (6 objects) remain with totally unsatisfactory or unknown spectral classes. (Notice that all of these percentage estimates are based on the published version of this catalog, and that the values in the current online version may be slightly different, as the latter includes a small number of updates and additions). In 2009, an additional data resource was added to this catalog by CDS, namely a file containing more accurate (sub-arcsecond) positions and V magnitudes (the skiff_vmag parameter), and also additional comments (the skiff_comments parameter). This new material has now been included in the HEASARC version of the PG Catalog. A full discussion of this addition can be found at <a href="http://cdsarc.u-strasbg.fr/ftp/cats/II/207A/pg_2009.txt">http://cdsarc.u-strasbg.fr/ftp/cats/II/207A/pg_2009.txt</a>. This database was initially made available at the HEASARC in June 1998 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/207A">CDS catalog II/207A</a> file catalog.dat which had been last updated on Oct 17 1997. In 2017, the HEASARC re-ingested this CDS catalog as it had been updated several times in the interim, notably in 2009 when an additional file (pg_pos.dat) with precise coordinates and comments provided by Brian Skiff was added. This is a service provided by NASA HEASARC .