AAVSOVSX Catalog
This database table contains Galactic stars known or suspected to be
variable. It lists all stars that have an entry in the American Association
of Variable Star Observers' (AAVSO) International Variable Star Index (VSX;
http://www.aavso.org/vsx).
It consisted initially of the General Catalogue of Variable Stars (GCVS) and
the New Catalogue of Suspected Variables (NSV) and was then supplemented with
a large number of variable star catalogues, as well as individual variable
star discoveries or variables found in the literature. Effort has also been
invested to update the entries with the latest information regarding
position, type and period and to remove duplicates. The VSX database is being
continually updated and maintained.
For historical reasons some objects outside of the Galaxy have been included.
ACRS Catalog
For a number of years there has been a great demand for a high-density
catalog of accurate stellar positions and proper motions that maintains
a consistent system of reference over the entire sky. The Smithsonian
Astrophysical Observatory Star Catalog (SAO; SAO Staff 1966) has
partially met those requirements, but its positions brought to current
epochs now contain errors on the order of 1 second of arc, plus the
proper motions in the SAO differ systematically with one another
depending on their source catalogs.
With the completion of the Second Cape Photographic Catalogue (CPC2; de
Vegt et al. 1989), a photographic survey comparable in density to the
AGK3 (Dieckvoss 1975) was finally available for the southern
hemisphere. These two catalogs were used as a base and matched against
the AGK2 (Schorr & Kohlschuetter 1951-58), Yale photographic zones
(Yale Trans., Vols. 11-32), First Cape Photographic Catalogue (CPC1;
Jackson & Stoy 1954, 55, 58; Stoy 1966), Sydney Southern Star Catalogue
(King & Lomb 1983), Sydney Zone Catalogue -48 to -54 degrees (Eichhorn
et al. 1983), 124 meridian circle catalogs, and catalogs of recent
epochs, such as the Carlsberg Meridian Catalogue, La Palma (CAMC), USNO
Zodiacal Zone Catalog (Douglass & Harrington 1990), and the Perth 83
Catalogue (Harwood [1990]) to obtain as many input positions as
possible. All positions were then reduced to the system of the FK4
(Fricke & Kopff 1963) using a combination of the FK4, the FK4
Supplement as improved by H. Schwan of the Astronomisches
Rechen-Institut in Heidelberg, and the International Reference Stars
(IRS; Corbin 1991), then combined with the CPC2 and AGK3. The total
number of input positions from which the ACRS was formed is 1,643,783.
The original catalog is divided into two parts. Part 1 contains the
stars having better observational histories and, therefore, more
reliable positions and proper motions. This part constitutes 78 percent
of the catalog; the mean errors of the proper motions are +/-0.47
arcsec per century and +/-0.46 arcsec per century in right ascension
and declination, respectively. The stars in Part 2 have poor
observational histories and consist mostly of objects for which only
two catalog positions in one or both coordinates were available for
computing the proper motions. Where accuracy is the primary
consideration, only the stars in Part 1 should be used, while if the
highest possible density is desired, the two parts should be combined.
The ACRS was compiled at the U. S. Naval Observatory with the intention
that it be used for new reductions of the Astrographic Catalogue (AC)
plates. These plates are small in area (2 x 2 deg) and the IRS is not
dense enough. Whereas the ACRS was compiled using the same techniques
developed to produce the IRS, it became clear as the work progressed
that the ACRS would have applications far beyond its original purpose.
With accurate positions and proper motions rigorously reduced to both
the FK4 and FK5 (Fricke et al. 1988) systems, it does more than simply
replace the SAO. Rather, it provides the uniform system of reference
stars that has been needed for many years by those who require
densities greater than the IRS and with high accuracy over a wide range
of epochs. It is intended that, as additional observations become
available, stars will be migrated from Part 2 to Part 1, with the hope
that eventually the ACRS will be complete in one part. Additional
details concerning the compilation and properties of the ACRS can be
found in Corbin & Urban (1989) except that the star counts and errors
given here supersede the ones given in 1989.
ASIAGOSN Catalog
This table contains the dynamic version of the Asiago Supernova Catalog. It
supersedes the original 1999 version by Barbon et al. (1999A&AS..139..531B,
Cat. II/227), and contains data about the supernovae observed since 1885 and
their parent galaxies through a few days prior to the most recent update. In
addition to the list of newly discovered SNe, the literature has been
searched for new information on past SNe as well. The data for the parent
galaxies have also been homogenized.
ATNFPULSAR Catalog
The Australia Telescope National Facility (ATNF) Pulsar Catalog is a catalog
of known pulsars compiled by R.N. Manchester et al. and is descended from
pulsar database used for the paper "Catalog of 558 Pulsars" by J.H. Taylor,
R.N. Manchester and A.G. Lyne 1993, ApJS, 88, 529-568. The current catalog
has been supplemented by inclusion of published data from more recent radio
surveys, in particular, the Parkes Multibeam (PM) Pulsar Survey (Manchester
et al. 2001, MNRAS, 328, 17-35) [available at the HEASARC as the PMPULSAR
table] and the Swinburne Intermediate Latitude Pulsar Survey (Edwards et al.
2001, MNRAS, 326, 358-374), both made using the ATNF Parkes 64-m radio
telescope. Binary parameters for known binary pulsars are also included as
well as all available astrometric and spin parameter information for all
pulsars. The catalog includes all published rotation-powered pulsars. Two
separate small subsets of pulsars detected only at high energies are also
included in the current table: the first group comprises X-ray and gamma-ray
pulsars which are apparently powered by spin-down energy, but which have not
been detected at radio wavelengths, while the second group contains anomalous
X-ray pulsars (AXPs) and soft-gamma-ray repeaters (SGRs) for which coherent
pulsations have been detected. Accretion-powered pulsars such as Her X-1 and
the recently discovered X-ray millisecond pulsars such as SAX J1808.4-3658
are not included in this table, however.
Many people have contributed to the compilation of the data contained in this
catalog and the database that it was derived from. The authors particularly
thank Andrew Lyne of the University of Manchester, Jodrell Bank Observatory,
David Nice of Princeton University, and Russell Edwards, then at Swinburne
University of Technology. The also acknowledge the efforts of Warwick
University students Adam Goode and Steven Thomas who compiled and checked a
recent version of the database. The original (summer 2003) database at the
ATNF website was compiled with the invaluable assistance of Maryam Hobbs,
while the ATNF web interface was designed and constructed by Albert Teoh, a
Summer Vacation Scholar at the ATNF in 2002/2003.
The authors would appreciate if anyone making use of this catalog in a
publication acknowledges the source of their information by quoting the
ATNF Pulsar Catalog website address of
http://www.atnf.csiro.au/research/pulsar/psrcat/
BATSEPULSR Catalog
BATSE data are divided into four groups: trigger, daily, occultation, and
pulsar. Each group has structured directories beneath it containing data
ordered by an appropriate criterion. Typically, several files of data are
necessary to form a complete set of data for a particular entity. The BATSE
pulsar data are organized similarly to the OCCULTATION data set, with the
difference being in the filename extensions: 'olc' files contain on-board
folded light curves, whereas 'pll' files (available in the HEASARC anonymous
FTP area, but not via this database table) contain pulsar low level data.
This database table allows the user to select 'olc' files or GIFs created
from these files for 8 out of the several dozen pulsars for which BATSE data
are available.
BESTARS Catalog
The BESTARS database tables contains a compilation of data concerning stars
of type Be. For the purposes of this compilation, a Be star is defined as a
non-supergiant B star which showed emission in one Balmer line at least once.
Stars without published MK spectral types have been excluded, except for 132
stars from Bidelman and MacConnell (1973), who used the above definition but
included no spectral types. There are 1,159 stars included in this list.
BNMDSPECAT Catalog
This table contains a spectroscopic catalog of the 1564 brightest (J < 9m)
M-dwarf candidates in the northern sky, as selected from the SUPERBLINK
proper-motion catalog (Lepine and Shara 2005, AJ, 129, 1483). Observations
confirm 1408 of the candidates to be late-K and M dwarfs with spectral
subtypes K7 - M6. From the low (mu > 40 mas yr-1) proper motion limit and
high level of completeness of the SUPERBLINK catalog in that magnitude range,
the authors estimate that their spectroscopic census most likely includes >
90% of all existing, northern-sky M dwarfs with apparent magnitude J < 9m.
Only 682 stars in this sample are listed in the Third Catalog of Nearby Stars
(CNS3, Gliese and Jahreiss 1991); most others are relative unknowns and have
spectroscopic data presented here for the first time. Spectral subtypes are
assigned based on spectral index measurements of CaH and TiO molecular bands;
a comparison of spectra from the same stars obtained at different
observatories, however, reveals that spectral band index measurements are
dependent on spectral resolution, spectrophotometric calibration, and other
instrumental factors. As a result, the authors find that a consistent
classification scheme requires that spectral indices be calibrated and
corrected for each observatory/instrument used. After systematic corrections
and a recalibration of the subtype-index relationships for the CaH2, CaH3,
TiO5, and TiO6 spectral indices, the authors find that they can consistently
and reliably classify all the stars to a half-subtype precision. The use of
corrected spectral indices further requires them to recalibrate the zeta
parameter, a metallicity indicator based on the ratio of TiO and CaH optical
bandheads. However, the authors find that their zeta values are not sensitive
enough to diagnose metallicity variations in dwarfs of subtypes M2 and
earlier (+/- 0.5 dex accuracy) and are only marginally useful at later M3-M5
subtypes (+/- 0.2 dex accuracy). Fits of their spectra to the Phoenix
atmospheric model grid are used to estimate effective temperatures. These
suggest the existence of a plateau in the M1-M3 subtype range, in agreement
with model fits of infrared spectra but at odds with photometric
determinations of Teff. Existing geometric parallax measurements are
extracted from the literature for 624 stars, and are used to determine
spectroscopic and photometric distances for all the other stars. Active
dwarfs are identified from measurements of H-alpha equivalent widths, and the
authors find a strong correlation between H-alpha emission in M dwarfs and
detected X-ray emission from ROSAT and/or a large UV excess in the GALEX
point source catalog. Proper motion data and photometric distances are
combined in order to evaluate the (U, V, W) distribution in velocity space,
which is found to correlate tightly with the velocity distribution of G
dwarfs in the solar neighborhood. However, active stars show a smaller
dispersion in their space velocities, which is consistent with those stars
being younger on average. The authors state that this catalog will be very
useful for guiding the selection of the best M dwarf targets for exoplanet
searches, in particular those using high-precision radial velocity
measurements.
BSC5P Catalog
The BSC5P database table contains data derived from the Bright Star Catalog,
5th Edition, preliminary, which is widely used as a source of basic
astronomical and astrophysical data for stars brighter than magnitude 6.5.
The database contains the identifications of included stars in several other
widely-used catalogs, double- and multiple-star identifications, indication
of variability and variable-star identifiers, equatorial positions for
B1900.0 and J2000.0, galactic coordinates, UBVRI photoelectric photometric
data when they exist, spectral types on the Morgan-Keenan (MK) classification
system, proper motions (J2000.0), parallax, radial- and rotational-velocity
data, and multiple-star information (number of components, separation, and
magnitude differences) for known non-single stars.
CHANVGUIDE Catalog
Variable stars have been identified among the optical-wavelength
light curves of guide stars used for pointing control of the Chandra X-ray
Observatory. The authors present a catalog of these variable stars along with
their light curves and ancillary data. Variability was detected to a lower
limit of 0.02 mag amplitude in the 4000-10000 Angstroms range using the
photometrically stable Aspect Camera on board the Chandra spacecraft. The
Chandra Variable Guide Star Catalog (VGUIDE) contains 827 stars, of which 586
are classified as definitely variable and 241 are identified as possibly
variable. Of the 586 definite variable stars, the authors believe 319 are new
variable star identifications. Types of variables in the catalog include
eclipsing binaries, pulsating stars, and rotating stars. The variability was
detected during the course of normal verification of each Chandra pointing and
results from analysis of over 75,000 guide star light curves from the Chandra
mission. The VGUIDE catalog represents data from only about 9 years
of the Chandra mission. Future releases of VGUIDE will include newly identified
variable guide stars as the mission proceeds. An important advantage of the
use of space data to identify and analyze variable stars is the relatively
long observations that are available. The Chandra orbit allows for
observations up to 2 days in length. Also, guide stars were often used
multiple times for Chandra observations, so many of the stars in the VGUIDE
catalog have multiple light curves available from various times in the
mission. The catalog is presented as both online data associated with this
paper (from which this HEASARC representation was created) and as a public Web
interface at http://cxc.harvard.edu/vguide/. Light curves with data at the
instrumental time resolution of about 2 s, overplotted with the data binned at
1 ks, can be viewed on the above-mentioned public Web interface and downloaded
for further analysis. (This HEASARC Browse table also contains links to these
light curves). VGUIDE is a unique project using data collected during the
mission that would otherwise be ignored. The stars available for use as
Chandra guide stars are generally 6-11 magnitudes and are commonly spectral
types A and later. Due to the selection of guide stars entirely for positional
convenience, this catalog avoids the possible bias of searching for
variability in objects where it is to be expected. Statistics of variability
compared to spectral type indicate the expected dominance of A-F stars as
pulsators. Eclipsing binaries are consistently 20%-30% of the detected var
iables across all spectral types.
CHASFRXRAY Catalog
This catalog contains a source list derived from observations of
the ROSAT all-sky survey (RASS) in the direction of the Chamaeleon star-forming
region cloud complex, as well as spectroscopic identifications for the detected
X-ray sources. The main purpose of this identification program was the search
for low-mass pre-main sequence stars. Sixteen previously known PMS stars were
detected with high confidence by ROSAT: eight are classical T Tauri stars and
eight are weak-line T Tauri stars. Seventy-seven new weak-line T Tauri stars
were identified on the basis of the presence of strong Li 6707 Angstrom
absorption, a spectral type later than F0, and chromospheric emission.
In addition, 6 new dKe-dMe candidates were found among the RASS sources.
Coordinates and count rates are given for all of the X-ray sources.
CNS3 Catalog
The CNS3 catalog contains all known stars as of 1991 that are within 25
parsecs of the Sun. It depends mainly on a preliminary version (Spring 1989)
of the new General Catalogue of Trigonometric Parallaxes (YPC) prepared by
Dr. William F. van Altena (Yale University).
The catalog contains every then-known star with a trigonometric parallax
greater than or equal to 0.0390 arcsec, even though it may be evident from
photometry or for other reasons that the star has a larger distance. For red
dwarf stars, new color-magnitude calibrations for broad-band colors were
carried out and applied. For white dwarfs, the recipes of McCook and Sion in
ApJS, 65, 603 (1987) were applied. Stroemgren photometry was used (not yet
systematically) for early-type stars and for late dwarfs, the latter supplied
by E. H. Olsen from Copenhagen Observatory (private communication).
In contrast to the CNS2 (Gliese 1969) catalog, trigonometric parallaxes and
photometric or spectroscopic parallaxes were not combined in this version.
The resulting parallax in the present version is the trigonometric parallax
if the relative error of the trigonometric parallax is smaller than 14
percent. The parallax may be the photometric or spectroscopic parallax
only if no trigonometric parallax is available or if the standard error of
the trigonometric parallax is considerably larger.
COCD Catalog
The Catalog of Open Cluster Data (COCD) is a result of studies of
the wide neighborhoods of 513 open clusters and 7 compact associations carried
out in the high-precision homogeneous All-Sky Compiled Catalog of 2.5 Million
Stars (ASCC-2.5, Kharchenko 2001, CDS Cat. <I/280>). On the basis of data on
about 33,000 possible members (including about 10,000 most probable ones) and
homogeneous methods of cluster parameter determination, the angular sizes of
cluster cores and coronae, cluster heliocentric distances, mean proper motions,
mean radial velocities and ages were established and collected in the COCD.
These include cluster distances for 200 clusters, average cluster
radial velocities for 94 clusters, and cluster ages for 195 clusters
derived for the first time. Clusters in the catalogue are sequenced in their
Right Ascension J2000 order.
The Open Cluster Diagrams Atlas (OCDA) presents a set of open cluster
diagrams used for the determination of parameters of the 513 open clusters
and 7 compact associations, and is intended to illustrate the quality
of the constructed cluster membership (Kharchenko et al. 2004, CDS Cat.
<J/AN/325/740>), and the accuracy of the derived cluster
parameters. Every diagram presents relation between
various stellar data from the ASCC-2.5 in the area of the specific cluster.
There are five diagrams provided for every cluster in the Atlas: the area map,
the density profile, the vector point diagram, the magnitude equation diagram
and the color-magnitude diagram. The OCDA PostScript plots (one file per
cluster) are available as a remote data product for entries in this table.
COCDEXT1 Catalog
This table contains a list of 130 Galactic open clusters, found in the
All-Sky Compiled Catalogue of 2.5 Million Stars (ASCC-2.5) and not included
in the original Catalog of Open Cluster Data (COCD): it is known as the
1st Extension of the COCD (COCD-1). For these new clusters, the authors
determined a homogeneous set of astrophysical parameters such as size,
membership, motion, distance and age. In their previous work (the Browse table
COCD based on the CDS Cat. J/A+A/438/1163), 520 already-known open clusters
out of a sample of 1700 clusters from the literature were confirmed in the
ASCC-2.5 using independent, objective methods. Using these same methods, the
whole sky was systematically screened for new clusters. The newly detected
clusters show the same distribution over the sky as the known ones. It
is found that without the a priori knowledge about existing clusters the
authors' search lead to clusters which are, on average, brighter, have more
members and cover larger angular radii than the 520 previously-known ones.
On the basis of data on about 6,200 possible members (including about
2,200 most probable ones) and homogeneous methods of cluster parameter
determination, the angular sizes of cluster cores and coronae, cluster
heliocentric distances, colour-excesses, mean proper motions, and ages of
130 clusters and mean radial velocities of 69 clusters were established and
collected in the COCD-1. Clusters in the catalogue are numbered in order
of increasing J2000.0 Right Ascension.
The 1st Extension of the Open Cluster Diagrams Atlas (OCDA-1) presents
a set of open cluster diagrams used for the determination of parameters
of the 130 newly discovered open clusters, and is intended to illustrate
the quality of the constructed cluster membership, and the accuracy of
the derived cluster parameters. Every diagram presents relations between
various stellar data from the all sky catalog ASCC-2.5(Kharchenko, 2001, CDS
Cat. <I/280>) in the area of the specific cluster. There are five diagrams
provided for every cluster in the Atlas: the area map, the density profile,
the vector point diagram, the "magnitude equation" (proper motion in each
coordinate versus V magnitude) diagram, and the color-magnitude diagram. The
130 OCDA-1 PostScript plots (one file per cluster) are available as a remote
data product for all of the entries in this table.
COROTEXLOG Catalog
CoRoT was a space astronomy mission devoted to the study of the variability
with time of stars' brightness, with an extremely high accuracy (100 times
better than from the ground), for very long durations (up to 150 days) and
with a very high duty cycle (more than 90%). The mission was led by CNES in
association with four French laboratories, and 7 participating countries and
agencies (Austria, Belgium, Brazil, Germany, Spain, and the ESA Science
Programme). The satellite is composed of a PROTEUS platform (the 3rd in the
series), and a unique instrument: a stellar photometer. It was launched on
December 27th, 2006 on a Soyuz Rocket, from Baikonour. The mission has lasted
almost 6 years (the nominal 3 years duration and a 3 years extension) and has
observed more than 160,000 stars. It suddenly stopped sending data on
November 2nd, 2012.
CoRoT performed Ultra High Precision Photometry of Stars to detect and
characterize the variability of their luminosity with two main objectives:
(i) the variability of the object itself: oscillations, rotation, magnetic
activity, etc.; (ii) variability due to external causes such as bodies in
orbit around the star: planets and companion stars.
The original scientific objectives were focused on the study of stellar
pulsations (asteroseismology) to probe the internal structure of stars, and
the detection of small exoplanets through their transit in front of their
host star, and the measurement of their sizes.
This lead to the introduction of two modes of observations, working
simultaneously:
- The bright star mode dedicated to very precise seismology of a small sample
(171) of bright and nearby stars (presented in the file named
"Bright_star.dat" in the CDS version at
ftp://cdsarc.u-strasbg.fr/pub/cats/B/corot/): these data are not included in
this HEASARC table, notice;
- The faint star mode, observing a very large number of stars at the same
time, to detect transits, which are rare events, as they imply the alignment
of the star, the planet and the observer (these data are presented in the
file named "Faint_star.dat" in the CDS version at
ftp://cdsarc.u-strasbg.fr/pub/cats/B/corot/): this HEASARC table is based on
this sample. The large amount of data gathered in this mode mode turned out
to be extremely fruitful for many topics of stellar physics.
Due to project constraints, two regions of the sky were accessible (circles
of 10 degrees centered on the equator around Right Ascensions of 06h 50m
and 18h 50m). They are called the CoRoT 'eyes': the first one is called
the "anticenter" eye, whereas the second one is called the "center eye".
Each pointing covers 1.4 x 2.8 square degrees.
The CoRoT project is still processing the data, aiming at removing
instrumental artifacts and defects. Therefore the format and content of
the catalog is still somewhat evolving. More details on the data can be
found in the file
http://idoc-corotn2-public.ias.u-psud.fr/jsp/doc/CoRoT_N2_versions_30sept2014.pdf.
More details on the CoRoT N2 data may be found in the documentation file
http://idoc-corotn2-public.ias.u-psud.fr/jsp/doc/DescriptionN2v1.5.pdf.
This HEASARC table contains information on stars observed by CoRoT in its
exoplanet detection program. A few percent of these stars have 2 entries
since they were observed in different windows (as specified by the
corot_window_id parameter) in a subsequent observing run to the initial run
in which they were observed. Each entry in this table corresponds to the
unique specification of target and corot_window_id, each with a link to its
associated N2 data products.
The original names of the parameters in this table, as given in the CoRoT
mission documentation, are given in square brackets at the end of the
parameter descriptions listed below.
CPSTARS Catalog
This table contains a catalog of 8205 known or suspected Ap, HgMn
and Am stars. This is a major update of the authors' first edition of their
catalog of Ap and Am stars, and includes revised identifications, additional
stars, and revised information obtained m the literature.
CRABTIME Catalog
The CRABTIME database contains the Crab Pulsar Monthly Ephemeris covering
the period from Feb 15 1982 (MJD=45015) to (close to) the present that was
created Dr. Andrew Lyne and collaborators at Jodrell Bank Observatory.
This database is periodically updated to include recent data as these become
available. To assist astronomers, the HEASARC has created two new parameters
which were not present in the original Jodrell Bank tables,
the pulsar period and its first derivative, using the standard relations
between period (P) and frequency 'Nu' (P=1./Nu) and their first derivatives
(P_dot = -Nu_dot/Nu2). The assumed pulsar position used in the reductions is
RA (1950.0) 05 31 31.406 DEC (1950.0) +21 58 54.391
RA (2000.0) 05 34 31.973 DEC (2000.0) +22 00 52.061
CVCAT Catalog
This catalog contains data for a large number of objects that have been
classified as cataclysmic variables (CVs) as well as a smaller number of
objects that are now not considered to be cataclysmic variables, but were
originally classified erroneously as such. As of 2000 December, 40% of the
objects in this catalog were dwarf novae, with another 30% being novae, and
the rest being mostly nova-like variables; also as of this date, a large
fraction (90%) of the CVs had references to published finding charts, while
64% of the objects had published spectra.
The catalog includes coordinates measured in the reference frame of the Hubble
Space Telescope Guide Star Survey for non-novae and from the literature for
novae. Also given are the variability type, the magnitude range, orbital
periods, flags indicating the existence of relevant space-based
observational datsets, references to finding charts and spectroscopy,
the galactic latitude and longitude, and the year of outburst (for novae).
This edition also includes plate identification information for the coordinate
measurements, and a reference to the classification.
The Catalog and Atlas of Cataclysmic Variables (Downes et al. in 2001, PASP,
113, 764 and http://archive.stsci.edu/prepds/cvcat/) presented here is the
ASCII Report mentioned in Section 2.1 of the PASP paper, and is similar to
the previously published versions of the CV Catalog (e.g., Downes, Webbink
and Shara 1997, PASP, 109, 345, Table 1). The online version of the CV
Catalog at http://archive.stsci.edu/prepds/cvcat/ contains additional data on
these systems not included in this database, including finding charts. For a
complete authoritative and up-to-date description of the CV Catalog, refer to
http://archive.stsci.edu/prepds/cvcat/description.html, from which the
HEASARC has constructed this help file.
DNCVOBCAT Catalog
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 deg2 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).
DUERBECK Catalog
This database table contains the Reference Catalog of Galactic Novae,
Duerbeck, version 1990. It lists all objects known or believed to be novae at
one time or other. Objects that were later found to be spurious have been
omitted. Completeness was attempted only for novae and not for dwarf novae,
X-ray novae, etc.
EXOPLANETS Catalog
The Extrasolar Planets Encyclopedia is a working tool, providing
all the latest detections and data that have been announced by professional
astronomers, Which is intended to be used to facilitate progress in
exoplanetology. Ultimately, researchers willing to make a quantitative,
scientific use of the catalog can make their own judgement on the
likelihood of the data and the detections.
The stellar data (positions, distances, V and other magnitudes, mass,
metallicities etc) are taken from Simbad or from professional papers on
exoplanets.
Ongoing large extrasolar planets ('exoplanets') projects include:
Anglo-Australian Planet Search
<http://www.phys.unsw.edu.au/~cgt/planet/AAPS_Home.html>
California & Carnegie Planet Search
<http://exoplanets.org/>
Geneva Extrasolar Planet Search Programmes
<http://obswww.unige.ch/~udry/planet/planet.html>
Transatlantic Exoplanet Survey
<http://www.astro.caltech.edu/~ftod/tres/tres.html>
University of Texas - Dept. of Astronomy
<http://www.as.utexas.edu/astronomy/research/ss.html>
EXOPLANODB Catalog
The Exoplanet Orbit Database is a database of well-determined orbital
parameters of exoplanets, and their host stars' properties. This database
comprises spectroscopic orbital elements measured for planets orbiting their
host stars from radial velocity and transit measurements as reported in the
literature. The authors have also compiled fundamental transit parameters,
stellar parameters, and the method used for the planets discovery. This
Exoplanet Orbit Database includes all planets with robust, well measured
orbital parameters reported in peer-reviewed articles. In addition to this
HEASARC representation, the database is available in a searchable,
filterable, and sortable form online through the Exoplanets Data Explorer
table at http://exoplanets.org, and the data can be plotted and explored
through the Exoplanet Data Explorer plotter which is available at that web
site. In their paper, the authors use the Data Explorer to generate
publication-ready plots, giving three examples of the signatures of exoplanet
migration and dynamical evolution: They illustrate the character of the
apparent correlation between mass and period in exoplanet orbits, the
different selection biases between radial velocity and transit surveys, and
that the multi-planet systems show a distinct semi-major-axis distribution from
apparently singleton systems.
FLARESTARS Catalog
This table contains the catalog of the UV Cet-type flare stars and
related objects in the solar vicinity. This new catalog of flare stars
includes 463 objects. It contains astrometric, spectral and photometric data
as well as information on the infrared, radio and X-ray properties and general
stellar parameters.
GALOBSTARS Catalog
An all-sky catalog of Galactic OB stars has been created by extending the
Case-Hamburg Galactic Plane Luminous Stars surveys to include 5,500
additional objects drawn from the literature. This work brings the total
number of known or reasonably suspected OB stars to over 16,000. This catalog
contains UBV photometry and MK spectral type classifications for these
objects as well as radial velocities.
This project originated in the summer of 1991 when the author began compiling
a cross-reference catalog and tabulation of published UBVbeta photometry for
stars listed in Stephenson and Sanduleak's Luminous Stars (LS) in the
Southern Milky Way Catalog (CDS Cat. III/43). This database was published in
July 1993 (Reed 1993, ApJS, 87, 367) and was subsequently expanded to include
compilations of published MK classifications (Reed & Beatty 1995, ApJS, 97,
189), 4-color photometry (Read 1996, A&AS, 117, 313), and radial velocities
(Reed & Kuhna 1997, AJ, 113, 823) for these objects. In mid-1997 the project
was again expanded to include UBVbeta photometry for stars listed in the
Northern-hemisphere volumes of the "Case-Hamburg" (CDS Cat. III/76) surveys
(Reed 1998, ApJS, 115, 271); MK classifications for the Northern stars were
similarly compiled and made electronically available to interested parties,
though they were not formally published.
Most of the LS objects are OB stars, but there are as well a number of A, F,
and G supergiants and a few white dwarfs and Wolf Rayet stars. These surveys
reached a limiting photographic magnitude of ~13.5, and were based on
objective-prism surveys of dispersion 580 Angstrom/mm at H-gamma.
OB stars is here taken to mean main-sequence stars down to temperature class
B2 and more luminous ones down to temperature class B9. The original
Case-Hamburg surveys (about 12,000 stars) also include some 2,000 evolved A-G
stars, along with some white dwarfs, planetary nebulae, and Wolf-Rayet stars.
It is worth noting that the definition of an OB star is not universal; for
example, Vanbeveren et al. (1998, in "The Brightest Stars") define them as
O-B2 V-IV, O-B3 III, O-B4 II, and all OBA Ib, Iab, Ia, and IaO stars.
GCVS Catalog
Work aimed at compiling detailed catalogs of variable stars in the Galaxy,
which has been carried out continuously by Moscow variable-star researchers
since 1946 on behalf of the International Astronomical Union, has entered the
stage of the publication of the 5th, completely electronic edition of the
General Catalog of Variable Stars (GCVS). The GCVS 5.1 is freely accessible
on the Internet. The authors recommend citing their paper as a unified
reference to the 5th edition of the GCVS.
The GCVS is the only reference source on all known variable stars. This
version contains the electronically-readable version as distributed by the
Sternberg Astronomical Institute and Institute of Astronomy (Russian Acad.
Sci.), Moscow.
After the publication of Volume III of the 4th edition of the GCVS, the
subsequent Name-lists with numbers from 67 to 77 contained only names of
variable stars in the GCVS systems, together with their coordinates and
variability types. The authors actually started compiling the 5th edition of
the GCVS ten years ago, with the 78th Name-list of Variable Stars, which
provided (as did all subsequent Name-lists) complete GCVS information for
each star (in addition to the variability types, ranges of brightness
variations, epochs of brightness maxima or minima, periods, etc.). In all,
the 78th-81st Name-lists contain more than 13300 variable stars. The complete
revision of information on the coordinates of variable stars (see the
Introduction section of the reference paper) was also a part of the
transition to the 5th edition.
The present electronic version of the GCVS5.1 is available from Sternberg
Astronomical Institute (Lomonosov Moscow University) and Institute of
Astronomy (Russian Academy of Sciences) at http://www.sai.msu.su/gcvs/gcvs/
as a first release of the fifth GCVS edition. Information on the contents and
principles of the fifth edition can be found in Samus et al. (2017), the
official reference to GCVS 5.1.
The GCVS 5.1 version contains data for individual variable objects discovered
and named as variable stars by 2021 and located mainly in the Milky Way
galaxy. The total number of named variable stars, not counting designated
non-existing stars or stars subsequently identified with earlier-named
variables, is now 58035. The stars of the GCVS 5.1 are stars of the GCVS
fourth edition plus Name-lists Nos. 67-84. The stars from the Name-lists
Nos.78-84 are presented in the complete GCVS format. Complete information for
stars of the Name-lists Nos. 67-77 is so far provided in the first 20
constellations (Andromeda to Cepheus). In these constellations, the GCVS
information has been completely revised with active use of new publications
as well as observations retrieved by the GCVS compilers by data mining and
used to determine new variability types and new light elements whenever
possible. The authors are continuing this work and will introduce new data
for the next constellations as soon as they are ready.
GCVSEGVARS Catalog
The General Catalog of Variable Stars (GCVS) is the only reference source on
all known variable stars. This database is based on the
electronically-readable version as distributed by the Sternberg Astronomical
Institute and Institute of Astronomy (Russian Acad. Sci.), Moscow. It is the
catalog of extragalactic variable stars, an updated version of the list
contained in the GCVS (4th edition), Volume V. The total number of entries in
this database is 10979 variable stars in 35 stellar systems (including the
Magellanic Clouds, the Andromeda Galaxy, etc.). These variables include 144
stars now considered to be non-members of the galaxies in whose fields they
lie, and 92 more stars that are possible non-members.
The present improved electronic version of the GCVS 4th Edition, Volumes I-V,
combined with the Name-Lists of Variable Stars Nos. 67 - 77, is also
available from the Sternberg Institute via anonymous ftp to
ftp://ftp.sai.msu.su/pub/groups/cluster/gcvs/gcvs/ and more information is
available via the Web at http://www.sai.msu.su/groups/cluster/gcvs/gcvs/.
GCVSNSVARS Catalog
This catalog is a compilation of stars that have been suspected of
variability but have (mostly) not been finally designated as variables. It is
the merging and latest updated version of the compilation of the New Catalog
of Suspected Variable Stars (NSV Catalog) originally published in 1982 by
Kukarkin et al. and the Supplement to the NSV originally published in 1998 by
Kazarovets et al. This version (NSV Release 2) has updated the previous
catalog in several ways. The accuracy of coordinates has been drastically
improved for the objects in the catalog; for most of them, the authors have
revised the photometric and spectroscopic data and updated the remarks. In
the cases with no existing finding charts, the authors recovered variability
of 2800 stars of the catalog, despite large errors of the previously
published coordinates.
The data contained in the present catalog include positions, magnitudes,
variability types, references to the literature, and spectra.
GLIESE2MAS Catalog
This table contains precise epoch 2000 coordinates and cross-identifications
to sources in the 2MASS Point Source Catalog for nearly all stars in the
Gliese, Gliese-Jahreiss, and Woolley catalogs of nearby stars. The only
Gliese objects where the authors were not successful are two Gliese sources
that are actually QSOs; two proposed companions to brighter stars, which they
believe do not exist; four stars included in one of the catalogs but
identified there as only optical companions; one probable plate flaw; and two
stars that simply remain unrecovered. For the 4251 recovered stars, 2693 have
coordinates based on Hipparcos positions, 1549 have coordinates based on
2MASS data, and 9 have positions from other astrometric sources. All
positions have been calculated at epoch 2000 using proper motions from the
literature, which are also given here.
GLOBCLUST Catalog
This is the Catalog of Parameters for Milky Way Globular Clusters (December
2010 Version) that was compiled by William E. Harris of McMaster University.
This is the first update since 2003 and the biggest single revision since the
original version of the catalog published in 1996. The list now contains a
total of 157 objects classified as globular clusters. Major upgrades have been
made especially to the cluster coordinates, metallicities, and structural
profile parameters, and the list of parameters now also includes the central
velocity dispersion.
This table contains basic parameters on distances, velocities, metallicities,
luminosities, colors, and dynamical parameters for over 150 objects that are
regarded as globular clusters in the Milky Way galaxy.
Please acknowledge the use of this catalog in any published work you derive
from it. The proper reference to the literature is the published paper
(Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the
catalog. When you cite it in your text, please use "Harris 1996 (2010
edition)". The author would also greatly appreciate receiving any new
information, in published or preprint form, which would help him to keep the
list up to date (contact W. E. Harris at harris@physics.mcmaster.ca).
A full discussion of the sources used in the creation of this catalog and of
the parameters that it contains can be found in the file:
http://physwww.mcmaster.ca/~harris/mwgc.ref.
GOSCAT Catalog
The authors have produced a catalog of 378 Galactic O stars (the GOS Catalog)
with accurate spectral classifications that is complete for V < 8 but
includes many fainter stars. The catalog provides cross-identifications with
other sources; coordinates (obtained in most cases from Tycho-2 data);
astrometric distances for 24 of the nearest stars; optical (Tycho-2, Johnson,
and Stroemgren) and NIR photometry; group membership, runaway character, and
multiplicity information.
There is also a web-based version of this catalog with links to online
services at http://www-int.stsci.edu/~jmaiz/research/GOS/GOSmain.html
HBC Catalog
This database table contains the Third Catalog of Emission-Line Stars of the
Orion Population (Herbig and Bell (1988)) which lists 735 pre-main sequence
stars, members of the Orion Population, that have been observed with slit
spectrographs or at equivalent resolution. It is intended to replace the
Second Catalog of Herbig and Rao (1972). It gives accurate coordinates (many
determined especially for this Catalog); light ranges for known variables;
UBVRI data near maximum light; references to ultraviolet, X-ray, and radio
observations, and to light curves; value of v sin i and the radial velocity
when known; spectral type; equivalent width of the H-alpha emission line;
references to spectral reproductions or scans and spectroscopic studies and to
identification charts; and a classification (as a T Tau star, FU Ori object,
etc.).
HDEC Catalog
The Henry Draper (HD) Catalog (Cannon and Pickering 1918 - 1924, Ann. Astron.
Obs. Harvard College 91 - 99) and its first extension, the Henry Draper
Extension (HDE) Catalog (Cannon 1934, Ann. Astron. Obs. Harvard College 100,
1 - 6), provided spectral classification and rough positions for 272,150
stars and has been widely made use of by the astronomical community for over
half a century. A second extension of the HD Catalog, the so-called Henry
Draper Extension Charts (HDEC), subsequently extended this spectral
classification to fainter magnitudes (Cannon 1937, Ann. Astron. Obs. Harvard
College 105, 1; Cannon and Mayall 1949, Ann. Astron. Obs. Harvard College
112), thus adding nearly another 87,000 stars with derived spectral types.
The information in the HDEC was published in the form of charts rather than
tables like the HD and HDE Catalogs, and consequently has been barely utiized
by modern astronomers. In the 1990's, after a pilot project of Roeser et al.
(1991, Astr. Ap. Suppl., 88, 277) had demonstrated that it seemed feasible to
`revive' the HDEC data, they were converted into a catalog of accurate
astrometric parameters along with magnitudes and spectral types by Nesterov
et al. (1995, Astr. Ap. Suppl., 110, 367), who used measurements of Cartesian
coordinates of stars in the charts and the positions in the Astrographic
Catalog (AC) for subsequent cross-identification. The Nesterov et al. (1991)
reference should be consulted for the full details on the procedures used to
create this HDEC catalog.
The HDEC catalog contains information on 86,933 stars, comprising accurate
(0.5 arcseconds error) positions, (for more than 96 per cent of them) proper
motions with a typical accuracy of 5.5 milliarcseconds (mas) per year, and
the original spectral classifications. The current database contains the main
portion of the catalog. An additional set of information, primarily
comprising HD entries with cross-identifications with known or suspected
variable stars, was included in the A.J. Cannon Memorial Volume (Cannon and
Mayall 1949). This list was extended by Nesterov et al. (1991) to more than
500 identifications with variable stars. This latter expanded list, together
with a list of entries which have uncertain identifications, is not included
in the HEASARC version of this catalog, but it is available on the HEASARC
website in the directory
/FTP/heasarc/dbase/misc_files/hdec/ as
the file hdec.remarks. If
the parameter "remarks" is set to "R" for an entry in the HDEC catalog, this
means that there is a remark about that particular star in the above file.
HIC Catalog
This database table contains the Hipparcos Input Main Cataloge of 118209
stars.
The Hipparcos Input Catalogue was constructed as the observing program for the
European Space Agency's Hipparcos astrometry mission. The requirements of the
project in terms of completeness, sky coverage, astrometric and photometric
accuracy, as well as the necessary optimization of the scientific impact,
resulted in an extended effort to compile and homogenize existing data, to
clarify sources and identifications, and, where needed, to collect new data
matching the required accuracy.
This has resulted in an unprecedented catalog of stellar data including
up-to-date information of positions, proper motions, magnitudes and colors, and
(wherever available) spectral types, radial velocities, multiplicity and
variability information. The catalog is complete to well-defined magnitude
limits and includes a substantial sampling of the most important stellar
categories present in the solar neighborhood beyond these limits. The
magnitudes vary from 7.3 to 9 mag as a function of galactic latitude and
spectral type, and there are no stars fainter than about V=13 mag.
The 118209 stars of the Hipparcos Input Catalogue were selected from some
214000 distinct candidates contained in some 214 observations programs.
HIPNEWCAT Catalog
A new reduction of the astrometric data as produced by the
Hipparcos mission has been published, claiming accuracies for nearly all stars
brighter than Hipparcos magnitude H_p = 8 to be better, by up to a factor 4,
than in the original catalog. The new Hipparcos astrometric catalog has been
checked for the quality of the data and the consistency of the formal errors
as well as the possible presence of error correlations. The differences with
the earlier publication of the Hipparcos Catalog are explained in the
reference paper.
The internal errors are followed through the reduction
process, and the external errors are investigated on the basis of a
comparison with radio observations of a small selection of stars, and
the distribution of negative parallaxes. Error correlation levels are
investigated and the reduction by more than a factor 10 as obtained in
the new catalog is explained. The formal errors on the parallaxes for
the new catalog are confirmed. The presence of a small amount of additional
noise, though unlikely, cannot be ruled out.
The new reduction of the Hipparcos astrometric data
provides an improvement by a factor 2.2 in the total weight compared
to the Hipparcos catalog published in 1997, and, according to the author,
provides much improved data for a wide range of studies on stellar
luminosities and local galactic kinematics.
Note that this catalog version is slightly different from the one published
in the book, as an error that sometimes affected the goodness of fit
value for the solution was corrected. The first version of these data
archived at the CDS (between June and 15 September 2008) also contained
errors which were corrected after this date.
HIPPARCOS Catalog
The Hipparcos and Tycho Catalogues are the primary products of the
European Space Agency's astrometric mission, Hipparcos. The satellite,
which operated for four years, returned high quality scientific data
from November 1989 to March 1993.
Each of the catalogues contains a large quantity of very high quality
astrometric and photometric data. In addition there are associated
annexes featuring variability and double/multiple star data, and solar
system astrometric and photometric measurements. In the case of the
Hipparcos Catalogue, the principal parts are provided in both printed
and machine-readable form (on CDROM). In the case of the Tycho
Catalogue, results are provided in machine-readable form only (on
CDROM). Although in general only the final reduced and calibrated
astrometric and photometric data are provided, some auxiliary files
containing results from intermediate stages of the data processing, of
relevance for the more-specialised user, have also been retained for
publication. (Some, but not all, data files are available from the
Centre de Donnees astronomiques de Strasbourg.)
The global data analysis tasks, proceeding from nearly 1000 Gbit of
raw satellite data to the final catalogues, was a lengthy and complex
process, and was undertaken by the NDAC and FAST Consortia, together
responsible for the production of the Hipparcos Catalogue, and the
Tycho Consortium, responsible for the production of the Tycho
Catalogue. A fourth scientific consortium, the INCA Consortium, was
responsible for the construction of the Hipparcos observing programme,
compiling the best-available data for the selected stars before launch
into the Hipparcos Input Catalogue. The production of the Hipparcos
and Tycho Catalogues marks the formal end of the involvement in the
mission by the European Space Agency and the four scientific
consortia.
For much more information about this catalog, such as fuller descriptions
of the parameters, the user is urged to check the Hipparcos and Tycho
Catalogs website at https://www.cosmos.esa.int/web/hipparcos/catalogues.
HMXBCAT Catalog
This table contains the 4th edition of the Catalog of High-Mass
X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s),
coordinates, finding charts, X-ray luminosities, system parameters, and
stellar parameters of the components and other characteristic properties for
114 HMXBs, together with a comprehensive selection of the relevant literature.
The aim of this catalog is to provide some basic information on the X-ray
sources and their counterparts in other wavelength ranges (gamma-rays, UV,
optical, IR, radio). About 60% of the high-mass X-ray binary candidates are
known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray
binaries. Some sources, however, are only tentatively identified as
high-mass X-ray binaries on the basis of their X-ray properties
similar to the known high-mass X-ray binaries. Further identification
in other wavelength bands is needed to finally determine the nature of
these sources. In cases where there is some doubt about the high-mass
nature of the X-ray binary this is noted. Literature published
before 1 October 2005 has, as far as possible, been taken into account.
Information on the numbers used to code references is available at the URL
ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz
Individual notes on each HMXB are available at the URL
ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz
HMXBCAT2 Catalog
High-Mass X-ray Binaries (HMXBs) are a particular class of high-energy
sources which require multi-wavelength observational efforts to be properly
characterized. New identifications and refinement of previous measurements
are regularly published in the literature by independent teams of researchers
and could, once collected in a catalog, offer a tool to facilitate further
studies on HMXBs. The authors aim to update on previous instances of catalogs
of HMXBs in the Galaxy, and provide the community easy access to the most
complete set of observables on Galactic HMXBs. On top of the fixed version
that is available in VizieR, they also aim to host and maintain a dynamic
version that can be updated upon request from users, and where any
modification will be logged. Using previous catalogs of HMXBs supplemented by
listings of hard X-ray sources detected in the past 20 years, the authors
produce a base set of HMXBs and candidates by means of identifier and sky
coordinate cross-matches. They query SIMBAD for unreferenced HMXBs. They
search for as many hard X-ray, soft X-ray, optical and infrared counterparts
to the HMXBs as we can in well-known catalogs and compile their coordinates.
Each HMXB is subject to a meticulous search in the literature to find
relevant measurements and their original reference. The authors provide a
catalog of HMXBs in the Galaxy with their best known coordinates, companion
star spectral type, systemic radial velocities, component masses, orbital
period, eccentricity and spin period when available. This catalog also
provides the coordinates and identifiers for each counterpart found from hard
X-rays to near-infrared, including counterparts from the recent Gaia DR3
catalog.
This catalog was created from data-mining the published literature. It takes
into account information available through 2022. Values for binary parameters
are joined with a reference in which the value was derived. Position data for
which the authors have manually found a counterpart also have a specific
reference; if not, then the data comes directly from the corresponding
catalog.
HYADESXRAY Catalog
This catalog contains the results of a complete X-ray survey of the Hyades
cluster region using X-ray data from the ROSAT All-Sky Survey (RASS)
that was published by Stern, Schmitt and Kahabka in 1995.
The Hyades survey covered over 900 square degrees of the sky. Over 185
optically identified Hyades were detected down to a limiting X-ray luminosity
of about 1-2x1028 ergs/s in the 0.1-1.8keV energy band. Among solar-like
stars, i.e., main-sequence stars of spectral type G, the RASS detection rate
was about 90%. Stern et al. argue that the presence of many binary systems
in the cluster is a key factor influencing the Hyades X-ray luminosity
function. Short-period (a few days or less) binaries are anomalously X-ray
bright, as might have been expected; however, the X-ray luminosity functions
of K and possibly M binary stars of all types are significantly different from
their single counterparts, confirming the results of Pye et al. (1994, MNRAS,
266, 798) based on a smaller K star sample drawn from deep ROSAT pointings.
Comparison with Einstein Observatory studies of a subset of Hyades stars
demonstrates a general lack of significant (> a factor of 2) long-term X-ray
variability. Stern et al. suggest that this may be the result of the dominance
of a small-scale, turbulent dynamo in the younger Hyades stars compared to the
large-scale, cyclic dynamo observed in the Sun.
The HYADESXRAY database consists of X-ray data for 440 probable and possible
Hyades members that were included in the Stern et al. survey and were listed
in Table 1 of their published paper. The database contains both stars which
were detected as X-ray sources and those which were not: for the latter,
upper limits to their X-ray emission are provided. For all listed stars,
their X-ray luminosities based on a Hyades distance of 45 pc are provided;
for some stars, for which individually determined distances from either the
Schwan (1991, A&A, 243, 386) or the Hanson (1975, AJ, 80, 379) proper motion
surveys are available, their X-ray luminosities based on these alternate
distances are also provided. There were 4 stars detected as RASS sources out
of over 180 new Hyades candidates listed in the Reid (1992, MNRAS, 257, 257)
proper motion survey which were included in Table 2 (but not Table 1) of the
Stern et al. paper. These stars are not included in the current database, but
are listed in the help section entitled Reid_Stars (q.v.). Similarly, there
were 20 stars detected as RASS sources but which were considered by Stern et
al. to be non-members of the Hyades which were included in their Table 3 (but
not Table 1). These stars are not included in the current database, but
are listed in the help section entitled Rejected_Hyades (q.v.).
INTOMCVS Catalog
The Optical Monitoring Camera (OMC) on board the high-energy INTEGRAL
satellite provides photometry in the Johnson V-band within a 5 by 5 degree
field of view. The OMC is able to detect optical sources brighter than around
V ~ 18, from a previously selected list of potential targets of interest.
After more than nine years of observations, the OMC database contains light
curves for more than 70 000 sources (with more than 50 photometric points
each). The objectives of the present work have been to characterize the
potential variability of the objects monitored by OMC, to identify periodic
sources and to compute their periods, taking advantage of the stability and
long monitoring time of the OMC.
The first catalog of variable sources observed by OMC has been developed with
observations from October 2002 to February 2010. To detect potential
variability, the authors have performed a chi-squared test, finding 5263
variable sources, for 1337 of which the periods have been determined, out of
an initial sample of 6071 objects with good photometric quality and more than
300 data points each. They have studied the potential periodicity of these
sources using a method based on the phase dispersion minimization technique,
optimized to handle light curves with very different shapes. For each object
in the catalog, the median of the visual magnitude, the magnitude at maximum
and minimum brightness in the light curve during the window of observations
and the period, when found, are provided. The types of variable objects in
the catalogue include eclipsing binaries, pulsating stars, rotating stars,
eruptive stars, extragalactic objects, X-ray binaries, cataclysmic variables,
Be stars and other objects with unknown kinds of variability.
Links to charts for each object, including the DSS image around the target,
the unfolded and folded light curves with the periods that the authors have
derived and/or with the cataloged ones are provided in this database.
IPCLXLBOL Catalog
Soft X-ray (0.2 - 3.5 keV) measurements for all normal, massive, o-type stars
surveyed with the Einstein Observatory are presented as a catalog containing 89
detections and 176 upper bounds, together with a detailed discussion of the
reduction process. Values of L[x]/L[bol] listed for most stars, range from
10e-5.44 to 10e-7.35; l[x] spans more than 3 orders of magnitude, ranging from
1.5 x 10e31 to 2 x 10e34 ergs se-1. It is noted that at least 30% of o-type
stars are variable in X-rays, but that there is little evidence for new objects
whose X-ray emission might be significantly enhanced by accretion processes
onto a neutron star. For further information, please contact the HEASARC.
LMCCLUSTRS Catalog
A new catalogue of clusters in the Large Magellanic Cloud has
been constructed from searches of the IIIa-J component of the ESO/SERC
Southern Sky Atlas. The catalogue contains coordinate and diameter
measurements of 1762 clusters in a 25 deg x 25 deg area of sky
centered on the LMC, but excluding the very crowded 3.5 square deg
region around the Bar. The distribution of these clusters appears
as two superimposed elliptical systems. The higher density inner
system extends over about 8 deg; the lower density outer system
can be represented by 13 deg X 10 deg disc inclined at 42 deg to
the line of sight. There are suggestions of two weak "arms" in the
latter.
LMCEXTOBJ Catalog
A survey of extended objects in the Large Magellanic Cloud (LMC)
was carried out on the ESO/SERC R and J Sky Survey Atlases, checking entries
in previous catalogs and searching for new objects. The census provided
6659 objects including star clusters, emission-free associations, and
objects related to emission nebulae. Each of these classes contains
three subclasses with intermediate properties, which are used to infer
total populations. The survey includes cross-identifications among
catalogs, and includes 3246 new objects (~49% of the unified catalog). The
authors have provided accurate positions, classification, and homogeneous
measurements of sizes and position angles, as well as information on cluster
pairs and hierarchical relation for superimposed objects. This unification and
enlargement of catalogs is important for future searches of fainter
and smaller new objects. The present catalog together with its
previous counterpart for the SMC and the inter-Cloud region provide a
total population of 7847 extended objects in the Magellanic System.
The angular distribution of the ensemble reveals important clues on
the interaction between the LMC and SMC.
LMXBCAT Catalog
This is the Fourth Edition of the Catalog of Low-mass X-ray
Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog
has a companion catalog of high-mass X-ray binaries (HMXBs) which is
called HMXBCAT in the HEASARC database system).
The catalog contains source name(s), coordinates, X-ray flux, system
parameters, and stellar parameters of the components and other characteristic
properties of 187 low-mass X-ray binaries, together with references to a
comprehensive selection of the relevant literature. The aim of this catalog
is to provide some basic information on the X-ray sources and their
counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and
radio). Some sources, however, are only tentatively identified as low-mass
X-ray binaries on the basis of their X-ray properties being similar to the
known low-mass X-ray binaries. Further identification in other wavelength
bands is needed to finally determine the nature of these sources. In cases
where there is some doubt about the low-mass nature of the X-ray binary,
this is mentioned. Literature published before 1 October 2006 has, as far as
possible, been taken into account.
LSPMNORTH Catalog
The LSPM catalog is a comprehensive list of 61,977 stars north of the J2000
celestial equator that have proper motions larger than 0.15" yr-1
(local-background-stars frame). The catalog has been generated primarily as a
result of the authors' systematic search for high-proper-motion stars in the
Digitized Sky Surveys using their SUPERBLINK software (note that this catalog
is consequently also sometimes referred to as the SUPERBLINK Catalog). At
brighter magnitudes, the catalog incorporates stars and data from the Tycho-2
Catalog and also, to a lesser extent, from the All-Sky Compiled Catalogue of
2.5 million stars (ASCC-2.5: Kharchenko 2001). The LSPM catalog considerably
expands over the old Luyten (Luyten Half-Second (LHS) and New Luyten
Two-Tenths (NLTT) catalogs, superseding them for northern declinations.
Positions are given with an accuracy of <~ 100 milliarcseconds (mas) at the
2000.0 epoch, and absolute proper motions are given with an accuracy of ~ 8
mas/yr. Corrections to the local-background-stars proper motions have been
calculated, and absolute proper motions in the extragalactic frame are given.
Whenever available, the authors also give optical BT and VT magnitudes
(from Tycho-2, ASCC-2.5), photographic BJ, RF, and IN magnitudes (from
the USNO-B1 catalog), and infrared J, H, and Ks magnitudes (from 2MASS). An
estimated V magnitude and V-J color is also provided for nearly all catalog
entries, which is useful for initial classification of the stars. The catalog
is estimated to be over 99% complete at high Galactic latitudes (|b| > 15
degrees) and over 90% complete at low Galactic latitudes (|b| < 15 degrees),
down to a magnitude of V = 19.0, and has a limiting magnitude V = 21.0. All
the northern stars listed in the LHS and NLTT catalogs have been
re-identified, and their positions, proper motions, and magnitudes
reevaluated. The catalog also lists a large number of completely new objects,
which promise to expand very significantly the census of red dwarfs,
sub-dwarfs, and white dwarfs in the vicinity of the Sun.
All of Luyten's NLTT stars north of the J2000 celestial equator that do NOT
appear in the LSPM Catalog are listed in Table 3 of the published paper,
together with the explanations as to why they were not included in the LSPM
Catalog.
LYNGACLUST Catalog
This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund
Observatory. The aim of this catalog is to give salient data for all known
open star clusters in our galaxy. As far as possible only published data
values have been quoted; for some of the parameters, these values have been
slected from references which can be obtained from the HEASARC.
This data in part results from the merging of the data resulting from a joint
project between K. Janes, C. Duke and Lynga, herein refered to as JDL data.
The aim of that project was to discuss properties of the open cluster system
by using existing data and by taking their accuracy into proper regard. Thus
the data were assessed, mostly by Janes, weight assigned and weighted mean
values derived of reddenings, turn-off colors and distances.
M31CLUSTRS Catalog
This database table contains a list of 288 globular cluster candidates and 132
miscellaneous objects found in a 70 arcminute square field centered on the
M 31 (Andromeda) Galaxy.
M31RBCGC Catalog
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)
M31STARS Catalog
Thie database table is a catalog of 11438 stars in the field of M31 and
8778 stars in 2 nearby "foreground" fields. It is based on a set of
Tautenburg Schmidt plates in U, B, V, and R taken by van den Bergh.
The range of visual magnitudes of stars is 11.5 < V < 20.
M31STARS2 Catalog
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).
MACS Catalog
The Magellanic Catalogue of Stars (MACS) is based on scans of ESO Schmidt
plates and contains about 244,000 stars covering large areas around the Large
Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC). The positions
refer to the FK5 system via the PPM Catalog. A comparison of positions from
different plates shows internal errors at a level of 0.15 to o.23 arcseconds;
the positional accuracy is estimated to be better than 0.5 arcseconds for 99%
of the stars. The limiting blue magnitude of the MACS is less than 16.5
magnitudes, but the catalog is not complete to this level, as only those
stars are included which are undisturbed by close neighbors as verified by
visual (interactive) screening (in order to obtain a clean astrometric
reference).
MAGHMXBCAT Catalog
This database table contains a catalog of high-mass X-ray binaries (HMXBs)
in the Small and Large Magellanic Clouds (SMC and LMC). The catalog lists
source name(s), coordinates, apparent magnitudes, orbital parameters, and
X-ray luminosities for 128 HMXBs, together with the stellar parameters of
the components, other characteristic properties and a comprehensive selection
of the relevant literature. The aim of this catalog is to provide easy access
to the basic information on the X-ray sources and their counterparts in other
wavelength ranges (UV, optical, IR, radio). Most of the sources have been
identified as Be/X-ray binaries. Some sources, however, are only tentatively
identified as HMXBs on the basis of a transient character and/or a hard X-ray
spectrum. Further identification in other wavelength bands is needed to
finally determine the nature of these sources. In cases where there is some
doubt about the high-mass nature of the X-ray binary this is mentioned.
Literature published before 1 May 2005 has, as far as possible, been taken
into account.
Information on the numbers used to code references is available at
CDS.
Individual notes on each HMXB are also available for
SMC systems
and for LMC systems
at the same site.
This Browse table contains the combination of 92 HMXBs in the SMC and 36 HMXBs
in the LMC which were listed in Tables 1 and 2, respectively, of the published
version of this catalog. The HEASARC has added a parameter called cloud_id
which can be used to identify which Magellanic Cloud any specified HMXB
belongs to (the SMC or the LMC).
MCKSION Catalog
The Web Version of the McCook-Sion White Dwarf Catalog contains
in excess of 500 more entries than the previous published version, the 4th
Edition (1999) of the Villanova White Dwarf Catalog. It is a catalog of white
dwarfs which have been identified spectroscopically. For each degenerate star,
the following data entries with references are provided:
(1) catalog coordinate designation or WD number,
(2) the right ascension and declination, (3) the spectral type based upon
the new system, (4) a catalog symbol denoting binary membership,
(5) proper motion and position angle, (6) broad-band UBV Photometry, V, B-V,
U-B, (7) multichannel spectrophotometry, V(MC), g-r, (8) Stromgren
narrow-band photometry y, b-y, u-b, (9) an absolute visual magnitude based
upon the best available color-magnitude calibration or trigonometric
parallax, (10) the observed radial velocity uncorrected for gravitational
redshift or solar motion, and (11) the trigonometric parallax, with mean
error, when available.
Note that finding charts for many of the white dwarfs present in this catalog
can be found at the following URLs:
http://procyon.lpl.arizona.edu/WD/charts/
http://deneb.astro.warwick.ac.uk/phsaap/wdcharts/
The second URL contains the finding charts from T.R. Marsh. This is list
with about 600 charts. The University of Arizona charts currently have about
2000 charts, but that list is a work in progress with the intent of
eventually having all charts available.
As discussed in more detail in the HEASARC_Implementation section, this
HEASARC representation of the White Dwarf Catalog contains only a subset of
the data presented in either the printed version or the version available at
the Villanova website, but is intended to be suitable for cross-identification
purposes with other catalogs, e.g., of X-ray sources. The original sources
for this catalog should always be consulted for the full set of information
that is available for these white dwarfs.
MDWARFASC Catalog
This table contains an all-sky catalog of M dwarf stars with
apparent infrared magnitude J < 10. The 8889 stars are selected from the
ongoing SUPERBLINK survey of stars with proper motion mu > 40 mas yr-1,
supplemented on the bright end with the Tycho-2 catalog. Completeness tests
which account for kinematic (proper motion) bias suggest that this catalog
represents ~75% of the estimated ~11,900 M dwarfs with J < 10 expected to
populate the entire sky. The catalog is, however, significantly more complete
for the northern sky (~90%) than it is for the south (~60%). Stars are
identified as cool, red M dwarfs from a combination of optical and infrared
color cuts, and are distinguished from background M giants and highly reddened
stars using either existing parallax measurements or, if such measurements are
lacking, using their location in an optical-to-infrared reduced proper motion
diagram. These bright M dwarfs are all prime targets for exoplanet surveys
using the Doppler radial velocity or transit methods; the combination of
low-mass and bright apparent magnitude should make possible the detection of
Earth-size planets on short-period orbits using currently available techniques.
Parallax measurements, when available, and photometric distance estimates are
provided for all stars, and these place most systems within 60 pc of the Sun.
Spectral type estimated from V-J color shows that most of the stars range from
K7 to M4, with only a few late M dwarfs, all within 20 pc. Proximity to the
Sun also makes these stars good targets for high-resolution exoplanet imaging
searches, especially if younger objects can be identified on the basis of
X-ray or UV excess. For that purpose, we include X-ray flux from ROSAT and
FUV/NUV ultraviolet magnitudes from GALEX for all stars for which a counterpart
can be identified in those catalogs. Additional photometric data include
optical magnitudes from Digitized Sky Survey plates and infrared magnitudes
from the Two Micron All Sky Survey.
MDWF10PCUX Catalog
M dwarfs are the most numerous stars in the galaxy. They are characterized by
strong magnetic activity. The ensuing high-energy emission is crucial for the
evolution of their planets and the eventual presence of life on them. The
authors systematically study the X-ray and ultraviolet emission of a
subsample of M dwarfs from a recent proper-motion survey, selecting all M
dwarfs within 10 pc to obtain a nearly volume-limited sample (~90%
completeness). Archival ROSAT, XMM-Newton and GALEX data are combined with
published spectroscopic studies of H-alpha emission and rotation to obtain a
broad picture of stellar activity on M dwarfs. The authors make use of
synthetic model spectra to determine the relative contributions of
photospheric and chromospheric emission to the ultraviolet flux. They also
analyze the same diagnostics for a comparison sample of young M dwarfs in the
TW Hya association (~10 Myr old). The authors find that generally the
emission in the GALEX bands is dominated by the chromosphere but the
photospheric component is not negligible in early-M field dwarfs. The surface
fluxes for the H-alpha, near-ultraviolet, far-ultraviolet and X-ray emission
are connected via a power-law dependence. The authors present in the
reference paper for the first time such flux-flux relations involving
broad-band ultraviolet emission for M dwarfs. Activity indices are defined as
the flux ratios between the activity diagnostics and the bolometric flux of
the star in analogy to the Ca II R'(HK) index. For a given spectral type,
these indices display a spread of 2-3 dex which is largest for M4-type stars.
Strikingly, at mid-M spectral types, the spread of rotation rates is also at
its highest level. The mean activity index for fast rotators, likely
representing the saturation level, decreases from X-rays over the FUV to the
NUV band and H-alpha, i.e. the fractional radiation output increases with
atmospheric height. The comparison to the ultraviolet and X-ray properties of
TW Hya members shows a drop of nearly three orders of magnitude for the
luminosity in these bands between ~10 Myr and a few Gyr age. A few young
field dwarfs (<1 Gyr) in the 10-pc sample bridge the gap indicating that the
drop in magnetic activity with age is a continuous process. The slope of the
age decay is steeper for the X-ray than for the UV luminosity. This sample is
based on the All-Sky Catalog of bright M dwarfs published by Lepine & Gaidos
(2011, AJ, 142, 138, CDS Cat. J/AJ/142/138, available at the HEASARC as the
MDWARFASC table). The authors selected all 163 stars from this reference that
are within 10pc. Four of these stars that were discovered to be actually late
K-type stars were removed from this initial sample, leaving a final sample of
159 stars.
MORBBINCAT Catalog
Orbital binary stars are essential objects for determining dynamical and
physical properties of stars through a combined analysis of photometric and
astrometric data. The authors have compiled a set of orbital binaries with
known trigonometric parallaxes and orbits of high quality, using data from
current versions of the Observatorio Astronomico Ramon Maria Aller Catalog
(OARMAC) of Orbits and Ephemerides of Visual Double Stars (Docobo et al.
2001, AcA, 51, 353) and the Sixth Catalog of Orbits of Visual Binary Stars
(ORB6: Mason and Hartkopf 2007, IAUS 240, 575; Hartkopf et al. 2001, AJ, 122,
3472), as well as including updated information from the Washington Double
Star (WDS) Catalog and SIMBAD. They constructed distributions of orbital
binaries of the dynamical mass, period, semi-major axis, and eccentricity of
systems, which characterize the set. Some problems related to the
parametrization of orbital binaries are also discussed in the paper.
To compile the orbit list, the authors combined data from both OARMAC and
ORB6. At this stage, they maintained systems without parallaxes, but removed
systems without a period or semi-major axis. The resulting list contained
3139 orbits for 2278 pairs: 1588 pairs have a single orbit, 548 pairs have
two orbits, 120 pairs have three orbits, 19 pairs have four orbits, one pair
has five orbits, and two pairs have seven orbits.
Table 1 in the reference paper (not part of this HEASARC table) contains a
compiled set of 3139 orbit solutions for visual binary stars. Separate
entries are provided for different pairs in multiple systems. Several
solutions per pair are possible. Each entry includes main orbital elements
(Semi-major axis, period, eccentricity with corresponding uncertainties),
indication of multiplicity and number of solutions, as well as visual
magnitudes, spectral classes of the components, parallax and interstellar
extinction estimate.
Table 2 in the reference paper (on which this HEASARC table is based)
contains a refined set of 652 solely binary systems with reliable orbits and
determined parallaxes. One entry in this table corresponds to one system.
Three mass estimates are provided: (1) The dynamical mass with its
uncertainty derived from Kepler's third law and its trigonometric parallax,
(2) a photometric mass estimated from the visual magnitudes, parallax and
mass-luminosity relation, and (3) a spectroscopic mass based on the
mass-spectrum relation introduced by Straizys and Kuriliene (1981, Ap&SS, 80,
353). Also provided for each system are the main orbital elements, the
parallax, and the component magnitudes and spectral types.
MWSC Catalog
Although they are the main constituents of the Galactic disk population, for
half of the open clusters in the Milky Way reported in the literature nothing
is known except the raw position and an approximate size. The main goal of
this study is to determine a full set of uniform spatial, structural,
kinematic, and astrophysical parameters for as many known open clusters as
possible. On the basis of stellar data from PPMXL and 2MASS, the authors used
a dedicated data-processing pipeline to determine kinematic and photometric
membership probabilities for stars in a cluster region. For an input list of
3,784 targets from the literature, they confirm that 3,006 are real objects,
the vast majority of them are open clusters, but associations and globular
clusters are also present. For each confirmed object, the authors determined
the exact position of the cluster center, the apparent size, proper motion,
distance, color excess, and age. For about 1,500 clusters, these basic
astrophysical parameters have been determined for the first time. For the
bulk of the clusters the authors also derived the tidal radii. In addition,
they estimated average radial velocities for more than 30% of the confirmed
clusters. The present sample (called MWSC) reaches both the central parts of
the Milky Way and its outer regions. It is almost complete up to 1.8 kpc from
the Sun and also covers the neighboring spiral arms. However, for a small
subset of the oldest open clusters (ages more than ~ 1 Gyr), the authors
found some evidence of incompleteness within about 1 kpc from the Sun.
This table contains the list of 3,006 Milky Way stellar clusters (MWSC) found
in the 2MAst (2MASS with Astrometry) catalog presented in Paper II of this
series (these clusters have source numbers below 4000), together with an
additional 139 new open clusters (these clusters have source numbers between
5000 and 6000) found by the authors at high Galactic latitudes (|b_II_| >
18.5 degrees) which were presented in Paper III of the series, and an
additional 63 new open clusters (these clusters have source numbers between
4000 and 5000) which were presented in Paper IV of the series.
The target list in Paper II from which the 3,006 open clusters was contained
was compiled on the basis of present-day lists of open, globular and
candidate clusters. The list of new high-latitude open clusters in Paper III
was obtained from a target list of 714 density enhancements found using the
2MASS Catalog. The list of new open clusters in Paper IV was obtained from an
initial list of 692 compact cluster candidates which were found by the
authors by conducting an almost global search of the sky (they excluded the
portions of the sky with |b_II_| < 5 degrees) in the PPMXL and the UCAC4
proper-motion catalogs.
For confirmed clusters, the authors determined a homogeneous set of
astrophysical parameters such as membership, angular radii of the main
morphological parts, mean cluster proper motions, distances, reddenings,
ages, tidal parameters, and sometimes radial velocities.
MYSTIXIRES Catalog
The Massive Young Star-Forming Complex Study in Infrared and X-rays (MYStIX)
project provides a comparative study of 20 Galactic massive star-forming
complexes with distances between 0.4 and 3.6 kpc. Probable stellar members in
each target complex are identified using X-ray and/or infrared data via two
pathways: (1) X-ray detections of young/massive stars with coronal
activity/strong winds or (2) infrared excess (IRE) selection of young stellar
objects (YSOs) with circumstellar disks and/or protostellar envelopes. In
this particular study, the authors present the methodology for the second
pathway using Spitzer/IRAC, 2MASS, and UKIRT imaging and photometry. Although
IRE selection of YSOs is well-trodden territory, MYStIX presents unique
challenges. The target complexes range from relatively nearby clouds in
uncrowded fields located toward the outer Galaxy (e.g., NGC 2264, the Flame
Nebula) to more distant, massive complexes situated along complicated, inner
Galaxy sightlines (e.g., NGC 6357, M 17). The authors combine IR spectral
energy distribution (SED) fitting with IR color cuts and spatial clustering
analysis to identify IRE sources and to isolate probable YSO members in each
MYStIX target field from the myriad types of contaminating sources that can
resemble YSOs: extragalactic sources, evolved stars, nebular knots, and even
unassociated foreground/background YSOs. Applying their methodology
consistently across 18 of the target complexes, they produce the MYStIX IRE
Source (MIRES) Catalog comprising 20,719 sources, including 8,686 probable
stellar members of the MYStIX target complexes. They also classify the SEDs
of 9,365 IR counterparts to MYStIX X-ray sources to assist the first pathway,
the identification of X-ray-detected stellar members.
The MYStIX project, described by Feigelson et al. (2013, ApJS, 209, 26),
provides a comprehensive, parallel study of 20 Galactic massive star-forming
regions. The basic input data for the MIRES Catalog were near-IR (NIR) and
mid-IR (MIR) photometric catalogs. The authors also used NIR and MIR images
and mosaics for visualizing the point-source populations with respect to
various nebular structures. They provide high-level descriptions of each
input catalog in section 2 of the reference paper.
This table contains the MYStIX IRE Source (MIRES) Catalog comprising IR data
on 20,719 sources, including 8,686 probable stellar members of the MYStIX
target complexes, viz., massive star-forming regions (MSFRs), which was given
in Table 2 of the reference paper. It does not include the IR data of the
above-mentioned 9,365 IR counterparts to MYStIX X-ray sources (the SED
Classification of IR Counterparts to MYStIX X-ray sources (SCIM-X Catalog)
that were listed in Table 7 of the reference paper.
MYSTIXMPCM Catalog
The Massive Young Star-forming complex Study in Infrared and X-rays (MYStIX)
project requires samples of young stars that are likely members of 20 nearby
Galactic massive star-forming regions. Membership is inferred from
statistical classification of X-ray sources, from detection of a robust
infrared excess that is best explained by circumstellar dust in a disk or
infalling envelope and from published spectral types that are unlikely to be
found among field stars. This table contains the MYStIX membership lists,
which total 31,549 probable complex members. In their reference paper, the
authors describe in detail the statistical classification of X-ray sources
via a "Naive Bayes Classifier". These membership lists provide the empirical
foundation for subsequent MYStIX science studies.
The MYStIX project, described by Feigelson et al. (2013, ApJS, 209, 26),
seeks to identify and study samples of young stars in 20 nearby (0.4 < D <
3.6kpc) Galactic massive star-forming regions (MSFRs). These samples are
derived using X-ray data from the Chandra X-ray Observatory, near-infrared
(NIR) photometry from the United Kingdom InfraRed Telescope (UKIRT) and from
the Two Micron All Sky Survey (2MASS), mid-infrared (MIR) photometry from the
Spitzer Space Telescope, and from published spectroscopically-identified
massive stars. The purpose of this study is to describe the authors' efforts
to minimize contaminants in the MYStIX catalogs of young stars. They refer to
these latter objects as the "MYStIX Probable Complex Members" or MPCMs. This
table contains the combined MPCM catalog for all 20 of the MYStIX MSFRs. This
MPCM catalog is the union of three sets of probable members identified by
three different established methods for identifying young stars (see
Feigelson et al. 2013, ApJS, 209, 26, Fig. 3).
Most of the X-ray information on the MPCMs (with the exception of the X-ray
luminosities and absorbing column densities obtained using XPHOT) was
produced by the ACIS Extract (AE) software package (Broos et al. 2010, ApJ,
714, 1582 and 2012, Astrophysics Source Code Library, 1203.001). The AE
software and User's Guide are available at
http://www.astro.psu.edu/xray/acis/acis_analysis.html. X-ray quantities using
the 'fb' prefix are for the full or total energy band from 0.5 - 8.0 keV,
those using the 'sb' prefix are for the soft band from 0.5 - 2.0 keV, and
those using the 'hb' prefix are for the hard band from 2.0 - 8.0 keV. L. K.
Townsley and P. S. Broos (2013, in preparation) and Kuhn et al. (2013, ApJS,
209, 27) identify a few very bright X-ray sources in each region that suffer
from a type of instrumental non-linearity known as photon pile-up
(http://cxc.harvard.edu/ciao/why/pileup_intro.html); X-ray properties
reported for those sources are biased and should be used with caution.
NEWMDWARFS Catalog
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 LX/Lbol 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 vtan for these stars. There is a slight
trend of decreasing chromospheric activity with age, such that the stars
with higher vtan values have lower H-alpha equivalent widths. The coronal
emission, however, remains saturated at a value of log LX/Lbol ~ -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 vtan < 40 km
s-1, suggesting that they belong to a young population.
NGC6530OID Catalog
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".
NLTT Catalog
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.
NUVBEMDCAT Catalog
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.
OPENCLUST Catalog
This is a new catalog of open clusters in the Galaxy which updates the
previous catalogs of Lynga (1987, CDS Cat. VII/92, 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, http://www.univie.ac.at/webda/). 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).
ORIYSOIR Catalog
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 NH, 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.
OSTARS Catalog
This database table is based upon the information contained in the
Catalog of Galactic O-Type Stars (Garmany, Conti, and Chiosi 1982), which is a
compilation from the literature of all O-type stars for which spectral types,
luminosity classes, and UBV photometry exist. Most of the entries come from
Cruz-Gonzalez, et al. (1974) and Humphreys (1978), with additional stars
from Garrison and Kormendy (1976); Garrison, Hiltner, and Schild (1977);
Garrison and Schild (1979); Feinstein, Marraco, and Muzzio (1973); Feinstein,
Marraco, and Forte (1976); and Moffat, Fitzgerald, and Jackson (1979).
As discussed below, the HEASARC has deleted 5 of the original 765 entries
which we believe to be erroneous and/or redundant, and modified the names
and/or positions of 14 other entries. As part of the checking process,
the HEASARC created new, more accurate positions for all the entries using the
SIMBAD database.
The catalog contains 760 stars, for each of which designations (HD, DM,
etc.), spectral types, V magnitudes, B-V magnitudes, cluster memberships,
positional information, and source references are given. In addition, the
authors have included derived values of absolute visual and bolometric
magnitudes, and distances. The source reference should be consulted for
additional details concerning the derived quantities.
PG Catalog
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
http://cdsarc.u-strasbg.fr/ftp/cats/II/207A/pg_2009.txt.
PLEIADXRAY Catalog
This catalog contains the results of a deep X-ray survey of
the core region of the Pleiades open cluster carried out with ROSAT. In
a single PSPC field (~1 degree in radius), 99 of 214 Pleiades stars are
detected in X-rays, and upper limits are computed for the remainder.
This catalog lists the characteristics of these stars taken from the
literature, including their rotational data, as well as their X-ray
characteristics. The nucleus of the composite catalog used in this study
is the catalog compiled from the published literature for the Einstein
investigations of the Pleiades (Micela et al. 1990, ApJ, 348, 557). This list
has been extended by the results of recent surveys to a completeness limit of
visual magnitude of about 18.
PMSUCAT Catalog
The Palomar/Michigan State University Catalogue contains
basic data for 1971 stars confirmed by the authors to be late K or M
main-sequence stars with absolute visual magnitudes of 8.0 or fainter
taken from Tables 1A of papers I and II and Table 1D of paper I.
Note that known degenerates have been excluded from this sample.
All but 6 of these these star were selected from the Catalogue of Nearby Stars
(Gliese & Jahreiss, "Preliminary Version of the Third Catalogue of Nearby
Stars", CNS3), and most (88%) lie within 25 parsecs.
PPM Catalog
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.
PPMXLBMD Catalog
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.
PULSAR Catalog
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.
RASSASASEB Catalog
The authors have combined their catalog of eclipsing binaries from the
All-Sky Automated Survey (ASAS) with the ROSAT All-Sky Survey (RASS) Bright
and Faint Source Catalogs (RASSBSC and RASSFSC). The combination using a
matching radius of 50 arcseconds results in 836 eclipsing binaries that
display coronal activity and is the largest sample of active binary stars
assembled to the date of publication. By using the (V-I) colors of the ASAS
eclipsing binary catalog, the authors are able to determine the distances and
thus bolometric luminosities for the majority of eclipsing binaries that
display significant stellar activity. A typical value for the ratio of soft
X-ray to bolometric luminosity is LX/Lbol ~ a few x 10-4, similar to
the ratio of soft X-ray to bolometric flux FX/Fbol in the most active
regions of the Sun. Unlike rapidly rotating isolated late-type dwarfs - stars
with significant outer convection zones - a tight correlation between Rossby
number and activity of eclipsing binaries is absent. The authors find
evidence for the saturation effect and marginal evidence for the so-called
"super-saturation" phenomena. Their work shows that wide-field stellar
variability searches can produce a high yield of binary stars with strong
coronal activity.
The authors expect that only 1.4% (i.e., 12 out of 836) of the matches
between the ASAS eclipsing binary and RASS sources will be false given their
maximum angular separation criterion of 50 arcseconds. This Browse table
excludes 29 contact binaries for which the separate distance estimates made
by the authors using the source V-band and I-band magnitudes differed by more
than 20%, and hence contains 807 (836 - 29) eclipsing and X-ray emitting
binary systems.
Complete information on ASAS and its freely accessible data are available at
the ASAS web site: http://www.astrouw.edu.pl/asas/.
RASSASASPV Catalog
Photometric data from the All-Sky Automatic Survey (ASAS) - South
(Declination less than 29 degrees) Survey have been used for the
identification of bright stars located near the sources from the ROSAT All
Sky Survey Bright Source Catalog (RASSBSC). In total, 6,028 stars brighter
than 12.5 magnitude in the I- or the V-bands have been selected and analyzed
for periodicity. Altogether, 2,302 variable stars have been found with
periods ranging from 0.137 days to 193 days. Most of these stars have X-ray
emission of coronal origin, but there are a few cataclysmic binaries and
early type stars with colliding winds. Whenever it was possible, the authors
collected data available in the literature so as to verify the periods and to
classify variable objects.
The catalog includes 1,936 stars (1,233 new) considered to be variable due to
presence of spots (rotationally variable), 127 detached eclipsing binary
stars (33 new), 124 contact binaries (11 new), 96 eclipsing stars with
deformed components (19 new), 13 ellipsoidal variables (4 new), 5
miscellaneous variables and one pulsating RR Lyr type star (blended with an
eclipsing binary). More than 70% of the new variable stars have amplitudes
smaller than 0.1 magnitudes, but for the star ASAS 063656-0521.0 the authors
have found the largest known amplitude of brightness variations due to the
presence of spots (up to Delta V = 0.8 magnitudes).
RASSCNDINS Catalog
Using new and archival observations made with the Swift satellite and other
facilities, the authors examine 147 X-ray sources selected from the ROSAT
All-Sky-Survey Bright Source Catalog (RASS/BSC) to produce a new limit on the
number of isolated neutron stars (INSs) in the RASS/BSC, the most
constraining such limit to date. Independent of X-ray spectrum and
variability, the number of INSs is <= 48 (90% confidence). Restricting
attention to soft (kTeff < 200 eV), non-variable X-ray sources - as in a
previous study - yields an all-sky limit of <= 31 INSs. In the course of
their analysis, the authors identify 5 new high-quality INS candidates for
targeted follow-up observations. A future all-sky X-ray survey with eROSITA,
or another mission with similar capabilities, can be expected to increase the
detected population of X-ray-discovered INSs from the 8 - 50 in the BSC, to
(for a disk population) 240 - 1500, which will enable a more detailed study
of neutron star population models.
Following selection of the INS candidates, short (~ 1 ks) follow-up
observations with Swift/XRT were obtained for 92 of the candidates; these
observations decreased the X-ray positional uncertainty (the systematic
positional error associated with Swift blind pointing observations is on the
order of 3.5"). The authors obtained (where possible) contemporaneous UV
observations with Swift/UVOT for counterpart identification with off-band
objects.
RASSCNS3 Catalog
This catalog presents X-ray data for all entries in the Third
Catalogue of Nearby Stars (CNS3: Gliese and Jahreiss, 1991, ADC/CDS Cat.
<V/70>) that have been detected as X-ray sources in the ROSAT All-Sky Survey
(RASS). The catalog contains 1252 entries, yielding an average detection rate
of 32.9 percent of the 3802 CNS3 stars. In addition to count rates, source
detection parameters, X-ray hardness ratios, and X-ray fluxes, X-ray
luminosities derived from Hipparcos parallaxes are also listed.
For a star to have been considered by the authors to have been detected as
an X-ray source in the RASS, an X-ray source with an existence likelihood of
7 or more (equivalent to a source existence probablity of 99.9 percent or
more) had to lie within 90 arcseconds of its 1990 epoch CNS3 position. The
choice of this cut-off radius was based on a Monte Carlo simulation of about
the same number of random positions that were used as input positions. At an
offset of 90 arcseconds between the optical and X-ray positions the probability
that the X-ray source is attributable to the star and not to a unrelated
background object is 50 percent; this probability increases very rapidly for
smaller values of the offset, notice.
RASSDSSTAR Catalog
The ROSAT All-Sky Survey (RASS) was the first imaging X-ray survey of the
entire sky. Combining the RASS Bright and Faint Source Catalogs yields an
average of about three X-ray sources per square degree. However, while X-ray
source counterparts are known to range from distant quasars to nearby M
dwarfs, the RASS data alone are often insufficient to determine the nature of
an X-ray source. As a result, large-scale follow-up programs are required to
construct samples of known X-ray emitters. The authors use optical data
produced by the Sloan Digital Sky Survey (SDSS) to identify 709 stellar X-ray
emitters cataloged in the RASS and falling within the SDSS Data Release 1
footprint. Most of these are bright stars with coronal X-ray emission
unsuitable for SDSS spectroscopy, which is designed for fainter objects (g >
15mag). Instead, the authors use SDSS photometry, correlations with the Two
Micron All Sky Survey (2MASS) and other catalogs, and spectroscopy from the
Apache Point Observatory 3.5 m telescope to identify these stellar X-ray
counterparts. Their sample of 707 X-ray-emitting F, G, K, and M stars is one
of the largest X-ray-selected samples of such stars. The authors derive
distances to these stars using photometric parallax relations appropriate for
dwarfs on the main sequence, and use these distances to calculate their X-ray
luminosities LX. They also identify a previously unknown cataclysmic
variable (CV) as a RASS counterpart.
Much more information on the SDSS is available at the project's web site at
http://www.sdss.org/.
RASSDWARF Catalog
This catalog presents X-ray data for all the main-sequence and
subgiant stars of spectral types A, F, G, and K and luminosity classes IV and
V listed in the Bright Star Catalogue (also known as the HR Catalogue) that
have been detected as X-ray sources in the ROSAT All-Sky Survey (RASS).
A number of stars in the appropriate spectral type range that do not have
assigned luminosity classes have also been included. The catalogue contains
980 such HR stars detected as X-ray sources out of a total of 3054 stars in the
HR Catalogue that satisfy the selection criteris, implying an average detection
rate of 32%. In addition to the measured ROSAT PSPC count rates,
source detection parameters, hardness ratios, and X-ray fluxes,
X-ray luminosities derived from Hipparcos parallaxes are also listed.
RASSGIANT Catalog
The ROSAT All-Sky Survey Catalogue of Optically Bright Late-Type
Giant and Supergiant Stars contains X-ray data for all late-type (spectral
types of A through M, inclusive) giants and supergiants (luminosity classes of
I through III-IV, inclusive) listed in the Bright Star Catalogue (BSC) that
have been detected in the ROSAT All-Sky Survey. The RASS giants and supergiants
catalog contains 450 entries of X-ray emitting, evolved late-type stars, which
corresponds to an average detection rate of 11.7 percent. For each star, the
ROSAT PSPC count rate, the hardness ratio, the apparent X-ray flux (calculated
using an individual energy-conversion-factor based on the hardness ratio), and
the ratio of X-ray to bolometric flux are given. The full details of the data
selection, the source detection criteria, etc., are given in the paper by
Huensch, Schmitt and Voges (1998, A&AS, 127, 251) describing this catalog;
essentially for a star to be identified as an X-ray source, the X-ray source
had to have at least a 99.9 percent existence probability, corresponding to
a likelihood of greater than or equal to 7, and lie within 90 arcseconds
of the optical position. Given the number of sky locations examined and
the total number of RASS sources, it is expected that of order 27.4 of the
450 claimed associations in this catalog will be chance coincidences.
RASSOB Catalog
For detailed statistical analysis of the X-ray emission of hot stars, stars of
spectral type O and B listed in the Yale Bright Star Catalogue were selected
and searched for in the ROSAT All-Sky Survey. This database table displays a
compilation of the derived X-ray data for a complete sample of bright OB stars.
RASSWD Catalog
This database table lists all white dwarf stars, both previously-cataloged and
newly discovered, which have been detected in the ROSAT All-Sky Survey. The
positions and count rates of the X-ray sources associated with each star
are given, as well as spectral types and other star names for those stars
which have been previously cataloged. This database table also lists distances
estimated via Balmer line profile fitting, corrected (for IS absorption)
X-ray luminosities, and each star's contribution to the X-ray luminosity
function for all DA white dwarfs which were detected in the ROSAT All-Sky
Survey.
RCW38YSO Catalog
This table contains some of the results from a study of the structure of the
high-mass star-forming region RCW 38 and the spatial distribution of its
young stellar population. Spitzer Infrared Array Camera (IRAC) photometry
(3-8 micron) is combined with Two Micron All Sky Survey (2MASS) near-IR data
to identify young stellar objects (YSOs) by IR-excess emission from their
circumstellar material. Chandra X-ray data are used to identify class III
pre-main-sequence stars lacking circumstellar material. The authors identify
624 YSOs: 23 class 0/I and 90 flat spectrum (FS) protostars, 437 class II
stars, and 74 class III stars. They also identify 29 (27 new) O star
candidates over the IRAC field. Seventy-two stars exhibit IR-variability,
including 7 class 0/I and 12 flat spectrum YSOs. A further 177 tentative
candidates are identified by their location in the IRAC [3.6] versus
[3.6]-[5.8] color-magnitude diagram. The authors find strong evidence of
subclustering in the region. Three subclusters were identified surrounding
the central cluster, with massive and variable stars in each subcluster. The
central region shows evidence of distinct spatial distributions of the
protostars and pre-main-sequence stars. A previously detected IR cluster,
DB2001_Obj36, has been established as a subcluster of RCW 38. This suggests
that star formation in RCW 38 occurs over a more extended area than
previously thought. The gas-to-dust ratio is examined using the X-ray derived
hydrogen column density, NH and the K-band extinction, and found to be
consistent with the diffuse interstellar medium, in contrast with Serpens and
NGC 1333. The authors posit that the high photoionizing flux of massive stars
in RCW 38 affects the agglomeration of the dust grains.
This table contains the list of 624 young stellar objects (given in Tables 3
and 4 of the reference paper) found among the Spitzer sources in the field of
RCW 38 using the two selection techniques described in Section 3 of the
reference paper: (1) selection of stars with IR excesses in IR color-color
diagrams, and (2) identification of X-ray luminous YSOs by comparing X-ray
sources with IR detections. The latter technique was used to identify Type
III YSOs lacking emission from a dusty disk. This table does NOT contain (i)
the 177 candidate YSOs listed in Table 5 of the reference paper which were
identified using the [3.6] versus [3.6] - [5.8] color-magnitude diagram,
since contamination removal methods could not be utilized for these objects,
(ii) the 24 candidate variable YSOs listed in Table 6 of the reference paper,
nor (iii) 21 of the 29 candidate O-star cluster members which were listed in
table 7 of the reference paper.
REVISEDLHS Catalog
The Revised Luyten Half-Second (LHS) Catalog contains refined
coordinates and proper motion data for the high proper motion (HPM) stars
listed in the Original Luyten Half-Second (LHS) catalog. The positional
uncertainty in the Original LHS catalog is typically >10" and is often >30".
The authors of the Revised LHS Catalog used the digital scans of the Palomar
Observatory Sky Survey (POSS) I and POSS II plates to derive more accurate
positions and proper motions for these objects. Out of the 4470 candidates in
the LHS catalog, 4323 objects were manually re-identified in the POSS I and
POSS II scans. A small fraction of the stars were not found due to the lack
of finder charts and digitized POSS II scans. The uncertainties in the revised
positions are typically ~2", but can be as high as ~8" in a few cases,
which is a large improvement over the original data. Cross-correlation
with the Tycho-2 and Hipparcos catalogs yielded 819 candidates (with
red magnitude m_R <~12. For these brighter sources, the position and proper
motion data were replaced with the more accurate Tycho/Hipparcos data. In
total, there are revised proper motion measurements and coordinates for
4040 stars and revised coordinates for 4330 stars.
RITTERCV Catalog
This HEASARC database table contains information on cataclysmic binaries
only, as taken from the Catalog of Cataclysmic Binaries, Low-Mass X-ray
Binaries, and Related Objects (7th Edition, Release 7.21, March 2014) of
Ritter & Kolb. The complete catalog lists coordinates, apparent magnitudes,
orbital parameters, stellar parameters of the components, and other
characteristic properties of 1166 cataclysmic binaries, 105 low-mass X-ray
binaries, and 500 related objects with known or suspected orbital periods.
The HEASARC has for simplicity split this catalog into three Browse database
tables, one for each class of objects: the present table (RITTERCV)
containing the cataclysmic binaries' data, a second one
(RITTERLMXB) containing the low-mass
X-ray binaries' data, and a third one
(RITTERRBIN) containing the related
binaries' data. The literature published before 1 January 2014 has, as far as
possible, been taken into account.
Cataclysmic binaries are semi-detached binaries consisting of a white dwarf
(or a white dwarf precursor) primary and a low-mass secondary which is filling
its critical Roche lobe. The secondary is not necessarily unevolved, it may
even be a highly evolved star, as, for example, in the case of the AM
CVn-type stars.
RITTERLMXB Catalog
This HEASARC database table contains information on low-mass X-ray binaries
(LMXBs) only, as taken from the Catalog of Cataclysmic Binaries, Low-Mass
X-ray Binaries, and Related Objects (7th Edition, Release 7.21, March 2014) of
Ritter & Kolb. The complete catalog lists coordinates, apparent magnitudes,
orbital parameters, stellar parameters of the components, and other
characteristic properties of 1166 cataclysmic binaries, 105 low-mass X-ray
binaries, and 500 related objects with known or suspected orbital periods.
The HEASARC has for simplicity split this catalog into three Browse database
tables, one for each class of objects: the present table (RITTERLMXB)
containing the low-mass X-ray binaries' data, a second one
(RITTERCV) containing cataclysmic
binaries' data, and a third one
(RITTERRBIN) containing the related
binaries' data. The literature published before 1 January 2014 has, as far as
possible, been taken into account.
Low-mass X-ray binaries are semi-detached binaries consisting of either
a neutron star or a black hole primary, and a low-mass secondary which is
filling its critical Roche lobe.
RITTERRBIN Catalog
This HEASARC database table contains information on the so-called "Related
Objects" only, as taken from the Catalog of Cataclysmic Binaries, Low-Mass
X-ray Binaries, and Related Objects (7th Edition, Release 7.21, March 2014) of
Ritter & Kolb. The complete catalog lists coordinates, apparent magnitudes,
orbital parameters, stellar parameters of the components, and other
characteristic properties of 1166 cataclysmic binaries, 105 low-mass X-ray
binaries, and 500 related objects with known or suspected orbital periods.
The HEASARC has for simplicity split this catalog into three Browse database
tables, one for each class of objects: the present table (RITTERRBIN)
containing the related binaries' data, a second one
(RITTERCV) containing cataclysmic
binaries' data, and a third one
(RITTERLMXB) containing the low-mass
X-ray binaries' data. The literature published before 1 January 2014 has, as far
as possible, been taken into account.
Related objects are detached binaries consisting of either a white dwarf or a
white dwarf precursor primary and of a low-mass secondary. The secondary may
also be a highly evolved star.
ROTXRAYCAT Catalog
This table contains photometric and derived stellar parameters for a sample
of 820 solar and late-type stars (the original table of 824 entries had 4
near-duplicate entries for the stars HD 19668, HD 95188, HD 216803 and HD
285382 which have been removed by the HEASARC) from nearby open clusters and
the field, including rotation periods and X-ray luminosities. This sample was
used by the authors to study the relationship between rotation and stellar
activity and derive a new estimate of the convective turnover time. From an
unbiased subset of this sample the power law slope of the unsaturated regime,
LX/Lbol ~ Robeta, is fit as beta = -2.70 +/- 0.13. This is
inconsistent with the canonical beta = -2 slope to a confidence of 5 sigma,
and argues for an additional term in the dynamo number equation. From a
simple scaling analysis, this implies Delta(Omega)/Omega ~ Omega0.7, i.e.
the differential rotation of solar-type stars gradually declines as they spin
down. Super-saturation is observed for the fastest rotators in this sample
and its parametric dependencies are explored. Significant correlations are
found with both the corotation radius and the excess polar updraft, the
latter theory providing a stronger dependence and being supported by other
observations. The authors estimate mass-dependent empirical thresholds for
saturation and super- saturation and map out three regimes of coronal
emission. Late F-type stars are shown never to pass through the saturated
regime, passing straight from super-saturated to unsaturated X-ray emission.
The theoretical threshold for coronal stripping is shown to be significantly
different from the empirical saturation threshold (Ro < 0.13), suggesting
it is not responsible. Instead, the authors suggest that a different dynamo
configuration is at work in stars with saturated coronal emission. This is
supported by a correlation between the empirical saturation threshold and the
time when stars transition between convective and interface sequences in
rotational spin-down models.
SACY Catalog
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 (CDS Cat. <I/239>) and Tycho-2
(CDS Cat. <I/259>) stars within an error radius of 2.6 times the positional
error of the ROSAT All-Sky Bright Source Catalogue (1RXS, CDS Cat. <IX/10>).
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).
SAISNCAT Catalog
This table comprises the Sternberg Astronomical Institute (SAI)
Catalog of Supernovae. This version contains data on 2991 extragalactic
supernovae (SNe) which were discovered from 1885 until December 12, 2004
and on their host galaxies. Data for host galaxies were compiled from
the following catalogues: (1) RC3 (de Vaucouleurs et al. 1991, Cat. <VII/155>);
(2) UGC (Nilson 1973. Cat. <VII/26>); (3) PGC (Paturel et al. 1989, Cat.
<VII/119>); (4) MCG (Vorontsov-Velyaminov et al. 1962-1968, Cat. <VII/62>,
<VII/100>); (5) ESO (Lauberts 1982, Cat. <VII/34>); (6) CfA (Huchra et al.
1994, see Cat <VII/193>), and (7) from van den Bergh (1994, Cat.
<J/ApJS/92/219>). The main source of morphological types, major diameters
and axial ratios was the RC3; the data from other sources were reduced to the
system of RC3. Photographic magnitudes of galaxies were adopted from
the UGC and the PGC together with individual data from the literature.
The sources of recession velocities or cz values were the RC3, the
CfA, the PGC and IAU Circulars. Position angles were taken from the
RC3, UGC and the ESO catalogues, and inclination angles were mainly
derived from data in RC3 according to Holmberg (1958MeLu2.136....1H).
Some data for SNe and host galaxies were adopted from the GCVS (Samus et al.
1995, Cat. <II/205>).
SAO Catalog
This database is based on the electronic version of the SAO catalog from the
Astronomical Data Center, which is itself based on an original binary version
of the Smithsonian Astrophysical Observatory Star Catalog (SAO, SAO Staff
1966). Subsequent improvements by T. A. Nagy (1979) included the addition of
cross-identifications from the Table of Correspondences SAO/HD/DM/GC (Morin
1973). As a prelude to creation of the 1984 version of the SAO, a new version
of the SAO-HD-GC-DM Cross Index was prepared (Roman, Warren, and Schofield
1983). The 1984 version of the SAO contained the corrected and extended cross
identifications, all errata published up to January 1984 and known to the ADC,
numerous errors forwarded to the ADC by colleagues, and errors discovered at
the ADC during the course of this work. Clayton A. Smith of the U. S. Naval
Observatory provided J2000.0 positions and proper motions for the SAO stars.
Published and unpublished errors discovered in the previous version (1984)
have been corrected (up to May 1991).
For this HEASARC representation, some parameters such as the RA and Dec in
radians have been omitted.
SBORBITCAT Catalog
The Ninth Catalog of Spectroscopic Binary Orbits (SB9) continues the series
of compilations of spectroscopic orbits carried out over the past 35 years by
Batten and collaborators, e.g., the 8th SBO Catalog (SB8, CDS Catalog V/64)
of Batten, Fletcher and MacCarthy 1989, Publ. DAO, 17, 1. This catalog is
regularly updated. This version of SB9 contains orbits for over three thousand
binary systems; notice that the numbers of orbits and binary systems included
in this version differ from those in the reference publication, as the latter
reflected the 2004 May 1 status of the catalog, when it had 2694 orbits for
2386 binary systems. There is an online version of this catalog, maintained
by the authors, which is continuously updated, at http://sb9.astro.ulb.ac.be/.
SDSSCVCAT Catalog
The reference paper completed the series of cataclysmic variables (CVs)
identified from the Sloan Digital Sky Survey (SDSS) I and II. The
coordinates, magnitudes, and SDSS spectra of 33 more CVs were presented.
Among the 33 are eight systems known prior to SDSS (CT Ser, DO Leo, HK Leo,
IR Com, V849 Her, V405 Peg, PG1230+226, and HS0943+1404), as well as nine
objects recently found through various photometric surveys. Among the systems
identified since the SDSS are two polar candidates, two intermediate polar
candidates, and one candidate for containing a pulsating white dwarf. A
complete summary table of the 285 CVs with spectra from SDSS I/II which were
listed in the reference paper and the 7 previous papers in the series is
contained herein.
SDSSDR10WD Catalog
The authors report the discovery of 9,088 new spectroscopically confirmed
white dwarfs and subdwarfs in the Sloan Digital Sky Survey (SDSS) Data
Release 10 (DR10). They obtain Teff, log g and masses for
hydrogen-atmosphere white dwarf stars (DAs) and helium-atmosphere white dwarf
stars (DBs), and estimate the calcium/helium abundances for the white dwarf
stars with metallic lines (DZs) and carbon/helium for carbon-dominated
spectra (DQs). They found 1 central star of a planetary nebula, 2 new oxygen
spectra on helium-atmosphere white dwarfs, 71 DQs, 42 hot DO/PG1159s, 171
white dwarf+main-sequence star binaries, 206 magnetic DAHs, 327
continuum-dominated DCs, 397 metal-polluted white dwarfs, 450
helium-dominated white dwarfs, 647 subdwarfs and 6887 new hydrogen-dominated
white dwarf stars.
The targeted white dwarfs were required to be point sources with clean
photometry, and to have USNO-B Catalog counterparts (Monet et al.. 2003, AJ,
125, 984, CDS Cat. I/284). They were also restricted to regions inside the
DR7 imaging footprint and required to have colors within the ranges g <
19.2, (u-r) < 0.4, -1 < (u-g) < 0.3, -1 < (g-r) < 0.5 and to have low
Galactic extinction Ar < 0.5 mag. Additionally, targets that did not have
(u-r) < -0.1 and (g-r) < -0.1 were required to have USNO proper motions larger
than 2 arcseconds per century (20 milliarcseconds per year). Objects
satisfying the selection criteria that had not been observed previously by
the SDSS were denoted by the WHITEDWARF_NEW target flag, while those with
prior SDSS spectra are assigned the WHITEDWARF_SDSS flag. Some of the latter
were re-observed with BOSS in order to obtain the extended wavelength
coverage that the BOSS spectrograph offers.
The color selection used includes DA stars with temperatures above ~14,000
K, helium-atmosphere white dwarfs above ~8000 K, as well as many rarer
classes of white dwarfs. Hot subdwarfs (sdB and sdO) were targeted as well.
Note that this catalog does not include stars from the earlier SDSS white
dwarf catalogs, e.g., Eisenstein et al. (2006, ApJS, 167, 40, available in
the HEASARC database as the SDSSDWDSD table), Kleinman et al. (2013, ApJS,
205, 5, available in the HEASARC database as the SDSSDR7WD table)..
SDSSDR7WD Catalog
This table contains a new catalog of spectroscopically confirmed
white dwarf stars from the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7)
spectroscopic catalog. The authors find 20,407 white dwarf spectra,
representing 19,712 stars, and provide atmospheric model fits to 14,120 DA and
1011 DB white dwarf spectra from 12,843 and 923 stars, respectively. These
numbers represent more than a factor of two increase in the total number of
white dwarf stars from the previous SDSS white dwarf catalogs based on DR4
data. The distribution of subtypes varies from previous catalogs due to the
authors' more conservative, manual classifications of each star in our catalog,
supplementing their automatic fits. In particular, they find a large number of
magnetic white dwarf stars whose small Zeeman splittings mimic increased Stark
broadening that would otherwise result in an overestimated log g if fit as a
non-magnetic white dwarf. The authors calculate mean DA and DB masses for their
clean, non-magnetic sample and find the DB mean mass is statistically larger
than that for the DAs.
This table lists the 20,407 white dwarf spectra corresponding to 19,712
distinct stars.
SDSSWDSD Catalog
This is the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4)
Catalog of White Dwarfs (WDs) and Hot Subdwarf (SD) stars. It contains 9316
spectroscopically confirmed white dwarfs which have been selected through
photometric cuts and spectroscopic modeling, backed up by a set of visual
inspections. About 6000 of the WD stars are new discoveries, roughly
doubling the number of spectroscopically confirmed WD stars. The authors
have analyzed the stars by performing temperature and surface gravity fits
to grids of pure hydrogen and helium atmospheres. Among the rare outliers
are a set of presumed helium-core DA WDs with estimated masses below
0.3 solar masses, including two candidates that may be the lowest-mass WDs
yet found. This catalog also contains a list of 928 hot SD stars.
The SDSS DR4 (Adelman-McCarthy et al. 2006, ApJS, 162, 38; see also
http://www.sdss.org/dr4/ ) contains 800,000 spectra from 4783 square degrees.
The authors have used automated techniques supplemented by visual
classification to select 13,000 candidates. An extensive analysis of
these objects has yielded 9316 white dwarfs, including 8000 DA, 713 DB,
41 DO or PG1159, 289 DC, 104 DQ, and 133 DZ types, as well as 928 hot
subdwarf stars. As well as the 10,244 primary spectra, the authors
have also presented 774 duplicate spectra of WD stars and 60 duplicate spectra
of SD stars. Thus, the present table has 11,078 (=10,244 + 774 + 60) entries.
Much more information on the SDSS is available at the project's web site
at http://www.sdss.org/.
SFGALHMXB Catalog
Based on a homogeneous set of X-ray, infrared and ultraviolet observations
from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied
populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby
star-forming galaxies and their relation with the star formation rate (SFR).
In agreement with previous results, the authors find that HMXBs are a good
tracer of the recent star formation activity in the host galaxy and their
collective luminosity and number scale with the SFR, in particular, LX ~
2.6 x 1039 x SFR. However, the scaling relations still bear a rather large
dispersion of rms ~ 0.4 dex, which the authors believe is of a physical
origin.
This table contains the catalog of 1055 compact X-ray sources detected within
the D25 ellipse for galaxies of this sample which the authors used to
construct the average X-ray luminosity function (XLF) of HMXBs with
substantially improved statistical accuracy and better control of systematic
effects than achieved in previous studies. The XLF follows a power law with
slope of 1.6 in the log(LX) ~ 35 - 40 luminosity range with a moderately
significant evidence for a break or cut-off at LX ~ 1040 erg/s. As
before, the authors did not find any features at the Eddington limit for a
neutron star or a stellar mass black hole.
In their paper, the authors discuss the implications of their results for the
theory of binary evolution. In particular, they estimate the fraction of
compact objects that once during their lifetime experienced an X-ray active
phase powered by accretion from a high mass companion and obtain a rather
large number, fX ~ 0.2 x (0.1 Myr/taux), where taux is the life time of
the X-ray active phase. This is about 4 orders of magnitude more frequent
than in low-mass X-ray binaries (LMXBs). The authors also derive constrains
on the mass distribution of the secondary star in HMXBs.
Note that, in their paper, the authors estimate that ~ 300 of the 1055
sources are likely to be background AGNs (cosmic X-ray background or CXB
sources) and that the majority (<~ 700) of the remaining ~ 750 sources are
young HMXB systems associated with star formation in their host galaxies.
SFINCSPCM Catalog
The Star Formation in Nearby Clouds (SFiNCs) project is aimed at providing a
detailed study of the young stellar populations and of star cluster formation
in the nearby 22 star-forming regions (SFRs) for comparison with the authors'
earlier MYStIX survey of richer, more distant clusters. As a foundation for
the SFiNCs science studies, in the reference paper homogeneous data analyses
of the Chandra X-ray and Spitzer mid-infrared (MIR) archival SFiNCs data are
described, and the resulting catalogs of over 15,300 X-ray and over 1,630,000
mid-infrared point sources are presented. On the basis of their
X-ray/infrared properties and spatial distributions, nearly 8500 point
sources have been identified as probable young stellar members of the SFiNCs
regions. Compared to the existing X-ray/mid-infrared publications, the SFiNCs
member list increases the census of YSO members by 6%-200% for individual
SFRs and by 40% for the merged sample of all 22 SFiNCs SFRs.
Sixty-five X-ray observations of the 22 SFiNCs SFRs made with the imaging
array on the Advanced CCD Imaging Spectrometer (ACIS) were extracted from the
Chandra archive (spanning from 2000 January to 2015 April). See Tables 1 and
2 of the reference paper for the list of SFRs and the log of Chandra ACIS
observations, respectively. The final Chandra-ACIS catalog for the 22 SFiNCs
SFRs comprises 15,364 X-ray sources (presented in Tables 3 and 4 and section
3.2 of the reference paper, and available as the HEASARC table, SFINCSXRAY).
To obtain MIR photometry for X-ray objects and to identify and measure MIR
photometry for additional non-Chandra disky stars that were missed in
previous studies of the SFiNCs regions (typically faint YSOs), the authors
have reduced the archived Spitzer-IRAC data by homogeneously applying the
MYStIX-based Spitzer-IRAC data reduction methods of Kuhn et al. (2013, ApJS,
209, 29) to the 423 Astronomical Object Request (AORs) data sets for the 22
SFiNCs SFRs (listed in Table 5 of the reference paper). As in MYStIX, the
SFiNCs IRAC source catalog retains all point sources with the photometric
signal-to-noise ratio > 5 in both [3.6] and [4.5] um channels. This catalog
covers the 22 SFiNCs SFRs and their vicinities on the sky and comprises
1,638,654 IRAC sources with available photometric measurements for 100%,
100%, 29%, and 23% of these sources in the 3.6, 4.5, 5.8, and 8.0um bands,
respectively (see table 6 and section 3.4 of the reference paper).
Source position cross-correlations between the SFiNCs Chandra X-ray source
catalog and an IR catalog, either the "cut-out" IRAC or 2MASS, were made
using the steps described in section 3.5 of the reference paper.
Using the ensemble of X-ray and infrared data that they have obtained, the
authors selected probable YSOs in the 22 SFRs using selection criteria
described in section 4.1 of the reference paper. Tables 7 and 8 of the
reference paper provide the list of 8,492 SFiNCs probable cluster members
(SPCMs: but see below for a caveat on this number) and their main IR and
X-ray properties (see section 4 of the reference paper). This present HEASARC
table comprises the contents of these two tables. A fuller list of the X-ray
properties of the X-ray-detected SPCMs is available in the HEASARC's
SFINCSXRAY table (q.v.).
SMCCLUSTRS Catalog
This is the Small Magellanic Cloud (SMC) and Inter-Magellanic Cloud ('Bridge')
portion of the 'Revised and Extended Catalog of Magellanic System Clusters,
Associations, and Emission Nebulae' (Table 2 of Bica and Schmitt 1995). A
survey of extended objects in the SMC and Bridge was carried out on the
ESO/SERC R and J Sky Survey Atlases and 1188 such objects were identified,
including 544 classified as star clusters, 343 as emissionless associations,
and 291 as emission nebulae. Only those objects which could be detected on the
ESO/SERC Schmidt films as non-stellar (typically larger than 15 arcseconds) are
included in this catalog, note. The catalog also includes cross-identifications
with previous catalogs, and 284 newly identified objects. Accurate positions,
classification, homogeneous sizes, and position angles are provided, as well
as information on cluster pairs and hierarchical relations for superimposed
objects.
SMCSTARS Catalog
An objective prism survey was conducted to discover probable members of the
Small Magellanic Cloud. Interference filters were used to restrict the
wavelength range and, hence, decrease the background and crowding. The
limiting absolute magnitude of the survey is about -4.5. The 1975 paper
listed 506 stars that show high luminosity characteristics; 193 of them had
been confirmed by other authors. The 1979 paper added 14 additional probable
members and photometric observations of 11 stars from the earlier paper that
confirmed their membership. For completeness, four new Wolf-Rayet stars
detected by Azzopardi and Breysacher (1979) were included.
The catalog contains a catalog number in order of right ascension with the
suffixes "a" or "b" used for the newer stars interpolated in the original
list. Also included are the 1975 position, the MK spectral classification,
the V magnitude, the (B-V) and (U-B) color indices, the number of
observations, the identification chart number, and remarks indicating
previous identifications.
A later catalog of the Small Magellanic Could star members is also published
by Azzopardi and Vigneau (1982A&AS...50..291A).
SMCSTARS2 Catalog
This database table contains a list of H-alpha emission-line
stars and small nebulae in the Small Magellanic Cloud (SMC) that were
discovered in an objective-prism survey. This survey was performed
through an H-alpha + [N II] interference filter using the 0.90m Curtis
Schmidt telescope at Cerro Tololo Inter-American Observatory (CTIO).
1898 emission-line objects were detected in the main body of the SMC,
almost quadrupling the number of those discovered in previous
objective-prism surveys of the same region. Among these 1898 objects
are newly discovered planetary nebulae, compact H II regions, and
late-type stars. Continuum intensities, the shapes and strengths of
the H-alpha emission line, co-ordinates and (where available)
cross-identifications are provided for the listed objects.
SPORIABYSO Catalog
This table contains results from a survey of the Orion A and B
molecular clouds undertaken with the IRAC and MIPS instruments on board
Spitzer. In total, five distinct fields were mapped, covering 9 deg2 in five
mid-IR bands spanning 3 - 24 microns (um). The survey includes the Orion Nebula
Cluster, the Lynds 1641, 1630, and 1622 dark clouds, and the NGC 2023, 2024,
2068, and 2071 nebulae. These data are merged with the Two Micron All Sky
Survey point source catalog to generate a catalog of eight-band photometry. The
authors identify 3479 dusty young stellar objects (YSOs) in the Orion molecular
clouds by searching for point sources with mid-IR colors indicative of
reprocessed light from dusty disks or in-falling envelopes. The YSOs are
subsequently classified on the basis of their mid-IR colors and their spatial
distributions are presented. The authors classify 2991 of the YSOs as
pre-main-sequence stars with disks and 488 as likely protostars. Most of the
sources were observed with IRAC in two to three epochs over six months; the
authors search for variability between the epochs by looking for correlated
variability in the 3.6 and 4.5 um bands. They find that 50% of the dusty YSOs
show variability. The variations are typically small (~ 0.2 mag) with the
protostars showing a higher incidence of variability and larger variations.
The observed correlations between the 3.6, 4.5, 5.8, and 8 um variability
suggests that we are observing variations in the heating of the inner disk due
to changes in the accretion luminosity or rotating accretion hot spots.
SYMBIOTICS Catalog
This database table contains a catalog of confirmed and suspected symbiotic
stars. The list includes 188 symbiotic stars as well as 30 objects suspected
of being symbiotic. For each star, basic observational material is presented:
coordinates, V and K magnitudes, ultraviolet (UV), infrared (IR),
X-ray and radio observations. Also listed are the spectral type of the
cool component, the maximum ionization potential observed, references
to finding charts, spectra, classifications and recent (as of 2000) papers
discussing the physical parameters and nature of each object.
This table does NOT contain the information on orbital photometric ephemerides
and orbital elements of known symbiotic binaries, pulsational periods for
symbiotic Miras, Hipparcos parallaxes and information about outbursts
and flickering that is contained in the printed version of the catalog (see
Tables 3-7 in the paper for this material).
TYCHO2 Catalog
The Hipparcos and Tycho catalogs are the primary products of the European
Space Agency's astrometric mission, Hipparcos. The satellite, which operated
for four years, returned high quality scientific data from November 1989 to
March 1993.
The Tycho-2 catalog is an astrometric reference catalog containing positions
and proper motions as well as two-color photometric data for the 2.5 million
brightest stars in the sky. The Tycho-2 positions and magnitudes are based on
precisely the same observations as the original Tycho catalog (hereafter
Tycho-1; see CDS Cat. I/239) collected by the star mapper of the ESA
Hipparcos satellite, but Tycho-2 is much bigger and slightly more precise,
owing to a more advanced reduction technique. Components of double stars with
separations down to 0.8 arcsec are included. Proper motions precise to about
2.5 mas/yr are given as derived from a comparison with the Astrographic
Catalogue and 143 other ground-based astrometric catalogs, all reduced to the
Hipparcos celestial coordinate system. Tycho-2 supersedes in most
applications Tycho-1, as well as the ACT (CDS Cat. I/246) and the TRC (CDS
Cat. I/250) catalogs based on Tycho-1.
Supplement-1 (not part of this HEASARC database but available at
https://cdsarc.cds.unistra.fr/ftp/cats/I/259/suppl_1.dat.gz) lists stars from
the Hipparcos and Tycho-1 catalogs which are not in Tycho-2.
Supplement-2 (not part of this HEASARC database but available at
https://cdsarc.cds.unistra.fr/ftp/cats/I/259/suppl_2.dat.gz) lists 1146
Tycho-1 stars which are probably either false or heavily disturbed.
The principal characteristics of the Tycho-2 catalog are
summarized below. By means of proper motions the positions
are transferred to the year 2000.0, the epoch of the catalog.
The median values of internal standard errors are given:
Mean satellite observation epoch ~J1991.5
Epoch of the Tycho-2 catalog J2000.0
Reference system ICRS
coincidence with ICRS (1) +/-0.6 mas
deviation from inertial (1) +/-0.25 mas/yr
Number of entries 2,539,913
Astrometric standard errors (2)
V_T < 9 mag 7 mas
all stars, positions 60 mas
all stars, proper motions 2.5 mas/yr
Photometric std. errors (3) on V_T
V_T < 9 mag 0.013 mag
all stars 0.10 mag
Star density
b= 0 deg 150 stars/sq.deg.
b= +/-30 deg 50 stars/sq.deg.
b= +/-90 deg 25 stars/sq.deg.
Completeness to 90 per cent V ~ 11.5 mag
Completeness to 99 per cent V ~ 11.0 mag
Number of Tycho observations ~300 106
Note (1): about all 3 axes
Note (2): ratio of external to internal standard errors is ~1.0
for positions and for proper motions. Systematic errors
are less than 1 mas and 0.5 mas/yr
Note (3): ratio of photometric external to internal standard errors
at V_T > 9 mag is below 1.5
For more information on the original catalog, please consult the Tycho-2
home page at http://www.astro.ku.dk/~erik/Tycho-2
For more information on the HEASARC implementation of the Tycho-2 catalog,
please consult the "HEASARC Implementation" section
of this help.
ULXRBCAT Catalog
This table is a catalog of ultraluminous X-ray sources (ULXs) in external
galaxies, where ULXs have been defined as compact, off-nuclear X-ray sources
with X-ray luminosities in the range of 1039 - 1041 erg/s. The aim of this
catalog is to provide easy access to the properties of ULXs, their possible
counterparts at other wavelengths (optical, IR, and radio), and the
properties of their host galaxies. The catalog contains 229 ULXs found in 85
galaxies which had been reported in the astronomy literature as of April
2004. Most ULXs are stellar-mass-black hole X-ray binaries, but it cannot be
excluded that some ULXs might be intermediate-mass black holes. A small
fraction of the candidate ULXs might be background Active Galactic Nuclei
(AGN) or Supernova Remnants (SNRs). ULXs with luminosity above 1040 erg/s
are found in both starburst galaxies and in the halos of early-type galaxies.
Some notes on individual galaxies and/or ULXs in this catalog can be found in
the file https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/429/1125/notes.dat
which is available at the CDS.
UVOTBSCAT Catalog
This catalog was compiled from 4 catalogs: Tycho-2, GVCS III, NGC, and the
Yale Bright Star Catalog. All catalogs were preprocessed before compiling
this catalog to achieve uniform columns and units. Next, they were merged
into one catalogue before eliminating "red" objects and precessing all
coordinates to epoch 2000.0. The catalog was then corrected for missing
decimal points. Finally, the catalog was sorted by R.A. for ease of locating
objects within the catalogue. The original catalog contained 239,853 objects
brighter than 12.0 mags.
VLAGBSOPH Catalog
This table contains results from large-scale (~2000 arcmin2), deep (~20
microJy), high-resolution (~1") radio observations of the Ophiuchus
star-forming complex obtained with the Karl G. Jansky Very Large Array (JVLA)
at wavelengths of 4 and 6 cm (frequencies of 7.5 and 4.5 GHz). In total, 189
sources were detected, 56 of them associated with known young stellar objects
(YSOs), and 4 with known extragalactic objects; the other 129 remain
unclassified, but most of them are most probably background quasars. The vast
majority of the young stars detected at radio wavelengths have spectral types
K or M, although four objects of A/F/B types and two brown dwarf candidates
are also detected. At least half of these young stars are non-thermal
(gyrosynchrotron) sources, with active coronae characterized by high levels
of variability, negative spectral indices, and (in some cases) significant
circular polarization. As expected, there is a clear tendency for the
fraction of non-thermal sources to increase from the younger (Class 0/I or
flat spectrum) to the more evolved (Class III or weak-line T Tauri) stars.
The young stars detected both in X-rays and at radio wavelengths broadly
follow a Gudel-Benz relation, but with a different normalization than the
most radio-active types of stars. Finally, the authors detected a ~70 mJy
compact extragalactic source near the center of the Ophiuchus core, which
should be used as gain calibrator for any future radio observations of this
region.
The observations were obtained with the JVLA of the National Radio Astronomy
Observatory (NRAO). Two frequency sub-bands, each 1-GHz wide, and centered at
4.5 and 7.5 GHz, respectively, were recorded simultaneously. The observations
were obtained on three different epochs (2011 February 17/19, April 3/4, and
May 4/6) typically separated from one another by a month. The angular
resolution of the observations is of the order of 1 arcsecond.
To identify sources in their observations, the authors used the images
corresponding to the concatenation of the three epochs, which provided the
highest sensitivity. The criteria used to consider a detection as firm were:
(1) sources with reported counterparts and a flux larger than four times the
rms noise of the area, or (2) sources with a flux larger than five times the
rms noise of the area and without reported counterparts.
The authors searched the literature for previous radio detections, and for
counterparts at X-ray, optical, near-infrared, and mid-infrared wavelengths.
The search was done in SIMBAD, and accessed all the major catalogs (listed
explicitly in the footnote of Table 3 in the reference paper). Note that the
Spitzer c2d catalog includes cross-references to other major catalogs which
were taken into account in their counterpart search. The authors considered a
radio source associated with a counterpart at another wavelengths if the
separation between the two was below the combined uncertainties of the two
data sets. This was about 1.5 arcseconds for the optical and infrared
catalogs, but could be significantly larger for some of the radio catalogs
(for instance, the NVSS has a positional uncertainty of about 5 arcseconds).
The authors found that only 76 of the sources detected here had previously
been reported at radio wavelengths (matches are listed in the radio_name
parameter in such cases), while the other 113 are new radio detections. On
the other hand, they found a total of 100 counterparts at other wavelengths.
Note that there are a significant number of sources that were previously
known at radio wavelengths and have known counterparts at other frequencies.
As a consequence, the number of sources that were previously known (at any
frequency) is 134, while 55 of the sources in this sample are reported here
for the first time. The authors argue that most of these 55 objects are
likely background sources. They note, however, that 18 of the 129
unclassified objects (55 identified here for the first time and 74 previously
known at radio wavelengths) are compact, have a positive spectral index, or
exhibit high variability. Since these latter two properties are not expected
of quasars (which are certainly variable, but usually not strongly on such
short timescale), but would be natural characteristics of young stars, the
authors argue that a small population of YSOs might be present among the
unclassified sources. This population could account for, at most, 15% of the
unclassified sources, and possibly significantly less.
VLAGBSORI Catalog
This table contains results from a high-sensitivity (60 microJy), large-scale
(2.26 deg2) survey obtained with the Karl G. Jansky Very Large Array (JVLA)
as part of the Gould's Belt Survey (GBS) program. The authors detected 374
and 354 sources at 4.5 and 7.5 GHz, respectively. Of these, 148 are
associated with previously known young stellar objects (YSOs). Another 86
sources previously unclassified at either optical or infrared wavelengths
exhibit radio properties that are consistent with those of young stars. The
overall properties of these sources at radio wavelengths such as their
variability and radio to X-ray luminosity relation are consistent with
previous results from the GBS. These detections provide target lists for
follow-up Very Long Baseline Array radio observations to determine their
distances, as YSOs are located in regions of high nebulosity and extinction,
making it difficult to measure their optical parallaxes.
The observations were obtained with the JVLA of the National Radio Astronomy
Observatory (NRAO) in its A configuration. The observations of the 210 fields
in the Orion Molecular Clouds A and B were obtained in three different epochs
(2011 June 25 to July 4, July 23 to 30, and August 25 to 29, as described in
Table 1 of the reference paper) typically separated from one another by a
month. The 210 individual fields have been split into 7 maps, with 30 fields
being observed per map, as follows: 12 in the lambda Ori region, 3 in L1622,
27 are shared between NGC 2068 and NGC 2071, 14 are shared between NGC 2023
and NGC 2024, 11 in the sigma Ori region, 109 in the Orion Nebula Cluster
(ONC), 16 in L1641-N, 8 in L1641-C, and 10 in L1641-S (see Figures 1 to 7 in
the reference paper). Two frequency sub-bands, each 1-GHz wide, and centered
at 4.5 and 7.5 GHz, respectively, were recorded simultaneously. The authors
achieved a nearly uniform rms noise of 60 microJy beam-1 at both
frequencies in all the regions. The only exception to this is in the
Trapezium region due to nebular emission; there the noise was 200 microJy
beam-1 after excluding baselines smaller than 150 kilo-lambda during
imaging to remove extended emission.
Sources were identified through a visual inspection of the individual fields
at 4.5 GHz during the cleaning and imaging process since an automated source
identification was deemed to be not sufficiently advanced and produced
results that were too unreliable. In particularly clustered regions such as
the Trapezium and NGC 2024, in addition to standard imaging, data from all
three epochs were combined into a single image for source identification
purposes only to improve statistical significance of each detection. The
authors detected a combined total of 374 sources among the three epochs for
all of the regions. All sources but one had fluxes greater than five times
the rms noise in at least one epoch. The remaining source, 'GBS-VLA
J053518.67-052033.1', was detected at two epochs with maximum detection
probability of 4.9 sigma in a single epoch data. It is found in the Trapezium
region, and has known counterparts in other wavelength regimes.
The authors cross-referenced their catalog of sources with previous major
radio, infrared, optical and X-ray surveys of the regions published in the
literature. They have generally considered sources in these surveys to be
counterparts if they had positional coincidences less than 1 arcsecond, but
have allowed for larger offsets if the combined uncertainty between the
databases was large. Of 374 detected sources, 261 have been previously found
at another wavelength region, while 113 are new detections. 146 sources have
been detected in X-rays, 94 at optical wavelengths, 218 at infrared, and 63
in previous radio surveys. Of the previously identified sources, 1 is
extragalactic, while the other 148 as young stellar objects (YSOs). Of the
YSOs, 106 have been placed on the standard class system based on the IRAC
color-color classification of Allen et al. (2004, ApJS, 154, 363). There are
11 Class 0/I, 26 Class II, and 70 Class III type stars. A total of 225
sources are either new detections or, to the authors' knowledge, have not
been previously classified in the literature. Of these remaining objects,
they have identified 86 as exhibiting variability or high levels of circular
polarization. While the authors cannot exclude the possibility that any of
them are extragalactic in nature, quasars are not expected to vary as
strongly on timescales of few weeks to few months, and exhibit very weak
circular polarization, so these sources (listed in Table 5 of the reference
paper) are likely YSO candidates. Using the same criteria of variability and
circular polarization would identify only 107 of the 148 previously-known
YSOs; thus we cannot tell which of the remaining 139 unidentified sources are
YSOs or extragalactic objects.
VLAGBSSER Catalog
This table contains results from a deep (~17 µJy) radio continuum
observations of the Serpens molecular cloud, the Serpens south cluster, and
the W40 region that were obtained using the Jansky Very Large Array (JVLA) in
its A configuration. The authors detected a total of 146 sources, 29 of which
are young stellar objects (YSOs), 2 of which are BV stars, and 5 more of
which are associated with phenomena related to YSOs. Based on their radio
variability and spectral index, the authors propose that about 16 of the
remaining 110 unclassified sources are also YSOs. For approximately 65% of
the known YSOs detected here as radio sources, the emission is most likely
non-thermal and related to stellar coronal activity. As also recently
observed in Ophiuchus, this sample of YSOs with X-ray counterparts lies below
the fiducial Guedel & Benz (1993, ApJ, 405, L63) relation. In the reference
paper, the authors analyze the proper motions of nine sources in the W40
region, thus allowing them to better constrain the membership of the radio
sources in the region.
The Serpens molecular cloud and the Serpens South cluster were observed in
the same observing sessions on three different epochs (2011 June 17, July 19,
and September 12 UT), using 25 and 4 pointings, respectively, with the JVLA
at 4.5 and 4.5GHz. The W40 region, on the other hand, was only observed on
two epochs (2011 June 17 and July 16), using 13 pointings. The details of the
observations are listed in Table 1 of the reference paper.
The authors adopted the same criteria as Dzib et al. (2013, ApJ, 775, 63) to
consider a detection as firm. For new sources, i.e., those without reported
counterparts in the literature, they considered 5-sigma detections, where
sigma is the rms noise of the area around the source. For known sources with
counterparts in the literature, on the other hand, they included 4-sigma
detections. According to these criteria, they detected 94 sources in the
Serpens molecular cloud, 41 in the W40 region, and 8 in the Serpens South
cluster, for a total of 143 detections. Out of the 143 sources, 69 are new
detections (see Section 3.2 of the reference paper).
GBS-VLA source positions were compared with source positions from X-ray,
optical, near-IR, mid-IR, and radio catalogs. GBS-VLA sources were considered
to have a counterpart at another wavelength when the positional coincidences
were better than the combined uncertainties of the two data sets. These were
about 1 arcsecond for the IR catalogs. For the X-ray and radio catalogs it
depended on the instrument and its configuration. The search was done in
SIMBAD and included all the major catalogs. The authors also accessed the
lists with all YSOs in the c2d-GB clouds compiled by Dunham et al.(2013, AJ,
145, 94) and L.E. Allen et al. (2015, in preparation). In total, 354 c2d-GB
sources lie inside the regions observed by the present survey. In order to
find their radio counterparts, the authors imaged regions of 64 pixels in
each dimension, centered in the c2d-GB positions, and combining accordingly
with each region, the three or two epochs. For this search, they only used
the field whose phase center was closest to the source. Three additional
radio sources were found in Serpens South in this pursuit, increasing the
number of the radio detections to 146.
VLAGBSTAU Catalog
This table contains results from a multi-epoch radio study of the
Taurus-Auriga complex made with the Karl G. Jansky Very Large Array (JVLA) at
frequencies of 4.5 GHz and 7.5 GHz. A total of 610 sources were detected, 59
of which are related to young stellar objects (YSOs) and 18 to field stars.
The properties of 56% of the young stars are compatible with non-thermal
radio emission. The authors also show that the radio emission of more evolved
YSOs tends to be more non-thermal in origin and, in general, that their radio
properties are compatible with those found in other star-forming regions. By
comparing their results with previously reported X-ray observations, the
authors noticed that YSOs in Taurus-Auriga follow a Guedel-Benz relation with
a scaling factor, kappa, of 0.03, as they previously suggested for other
regions of star formation. In general, YSOs in Taurus-Auriga and in all the
previous studied regions seem to follow this relation with a dispersion of ~1
dex. Finally, the authors propose that most of the remaining sources are
related with extragalactic objects but provide a list of 46 unidentified
radio sources whose radio properties are compatible with a YSO nature
(identified in this implementation of their catalog by values for the
parameter radio_yso_flag of 'Y').
The observations were obtained with the JVLA of the National Radio Astronomy
Observatory (NRAO) in its B and BnA configuration. Two frequency sub-bands,
each 1 GHz wide, and centered at 4.5 and 7.5 GHz, respectively, were recorded
simultaneously. The observations were obtained in three different time
periods (February 25/26/28 to March 6, April 12/17/20/25, and April 30 to May
1/5/14/22, all in 2011) typically separated from one another by a month: see
Table 1 of the reference paper for more details. For their study, the authors
observed 127 different target fields distributed across the cloud complex
(Figure 1 of the reference paper). The fields were chosen to cover previously
known YSOs. In 33 of those fields, the authors could observe more than one
YSO target, while in the remaining 94 fields, only one YSO was targeted. In
most cases, the infrared evolutionary class (i.e., Classes I, II, or III) or
T Tauri evolutionary status (classical or weak line) of the targeted sources
was known from the literature.
The final images covered circular areas of 8.8 and 14.3 arcminutes in
diameter, for the 7.5 and 4.5 GHz sub-bands, respectively, and were corrected
for the effects of the position-dependent primary beam response. The noise
levels reached for each individual observation was about ~40 microJy and ~30
microJy, at 4.5 GHz and7.5 GHz, respectively. The visibilities of the three,
or two, observations obtained for each field were concatenated to produce a
new image with a lower noise level (of about ~25 microJy at 4.5 GHz and ~18
microJy at 7.5 GHz). The angular resolution of ~1 arcsecond (see the
synthesized beam sizes in Table 1 of the reference paper) allows an
uncertainty in position of ~0.1 arcseconds or better.
In the observed area, there are a total of 196 known YSOs.The first step was
the identification of radio sources in the observed fields. The authors
follow the procedure and criteria presented by Dzib et al. (2013, ApJ, 775,
63) who consider a detection as firm if the sources have a flux larger than 4
times the noise level and there is a counterpart known at another wavelength,
else they require a flux which is 5 times the noise level. The identification
was done using the images corresponding to the concatenation of the observed
epochs, which provides the highest sensitivity. From this, a total of 609
sources were detected. Of these sources, 215 were only detected in the 4.5
GHz sub-band, while six were only detected in the 7.5 GHz sub-band. The
remaining 388 sources were detected in both sub-bands.
The authors searched the literature for previous radio detections, and for
counterparts at X-ray, optical, near-infrared, and mid-infrared wavelengths.
The search was done using SIMBAD, and accessed all the major catalogs. They
considered a radio source to be associated with a counterpart at another
wavelength if the separation between the two was below the combined
uncertainties of the two data sets. This was about 1.0 arcsecond for the
optical and infrared catalogs, but could be significantly larger for some of
the radio catalogs (for instance, the NVSS has a positional uncertainty of
about 5 arcseconds). They found that only 120 of the sources detected here
had previously been reported at radio wavelengths, while the other 491 are
new radio detections. On the other hand, the authors found a total of 270
counterparts at other wavelengths. In the literature, 18 are classified as
field stars, 49 as extragalactic, 1 is classified as either a star or an
extragalactic source in different surveys, 49 are classified as YSOs, 11 are
classified as either YSO and extragalactic, and the remaining 143 sources are
unclassified. Note that 56 sources were previously known at radio wavelengths
but do not have known counterparts at other frequencies. As a consequence,
the number of sources that were previously known (at any frequency) is 327,
while 284 of the sources in this sample are reported here for the first time.
VLULXCAT Catalog
Using Chandra archive data, the authors conducted a thorough survey of
luminous X-ray sources. They directly analyzed about 9400 Chandra ACIS
observations and cross-correlated the detected X-ray sources with 77,000
galaxies within a distance of 250 Mpc. The final catalog includes 119 unique
luminous X-ray source candidates with LX > 3 x 1040 erg/s from 93
galaxies or 41 HLX candidates with LX > 1 x 1041 erg/s from 35 galaxies.
The authors derive a moderate contamination rate due to foreground or
background sources. In the reference paper, they also cross-correlate the
catalog with FIRST, perform variability and periodicity tests, and analyze
one HLX candidate in particular. This catalog could be a starting point to
perform follow-up observations.
In order to know whether an X-ray source falls within a particular galaxy,
for each galaxy, the authors collected its center's RA, Dec, distance, and
D25 isophotal info, which includes major axis length, minor axis length,
and the position angle of the major axis from the PGC2003 Catalog (Paturel et
al. 2003, A&A, 412, 45), which includes the full RC3 catalog and has all of
the necessary parameters except for distance. The authors restricted the
minimum major axis length to be 10 arcseconds, and collected their distances
from NED as much as possible. Their final sample includes 77,000 galaxies
within 250 Mpc.
The authors used all of the Chandra ACIS data in TE mode that were released
before 2014, which includes 9400 ObsIDs. A roughly linear relation between
the flux and count rate derived by PIMMS 4.6b was established assuming a
power-law spectral shape and galactic foreground extinction (Kalberla et al.
2005, A&A, 440, 775). Any source with a PIMMS luminosity larger than 5 x
1039 erg s-1 would be recalculated by the CIAO script model flux assuming
a power-law index of 1.7 in the 0.3 - 8.0 keV energy band. After the
recalculation, 1,809 X-ray sources with Lx > 3 x 1040 erg s-1 falling
within 640 D25 contours covered by 905 ObsIDs were picked out. A large
fraction of the 1,809 sources are galactic nuclei and some of them are
repeated. Only off-nuclear sources are considered in this paper. In addition,
the centers of the galaxies given by PGC2003 are not necessarily precise and
the specific environments of the 1,809 sources are different. Therefore, the
authors visually checked the Chandra and DSS images simultaneously, since
two-band inspection can help to exclude the nuclear sources, bright knots,
and extended sources. X-ray sources with clear DSS features would be dropped
because, for a source with a visual magnitude <20 and a distance >30 Mpc, its
absolute magnitude would be brighter than -12.4, which is beyond the limit of
the brightest star clusters.
WACKERLING Catalog
The Wackerling Catalog contains entries for 5326 early-type emission-line
stars. Of these stars, 1424 have no spectral classification but are assumed
to be of early type. Some 71 percent of the stars in this catalog can also be
found in the Mount Wilson and the Mount Wilson-Michigan survey catalogs. The
Wackerling Catalog contains numerous cross identifications to other
designations (common name, HD, DM, LS, MWC, TON, HIL, WRA, HEN, etc.), rough
spectroscopic types, magnitudes (visual and blue), and positions.
The version of the Wackerling Catalog on which the HEASARC database is based
was obtained from the ADC and differs in some respects from the original
published version, notice.
WDS Catalog
The Washington Double Star Catalog (WDS), maintained by the United States
Naval Observatory (USNO), is the world's principal database of astrometric
double and multiple star information. The WDS Catalog contains positions,
discoverer designations, epochs, position angles, separations, magnitudes,
spectral types, proper motions and when available, Durchmusterung numbers and
notes for the components of close to 100,000 systems based on ~600,000 means.
The current version at the HEASARC is updated weekly and is derived from the
version available online at https://crf.usno.navy.mil/wds/ (and mirrored at
http://www.astro.gsu.edu/wds/), the latter being potentially updated nightly.
The Washington Visual Double Star Catalog (WDS) is the successor to the Index
Catalogue of Visual Double Stars, 1961.0 (IDS; Jeffers & van den Bos, 1963).
Three earlier double star catalogs in the 20th century, those by Burnham
(BDS; 1906), Innes (SDS; 1927), and Aitken (ADS; 1932), each covered only a
portion of the sky. Both the IDS and the WDS cover the entire sky, and the
WDS is intended to contain all known visual double stars for which at least
one differential measure has been published. The WDS is continually updated
as published data become available. Prior to this, two major updates have
been published (Worley & Douglass 1984, 1997). The Washington Double Star
Catalog (WDS) has seen numerous changes since the last major release of the
catalog. The application of many techniques and considerable industry over
the past few years has yielded unprecedented gains in both the number of
systems and the number of measures.
WOODEBCAT Catalog
This catalog, also called the Finding List (FL) of Interacting Binaries (5th
edition), was abstracted from the Card Catalog maintained
at the University of Florida which contains information on all published, and
to the extent available, unpublished work on eclipsing binaries.
The Card Catalog originated with Raymond Smith Dugan in the 1930's, who
published from it the first edition of "A Finding List for Observers of
Eclipsing Variables" (Dugan 1934, Princeton Univ. Obs. Contrib. No. 15).
Successive editions of FL were subsequently published by Pierce (1947,
Princeton Univ. Obs. Contrib. No. 22), by Wood (1953, Univ. Pennsylvania
Astron. Series, Vol. VIII), by Koch et al. (1963, Univ. Pennsylvania
Astron. Series, Vol. IX), and by Wood et al. (1980, Univ. Pennsylvania
Astron. Series, Vol. XII). The FL was conceived as an aid to observers
of eclipsing variables in selecting an observing program efficiently from
the collection of all known data in an easy-to-use format. Although this
format has changed over the years to meet existing requirements, the basic
information content remains the same. The current edition differs from
previous ones in the extension of the magnitude limit at minimum light from
13 to 15. In earlier editions, a binary system was not included unless the
editors were reasonably certain that the system was indeed an eclipsing or
(rarely) an ellipsoidal variable. The fifth edition includes all systems that
the editors were fairly certain are either eclipsing or radiometrically
variable binaries.
The catalog fields are Finding List number; star name; position (given in the
original catalog in equinox 1900); blue magnitude at maximum light; bandpass
of maximum light; depth of primary minimum in same bandpass; bandpass primary
minimum; depth of secondary minimum and its bandpass; spectral class of star
eclipsed at primary light and optional uncertainty character; spectral class
of star eclipsed at secondary light; most recent reliable epoch of
primary minimum; most recent orbital period; duration of primary
minimum; duration of totality of primary minimum; BD, CoD, CPD, and
HD number; alternate designations of system; and codes indicating the
nature of the system.
WOOLLEY Catalog
This catalog was constructed at the Royal Greenwich Observatory in order to
enlarge the Gliese (1957, Mitt. Astron. Rechen-Inst., Ser. A, No. 8)
compilation. It contains data on stars nearer than 25 pc that were not
included in that version of Gliese's catalog, plus some additional
information that had been published after 1957 on stars which were present in
the 1957 version of the Gliese catalog. The electronic version contains
essentially all information given in Table Ia of the published Woolley
catalog, plus positional data, and most cross references to other catalogs
given in Table IIa. The notes flags in Table Ia are not included because the
notes are not machine-readable. Omitted from Table IIa are the finding-chart
indicators (Lowell G numbers or notes references) and miscellaneous cross
identifications to other names and catalog identifiers. Tables Ib and IIb,
containing 21 systems originally included in Gliese's (1957) catalog but for
which revised parallaxes have placed them farther than 25 pc are not included
in the electronic version.
Data in the electronic version include the Gliese number (newly added stars
by Woolley have numbers beginning with 9001, but new parallaxes have removed
9419 and added 9849 and 9850 from the < 25 parsecs sample), component
identifications for multiple systems, parallaxes, annual proper motions,
radial velocities, (U,V,W) space velocities, box orbit parameters (omega, e,
i), spectral types, UBV data, absolute visual magnitudes, positions, GCTP
(General Catalogue of Trigonometric Stellar Parallaxes) and its Supplement
(Jenkins 1952, 1963) names, HD, DM, GCRV (General Catalogue of Stellar Radial
Velocities, Publ. Carnegie Inst., Washington, No. 601, Wilson 1953) and other
catalog identifiers, BS (= HR) (Hoffleit 1964) numbers, and remarks codes for
spectroscopic binaries (SB), doubles, variables, etc.
Note that there is an entry in this catalog for the Sun, for which many
fields, such as RA and Dec, have not been populated.
WRCAT Catalog
The VIIth Catalogue of Galactic Population I Wolf-Rayet (WR) Stars
provides improved coordinates, spectral types, and bv photometry of known WR
stars and adds 71 new stars compared to the VIth Catalog. This census of
galactic WR stars has reached 227 stars (226 entries in this catalog),
comprising 127 WN stars, 87 WC stars, 10 WN/WC stars, and 3 WO stars.
This includes 15 WNL and 11 WCL stars within 30 pc of the Galactic Center.
The catalog includes information on periodicity, binarity, terminal wind
velocities, correlations with open clusters, OB associations, H I bubbles,
H II regions, and ring nebulae, observed and dereddened narrow-band bv
photometry, and distances, both heliocentric and galactocentric, and lists
the references from which this information was obtained.
XMMOBSTARS Catalog
Following the advent of increasingly sensitive X-ray observatories, deep
observations of early-type stars became possible. However, the results for
only a few objects or clusters have until now been reported and there has
been no large survey comparable to that based upon the ROSAT All-Sky Survey
(RASS). A limited survey of X-ray sources, consisting of all public XMM
observations (2XMMi) and slew survey data (XMMSL1), is now available. The
X-ray counterparts to hot, massive stars have been searched for in these
catalogs. About 300 OB stars were detected with XMM. Half of them were
bright enough for a spectral analysis to be possible, and we make available
the detailed spectral properties that were derived. The X-ray spectra
of O stars are represented well by low (< 1 keV) temperature components
and seem to indicate that an absorption column is present in addition
to the interstellar contribution. The X-ray fluxes are well correlated
with the bolometric fluxes, with a scatter comparable to that of the RASS
studies and thus larger than found previously with XMM for some individual
clusters. These results contrast with those of B stars that exhibit a large
scatter in the LX - Lbol relation, no additional absorption being found,
and the fits indicate a plasma at higher temperatures. Variability (either
within one exposure or between multiple exposures) was also investigated
whenever possible: short-term variations are far more rare than long-term ones
(the former affects a few percent of the sample, while the latter concerns
between one third and two thirds of the sources).
This is a catalog of X-ray emitters amongst early-type stars following a
correlation between the Reed (2003, AJ, 125, 2531) Catalog of galactic OB
Stars and the 2XMMi Catalog (Watson et al. 2009, A&A, 493, 339). See the
reference paper for more details.
XRBCAT Catalog
XRBCAT is a catalog of X-ray binaries, based on the van Paradijs (1996)
compilation, and updated by Nick White to include all the new (mostly
transient) systems discovered since then up until the last update (see below).
The information in XRBCAT is basic and does not attempt to be complete. It
includes the name of the source, the position, the pulse or orbital period
(if one is known), the object class, a flux (a maximum and, if available, a
minimum), and an optical V magnitude (if available). To reference XRBCAT,
please use the following acknowledgment:
"This paper utilized the HEASARC XRBCAT X-ray Binary catalog".
Since it is a very time consuming task to keep track of all the new sources
and discoveries, there may be incomplete or missing sources.
This catalog was last updated on April 22, 1998.
