A2PIC Catalog
The HEAO 1 A-2 experiment's operations began on day 224 of 1977 (12 August
1977) and ended on day 739 of 1977 (9 January 1979). The A-2 experiment
performed two independent, low-background, high-sensitivity surveys of the
entire sky 6 months apart, the first scan during days 248 to 437 of 1977
(5 September 1977 - 13 March 1978) and the second scan during days 73 to 254
of 1978 (14 March 1978 - 11 September 1978). The authors analyzed the A-2
data in order to obtain a complete flux-limited sample of extragalactic
X-ray sources. The region between galactic latitudes of -20 and +20 degrees
was excluded to minimize contamination from galactic sources. A circle of
6 degrees radius around the Large Magellanic Cloud sources was also
excluded to prevent confusion problems. Therefore, there remained 65.5%
of the sky (8.23 steradians) covered by this survey. The lowest statistical
significance for the existence of the sources included in this catalog
is 5 sigma, as required by the maximum likelihood methods used by the
authors to determine the log N - log S parameters. Taking into account this
statistical significance requirement, the authors estimated the completeness
level of the first and second scans to be 1.25 and 1.8 R15 ct/s, respectively.
1 R15 ct/s is approximately 2.17 x 10-11 erg/cm2/s in the 2-10 keV energy
band for a power-law spectrum with a photon index of 1.65. This catalog
contains data for 68 non-galactic sources (61 extragalactic and 7 unidentified
sources) which were listed in Table 1 of the published catalog.
The identified sources fall into several categories, including narrow
emission line galaxies, broad emission line galaxies, BL Lacertae objects,
and clusters of galaxies.
ABELL Catalog
The ABELL database contains information from a catalog of clusters of galaxies,
each having at least 30 members within the magnitude range m3 to m3+2 (m3 is
the magnitude of the third brightest cluster member) and each with a nominal
redshift less than 0.2. The database contains the revised Northern Abell
catalog, the Southern Abell catalog, and the Supplementary Southern Abell
catalog; the catalogs are published as tables 3, 4 and 5 of Abell, Corwin &
Orowin (1989).
ABELLZCAT Catalog
The all-sky ACO (Abell, Corwin and Olowin 1989, ApJS, 70, 1)
Catalog of 4073 rich clusters of galaxies and 1175 southern poor or distant
S-clusters has been searched for published redshifts. Data for 1059
of them were found and classified into various quality classes, e.g. to reduce
the problem of foreground contamination of redshifts. Taking the ACO selection
criteria for redshifts, a total of 992 entries remain, 21 percent more than
ACO. Redshifts for rich clusters are now virtually complete out to a redshift
z of 0.05 in the north and of 0.04 in the south. In the north, the
magnitude-redshift (m_10 - z) relation agrees with that of Kalinkov et al.
(1985, Astr. Nachr., 306, 283). For the southern rich clusters, minor
adjustments to the m_10 - z relation of ACO are suggested, while for the
S-clusters the redshifts are about 30 percent lower than estimated.
ACCEPTCAT Catalog
This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT)
Catalog, contains the radial entropy profiles of the intracluster medium
(ICM) for a collection of 239 clusters taken from the Chandra X-ray
Observatory's Data Archive. Entropy is of great interest because it controls
ICM global properties and records the thermal history of a cluster. The
authors find that most ICM entropy profiles are well fitted by a model which
is a power law at large radii and approaches a constant value at small radii:
K(r) = K0 + K100 (r/100 kpc)alpha, where K0 quantifies the typical
excess of core entropy above the best-fitting power law found at larger
radii. The authors also show that the K0 distributions of both the full
archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample
of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K0
~ 30 - 50 keV cm2 and population peaks at K0 ~ 15 keV cm2 and K0 ~
150 keV cm2. The effects of point-spread function smearing and angular
resolution on best-fit K0 values are investigated using mock Chandra
observations and degraded entropy profiles, respectively. The authors find
that neither of these effects is sufficient to explain the entropy-profile
flattening they measure at small radii. The influence of profile curvature
and the number of radial bins on the best-fit K0 is also considered, and
they find no indication that K0 is significantly impacted by either.
All data and results associated with this work are publicly available via the
project web site http://www.pa.msu.edu/astro/MC2/accept/.
The sample is collected from observations taken with the Chandra X-ray
Observatory and which were publicly available in the CDA (Chandra Data
Archive) as of 2008 August.
AGNSDSSXM2 Catalog
X-ray emission from active galactic nuclei (AGN) is dominated by the
accretion disk around a supermassive black hole. The radio luminosity,
however, has not such a clear origin except in the most powerful sources
where jets are evident. The origin (and even the very existence) of the local
bi-modal distribution in radio-loudness is also a debated issue. By analyzing
X-ray, optical and radio properties of a large sample of type 1 AGN and
quasars (QSOs) up to z > 2, where the bulk of this population resides, the
authors aim to explore the interplay between radio and X-ray emission in AGN,
in order to further our knowledge on the origin of radio emission, and its
relation to accretion. They analyze a large (~800 sources) sample of type 1
AGN and QSOs selected from the 2XMMi XMM-Newton X-ray source catalog,
cross-correlated with the SDSS DR7 spectroscopic catalog, covering a redshift
range from z ~ 0.3 to z ~ 2.3. Supermassive black hole masses are estimated
from the Mg II emission line, bolometric luminosities from the X-ray data,
and radio emission or upper limits from the FIRST catalog. Most of the
sources accrete close to the Eddington limit and the distribution in
radio-loudness does not appear to have a bi-modal behavior. This study
confirms that radio-loud AGN are also X-ray loud, with an X-ray-to-optical
ratio up to twice that of radio-quiet objects, even excluding the most
extreme strongly jetted sources. By analyzing complementary radio-selected
control samples, the authors find evidence that these conclusions are not an
effect of the X-ray selection, but are likely a property of the dominant QSO
population.
The authors of this catalog conclude that their findings are best interpreted
in a context where radio emission in AGN, with the exception of a minority of
beamed sources, arises from very close to the accretion disk and is therefore
heavily linked to X-ray emission. They also speculate that the
radio-loud/radio-quiet dichotomy might either be an evolutionary effect that
developed well after the QSO peak epoch, or an effect of incompleteness in
small samples.
Basic information and derived properties are presented for the sample of
X-ray selected type 1 AGN (as well as for the 11 X-ray undetected type 1 AGN
in the "control sample"): coordinates, redshift, X-ray and radio fluxes,
optical magnitudes, from the SDSS, 2XMMi, and FIRST catalogs; continuum
luminosities at 3000 Angstroms and in the X-ray band, black hole masses,
bolometric luminosities, Eddington ratios; for the sources falling in the
FIRST field, optical fluxes at 2500 and 4400 Angstroms, X-ray-to-optical
index, radio classification, and the ratios between the radio and the UV,
optical, and X-ray fluxes.
AGNSDSSXMM Catalog
Bright XMM-Newton data are combined with the Chandra Deep Field South
observations to explore the behavior of the intrinsic AGN absorption, as a
function of redshift and luminosity. The sample consists of 359 sources
selected in the hard 2 - 8 keV band, spanning the flux range from 6 x 10-16
- 3 x 10-13 erg/cm2/s with a high rate of spectroscopic or photometric
redshift completeness (100 and 85 percent for the Chandra and XMM-Newton
data, respectively). The authors derive the column density values using X-ray
spectral fits. They find that the fraction of obscured AGN falls with
increasing luminosity in agreement with previous findings. The fraction of
obscured AGN shows an apparent increase at high redshifts (z > 2).
Simulations show that this effect can most probably be attributed to the fact
that at high redshifts the column densities are overestimated.
This table contains the subset of 153 brighter hard X-ray sources in the
XMM-Newton/Sloan Digital Sky Survey (SDSS) sample which have 2-8 keV fluxes >
3 x 10-14 erg cm-2 s-1, excluding a number of sources with extended
optical morphology and blue colors, as well as 4 sources with X-ray to
optical fluxes < 0.1 which are fit better with stellar rather than QSO
templates.
Much more information on the SDSS is available at the project's web site
at http://www.sdss.org/.
ALLWISEAGN Catalog
This table contains an all-sky sample of ~1.4 million active galactic nuclei
(AGNs) meeting a two-color infrared photometric selection criterion for AGNs
as applied to sources from the Wide-field Infrared Survey Explorer final
catalog release (AllWISE). The authors assess the spatial distribution and
optical properties of their sample and find that the results are consistent
with expectations for AGNs. These sources have a mean density of ~38 AGNs per
square degree on the sky, and their apparent magnitude distribution peaks at
g ~ 20, extending to objects as faint as g ~ 26. The authors test the AGN
selection criterion against a large sample of optically identified stars and
determine the "leakage" (that is, the probability that a star detected in an
optical survey will be misidentified as a quasi-stellar object (QSO) in their
sample) rate to be <= 4.0 x 10-5. They conclude that their sample contains
almost no optically identified stars (<= 0.041%), making this sample highly
promising for future celestial reference frame work as it significantly
increases the number of all-sky, compact extragalactic objects. The authors
further compare their sample to catalogs of known AGNs/QSOs and find a
completeness value of >= 84% (that is, the probability of correctly
identifying a known AGN/QSO is at least 84%) for AGNs brighter than a
limiting magnitude of R <= 19. This sample includes approximately 1.1 million
previously uncataloged AGNs.
The WISE survey is an all-sky mid-IR survey at 3.4, 4.6, 12, and 22 microns
(W1, W2, W3, and W4, respectively) conducted between 2010 January 7 and
August 6, during the cryogenic mission phase, and first made available to the
public on 2011 April 14. WISE has angular resolutions of 6.1, 6.4, 6.5, and
12.0 arcseconds in its four bands, respectively. The AllWISE data release,
which was used for this work, incorporates data from the WISE Full Cryogenic,
3-Band Cryo, and NEOWISE Post-Cryo survey (Mainzer et al. 2014, ApJ, 792, 30)
phases, which were co-added to achieve a depth of coverage ~0.4 mag deeper
than previous data releases. AllWISE contains the positions, apparent
motions, magnitudes, and point-spread function (PSF)-profile fit information
for almost 748 million objects. Astrometric calibration of sources in the
WISE catalog was done by correlation with bright stars from the 2MASS point
source catalog, and the astrometric accuracy for sources in the AllWISE
release was further improved by taking into account the proper motions of
these reference stars, taken from the fourth USNO CCD Astrograph Catalog
(UCAC4, Zacharias et al. 2013, AJ, 145, 44). A comparison with ICRF sources
shows that AllWISE Catalog sources in the brightness range of 8 < W1 < 12 mag
have positional accuracies to within 50 mas, and half of these sources have
positional accuracies to within 20 mas. For more details on the WISE mission,
see Wright et al. (2010, AJ, 140, 1868).
The authors took all sources from the AllWISE catalog following Equations (3)
and (4) from Mateos et al. (2012, MNRAS, 426, 3271) and they require that all
of their sources have S/N >= 5 in the first three bands, as recommended in
Mateos et al. (2012); as a further constraint, they limit their results to
those with cc_flags = "0000," meaning that the sources are unaffected by known
artifacts such as diffraction spikes, persistence, halos, or optical ghosts.
In order to characterize the optical properties of their sample, the authors
cross-matched it to SDSS-DR12, which is the final data release of SDSS-III
(Eisenstein et al. 2011, AJ, 142, 72), within a radial tolerance of R < 1",
obtaining 424,366 matches. To determine the fraction of false positive
positional matches (that is, incorrectly correlating an object in their
sample with a different SDSS object due to random positional agreement), they
performed the same match on a scrambled version of their sample coordinates,
determining that less than 1% of other cross-matches are false positive
positional matches between the two catalogs. The authors also cross-matched
their sample sources with he second release of the Large Quasar Astrometric
Catalog (LQAC-2; Souchay et al. 2012, A&A, 537, A99), which contains 187,504
quasars, including radio-selected quasars from the ICRF2, optically selected
quasars from SDSS, and infrared-selected quasars from 2MASS, and thus
represents a robust sample of quasars over a wide range of wavelengths. They
find that 93,403 quasars from LQAC-2 have clean detections. The majority of
non-detections are due to sources in LQAC-2 that are too faint, having R >~
19.
ARXA Catalog
The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged
or APM/USNO-A optical objects which are found to be associated with
XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with
NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double
radio lobes where found. The source number counts are:
Optical objects - 602,570.
NVSS - 266,148 core associations, plus 8309 double lobes.
FIRST - 173,383 core associations, plus 12,844 double lobes.
SUMSS - 59,138 core associations, plus 2529 double lobes.
XMM associations - 57,778.
Chandra associations - 32,951.
ROSAT RASS - 47,486.
ROSAT HRI - 15,523.
ROSAT PSPC - 35,607.
WGA - 24,226.
Each optical object is given as one entry in this catalog, containing the sky
coordinates, the object name (from the literature where available), APM and
USNO-A sourced red and blue photometry, redshift, the source catalogs for the
name and redshift, the calculated odds that the object is a quasar, galaxy,
star, or erroneous association, and the radio & X-ray identifiers, up to 10 of
them possible although usually just 1 or 2.
This catalog supersedes the previous similar compilation by the same author,
the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see
http://quasars.org/qorg-data.htm).
Questions or comments on ARXA may be directed to eric@flesch.org.
See also:
APM home page http://www.ast.cam.ac.uk/~apmcat
USNO-A home page http://www.nofs.navy.mil/
NVSS home page http://www.cv.nrao.edu/nvss/
FIRST home page http://sundog.stsci.edu/
SUMSS home page http://www.astrop.physics.usyd.edu.au/SUMSS/index.html
XMM-Newton home page http://xmmssc-www.star.le.ac.uk
HRI & PSPC home page http://www.mpe.mpg.de/ROSAT/
WGA home page http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html
RASS-FSC home page http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc
RASS-BSC home page http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc
Chandra home page http://chandra.harvard.edu
XAssist home page http://xassist.pha.jhu.edu/zope/xassist
(XMMX & CXOX sources are from XAssist)
If using this catalog in published research, please add a small mention
in the acknowledgements.
This table is based on research which made use of the NASA/IPAC
Extragalactic Database (NED) operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with NASA.
ASCAEGCLUS Catalog
Utilizing ASCA archival data of about 300 objects - elliptical galaxies,
groups, and clusters of galaxies - the authors performed systematic
measurements of the X-ray properties of hot gas in their systems, and
compiled them in this study. The steepness (power-law slope) of the
luminosity-temperature (L-T) relation, LX ~ kTalpha, in the range of kT
~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous
measurements. In the relation, the authors find two breaks at around
intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/-
0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07
below 1.5 keV. Two such breaks are also evident in the temperature and size
relation. The steepness in the L-T relation at kT > 4 keV is consistent with
the scale-relation derived from the CDM model, indicating that the
gravitational effect is dominant in richer clusters, while poorer clusters
suffer non-gravity effects. The steep L-T relation below 1 keV is mostly
attributed to X-ray faint systems of elliptical galaxies and galaxy groups.
The authors find that the ICM mass within the scaling radius R1500 (the
radius within which the averaged mass density is 1500 times higher than the
critical density) follows the relation of Mgas ~ T(2.33+/-0.07) from
X-ray faint galaxies to rich clusters. Thus, the authors speculate that even
such X-ray faint systems contain large-scale hot gas, which is too faint to
detect.
For this project, the authors utilized all of the ASCA data of elliptical
galaxies and clusters of galaxies. Several clusters were observed more than
once, and they chose the observation with the longest exposure. The total
number of objects that the authors identified as elliptical galaxies and
clusters was 313, and these are listed in this table. Some of the objects
could not be utilized for deriving various correlations, due to either having
an unknown redshift (17 objects), an insignificant detection (13 objects
listed below), or contamination of the environmental X-ray emission, such as
cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC
4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04
and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292
objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this
study, the authors assumed the Hubble constant to be 50 h50 km s-1
Mpc-1 and q0 to be 0.
Table 1 of the reference paper (reproduced below) lists the 13 clusters for
which only 90% confidence level upper limits to the flux in the observer's
frame are available:
Name Flux (0.5 - 2 keV) Upper Limit
(erg/s/cm2)
NGC 5018 9.8 x 1014
GHO 1322+3114 1.3 x 1013
J1888.16CL 5.9 x 1014
CL 0317+1521 4.5 x 1014
MS 1512.4+3647 1.0 x 1012
PRG 38 6.9 x 1014
SCGG 205 6.9 x 1014
RGH 101 9.1 x 1014
3C 184 8.5 x 1014
RX J1756.5+6512 1.6 x 1013
3C 324 5.4 x 1014
PDCS 01 2.8 x 1014
MS 0147.8-3941 5.0 x 1014
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.
BAXGALCLUS Catalog
This table contains the BAX X-Ray Galaxy Clusters and Groups
Catalog. BAX (`Base de Donnees Amas de Galaxies X': see
http://bax.ast.obs-mip.fr/ for more details) is a multi-wavelength database
dedicated to X-ray clusters and groups of galaxies which allows detailed
information retrieval. BAX is designed to support astronomical research by
providing access to published measurements of the main physical
quantities and to the related bibliographic references: basic data
stored in the database are cluster/group identifiers, equatorial
coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and
temperature, and (in the online version at http://bax.ast.obs-mip.fr/) links
to additional linked parameters (in X-rays, such as spatial profile parameters,
as well as SZ parameters of the hot gas, lensing measurements, and data at
other wavelengths, such as the optical and radio bands). The clusters and
groups in the online BAX database can be queried by the basic parameters as
well as the linked parameters or combinations of these.
The authors expect BAX to become an important tool for the astronomical
community. BAX will optimize various aspects of the scientific analysis of
X-ray clusters and groups of galaxies, from proposal planning to data
collection, interpretation and publication, from both ground based facilities
like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton,
Chandra and Planck.
CBATPICAGN Catalog
Compton Gamma-Ray Observatory (CGRO) BATSE Earth-occultation data
have been used by Malizia et al. (1999, ApJ, 519, 637) to search for
emission in the 20-100 keV band from all sources in the Piccinotti sample
(Piccinotti et al. 1982, ApJ, 253, 485: the HEASARC A2PIC database),
which represents the only complete 20-10 keV survey to date of the
extragalactic sky down to a limiting flux of 3.1 x 10-11 ergs cm-2 s-1.
Nearly 4 years of observations have been analyzed to reach a 5-sigma
confidence level of about 7.8 x 10-11 ergs cm-2 s-1 in the band considered.
Of the 36 sources in the sample, 14 have been detected above the 5-sigma
confidence level, while marginal detection (3 <= sigma <= 5) can be claimed
for 13 sources; for nine objects, 2 sigma upper limits are reported. A
comparison of BATSE results with data at higher energies is used to estimate
the robustness of the data analysis. While the detection level of each source
is reliable, the flux measurement may be overestimated in some sources by as
much as 35%, probably because of incomplete data cleaning. Comparison of
BATSE fluxes with X-ray fluxes obtained in the 2-10 keV range and averaged
over years indicates that a canonical power law of photon index 1.7 gives a
good description of the broadband spectra of bright active galactic nuclei
(AGNs) and that spectral breaks preferentially occur above 100 keV.
CCOSRSSFAG Catalog
X-ray surveys contain sizable numbers of star-forming galaxies, beyond the
AGN which usually make up the majority of detections. Many methods to
separate the two populations are used in the literature, based on X-ray and
multi-wavelength properties. The authors aim at a detailed test of the
classification schemes and to study the X-ray properties of the resulting
samples. They build on a sample of galaxies selected at 1.4 GHz in the
VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14)
according to their optical colors and also observed by Chandra. A similarly
selected control sample of AGN is also used for comparison. The authors
review some X-ray based classification criteria and check how they affect the
sample composition. The efficiency of the classification scheme devised by
Smolcic et al. (2008) is such that ~30% of composite/misclassified objects
are expected because of the higher X-ray brightness of AGN with respect to
galaxies. The latter fraction is actually 50% in the X-ray detected sources,
while it is expected to be much lower among X-ray undetected sources. Indeed,
the analysis of the stacked spectrum of undetected sources shows,
consistently, strongly different properties between the AGN and galaxy
samples. X-ray based selection criteria are then used to refine both samples.
The radio/X-ray luminosity correlation for star-forming (SF) galaxies is
found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some
evolution of the ratio may be possible for sources at high redshift or high
luminosity, though it is likely explained by a bias arising from the radio
selection. Finally, in their paper the authors discuss the X-ray number
counts of star-forming galaxies from the VLA- and C-COSMOS surveys according
to different selection criteria, and compare them to the similar
determination from the Chandra Deep Fields. The classification scheme
proposed here may find application in future works and surveys.
This table contains the catalogs of radio-selected SF- and AGN-candidate
sources with an X-ray detection in C-COSMOS which were contained in Tables 2
and 3 of the reference paper, respectively. The HEASARC has merged these into
a single table, adding a new parameter sample which is set to 'SFG' for
radio-selected SF-candidate sources from Table 2 and to 'AGN' for the
AGN-candidate sources from Table 3.
CFA2S Catalog
The Center for Astrophysics (CfA) Redshift Survey South Galactic
Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies
with blue (Zwicky B(0) type) magnitude <= 15.5 covering the range from
20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination.
This sample is complete for all galaxies in the merge of the Zwicky et al.
and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these
were measured as part of the second CfA Redshift Survey. The data reveal large
voids in the foreground and background of the Perseus-Pisces Supercluster.
The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter
of ~ 5000km/s, and is enclosed by a complex of dense structures. The large
structure known as the Perseus-Pisces Supercluster forms the near side
of this complex. On the far side of this large void, at a mean velocity of
~ 12000km/s, there is another coherent dense wall. The structures in this
survey support the view that galaxies generally lie on surfaces surrounding
or nearly surrounding low-density regions or voids.
CGMW Catalog
This catalog gathers the searches for galaxies of apparent size
greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky
Way from photographic surveys in the near-infrared. The four volumes
(CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from
-7 to +43 degrees, and from 210 to 250 degrees.
The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies
behind the Milky Way between l = 210 degrees and 250 degrees, represent
a systematic search for galaxies by means of 32 film copies of the UK
Schmidt Southern Infrared Atlas on the Milky Way covering about 900
square degrees. In the search galaxies with apparent sizes greater
than 0.1mm on film (6.7 arcsec in size) were detected by visual
inspection. The material and procedure of search are described as well
as the detectability of galaxies in paper I and paper II appended
before Vol. 1 and Vol. 2 of the catalog, respectively, which have been
published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43
(1991). The parameters of catalogued galaxies are also explained in
paper I. Cross-identifications with other catalogs are also given.
The third volume CGMW3 lists about 5300 galaxy candidates having sizes
larger than 0.1 arcminutes that were found in a search of Schmidt atlases
covering a Milky Way region of about 800 square degrees around l = 8 to 43
degrees, and b = -17 to +17 degrees. This surveyed region is located between
the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists
about 7150 galaxies and galaxy candidates having sizes larger than 0.1
arcminutes that were found in a search of Schmidt atlases covering a Milky
Way region of about 260 square degrees around l = -7 to +16 degrees, and
b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center
region.
COSMOSVLBA Catalog
This table contains the results of a project using wide-field Very Long
Baseline Interferometry (VLBI) observations at 1.4 GHz of 2,865 known radio
sources in the Cosmic Evolution Survey (COSMOS) field, a field which has
exceptional multi-wavelength coverage. The main objective of this study is to
identify the active galactic nuclei (AGN) in this field. Wide-field VLBI
observations were made of all known radio sources in the COSMOS field at 1.4
GHz using the Very Long Baseline Array (VLBA). The authors also collected
complementary multiwavelength information from the literature for the
VLBA-detected sources.The combination of the number of sources, sensitivity,
angular resolution and the area covered by this project are unprecedented. A
catalog which contains the VLBI-detected sources is presented, the main
purpose of which is to be used as an AGN catalog. the complementary
multiwavelength (optical, infrared and X-ray) information of the
VLBI-detected sources is also presented.
The authors have detected 468 radio sources, expected to be AGN, with the
VLBA. This is, to date, the largest sample assembled of VLBI-detected sources
in the sub-mJy regime. They find a detection fraction of 20% +/- 1%,
considering only those sources from the input catalog which were in principle
detectable with the VLBA (2,361). As a function of the VLA flux density, the
detection fraction is higher for higher flux densities, since at high flux
densities a source could be detected even if the VLBI core accounts for a
small percentage of the total flux density. As a function of redshift, the
authors see no evolution of the detection fraction over the redshift range
0.5 < z < 3. In addition, they find that faint radio sources typically have a
greater fraction of their radio luminosity in a compact core: ~70% of the
sub-mJy sources detected with the VLBA have more than half of their total
radio luminosity in a VLBI-scale component, whereas this is true for only
~30% of the sources that are brighter than 10 mJy. This suggests that fainter
radio sources differ intrinsically from brighter ones. Across the entire
sample, the authors find the predominant morphological classification of the
host galaxies of the VLBA-detected sources to be early type (57%), although
this varies with redshift and at z > 1.5 they find that spiral galaxies
become the most prevalent (48%). The number of detections is high enough to
study the faint radio population with statistically significant numbers. The
authors demonstrate that wide-field VLBI observations, together with new
calibration methods such as multi-source self-calibration and mosaicking,
result in information which is difficult or impossible to obtain otherwise.
This table contains 504 entries, including the 468 VLBA-detected sources and,
for sources with multiple components, entries for the individual components.
Among the detected sources, there are 452 single, 13 double, 2 triple and 1
quadruple source. Source entries have no suffix in their vlba_source_id,
e.g., 'C3293', whereas component entries have a, b, c or d suffixes, e.g.,
'C0090a' (and a value of 2 for the multi_cpt_flag parameter).
COSXFIRMWC Catalog
The coeval AGN and galaxy evolution and the observed local relations between
super-massive black holes (SMBHs) and galaxy properties suggest some
connection or feedback between SMBH growth and galaxy build-up. The authors
looked for correlations between properties of X-ray detected AGN and their
far-infrared (FIR) detected host galaxies, to find quantitative evidences for
this connection, highly debated in recent years. They exploit the rich
multi-wavelength data set (from X-ray to FIR) that is available in the COSMOS
field for a large sample (692 sources) of AGN and their hosts, in the
redshift range 0.1 < z < 4, and use X-ray data to select AGN and determine
their properties (intrinsic luminosity and nuclear obscuration), and
broad-band (from UV to FIR) spectral energy distribution (SED) fitting to
derive host galaxy properties, viz., the stellar mass (M*) and the star
formation rate (SFR). The authors find that the AGN 2-10 keV luminosity
(LX) and the host galaxy 8-1000 um star formation luminosity (LSFIR)
are significantly correlated. However, the average host LSFIR has a flat
distribution in bins of AGN LX, while the average AGN LX increases in
bins of host LSFIR, with a logarithmic slope of ~ 0.7, in the redshifts
range 0.4 < z < 1.2. In the reference paper, the authors also discuss the
comparison between the distribution of these two quantities and the
predictions from hydrodynamical simulations. Finally, they find that the
average column density (NH) shows a positive correlation with the host
M*, at all redshifts, but not with the SFR (or LSFIR). This translates
into a negative correlation with specific SFR. These results are in agreement
with the idea that BH accretion and SFRs are correlated, but occur with
different variability time scales. The presence of a positive correlation
between NH and host M* suggests that the X-ray NH is not entirely due
to the circumnuclear obscuring torus, but may also include a contribution
from the host galaxy.
This table summarizes the multiwavelength properties of the 692 AGN-host
systems detected in the COSMOS field both in the X-ray and in the FIR (the
X-FIR sample).
DENISIGAL Catalog
This database contains the release of the provisional extragalactic
catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS)
and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog).
It was created using an automatic galaxy recognition program based on a
discriminating analysis, the efficiency of which is estimated to be better than
99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star
Catalog is about 6 arcseconds. The cross-identification with galaxies
available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration
of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81,
413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains
total I-band magnitude, isophotal diameter, axis ratio, position angle and a
rough estimate of the morphological type code for 20620 galaxies. The internal
completeness of this catalog reaches a limiting I-band magnitude of 14.5, with
a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed
in this study.
EINGALCLUS Catalog
The Einstein Observatory Clusters of Galaxies Catalog presents the
X-ray characteristics of a sample of 368 clusters of galaxies with redshifts
less than 0.2 which were observed with the Einstein Imaging Proportional
Counter (IPC). For each cluster, the authors measured the 0.5 - 4.5 keV
counting rate and computed the 0.5 - 4.5 keV source luminosity, as well as
the bolometric luminosity within fixed metric radii. They detected 85% of
Abell clusters with z < 0.1, demonstrating that the large majority of these
optically selected clusters are not the results of chance superpositions. For
163 clusters, they measured their X-ray surface brightness profiles and
determined their core radii. For about 230 clusters, they then used either
their measured core radii and beta values, or mean values derived for this
sample, to measure central gas densities and gas masses. They used estimated
or measured cluster gas temperatures, along with the derived gas-density
profiles, to estimate total cluster masses, under the assumptions that the
gas is isothermal and in hydrostatic equilibrium.
ESOUPPSALA Catalog
This database table was derived from information provided in "The ESO/Uppsala
Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the
European Southern Observatory (ESO) and the Uppsala Observatory to provide a
systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick
Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La
Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The
fields are similar in size and scale to those of the Palomar Observatory Sky
Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a
passband similar to the Johnson B color. Additional information is available
from the HEASARC.
ETGALXRAY Catalog
This table contains a catalog of X-ray luminosities for 401 early-type
galaxies (and 24 other galaxies which were listed in previuous studies as
early but which have LEDA T-types >= -1.5), of which 136 are based on newly
analysed ROSAT PSPC pointed observations. The remaining luminosities are
taken from the literature and converted to a common energy band, spectral
model and distance scale. In their paper, the authors use this sample to
fit the LX/LB relation for early-type galaxies and find a best-fit
slope for the catalog of ~ 2.2. The authors demonstrate the influence of
group-dominant galaxies on the fit and present evidence that the relation
is not well modeled by a single power-law fit. They also derive estimates
of the contribution to galaxy X-ray luminosities from discrete-sources
and conclude that they provide L(discrete-source-contribution)/LB ~
29.5 erg s-1/LBsun. The authors compare this result with luminosities
from their catalog. Lastly, they examine the influence of environment on
galaxy X-ray luminosity and on the form of the LX/LB relation. They
conclude that although environment undoubtedly affects the X-ray properties
of individual galaxies, particularly those in the centres of groups and
clusters, it does not change the nature of whole populations.
The sample of early-type galaxies was selected from the Lyon-Meudon
Extragalactic Data Archive (LEDA). This catalog at that time contained
information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and
morphological data. Galaxies were selected using the following criteria:
(i) Morphological Type T < -1.5 (i.e. E, E-S0 and S0 galaxies).
(ii) Virgo-corrected recession velocity V <= 9,000 km s-1.
(iii) Apparent Magnitude BT <= 13.5.
The redshift and apparent magnitude restrictions were chosen in order to
minimize the effects of incompleteness on their sample. The LEDA catalogue
is known to be 90 per cent complete at BT = 14.5, so the selection should
be close to statistical completeness. The selection process produced ~
700 objects. The authors then cross-correlated this list with a list of
public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the
target were accepted, as, further off-axis, the PSPC point-spread function
becomes large enough to make analysis problematic. This left 209 galaxies
with X-ray data available.
The authors also added data from previously published catalogs, ROSAT
PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209),
and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531)
and Roberts et al. (1991, ApJS, 75, 751). These other references use a
range of models to fit the data, different wavebands, distances and blue
luminosities. O'Sullivan et al. corrected for these differences by converting
the catalogs to a common set of values, as used for their own results.
All of the X-ray luminosities have been converted to a common format based
on a reliable distance scale (assuming H0 = 75 km s-1 Mpc-1), and
correcting for differences in spectral fitting techniques and waveband.
EXGALEMOBJ Catalog
This is the Hewitt & Burbidge (1991) Optical Catalog of
Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects.
It contains a total of 935 galaxies which have optical properties
similar to QSOs. Most of the objects appear to be nonstellar. The
majority, more than 700, have redshifts z that are <= 0.2, and most
have been classified as Seyfert galaxies, N systems, or radio galaxies.
The redshift distribution peaks at z ~ 0.025, but there are about 200
powerful radio galaxies in the extended tail of the distribution which
have z > 0.2. There is a separate and distinct peak in the redshift
distribution at z = 0.06.
Notice that this catalog does not include star-like objects with
emission-line redshifts >= 0.1 (these can be found in the HEASARC QSO
database which contains the Revised and Updated Catalog of Quasi-Stellar
Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947).
Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or
starburst galaxies.
FRICAT Catalog
The authors have built a catalog of 219 Fanaroff and Riley class I
edge-darkened radio galaxies (FR Is), called FRICAT, that is selected from a
published sample and obtained by combining observations from the NVSS, FIRST,
and SDSS surveys. They included in the catalog the sources with an
edge-darkened radio morphology, redshift <= 0.15, and extending (at the
sensitivity of the FIRST images) to a radius r larger than 30 kpc from the
center of the host. The authors also selected an additional sample (sFRICAT)
of 14 smaller (10 < r < 30 kpc) FR Is, limiting to z < 0.05. The hosts of the
FRICAT sources are all luminous (-21 >~ Mr >~ 24), red early-type galaxies
with black hole masses in the range 108 <~ MBH <~ 3 x 109 solar
masses); the spectroscopic classification based on the optical emission line
ratios indicates that they are all low excitation galaxies. Sources in the
FRICAT are then indistinguishable from the FR Is belonging to the Third
Cambridge Catalogue of Radio Sources (3C) on the basis of their optical
properties. Conversely, while the 3C-FR Is show a strong positive trend
between radio and [O III] emission line luminosity, these two quantities are
unrelated in the FRICAT sources; at a given line luminosity, they show radio
luminosities spanning about two orders of magnitude and extending to much
lower ratios between radio and line power than 3C-FR Is. The authors' main
conclusion is that the 3C-FR Is represent just the tip of the iceberg of a
much larger and diverse population of FR Is.
This HEASARC table contains both the 219 radio galaxies in the main FRICAT
sample listed in Table B.1 of the reference paper and the 14 radio galaxies
in the additional sFRICAT sample listed in Table B.2 of the reference paper.
To enable users to distinguish from which sample an entry has been taken, the
HEASARC created a parameter galaxy_sample which is set to 'M' for galaxies
from the main sample, and to 'S' for galaxies from the supplementary sFRICAT
sample.
Throughout the paper, the authors adopted a cosmology with H0 = 67.8 km
s-1 Mpc-1, OmegaM = 0.308, and OmegaLambda = 0.692 (Planck
Collaboration XIII 2016).
FRIICAT Catalog
This table contains a catalog of 123 Fanaroff and Riley class II
edge-brightened radio galaxies (FR IIs), called FRIICAT, that has been
selected from a published sample obtained by combining observations from the
NVSS, FIRST, and SDSS surveys. The catalog includes sources with redshift
<=0.15, an edge-brightened radio morphology, and those with at least one of
the emission peaks located at a radius r larger than 30 kpc from the center
of the host.
The radio luminosity at 1.4 GHz of the FRIICAT sources covers the range
L1.4 ~ 1039.5 - 1042.5 erg/s. The FRIICAT catalog has 90% of low- and
10% of high-excitation galaxies (LEGs and HEGs), respectively. The properties
of these two classes are significantly different. The FRIICAT LEGs are mostly
luminous (-20 >~ Mr >~ -24), red early-type galaxies with black hole masses
in the range 108 Msun <~ MBH <~ 109 M_sun_; they are essentially
indistinguishable from the FR Is belonging to the FRICAT sample (Capetti et
al. 2017, A&A, 598, A49: also available as a HEASARC table). The HEG FR IIs
are associated with optically bluer and mid-IR redder hosts than the LEG FR
IIs and to galaxies and black holes that are smaller, on average, by a factor
of ~2. FR IIs have a factor of ~3 higher average radio luminosity than FR Is.
Nonetheless, most (~90%) of the selected FR IIs have a radio power that is
lower, by as much as a factor of ~100, than the transition value between FR
Is and FR IIs found in the 3C sample. The correspondence between the
morphological classification of FR I and FR II and the separation in radio
power disappears when including sources selected at low radio flux
thresholds, which is in line with previous results. In conclusion, a radio
source produced by a low-power jet can be edge brightened or edge darkened,
and the outcome is not related to differences in the optical properties of
the host galaxy.
The authors searched for FR II radio galaxies in the sample of 18,286 radio
sources built by Best & Heckman (2012, MNRAS, 421, 1569) by limiting their
search to the subsample of objects in which, according to these latter
authors, the radio emission is produced by an active nucleus. They
cross-matched the optical spectroscopic catalogs produced by the group from
the Max Planck Institute for Astrophysics and Johns Hopkins University
(Brinchmann et al. 2004, MNRAS, 351, 1151; Tremonti et al. 2004, ApJ, 613,
898) based on data from the Data Release 7 of the Sloan Digital Sky Survey
(DR7/SDSS; Abazajian et al. 2009, ApJS, 182, 543) with the National Radio
Astronomy Observatory Very Large Array Sky Survey (NVSS; Condon et al. 1998,
AJ, 115, 1693, CDS Cat. VIII/65) and the Faint Images of the Radio Sky at
Twenty centimeters survey (FIRST; Becker et al. 1995, ApJ, 450, 559; Helfand
et al. 2015, ApJ, 801, 26, CDS Cat. VIII/92) adopting a radio flux density
limit of 5 mJy in the NVSS. The authors focused on those sources with
redshift z < 0.15.
The majority (108) of the selected FR IIs are classified as LEG, but there
are also 14 HEG and just one source that cannot be classified
spectroscopically because of the lack of emission lines, namely SDSS
J144625.13+214209.8.
Throughout this study, the authors adopted a cosmology with H0 = 67.8 km
s-1 Mpc-1, OmegaM = 0.308, and OmegaLambda = 0.692 (Planck
Collaboration XIII 2016, A&A, 594, A13).
FSVSCLUSTR Catalog
The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups
contains a a large sample of 598 galaxy clusters and rich groups discovered
in the data of the Faint Sky Variability Survey (FSVS). The clusters have
been identified using a fully automated, semi-parametric technique based on a
maximum likelihood approach applied to Voronoi tessellation, and enhanced by
color discrimination. The sample covers a wide range of richness, has a
density of ~28 clusters per square degree, and spans a range of estimated
redshifts of 0.05 < z < 0.9 with mean <z> = 0.345. Assuming the presence of a
cluster red sequence, the uncertainty of the estimated cluster redshifts is
assessed to be sigma ~ 0.03. Containing over 100 clusters with z > 0.6, the
catalog contributes substantially to the current total of optically-selected,
intermediate-redshift clusters, and complements the existing, usually X-ray
selected, samples. The FSVS fields are accessible for observation throughout
the whole year, making them particularly suited for large follow-up programs.
The construction of this FSVS Cluster Catalogue completes a fundamental
component of the authors' continuing program to investigate the environments
of quasars and the chemical evolution of galaxies. The present table contains
the list of all clusters with their basic parameters.
GCSCAT Catalog
This table contains a catalog of 422 galaxies with published measurements of
their globular cluster (GC) populations. Of these, 248 are E galaxies, 93 are
S0 galaxies, and 81 are spirals or irregulars. Among various correlations of
the total number of GCs with other global galaxy properties, the authors find
that the number of globular clusters NGC correlates well though nonlinearly
with the dynamical mass of the galaxy bulge Mdyn = 4 sigma _e_2 Re/G,
where sigmae is the central velocity dispersion and Re the effective
radius of the galaxy light profile. In their paper, the authors also present
updated versions of the GC specific frequency SN and specific mass SM
versus host galaxy luminosity and baryonic mass. These graphs exhibit the
previously known U-shape: highest SN or SM values occur for either dwarfs
or supergiants, but in the mid-range of galaxy size (109 - 1010 Lsun)
the GC numbers fall along a well-defined baseline value of SN ~= 1 or SM
= 0.1, similar among all galaxy types. Along with other recent discussions,
the authors suggest that this trend may represent the effects of feedback,
which systematically inhibited early star formation at either very low or
very high galaxy mass, but which had its minimum effect for intermediate
masses. Their results strongly reinforce recent proposals that GC formation
efficiency appears to be most nearly proportional to the galaxy halo mass
Mhalo. The mean "absolute" efficiency ratio for GC formation that the
authors derive from the catalog data is MGCS/Mhalo = 6 x 10-5. They
suggest that the galaxy-to-galaxy scatter around this mean value may arise in
part because of differences in the relative timing of GC formation versus
field-star formation. Finally, they find that an excellent empirical
predictor of total GC population for galaxies of all luminosities is
NGC ~ (Re sigmae)1.3, a result consistent with fundamental plane
scaling relations.
GLXSDSSQS2 Catalog
A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy
Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should
isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use
SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy
contaminants in the sample to a very high level, based on the 7-band
photometry. In their paper, they discuss the distributions of redshift,
luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be
present in their final sample of 19,812 point sources. This latter catalog is
available in the present table.
This paper is based on archival data from the Galaxy Evolution Explorer
(GALEX) which is operated for NASA by the California Institute of Technology
under NASA contract NAS5-98034, and on data from the SDSS.
HCG Catalog
The HCG database table is based on the Hickson Catalog, which is a list of
100 compact groups of galaxies that were identified by a systematic search of
the Palomar Observatory Sky Survey red prints. Each group contains four or
more galaxies, has an estimated mean surface brightness brighter than 26.0
magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical
parameters which were derived for 92 of the 100 groups are also included in
the database. (Note that the Hubble constant was assumed to be Ho = 100
km/s/Mpc.)
This database table essentially contains the information given in Table 1 of
Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992,
ApJ, 399, 353). Consequently, the information on individual galaxies in the
Hickson groups that is also given in these references, e.g., in Table 2 of
Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table;
however, the latter data can be found in the related HEASARC database table
HCGGALAXY.
HCGGALAXY Catalog
The HCGGALAXY database table is based on the Hickson Catalog of Compact
Groups, and contains data on 463 galaxies in 100 compact groups of galaxies
that were identified by a systematic search of the Palomar Observatory Sky
Survey red prints. Each group contains four or more galaxies, has an
estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2
and satisfies an isolation criterion. Astrometry, photometry, and
morphological types, derived from CCD images, are presented for the 463
galaxies. Radial velocities are given for 457 of the 463 galaxies: more than
84% of the galaxies measured have radial velocities that are within 1000 km/s
of the group median velocity. Morphological information derived from either
an isophotal analysis or from a visual inspection of images is given for 210
of the 463 galaxies.
This database table essentially contains the information given in Table 2 of
Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al.
(1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P.
(1994, ApJ, 427, 684). Consequently, the information on the properties of the
Hickson Compact Groups as units that is also given in some of these
references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is
not in the HCGGALXY database table; however, the latter data can be found in
the related HEASARC database table HCG.
INTIBISAG2 Catalog
In the most recent IBIS survey based on observations performed during the
first 1000 orbits of INTEGRAL, there are listed 363 high-energy emitters
firmly associated with AGN, 107 of which are reported here for the first
time. The authors have used X-ray data to image the IBIS 90% error circle of
all the AGN in the sample of 107, in order to obtain the correct X-ray
counterparts, locate them with arcsecond accuracy and therefore pinpoint the
correct optical counterparts. This procedure has led to the optical and
spectral characterization of the entire sample. This new set consists of 34
broad line or type 1 AGN, 47 narrow line or type 2 AGN, 18 blazars and 8
sources of unknown class. These eight sources have been associated with AGN
from their positional coincidence with 2MASX/Radio/X-ray sources. Seven
high-energy emitters have also been included since they are considered to be
good AGN candidates. Spectral analysis has been already performed on 55
objects and the results from the most recent and/or best statistical
measurements have been collected. For the remaining 52 sources, the authors
report the spectral analysis for the first time in this work. They have been
able to obtain full X-ray coverage of the sample making use of data from
Swift/XRT, XMM-Newton and NuSTAR. In addition to the spectral
characterization of the entire sample, this analysis has enabled the authors
to identify peculiar sources and by comparing different data sets, highlight
flux variability in the 2-10 keV and 20-40 keV bands.
In the reference paper, the authors present the X-ray and optical follow-up
work on 107 new AGN recently detected by INTEGRAL. Fortunately, they have
been able to obtain full X-ray coverage of the entire sample making use of
data from the Swift/XRT, Newton-XMM, and NuSTAR archives or through Swift/XRT
follow-up observations that they triggered.
The HEASARC notes that this table of AGN newly detected by INTEGRAL and not
included in the original INTEGRAL IBIS AGN Catalog (Malizia et al. 2012,
MNRAS, 426, 1750, available at the HEASARC as the INTIBISAGN table) actually
contains 108 AGN plus 8 candidate AGN, for a total of 116 objects, rather
than the 107 plus 7 candidate AGN totalling 114 objects that are quoted in
the abstract of the reference paper (and stated above). The reason for this
discrepancy is not known to the HEASARC.
IRASPSCZ Catalog
The IRAS Point Source Catalog Redshift (PSCz) Survey consists of redshifts,
infrared and optical photometry, and assorted other information for 18351
IRAS sources, mostly selected from the Point Source Catalog. The survey was
designed to select almost all galaxies with flux brighter than 0.595 Jy at 60
microns (µm), over the 84% of the sky with extinction small enough that
reliable and complete optical identification and spectroscopy was possible.
Some of the sources are not galaxies and some are multiple entries for the
same galaxy as described in the reference paper. There are in total 15,411
galaxies or possible galaxies, for which redshifts are available for 14,677.
The galaxies without redshift are mostly distant or at low latitude, as
described in the paper. Many of these galaxies have now been observed as part
of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the
Plane Survey"), and their redshifts were to be included in future revisions
of this catalog.
The full catalog for the PSCz Catalog contains more than 120 parameters and
is available at the CDS in the directory
http://cdsarc.u-strasbg.fr/ftp/cats/VII/221/ as the files pscz.dat (18,351
sources in the main catalog) and psczcg.dat (60 additional sources close to
the coverage gap). There is also a 'short' version of the catalog, psczvs.dat
and psczcgvs.dat, containing 19 parameters, sufficient information for most
studies. They correspond to the version 2.2.
Many fields are taken directly from the IRAS Point Source Catalogue (CDS Cat.
II/125). See the IRAS Explanatory Supplement (Beichman et al., 1988, NASAR,
1190, 1) for more information. If there are problems that cannot be resolved
by careful reading of these notes or the accompanying paper, please contact
Will Saunders <will@roe.ac.uk> or Will Sutherland
<W.Sutherland1@physics.ox.ac.uk>.
KUEHR Catalog
This catalog is a compilation of 518 extragalactic radio sources with flux
densities greater than 1 Jy at 5 GHz. It contains sources from the NRAO-MPI
5-GHz Strong Source Surveys and from re-observation at 5 GHz of sources found
in the Parkes 2.7-GHz surveys. All sources were found in 9.811 sr covered by
the two surveys. This is essentially the whole sky, excluding the galactic
plane (latitudes less than 10 degrees) and the Magellanic Clouds. The catalog
includes radio flux densities, radio positions, object classes, visual
magnitudes, redshifts, and spectral indices.
LBQS Catalog
Positions, redshifts, and magnitudes for the 1055 quasars in
the Large Bright Quasar Survey (LBQS) are presented in a single catalog.
Celestial positions have been rederived using the PPM catalog to
provide an improved reference frame. Redshifts calculated via
cross correlation with a high signal-to-noise ratio composite quasar
spectrum are included and the small number of typographic and redshift
misidentifications in the discovery papers are corrected.
Compared to the discovery papers (references below), 12 quasars that are
either fainter than the field magnitude limit or fall outside the final survey
area have been deleted, 12 quasars that were discovered subsequent to paper V
have been added, 10 redshifts have been corrected, and 13 quasars with
either incorrect or degenerate designations (LBQS names) have had their
designations corrected.
The information in this version of the LBQS Catalog is the same as in Table
4 of the published paper with the following exceptions: (i) the object
0021-0213 has a redshift of 2.348; this value was listed in Table 5 of the
paper but was not incorporated in Table 4 of the paper; (ii) the parameter
'Reference' in Table 4 of the published paper (which specified in which paper in
the LBQS series the quasar spectrum could be found) has been omitted; and
(iii) the parameter 'Notes' in Table 4 of the published paper had two non-blank
values: '+' and 'a'; in the HEASARC representation of this catalog we have
replaced the Notes value of '+' by 'C', and dropped the Notes value of 'a'
(used to indicate objects that had been listed as AGN in earlier papers).
LCRSCAT Catalog
The Las Campanas Redshift Survey (LCRS) consists of 26,418
redshifts of galaxies selected from a CCD-based catalog obtained in the R band.
The survey covers over 700 deg2 in six strips, each 1.5 x 80 degrees, three
each in the north and south Galactic caps. The median redshift in the
survey is about 30,000 km s-1. Essential features of the galaxy selection
and redshift measurement methods are described and tabulated in the
reference paper. These details are important for subsequent analysis of
the LCRS data. Two-dimensional representations of the redshift distributions
reveal many repetitions of voids, on the scale of about 5000 km s-1, sharply
bounded by large walls of galaxies as seen in nearby surveys.
Statistical investigations of the mean galaxy properties and of
clustering on the large scale are reported elsewhere. These include
studies of the luminosity function, power spectrum in two and three
dimensions, correlation function, pairwise velocity distribution,
identification of large-scale structures, and a group catalog.
This table contains entries for 94959 objects from the
LCRS for which photometric data were obtained and which were initially
classified as galaxies on the basis of this photometric information, although
subsequent spectroscopy indicated that a small fracton of them are actually
stars. There are 27021 objects out
of this total which have spectroscopic redshift information (either of
themselves or of a nearby object).
See also the LCRS home pages at:
http://qold.astro.utoronto.ca/~lin/lcrs.html.
LORCAT Catalog
A well-known property of the gamma-ray sources detected by Cos-B in the
1970s, by the Compton Gamma-Ray Observatory in the 1990s, and recently by the
Fermi Gamma-ray Observatory is the presence of radio counterparts,
particularly for those associated with extragalactic objects. This
observational evidence is the basis of the radio/gamma-ray connection
established for the class of active galactic nuclei known as blazars. In
particular, the main spectral property of the radio counterparts associated
with gamma-ray blazars is that they show a flat spectrum in the GHz frequency
range. The authors' recent analysis dedicated to search for blazar-like
candidates as potential counterparts for the unidentified gamma-ray sources
allowed them to extend the radio/gamma-ray connection in the MHz regime. They
also showed that blazars below 1 GHz maintain flat radio spectra. Thus, on
the basis of these new results, the authors have assembled a low-frequency
radio catalog of flat-spectrum sources built by combining the radio
observations of the Westerbork Northern Sky Survey (WENSS) and of the
Westerbork in the southern hemisphere (WISH) catalogs with those of the NRAO
Very Large Array Sky survey (NVSS). This catalog could be used in the future
to search for new, unknown blazar-like counterparts of gamma-ray sources.
First, the authors found NVSS counterparts of Westerbork Synthesis Radio
Telescope (WSRT) radio sources, and then they selected flat-spectrum radio
sources according to a new spectral criterion, specifically defined for radio
observations performed below 1 GHz. In their paper, they also describe the
main properties of the catalog listing 28,358 radio sources with spectral
indices between 1400 and 325/352 MHz between -1.0 and +0.4, and their log N -
log S distributions. Finally, a comparison with the Green Bank 6 cm radio
source catalog was performed so as to investigate the spectral shape of the
low-frequency flat-spectrum radio sources at higher frequencies.
LOWZVLQVLA Catalog
This table contains results from 6-GHz Jansky Very Large Array (JVLA)
observations covering a volume-limited sample of 178 low-redshift (0.2 < z
<0.3) optically selected quasi-stellar objects (QSOs). These 176 radio
detections fall into two clear categories: (1) about 20% are radio-loud QSOs
(RLQs) with spectral luminosities of L6 >~ 1023.2 W/Hz that are primarily
generated in the active galactic nucleus (AGN) responsible for the excess
optical luminosity that defines a bona fide QSO; and (2) the remaining 80%
that are radio-quiet QSOs (RQQs) that have 1021 <~ L6 <~ 1023.2 W/Hz
and radio sizes <~ 10 kpc, and the authors suggest that the bulk of their
radio emission is powered by star formation in their host galaxies.
"Radio-silent" QSOs (L_6_<~ 1021 W/Hz) are rare, so most RQQ host galaxies
form stars faster than the Milky Way; they are not "red and dead"
ellipticals. Earlier radio observations did not have the luminosity
sensitivity of L6 <~ 1021 W/Hz that is needed to distinguish between such
RLQs and RQQs. Strong, generally double-sided radio emission spanning >> 10
kpc was found to be associated with 13 of the 18 RLQ cores with peak flux
densities of Sp > 5 mJy/beam (log(L) >~ 24). The radio luminosity function
of optically selected QSOs and the extended radio emission associated with
RLQs are both inconsistent with simple "unified" models that invoke
relativistic beaming from randomly oriented QSOs to explain the difference
between RLQs and RQQs. Some intrinsic property of the AGN or their host
galaxies must also determine whether or not a QSO appears radio-loud.
The authors have reprocessed the VLA observations of a sample of SDSS QSOs
discussed in Kimball et al. (2011, ApJ, 739, L29). These were obtained using
the VLA C configuration with a central frequency of 6 GHz and a bandwidth of
2 GHz in each of the two circular polarizations: with natural weighting the
synthesized beam width was 3.5 arcseconds FWHM. The authors generated a
catalog of radio sources associated with each QSO. They detected radio
emission at 6 GHz from all but two of the 178 color-selected SDSS QSOs
contained in this volume-limited sample of QSOs more luminous than Mi = -23
and with redshifts 0.2 < z < 0.3.
All calculations in the reference paper assume a flat LambdaCDM cosmology
with H0 = 70 km s-1 Mpc-1 and OmegaLambda = 0.7. Spectral
luminosities are specified by their source-frame frequencies, flux densities
are specified in the observer's frame, and a mean spectral index of alpha =
d(log S)/d(log nu) = -0.7 is used to make frequency conversions
LQAC Catalog
Since the release of the original Large Quasar Astrometric Catalog (LQAC:
Souchay et al. 2009, A&A, 494, 815), a large number of quasars have been
discovered through very dense observational surveys. Following the same
procedure as in the first release of the LQAC, the authors aim is to compile
all the quasars recorded up until the present date, with the best
determination of their ICRS equatorial coordinates, i.e., with respect to the
newly established ICRF2 (the second realization of the International
Celestial Reference Frame) and with the maximum of information concerning
their physical properties, e.g., redshifts, photometry, absolute magnitudes.
In the second paper, the authors first of all made a substantial review of
the definitions and properties of quasars and AGN (Active Galactic Nuclei),
the differentiation of these objects being unclear in the literature and even
for specialists. This served their purpose when deciding which kinds of
objects would be taken into account in this compilation. Then, they carried
out the cross-identification between the 9 catalogs of quasars chosen for
their accuracy and their huge number of objects, using a flag for each of
them, and including all the available data related to magnitudes (infrared
and optical), radio fluxes and redshifts. They also performed cross
identification with external catalogs 2MASS, B1.0 and GSC2.3 in order to
complete photometric data for the objects. Moreover, they computed the
absolute magnitude of their extragalactic objects by taking into account
recent studies concerning Galactic absorption. In addition, substantial
improvements were brought with respect to the first release of the LQAC.
First, an LQAC name was given for each object based on its equatorial
coordinates with respect to the ICRS, following a procedure which creates no
ambiguity for identification. Secondly, the equatorial coordinates of the
objects were recomputed more accurately according to the algorithms used for
the elaboration of the Large Quasar Reference Frame (LQRF) (Andrei et al.,
2009, CDS Cat. I/313). Thirdly, the authors introduced a morphological
classification for the objects which enabled them in particular to define
clearly if the object is point-like or extended. The authors adopted a
cosmology with H0 = 70 km s-1 Mpc-1, OmegaM = 0.3, OmegaLambda =
0.7, and q0 = -0.65 in LQAC-3 (which is slightly different from that
adopted for LQAC-2, notice).
The final catalog, called LQAC-2, contained 187,504 quasars. This was roughly
65% larger than the 113,666 quasars recorded in the first version of the LQAC
(Souchay et al. 2009, CDS Cat. J/A+A/494/799) and a little more than the
number of quasars recorded in the up-dated version of the Veron-Cetty and
Veron (2010, CDS Cat. VII/258, HEASARC VERONCAT table) catalog, which was the
densest compilation of quasars up to the present one. In addition to the
quantitative and qualitative improvements implemented in this compilation,
the authors discussed the homogeneity of the data and carried out a
statistical analysis concerning the spatial density and the distance to the
nearest neighbor in their published paper. The authors adopted a cosmology
with H0 = 72 km s-1 Mpc-1 and q0 = -0.58 in this study.
From an astrometric point of view, quasars constitute quasi-ideal reference
objects in the celestial sphere, with an a priori absence of proper motion.
Since the second release of the LQAC, a large number of quasars have been
discovered, in particular with the upcoming new release of the SDSS quasars
catalog. Following the same procedure as in the two previous releases of the
LQAC, The authors' aim for LQAC-3 was to compile all the quasars recorded
until the present date, with accurate recomputation of their equatorial
coordinates in the ICRS and with the maximum of information concerning their
physical properties, such as the redshift, the photometry, and the absolute
magnitudes.
The authors carried out the cross-identification between the 9 catalogs of
quasars chosen for their huge number of objects, including all the available
data related to magnitudes, radio fluxes, and redshifts. This cross
identification was particularly delicate because of a slight change in
coordinates between the objects common to two successive releases of the SDSS
and the elimination of some of them. Equatorial coordinates were recomputed
more accurately according to the algorithms used for the elaboration of the
Large Quasar Reference Frame (LQRF). Moreover, absolute magnitudes and
morphological indexes of the new objects were given, following the same
method as in the LQAC-2.
The final catalog, called LQAC-3, contains 321,957 objects including a small
proportion of AGNs (14,128) and BL Lac objects (1,183). This is roughly 70%
more than the number of objects recorded in the LQAC-2. The LQAC-3 will be
useful for the astronomical community since it gives the most complete
information available about the whole set of already recorded quasars, with
emphasis on the precision and accuracy of their coordinates with respect to
the ICRF2.
MARKARIAN Catalog
A catalog of galaxies with UV-continuum (Markarian galaxies) detected during
the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to
search for peculiar faint extragalactic objects with UV-excess radiation and
to study them. The procedure of observations and processing, the FBS areas,
the object selection and classification criteria and also several selection
effects are described in the reference. The catalog contains the following
initial data on all the objects: the precise coordinates, visual magnitudes,
angular sizes, redshifts and classification types. The observational results
of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology
and some other data are also included in the catalog. While compiling the
catalog, the authors introduced some necessary corrections in the data of the
earlier published lists on galaxies with UV-continuum excesses. In addition,
the authors included the objects with numbers 1501-1515. In most cases,
they are well-known Seyfert galaxies omitted by the authors in the lists,
but detected on the plates. 48 objects from their lists are not included in
the catalog, since they are either stars of our Galaxy or star projections
on the galaxies. This catalog presents the largest homogeneous sample of
AGN of different types on the northern sky for bright objects (apparent
magnitude < 16.0). Up to the middle of 1987 redshifts were measured for
1459 out of 1469 objects in the catalog.
MARKARIAN2 Catalog
A database for the entire Markarian (First Byurakan Spectral Sky Survey or
FBS) Catalog is presented that combines extensive new measurements of their
optical parameters with a literature and database search. The measurements
were made using images extracted from the STScI Digitized Sky Survey (DSS)
of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained
by the Palomar and UK Schmidt telescopes. The authors provide accurate
coordinates, morphological type, spectral and activity classes, red and
blue apparent magnitudes, apparent diameters, axial ratios, and position
angles, as well as number counts of neighboring objects in a circle of
radius 50 kpc. Special attention was paid to the individual descriptions of
the galaxies in the original Markarian lists, which clarified many cases of
misidentifications of the objects, particularly among interacting systems,
larger galaxies with knots of star formation, possible stars, and cases
of stars projected on galaxies. The total number of individual Markarian
objects in the database is now 1544. The authors also have included redshifts
which are now available for 1524 of the objectswith UV-excess radiation,
as well as Galactic color excess E(B-V) values and their 2MASS or DENIS
infrared magnitudes. The table also includes extensive notes that summarize
information about the membership of Markarian galaxies in different systems
of galaxies and about new and revised activity classes and redshifts.
The new optical information on Markarian galaxies was obtained from images
extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and
J_pg (blue) band photographic sky survey plates obtained by the Palomar and
UK Schmidt telescopes.
MCG Catalog
The MCG database contains the "Morphological Catalogue of Galaxies," a
compilation of information for approximately 34,000 galaxies found and
examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers
are assigned for about 29,000 galaxies and information on the remaining 5,000
is present in the extensive notes of the published catalogs
(Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according
to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01
(+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are
numbered with increasing right ascension. The original goal of the
compilation was to be complete for galaxies brighter than magnitude 15.1, but
the final catalog lists many objects considerably fainter.
Information given in the original printed volumes includes: cross-
identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908)
catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes
and intensities of the bright inner region and the entire object,
estimated inclination, and coded description (by symbols) of the
appearance of the galaxy. Each field is then followed by notes on
individual objects. All of the above data except the coded description
are included in the machine version, except that special coding (e.g.
for uncertainty or source designation) is not present (other than for
the NGC/IC cross identifications [added at the Astronomical Data Center
for this machine version]). Although the notes are not computerized,
the presence of a note in the original is flagged in the machine version
Detailed descriptions of modifications, corrections and the record format
are provided for the machine-readable version of the "Morphological Catalogue
of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional
Information section below. In addition to hundreds of individual corrections,
a detailed comparison of the machine-readable with the published catalog
resulted in the addition of 116 missing objects, the deletion of 10 duplicate
records, and a format modification to increase storage efficiency.
MCXC Catalog
The MCXC is the Meta-Catalog of the compiled properties of X-ray detected
Clusters of galaxies. This very large catalog is based on publicly available
ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and
CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster
catalogs. Data have been systematically homogenised to an overdensity of 500,
and duplicate entries from overlaps between the survey areas of the
individual input catalogs have been carefully handled. The MCXC comprises
1743 clusters with virtually no duplicate entries. For each cluster, the MCXC
provides three identifiers, a redshift, coordinates, membership in the
original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx500,
total mass M500, and radius R500, where the 500 suffix means that the
quantity has been calculated up to a standard characteristic radius R500,
the radius within which the mean overdensity of the cluster is 500 times the
critical density at the cluster redshift . The meta-catalog additionally
furnishes information on overlaps between the input catalogs and the
luminosity ratios when measurements from different surveys are available, and
gives notes on individual objects. The MCXC is made available so as to
provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other
multiwavelength studies.
The catalogs and sub-catalogs included in this meta-catalog are listed in
Table 1 of the reference paper, and come from the following references:
Catalog Sub- Reference Title
Catalog or CDS Cat. (Author)
RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS)
(Voges+, 1999)
BCS
BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I.
(Ebeling+, 1998)
eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample
(Ebeling+ 2000)
CIZA X-ray clusters behind the Milky Way
CIZAI ApJ, 580, 774
(Ebeling+, 2002)
CIZAII J/APJ/662/224
(Kocevski+, 2007)
EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey
(Gioia+, 1990)
EMSS_1994 ApJS, 94, 583
(Gioia & Luppino, 1994)
EMSS_2004 ApJ, 608, 603
(Henry 2004)
MACS ApJ, 553, 668 Massive Cluster Survey
(Ebeling+, 2001)
MACS_MJFV ApJS, 174, 117
(Maughan+, 2008)
MACS_BRIGHT MNRAS, 407, 83
(Ebeling+, 2010)
MACS_DIST ApJ, 661, L33
(Ebeling+, 2007)
NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog
(Henry+, 2006)
NORAS/
REFLEX
NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I.
(Boehringer+, 2000)
REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat
(Boehringer+, 2004)
SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP
(Cruddace+, 2002)
SHARC
SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog
(Romer+, 2000)
SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog
(Burke+, 2003)
WARPS
WARPSI J/ApJS/140/265 WARPS survey. VI.
(Perlman+, 2002)
WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII.
(Horner+, 2008)
160SD
160SD J/ApJ/594/154 160 square degree ROSAT Survey
(Mullis+, 2003)
400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey
(Burenin+, 2007)
400SD_SER Serendipitous clusters
400SD_NONSER Not entirely serendipitous clusters
MILLIQUAS Catalog
This table contains the Million Quasars (MILLIQUAS) Catalog, Version 8
(2 August 2023). It is a compendium of 907,144 type-I QSOs and AGN, largely
complete from the literature to 30 June 2023. 66,026 QSO candidates are
also included, calculated via radio/X-ray association (including double radio
lobes) as being 99% likely to be quasars. Blazars and type-II objects are
also included, bringing the total count to 1,021,800. 60.7% of all objects
show Gaia-EDR3 astrometry.
Low-confidence/quality or questionable objects (so deemed by their
researchers) are not included in Milliquas. Additional quality cuts can be
applied as detailed in the HMQ paper (Flesch 2015,PASA,32,10). Full QSO/AGN
classification is accomplished via spectral lines, yielding a reliable
spectroscopic redshift. Two spectral lines are required, or one spectral line
refining a compatible photometric redshift. Obscured AGN with redshifts from
the hosts only are taken to be type-II objects. Some legacy quasars with
neither good spectra nor radio/X-ray association were flagged by Gaia-EDR3 as
5-sigma moving (i.e., stars), and so were removed from Milliquas. All objects
are de-duplicated across source catalogs. The author's aim here is to present
one unique reliable object per each data row. Two NIQs offset < 2 arcsec can
be reported as a single object if within the same host. Lenses are reported
as single objects onto the brightest quasar imaged. (Milliquas is not a
catalog of lenses.)
The contents are relatively simple; each object is shown as one entry with
the sky coordinates (of whatever epoch), its original name, object class, red
and blue optical magnitudes, PSF class, redshift, the citations for the name
and redshift, and up to four radio/X-ray identifiers where applicable.
Questions/comments/praise/complaints may be directed to Eric Flesch at
eric@flesch.org. If you use this catalog in published research, the author
requests that you please cite it.
The confirmed quasars of this catalog (to Jan 2015) were published as the
Half Million Quasars (HMQ) catalog: Flesch E., 2015,PASA,32,10. Note however
that Milliquas uses optical sky data from ASP (2017,PASA,34,25) whereas the
HMQ used optical sky data from QORG (2004,A&A,427,387) Appendix A.
NEARGALCAT Catalog
This table contains an all-sky catalog of 869 nearby galaxies
having individual distance estimates within 11 Mpc or corrected radial
velocities relative to the Local Group centroid VLG < 600 km s-1. The
catalog is a renewed and expanded version of the previous Catalog of
Neighboring Galaxies by Karachentsev et al. (2004, AJ, 127, 2031). It collects
data on the following galaxy observables: angular diameters, apparent
magnitudes in the far-UV, B, and Ks bands, H-alpha and H I fluxes,
morphological types, H I-line widths, radial velocities, and distance
estimates. In this Local Volume (LV) sample, 108 dwarf galaxies still remain
without measured radial velocities. The catalog also lists calculated global
galaxy parameters: the linear Holmberg diameters, absolute B magnitudes,
surface brightnesses, H I masses, stellar masses estimated via K-band
luminosity, H I rotational velocities corrected for galaxy inclination,
indicative masses within the Holmberg radius, and three kinds of "tidal index"
which quantify the local density environment. In the reference paper, the
authors briefly discuss the Hubble flow within the LV and different scaling
relations that characterize galaxy structure and global star formation in them.
They also trace the behavior of the mean stellar mass density, H I-mass
density, and star formation rate density within the volume considered.
NORAS Catalog
In the construction of an X-ray-selected sample of galaxy clusters
for cosmological studies, the authors have assembled a sample of 495 X-ray
sources which were found to show extended X-ray emission in the first
processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky
(NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region
with declination >=0 degrees and Galactic latitude |b| >= 20 degrees, and
comprises sources with a Position Sensitive Proportional Counter (PSPC) count
rate >= 0.06 counts/s and a source extent likelihood of L >= 7. In an optical
follow-up identification program, the authors found 378 (76%) of these sources
to be clusters of galaxies.
It was necessary to reanalyze the sources in this sample with a new
X-ray source characterization technique to provide more precise values
for the X-ray flux and source extent than obtained from the standard
processing. This new method, termed growth curve analysis (GCA), has the
advantage over previous methods in its ability to be robust, to be easy
to model and to integrate into simulations, to provide diagnostic plots
for visual inspection, and to make extensive use of the X-ray data. The
source parameters obtained assist the source identification and provide
more precise X-ray fluxes. This reanalysis is based on data from the
more recent second processing of the ROSAT Survey, RASS II. The authors
present a catalog of the cluster sources with the X-ray properties obtained
as well as a list of the previously flagged extended sources that are found
to have a non-cluster counterpart. In their paper, they discuss the process
of source identification from the combination of optical and X-ray data.
To investigate the overall completeness of the cluster sample as a
function of the X-ray flux limit, they extended the search for X-ray cluster
sources to the RASS II data for the northern sky region between 9 and 14
hours in right ascension. They included the search for X-ray emission from
known galaxy clusters as well as a new investigation of extended X-ray
sources. In the course of this search, they found X-ray emission from 85
additional Abell clusters and 56 very probable cluster candidates among
the newly found extended sources. A comparison of the X-ray cluster number
counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX)
Cluster Survey results leads to an estimate of the completeness of the NORAS
sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at
an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s-1 cm-2. The estimated
completeness achieved by adding the supplementary sample in the study area
amounts to about 82% in comparison to REFLEX. The low completeness introduces
an uncertainty in the use of the sample for cosmological statistical studies
that will be cured with the completion of the continuing Northern ROSAT
All-Sky (NORAS) Cluster Survey project.
OSQSONVSS Catalog
The authors used the 1.4-GHz NRAO VLA Sky Survey (NVSS) to study radio
sources in two color-selected QSO samples: a volume-limited sample of 1,313
QSOs defined by Mi < -23 in the redshift range 0.2 < z < 0.45 and a
magnitude-limited sample of 2,471 QSOs with mr <= 18.5 and 1.8 < z < 2.5.
About 10% were detected above the 2.4-mJy NVSS catalog limit and are powered
primarily by active galactic nuclei (AGNs). The space density, rho, of the
low-redshift QSOs evolves as rho ~ (1 + z)6. In both redshift ranges, the
flux-density distributions and luminosity functions of QSOs stronger than 2.4
mJy are power laws, with no features to suggest more than one kind of radio
source. Extrapolating the power laws to lower luminosities predicts the
remaining QSOs should be extremely radio quiet, but they are not. Most were
detected statistically on the NVSS images with median peak flux densities
Sp of ~ 0.3 mJy/beam and ~ 0.05 mJy/beam in the low- and high-redshift
samples, corresponding to spectral luminosities log L1.4GHz ~ 22.7 and ~
24.1 W/Hz, respectively. The authors suggest that the faint radio sources are
powered by star formation at rates dM/dt of ~ 20 M_{sun}_/yr in the moderate
luminosity (median Mi of ~ -23.4) low-redshift QSOs and dM/dt ~
500Msun/yr in the very luminous (median Mi ~ -27.5) high-redshift QSOs.
Such luminous starbursts (<log(LIR/Lsun)> ~ 11.2 and ~ 12.6,
respectively) are consistent with "quasar mode" accretion in which cold gas
flows fuel both AGN and starburst.
The SDSS DR7 QSO catalog (Schneider et al. 2010, AJ, 139, 2360) is complete
to i = 19.1 mag over a solid angle of 2.66 sr around the North Galactic Pole.
It contains the small sample of 179 color-selected QSOs defined by Mi < -23
in the narrow redshift range 0.2 < z < 0.3 studied by Kimball et al. (2011,
ApJ, 739, L29) and the larger sample of 1,313 QSOs in the wider redshift
range 0.2 < z < 0.45 discussed here. Note that these magnitudes were
calculated for an H0= 71 km/s/Mpc and OmegaM = 0.27 modern flat LambdaCDM
cosmology. The entire SDSS DR7 area is covered by the NVSS, whose source
catalog is complete for statistical purposes above a peak flux density Sp ~
2.4 mJy/beam at 1.4 GHz. In the redshift range 0.2 < z < 0.45 the 45" FWHM
(full width between half-maximum points) beam of the NVSS spans 150 - 250
kpc. There are 163 (12%) NVSS detections of the 1,313 QSOs in the redshift
range 0.2 < z < 0.45 which are listed in Table 1 of the reference paper.
The authors also chose a magnitude-limited sample of all 2,471 color-selected
DR7 QSOs brighter than mr = 18.5 in the redshift range 1.8 < z < 2.5. The
NVSS detected radio emission stronger than S = 2.4 mJy from only 191 (8%) of
them: these are listed in Table 3 of the reference paper.
This HEASARC table contains the contents of both samples described above.
It thus has 163 + 191 = 354 entries, the sum of Tables 1 and 3 from the
reference paper. To select only the entries from Table 1, the user should
select entries with redshifts from 0.2 to 0.45. To select only the entries
from Table 3, the user should select entries with redshifts > 1.8.
OSRILQXRAY Catalog
This catalog contains some of the results of an investigation into the X-ray
properties of radio-intermediate and radio-loud quasars (RIQs and RLQs,
respectively). The authors have combined large, modern optical (e.g., SDSS)
and radio (e.g., FIRST) surveys with archival X-ray data from Chandra,
XMM-Newton, and ROSAT to generate an optically selected sample that includes
188 RIQs and 603 RLQs. This sample is constructed independently of X-ray
properties but has a high X-ray detection rate (85%); it provides broad and
dense coverage of the luminosity-redshift (l-z) plane, including at high
redshifts (22% of the objects have z = 2-5), and it extends to high
radio-loudness RL values (33% of objects have RL = log(Lr/Lo) = 3 -
5), where Lr and Lo are the rest-frame monochromatic luminosities at 5
GHz and 2500 Angstroms, respectively). The authors measure the "excess" X-ray
luminosity of RIQs and RLQs relative to radio-quiet quasars (RQQs) as a
function of radio loudness and luminosity, and parametrize the X-ray
luminosity of RIQs and RLQs both as a function of optical/UV luminosity and
also as a joint function of optical/UV and radio luminosity. RIQs are only
modestly X-ray bright relative to RQQs; it is only at high values of radio
loudness (RL >~ 3.5) and radio luminosity that RLQs become strongly X-ray
bright.
This HEASARC table contains the primary sample from the reference paper. The
authors consider three categories of quasars in this work: RQQs, RIQs, and
RLQs (rather than just RQQs and RLQs), where the define RIQs to consist of
objects with 1 <= RL < 2; consequently, the objects they classify as RLQs
satisfy RL >= 2. The primary sample contained herein consists of 654
optically selected RIQs and RLQs with SDSS/FIRST observations and
high-quality X-ray coverage from Chandra (171), XMM-Newton (202), or ROSAT
(281). The primary sample is split nearly evenly between spectroscopic (312)
and high-confidence photometric (342) quasars. Most (562) of the primary
sample objects possess serendipitous off-axis X-ray coverage, while the
remainder (92) were targeted in the observations used in this sample. The
X-ray detection fraction for the primary sample is 84%; the detection
fraction for those objects with Chandra/XMM-Newton/ROSAT coverage is
95%/92%/70% (typical ROSAT observations are comparatively less sensitive and
have higher background).
The authors adopt a standard cosmology with H0 = 70 km s-1 Mpc-1,
OmegaM = 0.3, and OmegaLambda = 0.7 throughout their study.
PGC2003 Catalog
The Principal Galaxy Catalog, 2003 Version (PGC2003) is a
new catalog of principal galaxies. It constitutes the framework of the
HYPERLEDA database that supersedes the LEDA one, with more data and more
capabilities. The catalog is still restricted to confirmed galaxies,
i.e. about one million galaxies, brighter than a B-magnitude of ~18.
In order to provide the best possible identification for each galaxy,
the authors give accurate coordinates (typical accuracy of better than
2 arcseconds), diameters, axis ratios and position angles. Diameters and
axis ratios have been homogenized to the RC2 system at the limiting
surface brightness of 25 B-mag/arcsec2, using a new method (EPIDEMIC).
In order to provide the best designation for each galaxy, the authors
have collected names from 50 catalogs. The compatibility of the spelling
has been tested against NED and SIMBAD, and, as far as possible a
spelling is used that is compatible with both. For some cases, where no
consensus exists between NED, SIMBAD and LEDA, the authors have proposed
some changes that could make the spelling of names fully compatible.
The full catalog is distributed through the CDS and can be extracted
from HYPERLEDA, http://leda.univ-lyon1.fr/.
QORGCAT Catalog
The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray
sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the
ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003)
and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various
galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This
catalog displays calculated percentage probabilities for each optical,
radio/X-ray associated object of its likelihood of being a quasar, galaxy,
star, or erroneous radio/X-ray association.
This table contains the main Master QORG catalog (master.dat) and contains
all 501,756 radio/X-ray associated optical objects and known quasars which
are optically detected in APM/USNO-A. Up to six radio/X-ray catalog
identifications are presented for each optical object, plus any double radio
lobes (21,498 of these). These are superimposed (and laterally fitted) onto a
670,925,779-object optical background which combines APM and USNO-A data.
Other subsets of this master catalog are available at the CDS, including the
Free-Lunch catalog, a concise easy-to-read variant of the Master catalog
showcasing just one X-ray and/or radio identification for each object, a
subset catalog of QSO candidates, and a subset catalog of known
QSOs/galaxies/stars.
Objects presented in this catalog are those optical APM/USNO-A objects which
are associated with X-ray/radio detections, or any optically-found catalogued
QSO/AGN/Bl Lac objects, which have confidence levels >40% of being
radio/X-ray emitting optical objects. There are 501,756 objects included in
all (including 48,285 catalogued quasars), representing the 99.4% coverage of
the sky which is available from the APM and USNO-A. Each object is shown as
one entry giving the position in equatorial coordinates, red and blue optical
magnitudes (recalibrated) and PSF class, calculated probabilities of the
object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray
association, any radio identification from each of the NVSS, FIRST and SUMSS
surveys, including candidate double-lobe detections, any X-ray identification
from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and
field shifts of those identifications, plus, if already catalogued, the
object name and redshift where applicable.
The QORG catalog and supporting data can be accessed from the catalog home
page at http://quasars.org/qorg-data.htm Questions or comments on the catalog
contents may be directed to the first author Eric Flesch at eric@flesch.org.
The authors request that researchers using this catalog make a small
acknowledgement of such use in any published papers which thereby result.
QSO Catalog
This is (a somewhat condensed form of) the Hewitt & Burbidge (1993) Revised
and Updated Catalog of Quasi-Stellar Objects, and contains all then-known
(to 1992 December 31) quasi-stellar objects (QSOs) with measured emission
redshifts and BL Lac objects. The catalog contains 7315 objects, nearly all
of which are quasi-stellar objects, and 89 of which are BL Lac objects. It
contains extensive information on names, positions, magnitudes, colors,
emission-line redshifts, absorption-line systems, etc.
The published version of this catalog (Hewitt & Burbidge 1993, ApJS, 87, 451)
typically contained multiple rows on information for each object. This database
basically has only the information given in the first row for every object,
and is based on the CDS/ADC table VII/158 table1_1.dat.gz.
RASS6DFGS Catalog
This table contains a catalog of 3405 X-ray sources from the ROSAT
All Sky Survey (RASS) Bright Source Catalog which fall within the area covered
by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct
s-1 in the X-ray and covers the area of sky with Declination < 0 degrees and
|b| > 10 degrees. The RASS-6dFGS sample was one of the additional target
catalogs of the 6dFGS and as a result the authors obtained optical spectra for
2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts
with a median redshift of z = 0.16 (excluding the Galactic sources). For the
optically bright sources (b_J <= 17.5) in the observed sample, over 90%
have reliable redshifts. The catalog mainly comprises quasi-stellar
objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of
the sources with reliable redshifts, the majority are type 1 active galactic
nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and
13% are stars. The authors also identify a small number of optically faint,
very low redshift, compact objects which fall outside the general trend in the
b_J - z plane. The RASS-6dFGS catalog complements a number of Northern
hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA
Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and
furthermore, in the same region of sky (-40 degrees < Declination
< 0 degrees) reveals an additional 561 sources that were not
identified as part of that sample.
The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio
using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky
Survey (SUMSS) catalogues and find that the detection rate changes with
redshift. At redshifts larger than 1 virtually all of these sources have radio
counterparts and with a median flux density of 1.15 Jy, they are much stronger
than the median flux density of 28.6 mJy for the full sample. The authors
attribute this to the fact that the X-ray flux of these objects is being
boosted by a jet component, possibly Doppler boosted, that is only present in
radio-loud AGN.
The RASS-6dFGS sample provides a large set of homogeneous optical spectra
ideal for future studies of X-ray emitting AGN.
RASSBSCPGC Catalog
In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog
(RASS-BSC, CDS Cat. <XI/10>, the HEASARC table RASSBSC) with the Catalogue of
Principal Galaxies (PGC, CDS Cat. <VII/119>, the HEASARC table PGC2003), 904
X-ray sources were found that possess possible extragalactic counterparts
within a search radius of 100 arcseconds. A visual screening process was
applied to classify the reliability of the correlations. 547 correlations
have been quoted as reliable identifications. From these, 349 sources are
known to be active galaxies. Although for the other sources no hints for
activity were found in the literature, 69% of those for which we have
distances show X-ray luminosities exceeding those of normal galaxies, a clear
sign that these galaxies also own hitherto unreported X-ray active
components. Some objects are located inside or in the direction of a known
group or cluster of galaxies. Their X-ray flux may therefore be in part
affected by hot gas emission. In the paper, luminosity and log N-log S
distributions are used to characterize different subsamples. Nuclei that are
both optically and X-ray active are found predominantly in spirals. Two
special source samples are defined, one with candidates for X-ray emission
from hitherto unknown groups or clusters of galaxies, and one with high X-ray
luminosity sources, that are likely candidates to possess hitherto unreported
active galactic nuclei. Besides a compilation of X-ray and optical
parameters, X-ray overlays on optical images for all the objects are also
supplied as part of this work.
This table contains 1124 optical galaxy entries for the 904 relevant X-ray
candidates/counterparts from the RASS. Besides a compilation of X-ray and
optical parameters for each source, the results of an identification
screening are also given. The 904 optical images with X-ray overlay contours
(xID_nnn.ps.gz) used in the screening process are added for each user's own
judgement of the reliability of the associations.
RASSCALS Catalog
This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center
for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and
optical survey of low-mass galaxy groups as of its publication date in 2000.
The authors drew 260 groups from the combined Center for Astrophysics and
Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting
Zwicky magnitude of mz = 15.5. They detected 61 groups (23%) as extended
X-ray sources. The X-ray detections have a median membership of nine
galaxies, a median recession velocity cz = 7250 km/s, a median projected
velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) =
3 x 1042 /h(100)2 erg/s, where the Hubble constant is H(0) = 100 h(100)
km/s/Mpc.
The data in this table replace the preliminary analysis of the X-ray data
which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat.
<J/ApJ/518/69>.
RASSDSSAGN Catalog
This table contains further results of a program aimed at yielding ~ 104
fully characterized optical identifications of ROSAT X-ray sources. The
program employs X-ray data from the ROSAT All Sky Survey (RASS) and both
optical imaging and spectroscopic data from the Sloan Digital Sky Survey
(SDSS). RASS/SDSS data from 5740 deg2 of sky spectroscopically covered in
SDSS Data Release 5 (DR5) provide an expanded catalog of 7000 confirmed
quasars and other active galactic nuclei (AGN) that are probable RASS
identifications. Again, in this expanded catalog the identifications as X-ray
sources are statistically secure, with only a few percent of the SDSS AGNs
likely to be randomly superposed on unrelated RASS X-ray sources. Most
identifications continue to be quasars and Seyfert 1 galaxies with 15 < m <
21 and 0.01 < z < 4, but the total sample size has grown to include very
substantial numbers of even quite rare AGN, e.g., it now includes several
hundreds of candidate X-ray-emitting BL Lac objects and narrow-line Seyfert 1
galaxies. In addition to exploring rare subpopulations, such a large total
sample may be useful when considering correlations between the X-ray and the
optical and may also serve as a resource list from which to select the
``best'' object (e.g., the X-ray-brightest AGN of a certain subclass at a
preferred redshift or luminosity) for follow-up X-ray spectral or alternate
detailed studies.
Much more information on the SDSS is available at the project's web site
at http://www.sdss.org/.
RASSEBCS Catalog
This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample
(BCS) and the Low-Flux Extension, which together form the Extended BCS
(eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS,
301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest
clusters of galaxies in the northern hemisphere (Dec >=0 degrees), at high
Galactic latitudes (|b| >= 20 degrees), with measured redshifts z <= 0.3 and
X-ray fluxes higher than 4.4 x 10-12 erg/cm2/s in the 0.1 - 2.4 keV band.
This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS
data and is the largest X-ray-selected cluster sample compiled to the
publication date (1998). In addition to Abell clusters which form the bulk of
the sample, the BCS also contains the X-ray-brightest Zwicky clusters and
other clusters selected from their X-ray properties alone. Effort has been
made to ensure the highest possible completeness of the sample and the
smallest possible contamination by non-cluster X-ray sources. X-ray fluxes
were computed using an algorithm tailored for the detection and
characterization of X-ray emission from galaxy clusters. These fluxes are
accurate to better than 15% (mean 1-sigma error).
The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample
was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the
original BCS and employing an identical selection procedure, the BCS
extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern
hemisphere (Dec >=0 degrees) and at high Galactic latitudes (|b| >= 20
degrees). It comprises 99 X-ray-selected clusters of galaxies with measured
redshifts z <= 0.3 (as well as eight more at z > 0.3) and total fluxes
between 2.8 x 10-12 and 4.4 x 10-12 erg/cm2/s in the 0.1 - 2.4keV band
(the latter value being the flux limit of the original BCS). The extension
can be combined (as it has been in this HEASARC table) with the main sample
published in 1998 to form the homogeneously selected extended BCS (eBCS), the
largest and statistically best understood cluster sample to emerge from the
RASS to date. The nominal completeness of the combined sample (defined with
respect to a power-law fit to the bright end of the BCS log N -log S
distribution) is relatively low at 75% (compared with 90% for the high-flux
sample of Paper I). However, just as for the original BCS, this
incompleteness can be accurately quantified, and thus statistically corrected
for, as a function of X-ray luminosity and redshift. In addition to its
importance for improved statistical studies of the properties of clusters in
the local Universe, the low-flux extension of the BCS is also intended to
serve as a finding list for X-ray-bright clusters in the northern hemisphere
which the authors hoped will prove useful in the preparation of cluster
observations to be made with the next generation of X-ray telescopes such as
Chandra and XMM-Newton.
RASSSDSSGC Catalog
The authors use ROSAT All-Sky Survey (RASS) broad-band X-ray images and the
optical clusters identified from the Sloan Digital Sky Survey Data Release 7
(SDSS DR7) to estimate the X-ray luminosities around ~65,000 candidate galaxy
clusters with masses >~1013 h-1 Msun based on an optical to X-ray (OTX)
code that they developed. They obtain a catalog with X-ray luminosities for
all 64,646 clusters. A total of 34,522 (~53%) of these clusters have a
signal-to-noise ratio S/N > 0 after subtracting the background signal.
According to the reference paper (but see HEASARC Caveats section below),
this catalog contains 817 clusters (473 at redshift z <= 0.12) with S/N > 3
for their X-ray detections (an additional 12,629 clusters have 3 >= S/N > 1
and 21,076 clusters have 1 >= S/N > 0). The authors find about 65% of these
X-ray clusters have their most massive member located near the X-ray flux
peak; for the remaining 35%, the most massive galaxy is separated from the
X-ray peak, with the separation following a distribution expected from a
Navarro-Frenk-White profile. In the reference paper, the authors investigate
a number of correlations between the optical and X-ray properties of these
X-ray clusters, and find that the cluster X-ray luminosity is correlated with
the stellar mass (luminosity) of the clusters, as well as with the stellar
mass (luminosity) of the central galaxy and the mass of the halo, although
the scatter in these correlations is large. Comparing the properties of X-ray
clusters of similar halo masses but having different X-ray luminosities, they
find that massive haloes with masses >~1014 h-1 Msun contain a larger
fraction of red satellite galaxies when they are brighter in X-ray. An
opposite trend is found in central galaxies in relative low-mass haloes with
masses <~1014 h-1 Msun where X-ray brighter clusters have smaller
fraction of red central galaxies. Clusters with masses >~1014 h-1 Msun
that are strong X-ray emitters contain many more low-mass satellite galaxies
than weak X-ray emitters. These results are also confirmed by checking X-ray
clusters of similar X-ray luminosities but having different characteristic
stellar masses. The cluster catalog containing the optical properties of
member galaxies and the X-ray luminosity is also available at
http://gax.shao.ac.cn/data/Group.html.
The optical data used in this analysis are taken from the SDSS galaxy group
catalogs of Yang et al. (2007, ApJ, 671, 153), constructed using the adaptive
halo-based group finder of Yang et al. (2005, MNRAS, 356, 1293), here updated
to DR7. The parent galaxy catalog is the New York University Value-Added
Galaxy Catalog (NYU-VAGC; Blanton et al. 2005, AJ, 129, 2562) based on the
SDSS DR7 (Abazajian et al. 2009, ApJS, 182, 543), which contains an
independent set of significantly improved reductions.
In this study, the authors adopt a Lambda cold dark matter cosmology whose
parameters are consistent with the 7-year data release of the WMAP mission:
Omegam = 0.275, OmegaLambda = 0.725, h = H0/(100 km s-1 Mpc-1) =
0.702, and sigma8 = 0.816.
RC3 Catalog
This table contains the machine-readable version of the Third Reference
Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs,
H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by
Springer-Verlag in 1991, and including some corrections and additions made by
Corwin et al. (1994, AJ, 108, 2128).
Only brief parameter descriptions are given in this help file. Detailed
information about, for example, how certain quantities were derived, or
exactly what a given code means, can be found in the printed version of RC3.
REFLEX Catalog
This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey
Catalog. The REFLEX Cluster Survey provides information on the X-ray
properties, redshifts, and some identification details of clusters in the
REFLEX sample. The catalog describes a statistically complete X-ray
flux-limited sample of 447 galaxy clusters above an X-ray flux of 3 x 10-12
erg/s/cm2 (0.1 to 2.4 keV) in an area of 4.24 steradians in the southern
sky. The cluster candidates were first selected by their X-ray emission in
the ROSAT-All Sky Survey and subsequently spectroscopically identified in the
frame of an ESO key program. Previously described tests have shown that the
sample is more than 90% complete and there is a conservative upper limit of
9% on the fraction of clusters with a dominant X-ray contamination from AGN.
This data set is at present the largest, statistically complete X-ray galaxy
cluster sample. The sample forms the basis of several cosmological studies,
one of the most important applications being the assessment of the statistics
of the large-scale structure of the universe and the test of cosmological
models.
The X-ray luminosities and other distance-dependent cluster parameters are
calculated for a Lambda cosmology with a Hubble Constant H0 of 70 km/s/Mpc,
OmegaM of 0.3, and OmegaLambda of 0.7. The CDS version of this catalog
contains an additional table (reflex50.dat) with these parameters calculated
for an Einstein-de Sitter universe with H0 = 50 km/s/Mpc, OmegaM = 1.0,
and OmegaLambda = 0.0.
ROMABZCAT Catalog
This table contains the 5th edition of the Roma-BZCAT catalog of blazars
which contains coordinates and multi-frequency data of 3561 sources. It
presents several relevant changes with respect to the past editions which are
briefly described in the reference paper.
The Roma-BZCAT catalog contains data on 3561 sources, about 30% more than in
the 1st edition, which either confirmed blazars or exhibiting characteristics
close to this type of sources. With respect to the previous editions, this
new edition has relevant changes in the sources' classification. The authors
emphasize that all the sources in the Roma-BZCAT have a detection in the
radio band. Moreover, complete spectroscopic information is published and
could be accessed by the authors for all of them, with the exception of BL
Lac candidates. Consequently, peculiar sources such as the so called "radio
quiet BL Lacs", which are reported in some other catalogs, are not included
here because of possible contamination by hot stars and other extragalactic
objects.
In the 5th edition, the authors use a similar denomination for the blazars to
that adopted in the previous editions. Each blazar is identified by a code,
with 5BZ for all blazars, a fourth letter that specifies the type (B, G, Q or
U), followed by the truncated equatorial coordinates (J2000). The authors
introduced the edition number before the letters BZ to avoid possible
confusion due to the fact that several sources changed their old names
because of a newly adopted classification.
The 5th edition contains 1151 BZB sources (92 of which are reported as
candidates because their optical spectra could not be found in the
literature), 1909 BZQ sources, 274 BZG sources, and 227 BZU objects.
ROSATRLQ Catalog
Brinkmann et al. (1997) have compiled a sample of all quasars with
measured radio emission from the Veron-Cetty - Veron catalog (1993, VERON93,
CDS/ADC Cat. VII/166) detected by ROSAT (i) in the ALL-SKY SURVEY (RASS, Voges
1992, in Proc. of the ISY Conference `Space Science', ESA ISY-3, ESA
Publications, p.9, ADC/CDS Cat. IX/10), (ii) as targets of pointed
observations, or (iii) as serendipitous sources from pointed observations, as
publicly available from the ROSAT point source catalog (ROSAT-SRC, Voges et
al. 1995, ADC/CDS Cat. IX/11). The total number of ROSAT
detected radio quasars from the above three sources is 654 objects. 69
of the objects are classified as radio-quiet using the defining line
at a radio-loudness of 1.0, and 10 objects have no classification. The
5GHz data are from the 87GB radio survey, the NED database, or from
the Veron-Cetty - Veron catalog. The power law indices and their
errors are estimated from the two hardness ratios given by the SASS
assuming Galactic absorption. The X-ray flux densities in the ROSAT
band (0.1-2.4keV) are calculated from the count rates using the energy
to counts conversion factor for power law spectra and Galactic
absorption. For the photon index, the authors used the value obtained for a
individual source if the estimated 1 sigma error was smaller than 0.5,
otherwise they used the mean value of 2.14.
ROSATRQQ Catalog
A sample of all radio-quiet quasars or quasars without radio
detection taken from the Veron-Cetty - Veron catalog (1993, VERON93,
ADC/CDS Cat. VII/166) which were either (i) detected by ROSAT in the ALL-SKY
SURVEY (RASS, Voges 1992, in Proc. of the ISY Conference `Space Science', ESA
ISY-3, ESA Publications, p.9, ADC/CDS Cat. IX/10), or (ii) detected as targets
of pointed observations, or (iii) detected as serendipitous sources in pointed
observations that were publicly available in the ROSAT point source catalog
(ROSATSRC, Voges et al. 1995, ADC/CDS Cat. IX/11), has been compiled by Yuan
et al. (1998, A&A, 330, 108). For all sources, they used the results
of the Standard Analysis Software System (SASS, Voges et al. 1992, in
Proc. of the ISY Conference `Space Science', ESA ISY-3, ESA
Publications, p.223), employing the most recent processing for the
Survey data (RASS-II, Voges et al. 1996, ADC/CDS Cat. IX/10). The total
number of quasars in this ROSAT Radio-Quiet Quasars Catalog is 846.
Sixty-nine of the radio-quiet objects with radio detections have
already been presented in a previous paper (Brinkmann, Yuan,
and Siebert 1997, Cat. J/A+A/319/413) using the RASS-I results.
Seventeen objects were found to be radio-loud from recent radio surveys and
were marked in the table. When available, the power law photon indices
and the corresponding absorption column densities (NH) were estimated
from the two hardness ratios given by the SASS, both with free fitted
NH and for Galactic absorption. The unabsorbed X-ray flux densities in
the ROSAT band (0.1-2.4keV) were calculated from the count rates using
the energy to counts conversion factor for power law spectra and
Galactic absorption. The authors used as the photon index the value obtained
for the individual source if the estimated 1-{sigma} error was smaller
than 0.5, otherwise they used the redshift-dependent mean value (see the
paper for details). Notice that the positions of sources in this catalog
are not the positions of the X-ray sources, but the optical positions of the
quasars as given in the VERON93 Catalog (Wolfgang Brinkmann, 1998
private communication).
ROSNEPAGN Catalog
The ROSAT North Ecliptic Pole (NEP) Survey of Active Galactic Nuclei (AGN)
Catalog is an X-ray flux-limited sample of 219 AGN discovered in the
contiguous 80.7 square degrees region of the ROSAT North Ecliptic Pole (NEP)
Survey (Gioia et al. 2003, ApJS, 149, 29; CDS Cat. <J/ApJS/149/29>). This
catalog features complete optical identifications and spectroscopic
redshifts. The median redshift, X-ray flux, and X-ray luminosity are z =
0.41, fx = 1.1 x 10-13 erg/cm2/s, and Lx = 9.2 x 1043 h70-2 erg/s
(0.5 - 2.0 keV), respectively. Unobscured Type 1 AGN are the dominant
constituents (90%) of this soft X-ray-selected sample of AGN.
This catalog sample includes several notable revisions relative to previous
versions of the catalog (Mullis 2001, Ph. D. thesis, U. Hawaii; Gioia et al.
2003, ApJS, 149, 29, available in HEASARC Browse as the ROSNEPOID table).
Firstly, the AGN fluxes and luminosities previously reported were
overestimated by approximately 20% on average as a result of an error in the
conversion of X-ray count rate to flux. Secondly, the sample has grown by 1
because of the reclassification of one of the X-ray sources (RX
J1824.7+6509). Finally, in the present study the authors have adopted the
presently favored "concordance" cosmology in computing the X-ray
luminosities. The revised and updated catalog with corrected properties
presented here should be the reference point for any future work with the
ROSAT NEP AGN sample.
ROXA Catalog
Although blazars are a small fraction of the overall AGN
population, they are expected to be the dominant population of extragalactic
sources in the hard X-ray and gamma-ray bands and have been shown to
be the largest contaminant of CMB fluctuation maps. So far the number
of known blazars is of the order of several hundreds, but the
forthcoming AGILE, GLAST and Planck space observatories will detect
several thousand of objects of this type. In preparation for these
missions it is necessary to identify new samples of blazars to study
their multi-frequency characteristics and statistical properties. The authors
have compiled a sample of objects with blazar-like properties via a
cross-correlation between large radio (NVSS, ATCAPMN) and X-ray
surveys (RASS) using the SDSS-DR4 and 2dF survey data to
spectroscopically identify their candidates and test the validity of the
selection method. They present the Radio-Optical-X-ray catalog built
at ASDC (ROXA), a list of 816 objects among which 510 are confirmed
blazars. Only 19% of the candidates turned out to be certainly
non-blazars, demonstrating the high efficiency of our selection method.
This catalog includes 173 new blazar identifications, or about 10% of
all presently known blazars. The relatively high flux threshold in the
X-ray energy band (given by the RASS survey) preferentially selects
objects with high F_X/F_r ratio, leading to the discovery of new High
Energy Peaked BL Lac (HBLs). This catalog therefore includes many new
potential targets for GeV-TeV observations.
The selection method consisted of three steps: 1) a first cross-correlation
between radio and X-ray surveys (the NRAO VLA Sky Survey, ATCAPMN
(ATCA catalogue of compact PMN sources) and ROSAT All Sky Survey; 2)
for each radio/X-ray match, optical magnitudes were retrieved from the
Guide Star Catalog; 3) for all radio/optical/X-ray matches the authors
calculated the X-ray to optical (alpha_ox) and radio to optical
(alpha_ro) spectral slopes and took only sources with alpha_ox and
alpha_ro values within the blazar area. For each object, redshift, B
and G magnitudes, radio fluxes at 1.4 GHz and at 5 GHz, X-ray flux,
F_X/F_r ratio, X-ray luminosity, radio luminosity, Ca H&K break and
classification are given.
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>).
SBSGGENCAT Catalog
The Second Byurakan Survey (SBS) is a continuation of the First Byurakan
Survey (FBS), also known as the Markarian Survey. The goal of the SBS was to
reach fainter objects (as faint as limiting photographic magnitudes of 19.5,
about 2.5 magnitudes fainter than the Markarian survey) and discover new
active and star-forming galaxies using both UV excess and emission-line
techniques.
In this table, a database for the entire catalog of the Second Byurakan
Survey (SBS) galaxies is presented, i.e, the 1700 SBS stars listed in
Stepanian (2005) are not included herein. It contains new measurements of
their optical parameters and additional information taken from the literature
and other databases. The measurements were made using Ipg (near-infrared),
Fpg (red) and Jpg (blue) band images from photographic sky survey plates
obtained by the Palomar Schmidt telescope and extracted from the STScI
Digital Sky Survey (DSS). The database provides accurate coordinates,
morphological type, spectral and activity classes, apparent magnitudes and
diameters, axial ratios, and position angles, as well as number counts of
neighboring objects in circles of radii 50 kpc around the sources. The total
number of individual SBS objects in the database is now 1676. The 188
Markarian galaxies which were re-discovered by the SBS are not included in
this database. the authors also include redshifts that are now available for
1576 SBS objects, as well as 2MASS infrared magnitudes for 1117 SBS galaxies.
The new optical information on the SBS galaxies was obtained from images
extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red), J_pg
(blue) and I_pg (near-infared) band photographic sky survey plates obtained
by the Palomar telescope.
SDSSBALQS2 Catalog
This table contains a catalog of 5035 broad absorption line (BAL)
quasars (QSOs) in the Sloan Digital Sky Survey (SDSS) Data Release 5 (DR5)
QSO catalog that have absorption troughs covering a continuous velocity range
greater than or equal to 2000 km s-1. The authors have fitted ultraviolet
(UV) continua and line emission in each case, enabling them to report common
diagnostics of BAL strengths and velocities in the range from -25,000 to 0 km
s-1 for Si IV 1400 Angstroms, C IV 1549 A, Al III 1857 A, and Mg II 2799 A.
The authors calculate these diagnostics using the spectrum listed in the DR5
QSO catalog, and also for spectra from additional SDSS observing epochs when
available. They confirm and extend previous findings that BAL QSOs are more
strongly reddened in the rest-frame UV than non-BAL QSOs, and that BAL QSOs
are relatively X-ray weak compared to non-BAL QSOs. The observed BAL fraction
is dependent on the spectral signal-to-noise ratio (S/N); for higher S/N
sources, the authors find an observed BAL fraction of about 15%. BAL QSOs show
a similar Baldwin effect as for non-BAL QSOs, in that their C IV emission
equivalent widths decrease with increasing continuum luminosity. However, BAL
QSOs have weaker C IV emission in general than do non-BAL QSOs. Sources with
higher UV luminosities are more likely to have higher-velocity outflows, and
the BAL outflow velocity and UV absorption strength are correlated with
relative X-ray weakness. These results are in qualitative agreement with
models that depend on strong X-ray absorption to shield the outflow from
overionization and enable radiative acceleration. In a scenario in which BAL
trough shapes are primarily determined by outflow geometry, observed
differences in Si IV and C IV trough shapes would suggest that some
outflows have ion-dependent structure.
The authors fit SDSS spectra using the algorithm of Gibson et al. (2008, ApJ,
675, 985), which we summarize here. For QSOs at z >= 1.7, their continuum
model is a power law reddened using the Small Magellanic Cloud (SMC) reddening
curve of Pei (1992, ApJ, 395, 130). For QSOs at lower redshifts, the authors
use a fourth- or sixth-degree polynomial; in their experience this nonphysical
model is able to reproduce well the complex continuum at longer wavelengths.
They initially fit regions that are generally free from strong absorption or
emission features: 1250-1350, 1700-1800, 1950-2200, 2650-2710, 2950-3700,
3950-4050, 4140-4270, 4400-4800, 5100-6400, and > 6900 Angstroms. They then
iteratively fit the continuum, ignoring at each step wavelength bins that
deviate by more than 3 sigma from the current fit in order to exclude strong
absorption and emission features. They fit Voigt profiles to the strongest
emission lines expected in the spectrum: Si IV 1400, C IV 1549, Al III 1857,
C III 1909, and Mg II 2799. These wavelengths are taken from the SDSS vacuum
wavelength list used by the SDSS pipeline to determine emission-line
redshifts.
Much more information on the SDSS is available at the project's web site
at http://www.sdss.org/.
SDSSBALQSO Catalog
The Sloan Digital Sky Survey (SDSS) Broad Absorption Line (BAL) Quasars
Catalog (based on the 3rd SDSS Data Release) contains a total of 4784 unique
BAL quasars from the SDSS DR3 (CDS Cat. <VII/243>). An automated algorithm
was used to match a continuum to each quasar and to identify regions of flux
at least 10% below the continuum over a velocity range of at least 1000 km/s
in the C IV and Mg II absorption regions. The model continuum was selected as
the best-fit match from a set of template quasar spectra binned in
luminosity, emission line width, and redshift z, with the power-law spectral
index and amount of dust reddening as additional free parameters. The authors
characterize their sample through the traditional 'balnicity' index BI and a
revised absorption index AI, as well as through parameters such as the width,
outflow velocity, fractional depth, and number of troughs. From a sample of
16,883 quasars at 1.7 <= z <= 4.38, they identify 4386 (26.0%) quasars with
broad C IV absorption, of which 1756 (10.4%) satisfy traditional selection
criteria. From a sample of 34,973 quasars at 0.5 <= z <= 2.15, they identify
457 (1.31%) quasars with broad Mg II absorption, 191 (0.55%) of which satisfy
traditional selection criteria. They find that BAL quasars may have broader
emission lines on average than other quasars.
Much more information on the SDSS is available at the project's web site
at http://www.sdss.org/.
SDSSCXOQSO Catalog
The authors have studied the spectral energy distributions and
evolution of a large sample of optically selected quasars from the Sloan
Digital Sky Survey (SDSS) that were observed in 323 Chandra images analyzed
by the Chandra Multiwavelength Project (ChaMP). Their highest-confidence
matched sample (which this HEASARC table comprises) includes 1135 X-ray
detected quasars in the redshift range 0.2 < z < 5.4, representing some 36
Msec of effective exposure. In their paper, the authors provide catalogs of
QSO properties, and describe their novel method of calculating X-ray flux
upper limits and effective sky coverage. Spectroscopic redshifts are available
for about 1/3 of the detected sample; elsewhere, redshifts are estimated
photometrically. The authors have detected 56 QSOs with redshift z > 3,
substantially expanding the known sample. They find no evidence for evolution
out to z ~ 5 for either the X-ray photon index Gamma or for the ratio of
optical/UV to X-ray flux Alpha_ox. About 10% of detected QSOs show best-fit
intrinsic absorbing columns greater than 1022 cm-2, but the fraction might
reach ~1/3 if most nondetections are absorbed. The authors confirm a
significant correlation between Alpha_ox and optical luminosity, but it
flattens or disappears for fainter (M_B >~ -23) active galactic nucleus (AGN)
alone. They report significant hardening of Gamma both toward higher X-ray
luminosity, and for relatively X-ray loud quasars. These trends may represent
a relative increase in nonthermal X-ray emission, and their findings thereby
strengthen analogies between Galactic black hole binaries and AGN. For
uniformly selected subsamples of narrow-line Seyfert 1s and narrow absorption
line QSOs, they find no evidence for unusual distributions of either
Alpha_ox or Gamma.
Much more information on the SDSS is available at the project's web site
at http://www.sdss.org/.
SDSSLASQSO Catalog
This table contains a catalog of over 130,000 quasar candidates with
near-infrared (NIR) photometric properties, with an areal coverage of
approximately 1200 deg2. This is achieved by matching the Sloan Digital Sky
Survey (SDSS) in the optical ugriz bands to the UKIRT Infrared Digital Sky
Survey (UKIDSS) Large Area Survey (LAS) in the NIR YJHK bands. The authors
match the ~1 million SDSS DR6 Photometric Quasar catalog to Data Release 3 of
the UKIDSS LAS (ULAS) and produce a catalog with 130,827 objects with
detections in one or more NIR bands, of which 74,351 objects have optical and
K-band detections and 42,133 objects have the full nine-band photometry.
The majority (~85%) of the SDSS objects were not matched simply because these
were not covered by the ULAS. The positional standard deviation of the SDSS
Quasar to ULAS matches is 0.1370 arcseconds in RA and 0.1314 arcseconds in Dec.
The authors find an absolute systematic astrometric offset between the SDSS
Quasar catalog and the UKIDSS LAS, of |RA offset| = 0.025 arcseconds and
|Dec offset| = 0.040 arcseconds; they suggest the nature of this offset to be
due to the matching of catalog, rather than image, level data. Their matched
catalog has a surface density of ~53 deg-2 for K <= 18.27 objects; tests
using this matched catalog, along with data from the UKIDSS Deep Extragalactic
Survey, imply that its limiting magnitude is i ~ 20.6. Color-redshift diagrams,
for the optical and NIR, show a close agreement between this matched catalog
and recent quasar color models at redshift z <~ 2.0, while at higher redshifts,
the models generally appear to be bluer than the mean observed quasar colors.
SDSSNBCKDE Catalog
This table contains a catalog of 1,015,082 quasar candidates selected from
the photometric imaging data of the Sloan Digital Sky Survey (SDSS) using a
non-parametric Bayesian classification kernel density estimator (NBC-KDE). It
excludes 157,075 initial candidates that were culled as known or likely
contaminants. The objects are all point sources to a limiting magnitude of i
= 21.3 from 8417 deg2 of imaging from SDSS Data Release 6 (DR6). This
sample extends the previous catalog (Paper I: Richards et al. 2004, ApJS,
155, 257) by using the latest SDSS public release data and probing both
ultraviolet (UV)-excess and high-redshift quasars. While the addition of
high-redshift candidates reduces the overall efficiency (quasars:quasar
candidates) of the catalog to ~80%, it is expected to contain no fewer than
850,000 bona fide quasars, which is ~8 times the number of the previous
sample and ~10 times the size of the largest spectroscopic quasar catalog.
Cross-matching between this photometric catalog and spectroscopic quasar
catalogs from both the SDSS and 2dF survey yields 88,879 spectroscopically
confirmed quasars. For judicious selection of the most robust UV-excess
sources (~500,000 objects in all), the efficiency is nearly 97 - more than
sufficient for detailed statistical analyses. The catalog's completeness to
type 1 (broad-line) quasars is expected to be no worse than 70%, with most
missing objects occurring at z < 0.7 and 2.5 < z < 3.0. In addition to
classification information, the authors provide photometric redshift
estimates (typically good to Delta(z) +/- 0.3 [2-sigma]) and cross-matching
with radio, X-ray, and proper-motion catalogs. Finally, the authors have
considered the catalog's utility for determining the optical luminosity
function of quasars and are able to confirm the flattening of the bright-end
slope of the quasar luminosity function at z ~ 4 as compared to z ~ 2.
Much more information on the SDSS is available at the project's web site
at http://www.sdss.org/.
SDSSNBCQSC Catalog
The Nonparametric Bayes Classifier (NBC) Quasar Candidate Catalog is a
catalog of 100,563 unresolved, UV-excess (UVX) quasar candidates with
magnitudes to as faint as 21 in the g-band from 2099 square degrees of the
Sloan Digital Sky Survey (SDSS) Data Release One (DR1) imaging data. Existing
spectra of 22,737 sources reveals that 22,191 (97.6%) are quasars; accounting
for the magnitude dependence of this efficiency, the authors estimate that
95,502 (95.0%) of the objects in the catalog are quasars. Such a high
efficiency is unprecedented in broadband surveys of quasars. This
"proof-of-concept" sample is designed to be maximally efficient, but still
has 94.7% completeness to unresolved, g ~< 19.5, UVX quasars from the DR1
quasar catalog. This efficient and complete selection is the result of the
application of a probability density type analysis to training sets that
describe the four-dimensional color distribution of stars and
spectroscopically confirmed quasars in the SDSS. Specifically, the authors
use a nonparametric Bayesian classification, based on kernel density
estimation, to parametrize the color distribution of astronomical sources -
allowing for fast and robust classification. They further supplement the
catalog by providing photometric redshifts and matches to FIRST/VLA, ROSAT,
and USNO-B sources.
Much more information on the SDSS is available at the project's web site at
http://www.sdss.org/.
SDSSQUASAR Catalog
This table contains the Data Release 12 Quasar Catalog (DR12Q) from the
Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky
Survey III (SDSS-III). This catalog includes all SDSS-III/BOSS objects that
were spectroscopically targeted as quasar candidates during the full survey
and that are confirmed as quasars via visual inspection of the spectra, have
luminosities M_i_[z=2] < -20.5 (in a LambdaCDM cosmology with H0 = 70
km/s/Mpc, OmegaM = 0.3, and OmegaLambda = 0.7), and either display at
least one emission line with a full width at half maximum (FWHM) larger than
500 km/s or, if not, have interesting/complex absorption features. The
catalog also includes previously known quasars (mostly from SDSS-I and II)
that were re-observed by BOSS. The catalog contains 297,301 quasars (272,026
are new discoveries since the beginning of SDSS-III) detected over 9376
deg2 with robust identification and redshift measured by a combination of
principal component eigenspectra. The number of quasars with z > 2.15
(184,101, of which 167,742 are new discoveries) is about an order of
magnitude greater than the number of z > 2.15 quasars known prior to BOSS.
Redshifts and FWHMs are provided for the strongest emission lines (C IV, C
III], Mg II). The catalog identifies 29,580 broad absorption line quasars and
their characteristics are listed in the file dr12qbal.dat that is available
at the CDS (http://cdsarc.u-strasbg.fr/ftp/cats/VII/279/). For each object,
the catalog presents five-band (u, g, r, i, z) CCD-based photometry with
typical accuracy of 0.03 mag together with some information on the optical
morphology and the selection criteria. When available, the catalog also
provides information on the optical variability of quasars using SDSS and
Palomar Transient Factory multi-epoch photometry. The catalog also contains
X-ray, ultraviolet, near-infrared, and radio emission properties of the
quasars, when available, from other large-area surveys. The calibrated
digital spectra, covering the wavelength region 3600-10,500 Angstrom at a
spectral resolution in the range 1300 < R < 2500, can be retrieved from the
SDSS Catalog Archive Server at http://www.sdss.org/dr12/data_access/. In
their paper, the authors also provide a supplemental list of an additional
4,841 quasars that have been identified serendipitously outside of the
superset defined to derive the main quasar catalog, available as the file
dr12qsp.dat that is available at the CDS
(http://cdsarc.u-strasbg.fr/ftp/cats/VII/279/).
This table contains the final quasar catalog of the SDSS-III/BOSS survey
resulting from five years of observations. The catalog, which the authors
call "DR12Q", contains 297,301 quasars, 184,101 of which have z > 2.15. the
authors provide robust identification from visual inspection and refined
redshift measurements based on the result of a principal component analysis
of the spectra. The present catalog contains about 80% more quasars than
their previous release (Paris et al., 2014, "DR10Q", CDS Cat. VII/270).
In SDSS-III, all fluxes in the 5 SDSS bands (u, g, r, i and z) are expressed
in terms of "nanomaggies" (nMgy), which are a convenient linear unit. These
quantities are related to standard AB magnitudes thus: an object with a flux
F given in nMgy has a Pogson magnitude (on the AB scale) m = [22.5 mag] -
2.5*log10(F). A flux of 1 Mgy is therefore close to 3631 Jy, and 1 nMgy =
~3.631 uJy (µJy).
SDSSUNUQSR Catalog
Large spectroscopic surveys have discovered very peculiar and hitherto
unknown types of active galactic nuclei (AGN). Such rare objects may hold
clues to the accretion history of the supermassive black holes at the centres
of galaxies. The authors aim to create a sizeable sample of unusual quasars
from the unprecedented spectroscopic database of the Sloan Digital Sky Survey
(SDSS).
This table contains a catalog of 1005 quasars with unusual spectra in the
redshift interval from 0.6 to 4.3. [HEASARC Note: the redshifts in this table
actually range from 0.497 to 4.771]. The quasars were selected from the Sloan
Digital Sky Survey Data Release 7 (Abazajian et al., 2009, ApJS, 182, 543) by
means of Kohonen self-organising maps. The spectra are dominated by either
broad absorption lines (42%), unusual red continua (27%), weak emission lines
(18%), or conspicuously strong optical and/or UV iron emission (11%). This
large sample provides a useful resource for both studying properties and
relations of/between different types of unusual quasars and selecting
particularly interesting objects, even though the compilation is not aimed at
completeness in a quantifiable sense. The spectra are grouped into seven
types. The catalogue contains the redshift, the absolute magnitude, the
spectral type, the radio loudness parameter, a peculiarity index, and some
comments on peculiar spectral features.
SDSSWHLGC Catalog
Clusters of galaxies in most of the previous catalogs have
redshifts z <= 0.3. Using the photometric redshifts of galaxies from the
Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify
39,716 clusters in the redshift range 0.05 < z < 0.6 with more than eight
luminous (M_r <= -21) member galaxies. Cluster redshifts are estimated
accurately with an uncertainty of less than 0.022. The contamination rate
of member galaxies is found to be roughly 20%, and the completeness of
member galaxy detection reaches ~90%. Monte Carlo simulations show that the
cluster detection rate is more than 90% for massive (M_200 > 2 x 10^14
M_sun, where M_200 is the total mass within the radius in which the mean
mass density is 200 times the critical cosmic mass density) clusters of
z <= 0.42. The false detection rate is ~5%. The authors
obtain the richness, the summed luminosity, and the gross galaxy number
within the determined radius for identified clusters. They are tightly
related to the X-ray luminosity and temperature of the clusters. Cluster
mass is related to the richness and summed luminosity with M_200 ~
R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition,
790 new candidate X-ray clusters are found by cross-identification of
these clusters with the source list of the ROSAT X-ray All-Sky Survey.
SDSSXMMQSO Catalog
This table contains the 5th Data Release Sloan Digital Sky Survey (DR5
SDSS)/XMM-Newton Quasar Survey Catalog. This catalog contains 792 SDSS DR5
quasars with optical spectra that have been observed serendipitously in the
X-rays with XMM-Newton. These quasars cover a redshift range of z = 0.11 -
5.41 and a magnitude range of i = 15.3 - 20.7. Substantial numbers of
radio-loud (70) and broad absorption line (51) quasars exist within this
sample. Significant X-ray detections at >=2 sigma account for 87% of the
sample (685 quasars), and 473 quasars are detected at >=6 sigma, sufficient
to allow X-ray spectral fits. For detected sources, ~60% have X-ray fluxes
between F(2-10 keV) = (1-10) x 10-14 erg cm-2 s-1. The authors fit a
single power law, a fixed power law with intrinsic absorption left free to
vary, and an absorbed power-law model to all quasars with X-ray
signal-to-noise ratio >= 6, resulting in a weighted mean photon index Gamma =
1.91 +/- 0.08, with an intrinsic dispersion sigma(Gamma) = 0.38. For the 55
sources (11.6%) that prefer intrinsic absorption, the authors find a weighted
mean NH = 1.5 +/- 0.3 x 1021 cm-2. They find that Gamma correlates
significantly with optical color, Delta(g-i), the optical-to-X-ray spectral
index (alphaox), and the X-ray luminosity. While the first two correlations
can be explained as artifacts of undetected intrinsic absorption, the
correlation between Gamma and X-ray luminosity appears to be a real physical
correlation, indicating a pivot in the X-ray slope.
SHK Catalog
This catalog is a compilation of ten lists of compact groups of compact
galaxies found on the Palomar Sky Survey red charts and published in the
period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog
contains 377 groups of compact galaxies and includes identifications,
equatorial coordinates, numbers of constituent galaxies, magnitudes of the
brightest member, sizes of the groups as a whole, and coefficients of
relative compactness. The HEASARC has a related database table, SHKGALAXY,
which contains data on the individual galaxies in the Shakhbazian Compact
Groups.
SHKGALAXY Catalog
The largest survey of compact galaxy groups was published by Shakhbazian et
al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database
table). This present catalog provides accurate positions of the individual
galaxies in the groups; photometric properties of the Southern sky (delta not
greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST
catalog of the Southern sky.
This catalog contains 373 groups; this number differs from the number in
Shakhbazian's list (377 groups) by the following: (i) there are no data for
groups 001 (already published by other authors), 206 and 241 (could not be
re-identified), 252 (this is identical with 214), 301 and 353 (could not be
re-identified); (ii) Group 328 was published twice (in North and South); and
(iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni
and Fasano ([BF95]=1995AJ....109...32B).
This HEASARC version of the catalog contains a total of 3435 individual
galaxies identified as members of the compact groups, 2574 from the northern
part of this survey (taken from the ADS Catalog VII/196 file north.dat),
and 861 from the southern part of this survey (extracted from the 10746
entries in the ADS Catalog VII/196 file south.dat by including only
entries corresponding to bona fide group members).
SIXDFGS Catalog
The final redshift release of the 6dF Galaxy Survey (6dFGS) is a
combined redshift and peculiar velocity survey over the southern
sky (|b| > 10 degrees). Its 136,304 spectra have yielded 110,256 new
extragalactic redshifts and a new catalogue of 125,071 galaxies
making near-complete samples with limits in (K, H, J, rF, bJ)
(12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the
survey is 0.053.
The catalog includes basic data for the galaxies in the 6dFGS with
redshifts, using the best 6dFGS redshifts (radial velocity quality flag
Q =3 or 4) plus available
redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all).
It supersedes the previous DR2 version (CDS Cat. VII/249).
The home page of of the 6dFGS database is http://www-wfau.roe.ac.uk/6dFGS.
Any use of these data should explicitly state that they come from the Final
Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS,
399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004,
MNRAS, 355, 747).
SPTSZGALCL Catalog
This table contains a catalog of galaxy clusters selected via their
Sunyaev-Zel'dovich (SZ) effect signature from 2500 deg2 of South Pole
Telescope (SPT) data. This work represents the complete sample of clusters
detected at high significance in the 2500 deg2 SPT-SZ survey, which was
completed in 2011. A total of 677 (409) cluster candidates are identified
above a signal-to-noise threshold xi of 4.5 (5.0). Ground- and space-based
optical and near-infrared (NIR) imaging confirms overdensities of similarly
colored galaxies in the direction of 516 (or 76%) of the xi > 4.5 candidates
and 387 (or 95%) of the xi > 5 candidates; the measured purity is consistent
with expectations from simulations. Of these confirmed clusters, 415 were
first identified in SPT data, including 251 new discoveries reported in this
work. The authors estimate photometric redshifts for all candidates with
identified optical and/or NIR counterparts; they additionally report
redshifts derived from spectroscopic observations for 141 of these systems.
The mass threshold of the catalog is roughly independent of redshift above z
~ 0.25 leading to a sample of massive clusters that extends to high redshift.
The median mass of the sample is M500c(rhocrit) ~ 3.5x1014 Msun
h70-1, the median redshift is zmed = 0.55, and the highest-redshift
systems are at z > 1.4. The combination of large redshift extent, clean
selection, and high typical mass makes this cluster sample of particular
interest for cosmological analyses and studies of cluster formation and
evolution.
The South Pole Telescope (SPT) is a 10m diameter telescope located at the
National Science Foundation Amundsen-Scott South Pole station in Antarctica.
From 2008 to 2011 the telescope was used to conduct the SPT-SZ survey, a
survey of ~ 2500 deg2 of the southern sky at 95, 150, and 220 GHz. The
survey covers a contiguous region from 20h to 7h in Right Ascension and -65
to -40 degrees in Declination (see, e.g., Figure 1 in Story et al. 2013, ApJ,
779, 86) and was mapped to depths of approximately 40, 18, and 70
microK-arcmin at 95, 150, and 220 GHz, respectively.
The authors use optical and in some cases NIR imaging (Blanco Telescope,
Magellan/Baade, Magellan/Clay, Swope, MPG/ESO, New Technology Telescope,
Spitzer, WISE) to confirm candidates as clusters and to obtain redshifts for
confirmed systems (see section 4 of the reference paper for more details).
They have also used a variety of facilities to obtain spectroscopic
observations of the SPT clusters (including VLT/FORS2 & Gemini/GMOS-S).
This HEASARC table contains the total of 677 cluster candidates which were
identified above a signal-to-noise threshold of xi = 4.5 in the 2500 deg2
SPT-SZ survey.
SWSDSSQSO Catalog
The authors have compiled a catalog of optically selected quasars with
simultaneous observations in UV/optical and X-ray bands by the Swift
Gamma-ray Burst Explorer. Objects in this catalog are identified by matching
the Swift pointings with the Sloan Digital Sky Survey (SDSS) Data Release 5
(DR5) quasar catalog. The final catalog contains 843 objects, among which 637
have both Ultraviolet Optical Telescope (UVOT) and X-Ray Telescope (XRT)
observations and 354 of which are detected by both instruments. The overall
X-ray detection rate is ~ 60% which rises to ~ 85% among sources with at
least 10 ks of XRT exposure time. The authors construct the time-averaged
spectral energy distribution (SED) for each of the 354 quasars using UVOT
photometric measurements and XRT spectra. From model fits to these SEDs, they
find that the big blue bump contributes about ~ 0.3 dex to the quasar
luminosity. The authors re-visit the alphaox - L2500A relation by
selecting a clean sample with only Type 1 radio-quiet quasars; the dispersion
of this relation is reduced by at least 15% compared with studies that use
non-simultaneous UV/optical and X-ray data. They find only a weak correlation
between Lbol/LEdd and alphaUV. They do not find significant
correlations between alphax and alphaox, alphaox and alphaUV, and
alphax and log L(0.3-10 keV). The correlations between alphaUV and
alphax, alphaox and alphax, alphaox and alphaUV, Lbol/LEdd and
alphax, and Lbol/LEdd and alphaox are stronger among low-redshift
quasars, indicating that these correlations are likely driven by the changes
of SED shape with accretion state.
This quasar sample was compiled in the following steps:
1. Candidate objects for the catalog were selected as any SDSS DR5 quasar
that lie within 20 arcminutes of the center of the Swift FOV in any pointing
from launch through 2008 June.
2. XRT data were processed to obtain X-ray count rates, spectra, and spectral
parameters.
3. UVOT data were processed to obtain UV and optical photometry.
4. UVOT photometry were supplemented with measurements at other wavelengths
from published catalogs.
5. Quasar SEDs were constructed.
6. Additional parameters were calculated based on the SEDs of each quasar.
The raw sample is constructed by matching 3.5 years Swift pointings and the
SDSS DR5 quasar catalog and contains 1034 objects.
This HEASARC version of this catalog contains all 1034 objects in the "raw"
catalog. To select only the 843 objects in the "final" catalog, the user
should specify catalog_flag = 1 in any searches of this table.
SWXCSCAT Catalog
This table contains the Swift X-ray Cluster Survey (SWXCS) catalog obtained
using archival data from the X-ray telescope (XRT) on board the Swift
satellite acquired from 2005 February to 2012 November, extending the first
release of the SWXCS. The catalog provides positions and soft X-ray fluxes
for a flux-limited sample of X-ray group and cluster candidates. In Table 3
of the reference paper (available at the HEASARC as the linked table
SWXCSOXID), when possible, optical counterparts are given for these
candidates. The authors consider the fields with Galactic latitude |b| > 20
degrees so as to avoid regions of high H I column density. They discard all
of the observations targeted at groups or clusters of galaxies, as well as
particular extragalactic fields not suitable for searching for faint extended
sources. The authors finally select ~ 3000 useful fields covering a total
solid angle of ~ 400 deg2. They identify extended source candidates in the
soft-band (0.5-2 keV) images of these fields using the software EXSdetect,
which is specifically calibrated for the XRT data. Extensive simulations are
used to evaluate contamination and completeness as a function of the source
signal, allowing the authors to minimize the number of spurious detections
and to robustly assess the selection function. The final catalog includes 263
candidate galaxy clusters and groups down to a flux limit of 7 x 10-15
erg/cm2/s in the soft band (0.5 - 2.0 keV), and the log N - log S is in
very good agreement with previous deep X-ray surveys. In the reference paper,
the final list of sources is cross-correlated with published optical, X-ray,
and Sunyaev-Zel'dovich catalogs of clusters. The authors find that 137
sources have been previously identified as clusters in the literature in
independent surveys, while 126 are new detections. Currently, they have
collected redshift information for 158 sources (60% of the entire sample).
From the entire Swift XRT archive in the period 2005 February-2012 November,
the authors have selected all the fields that can be used to build an
unbiased, serendipitous X-ray cluster catalog.
SWXCSOXID Catalog
This table contains the Swift X-ray Cluster Survey (SWXCS) table of
cross-correlations of the X-ray galaxy cluster and group candidates with
optical, X-ray and Sunyaev-Zel'dovich catalogs and optical follow-up. The
SWXCS list of cluster candidates was obtained using archival data from the
X-ray telescope (XRT) on board the Swift satellite acquired from 2005
February to 2012 November, extending the first release of the SWXCS. The main
catalog (available at the HEASARC as the linked table SWXCSCAT) provides
positions and soft X-ray fluxes for a flux-limited sample of X-ray group and
cluster candidates. The table herein (based on Table 3 of the reference
paper) contains when possible, optical and other counterparts for these
candidates. The authors consider the fields with Galactic latitude |b| > 20
degrees so as to avoid regions of high H I column density. They discard all
of the observations targeted at groups or clusters of galaxies, as well as
particular extragalactic fields not suitable for searching for faint extended
sources. The authors finally select ~ 3000 useful fields covering a total
solid angle of ~ 400 deg2. They identify extended source candidates in the
soft-band (0.5-2 keV) images of these fields using the software EXSdetect,
which is specifically calibrated for the XRT data. Extensive simulations are
used to evaluate contamination and completeness as a function of the source
signal, allowing the authors to minimize the number of spurious detections
and to robustly assess the selection function. The final catalog includes 263
candidate galaxy clusters and groups down to a flux limit of 7 x 10-15
erg/cm2/s in the soft band (0.5 - 2.0 keV), and the log N - log S is in
very good agreement with previous deep X-ray surveys. In the reference paper,
the final list of sources is cross-correlated with published optical, X-ray,
and Sunyaev-Zel'dovich catalogs of clusters. The authors find that 137
sources have been previously identified as clusters in the literature in
independent surveys, while 126 are new detections. Currently, they have
collected redshift information for 158 sources (60% of the entire sample).
The authors checked for counterparts in previous X-ray cluster surveys, in
optical cluster surveys, and in the Planck SZ cluster survey. They simply
assume a search radius of 2 arcminutes from the X-ray centroid, which has
been shown to be an efficient criterion in Paper I. Nevertheless, they also
inspected the area within 5 arcminutes from the X-ray centroid in order to
investigate whether some possible identification is found at radii larger
than 2 arcminutes. Counterparts at distances between 2 and 5 arcminutes are
included when the optical or SZ corresponding source has a large uncertainty
in its position. This is often the case for optical, sparse clusters, or for
SZ cluster candidates. The authors list all of the counterparts associated
with the SWXCS sources herein, and they include the measured redshift when
available. In case of multiple counterparts, they list all of them. Except
for a few cases where there are multiple counterparts with statistically
inconsistent redshifts, the authors keep the counterpart with the smallest
angular distance from the X-ray center.
From optical surveys, the authors found 233 optical counterparts
corresponding to 116 SWXCS sources. From X-ray surveys, they found 70 X-ray
counterparts classified as clusters, corresponding to 36 SWXCS sources.
Finally, for 15 SWXCS sources, they found 16 cluster counterparts detected
via the SZ effect, 13 by Planck and 3 by the South Pole Telescope (SPT). The
Planck sources are typically at larger distances from the X-ray centroid
(between 1 and 3 arcminutes) because of the much larger position errors of
Planck clusters. Overall, about half (137) of the 263 SWXCS sources were
previously identified as groups or clusters of galaxies, while 126 SWXCS
sources are new cluster and group candidates. The authors have collected
spectroscopic or photometric redshifts for 130 of their sources. Moreover, to
increase the number of available redshifts, they also searched in NED
catalogs for single galaxies with published redshifts not associated with
previously known clusters within a search radius of 7 arcseconds from the
X-ray centroid of their sources. They find 50 galaxies with measured
redshifts for 47 of their sources as a complement to the redshifts obtained
from cluster counterparts. In 35 cases where the authors have both cluster
and galaxy counterparts, the galaxy redshifts are consistent with those of
clusters. In the 12 cases where no cluster counterpart is found, the authors
tentatively assign the galaxy redshift to their X-ray source.
TARTARUS Catalog
The Tartarus database contains the results of a detailed but systematic
analysis of ASCA observations of active galactic nuclei (AGN). It contains
source and background events files, spectra, ancillary response files and
response matrices, images, and assorted light curves for a large number of
ASCA AGN observations. Spectral fit results are done by automatic XSPEC
fitting. This database table allows easy access to reduced AGN data for the
whole community, allowing the maximum scientific return from the data.
Availability of publishable light curves, images, and spectra (which can also
be readily re-fitted) should be particularly valuable to astronomers with
little direct experience in the reduction of X-ray data.
Version 3.1 has been created by analyzing all ASCA observing sequences with
targets designated as AGN, as indicated by a leading "7" in the ASCA
observing sequence number. Version 3.1 contains products for all 611
observing sequences designated as AGN observations. This is a significant
improvement over Versions 1 and 2. Moreover, the 611 sequences for which
products are available are complete in the sense that either the target
object was not detected (in which case an upper limit on GIS2 source counts
is given) or the intended AGN target was detected and the data were fully
analyzed. In order to obtain the most accurate background subtraction and
minimize contamination from any nearby sources, version 3.1 makes more use of
custom extraction regions than previous versions. It is expected that version
3.1 will be replaced when the final ASCA calibration is completed.
TWODFQSOZ Catalog
The final catalog of the 2dF QSO Redshift Survey (2QZ) is based on
Anglo-Australian Telescope 2dF spectroscopic observations of 44,576
color-selected (u, bJ, r) objects with 18.25 < bJ < 20.85 selected from
automated plate measurement scans of UK Schmidt Telescope (UKST)
photographic plates. The 2QZ comprises 23,338 quasi-stellar objects
(QSOs), 12,292 galactic stars (including 2,071 white dwarfs) and 4,558
compact narrow emission-line galaxies. The authors obtained a reliable
spectroscopic identification for 86 per cent of objects observed with
2dF. They also report on the 6dF QSO Redshift Survey (6QZ), based on
UKST 6dF observations of 1,564 brighter (16 < bJ < 18.25) sources selected
from the same photographic input catalog. In total, the authors identified
322 QSOs spectroscopically in the 6QZ. The completed 2QZ is, by more
than a factor of 50, the largest homogeneous QSO catalog ever
constructed at these faint limits (bJ < 20.85) and high QSO surface
densities (35 QSOs/deg2). As such, it represents an important
resource in the study of the Universe at moderate-to-high redshifts.
The survey area comprised 30 UKST fields, arranged in two 75 degrees by 5
degrees declination strips, one passing across the South Galactic Gap
centered on Dec = -30 degrees (the SGP strip), and the other
across the North Galactic Gap centered on Dec = 0 degrees (referred
to in the reference paper as the equatorial strip, but also known as
the NGP strip. The total survey area is 721.6 deg2, when allowance is
made for regions of sky excised around bright stars.
Spectroscopic observations of the input catalogue were made with the
2dF instrument at the Anglo-Australian Telescope (AAT; the 2QZ sample)
and the 6dF instrument at the UKST (the 6QZ sample). 2dF spectroscopic
observations began in January 1997 and were completed in April 2002.
Six-degree Field observations were performed over the period 2001
March-2002 September.
TWOMASSRSC Catalog
This table is based on the results of the 2MASS Redshift Survey
(2MRS), a ten-year project to map the full three-dimensional distribution of
galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was
completed in 2003 and its final data products, including an extended source
catalog (XSC), are available online. The 2MASS XSC contains nearly a million
galaxies with Ks <= 13.5 mag and is essentially complete and mostly
unaffected by interstellar extinction and stellar confusion down to a galactic
latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are
sensitive to the old stellar populations that dominate galaxy masses, making
2MASS an excellent starting point to study the distribution of matter in the
nearby universe. The authors selected a sample of 44,599 2MASS galaxies with
Ks <= 11.75 mag and |b| >= 5 degrees (>= 8 degrees toward the Galactic bulge)
as the input catalog for their survey. They obtained spectroscopic observations
for 11,000 galaxies and used previously obtained velocities for the remainder
of the sample to generate a redshift catalog that is 97.6% complete to
well-defined limits and covers 91% of the sky. This provides an unprecedented
census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier
versions of their survey have been used in a number of publications that have
studied the bulk motion of the Local Group, mapped the density and peculiar
velocity fields out to 50 h-1 Mpc, detected galaxy groups, and estimated the
values of several cosmological parameters. Additionally, the authors present
morphological types for a nearly complete sub-sample of 20,860 galaxies with
Ks <= 11.25 mag and |b| >= 10 degrees.
The authors initially selected 45,086 sources which met the following criteria:
Ks <= 11.75 mag and detected at H,
E(B - V) <= 1 mag,
|b| >= 5 degrees for 30 degrees < l < 330 degrees,
|b| >= 8 degrees otherwise.
They rejected 324 sources of galactic origin (multiple stars, planetary
nebulae, and H II regions) or pieces of galaxies detected as separate sources
by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with
compromised photometry for reprocessing at a future date. Some of these
galaxies have bright stars very close to their nuclei which were not detected
by the pipeline. Others are in regions of high stellar density and their
center positions and/or isophotal radii have been incorrectly measured by the
pipeline. Lastly, some are close pairs or multiples but the pipeline only
identified a single object. A detailed explanation of the steps taken to
reject and reprocess the flagged galaxies is given in the Appendix of the
reference paper.
In summary, the final input catalog contained here has 44,599 entries (plotted
using black symbols in Figure 1 of the reference paper). In this table,
redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are
presented.
UGC Catalog
The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete
catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a
limiting apparent magnitude of 14.5 on the blue prints of the Palomar
Observatory Sky Survey (POSS). Coverage is limited to the sky north of
declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter
but brighter than 14.5 mag may be included from the Catalogue of Galaxies and
of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in
the CGCG are included in the UGC. The galaxies are numbered in order of their
1950.0 right ascension values.
The catalog contains descriptions of the galaxies and their surrounding
areas, plus conventional system classifications and position angles for
flattened galaxies. Galaxy diameters on both the blue and red POSS prints
are included and the classifications and descriptions are given in such a way
as to provide as accurate an account as possible of the appearance of the
galaxies on the prints. Only the data portion of the published UGC is
included in the machine-readable version, notice. For additional details
regarding the classifications, measurement of apparent magnitudes, and data
content, the source reference should be consulted.
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.
UVQS Catalog
This table contains data from the first data release (DR1) from the UV-bright
Quasar Survey (UVQS) for new z ~ 1 active galactic nuclei (AGN) across the
sky. Using simple GALEX UV and WISE near-IR color selection criteria, the
authors generated a list of 1,450 primary candidates with FUV < 18.5 mag,
that is contained in the HEASARC table (entries with source_sample = 'P').
They obtained discovery spectra, primarily on 3m-class telescopes, for 1,040
of these candidates and confirmed 86% as AGN, with redshifts generally at z >
0.5. Including a small set of observed secondary candidates, the authors
report the discovery of 217 AGN with GALEX FUV magnitudes < 18 mag that
previously had no reported spectroscopic redshifts. These are excellent
potential targets for UV spectroscopy before the end of the Hubble Space
Telescope mission. The main data products of UVQS are publicly available
through the Mikulski Archive for Space Telescopes (MAST).
The authors have performed an all-sky survey for z ~ 1, FUV-bright quasars
selected from GALEX and WISE photometry. In several of the observing runs,
conditions were unexpectedly favorable and we exhausted the primary
candidates at certain right ascension ranges. To fill the remaining observing
time, they generated a secondary candidate list. This secondary set of 2,010
candidates is also contained in this HEASARC table (entries with
source_sample = 'S').
The authors proceeded to obtain discovery-quality long-slit spectra (i.e.,
low-dispersion, large-wavelength coverage, modest signal-to-noise ratio (S/N)
of their UV-bright Quasar Survey (UVQS) candidates in one calendar year. The
principal facilities were: (i) the dual Kast spectrometer on the 3m Shane
telescope at the Lick Observatory; (ii) the Boller & Chivens (BCS)
spectrometer on the Irenee du Pont 100-inch telescope at the Las Campanas
Observatory; and (iii) the Calar Alto Faint Object Spectrograph on the CAHA
2.2-meter telescope at the Calar Alto Observatory (CAHA). They acquired an
additional ~20 spectra on larger aperture telescopes (Keck/ESI, MMT/MBC,
Magellan/MagE) during twilight or under poor observing conditions. Typical
exposure times were limited to < ~200s, with adjustments for fainter sources
or sub-optimal observing conditions. Table 3 in the reference paper provides
a list of the details of the observations of these candidates. From the total
candidates list of 3,460 objects, the authors measured high-quality redshifts
(redshift quality flag values of 3 or greater) for 1,121 sources. They
assumed that every source with a recessional velocity vr = z * c < 500 km
s-1 was "Galactic", which they associate with the Galaxy and members of the
Local Group. This included sources where the eigenspectra fits were poor yet
a low vr was indisputable (e.g., stars). Many of these were assigned z = 0
exactly. The remainder of the UVQS sources were assumed to be extragalactic
AGN, and the derived redshift information for these sources (which was given
in Table 4 of the reference paper) has been incorporated into this HEASARC
representation of UVQS. Finally, there were 93 sources with good-quality
spectra for which we cannot the authors could not recover a secure redshift.
The majority of these have been previously cataloged as blazars (or BL Lac
objects). Table 6 in the reference paper lists the sample of these unknown or
insecure redshift objects.
UZC Catalog
The Zwicky Catalog of Galaxies, with a magnitude limit mZw <= 15.5, has
been the basis for the Center for Astrophysics (CfA) redshift surveys. To
date, analyses of the Zwicky Catalog and redshift surveys based on it have
relied on heterogeneous sets of galaxy coordinates and redshifts. In this
Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs
are corrected by providing (1) coordinates with ~<2 arcsecond errors for all
of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz
(radial velocities) for the majority (98%) of the data taken at the CfA
(14,632 spectra), and (3) an estimate of the remaining "blunder" rate for
both the CfA redshifts and for those compiled from the literature. For the
reanalyzed CfA data a calibrated, uniformly determined error and an
indication of the presence of emission lines in each spectrum are included.
Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2
redshift survey that were not previously published; for another 5625 CfA
redshifts (radial velocities), the remeasured or uniformly rereduced values
are listed. Among the new measurements, 1807 are members of UZC "multiplets"
associated with the original Zwicky catalog position in the coordinate range
where the catalog is 98% complete. These multiplets provide new candidates
for examination of tidal interaction among galaxies. All of the new redshifts
(radial velocities) correspond to UZC galaxies with properties recorded in
the CfA redshift compilation known as ZCAT. The redshift catalog included in
the UZC is ~96% complete to mZw <= 15.5 and ~98% complete (12,925 galaxies
out of a total of 13,150) for the right ascension ranges 20 hr >= RA(1950) <=
4 hr and 8 hr <= RA(1950) <= 17 hr and the declination range -2.5 degrees <=
Dec(1950) <= 50 degrees. This more complete region includes all of the CfA2
survey as analyzed to the date of the publication of the UZC (1999).
VERONCAT Catalog
This database table contains the 13th edition of the Catalog of Quasars and
Active Galactic Nuclei by Veron-Cetty and Veron, and is an update of the
previous versions. As in the previous editions, no information about absorption
lines or X-ray properties is given, but absolute magnitides are provided,
assuming a Hubble constant H0 = 71 km/s/Mpc and a deceleration parameter
q0 = 0 (notice the change of cosmology from previous editions in which H0
was assumed to be 50 km/s/Mpc).
The present edition of this catalog contains 133336 quasars, 1374 BL Lac
objects and 34231 active galaxies (including 15627 Seyfert 1 galaxies),
for a grand total of 168941 objects, significantly more than the number of
objects listed in the 12th edition (108080).
The 13th edition includes positions and redshifts, as well as photometry (U,
B, and V) and 6-cm and 20-cm flux densities, when available. 178 objects
once proposed but now rejected as quasars are NOT included in the online
version of this catalog: their names and positions are listed in the file
https://cdsarc.cds.unistra.fr/ftp/cats/VII/258/reject.dat. This HEASARC table
also does NOT contain the additional information on gravitationally
lensed quasars and quasar pairs listed in Tables 3 and 4 of the published
paper: these tables are available in electronic form at the CDS
https://cdsarc.cds.unistra.fr/ftp/cats/VII/248/ files table2.dat and table3.dat
(sic).
The present edition of this catalog contains quasars with measured redshift
known prior to July 1st, 2009.
W2RAGNCAT Catalog
The authors of this catalog have developed the SIX statistic to identify
bright, highly likely active galactic nucleus (AGN) candidates solely on the
basis of Wide-field Infrared Survey Explorer (WISE), Two-Micron All-Sky
Survey (2MASS), and ROSAT All-Sky Survey (RASS) data. This statistic was
optimized with data from the preliminary WISE survey and the Sloan Digital
Sky Survey, and tested with Lick 3 m Kast spectroscopy. The authors find that
sources with SIX < 0 have a >~ 95% likelihood of being an AGN (defined in
this paper as a Seyfert 1, quasar, or blazar). This statistic was then
applied to the full WISE/2MASS/RASS dataset, including the final WISE data
release, to yield the "W2R" sample of 4316 sources with SIX < 0. Only 2209
of these sources are currently in the Veron-Cetty and Veron (VCV) Catalog of
spectroscopically confirmed AGNs, indicating that the W2R sample contains
nearly 2000 new, relatively bright (J <~ 16) AGNs. The authors utilize the
W2R sample to quantify biases and incompleteness in the VCV Catalog. They
find that it is highly complete for bright (J < 14), northern AGNs, but the
completeness drops below 50% for fainter, southern samples and for sources
near the Galactic plane. This approach also led to the spectroscopic
identification of 10 new AGNs in the Kepler field, more than doubling the
number of AGNs being monitored by Kepler. The W2R sample contains better than
1 bright AGN every 10 deg2, permitting construction of AGN samples in any
sufficiently large region of sky. This table contains the 4316 sources
comprising the W2R sample.
WARPS Catalog
The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog
which contains optical identifications for objects found in a serendipitous
survey of relatively deep, pointed ROSAT observations for clusters of
galaxies. The X-ray source detection algorithm used by WARPS is Voronoi
Tessellation and Percolation (VTP), a technique which is equally sensitive to
point sources and to extended sources of low surface brightness. WARPS-I is
based on the central regions of 86 ROSAT PSPC fields, covering an area of
16.2 square degrees. The X-ray source screening and optical identification
process for WARPS-I yielded 34 clusters at 0.06<z<0.75. Twenty-two of these
clusters form a complete, statistically well-defined sample drawn from 75 of
these 86 fields, covering an area of 14.1 square degrees, with a flux limit
of F(0.5-2.0keV) = 6.5x10-14 erg/cm2/s. This sample can be used to study
the properties and evolution of the gas, galaxy and dark matter content of
clusters and to constrain cosmological parameters.
WARPS2 Catalog
This table contains the galaxy cluster catalog from the second, larger phase
of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for
high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster
surveys and is being used to study the properties and evolution of galaxy
clusters. The WARPS-II sample contains 125 clusters serendipitously detected
in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of
56.7 deg2. Of these 125 clusters, 53 have not been previously reported in
the literature. The authors have nearly complete spectroscopic follow-up of
the clusters, which range in redshift from z = 0.029 to z = 0.92 with a
median redshift of z = 0.29 and they find 59 clusters with z >= 0.3 (29 not
previously reported in the literature) and 11 clusters with z >= 0.6 (6 not
previously reported). They also define a statistically complete subsample of
102 clusters above a uniform flux limit of 6.5 x 10-14 ergs/cm2/s (0.5 -
2.0 keV). In their paper, the authors also compare their redshifts, fluxes,
and detection methods to other similar published cluster surveys and state
that they find no serious issues with their measurements or completeness.
The list of ROSAT pointings used in WARPS-II is given in Table 1 of the
first reference paper. The WARPS-I cluster catalog (the second reference
listed below) is also available in Browse as the WARPS table.
WBL Catalog
The Catalog of Nearby Poor Clusters of Galaxies of White et al.
(1999), also known as the WBL Catalog, is a catalog of 732 optically selected,
nearby poor clusters of galaxies covering the entire sky north of -3 degrees
declination. The poor clusters, called WBL clusters, were identified as
concentrations of three or more galaxies with photographic magnitudes brighter
than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These
criteria are consistent with those used in the identification of the
original Yerkes poor clusters, and this new catalog substantially
increases the sample size of such objects. These poor clusters cover
the entire range of galaxy associations up to and including Abell
clusters, systematically including poor and rich galaxy systems
spanning over 3 orders of magnitude in the cluster mass function. As a
result, this new catalog contains a greater diversity of richness and
structures than other group catalogs, such as the Hickson and Yerkes
catalogs. This table contains the entries for the clusters (given in Table 2
of the published catalog) and includes redshift data (where available) and
cross-references to other group and cluster catalogs. The WBLGALAXY table
(q.v.) contains the entries for the individual galaxies in the clusters
which ere given in Table 3 of the published catalog.
WBLGALAXY Catalog
The Catalog of Nearby Poor Clusters of Galaxies of White et al.
(1999), also known as the WBL Catalog, is a catalog of 732 optically selected,
nearby poor clusters of galaxies covering the entire sky north of -3 degrees
declination. The poor clusters, called WBL clusters, were identified as
concentrations of three or more galaxies with photographic magnitudes brighter
than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These
criteria are consistent with those used in the identification of the
original Yerkes poor clusters, and this new catalog substantially
increases the sample size of such objects. These poor clusters cover
the entire range of galaxy associations up to and including Abell
clusters, systematically including poor and rich galaxy systems
spanning over 3 orders of magnitude in the cluster mass function. As a
result, this new catalog contains a greater diversity of richness and
structures than other group catalogs, such as the Hickson and Yerkes
catalogs. This table contains the entries for the individual galaxies in the
poor clusters which ere given in Table 3 of the published catalog, and
includes redshifts for the individual galaxies and cross-references to other
galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters
themselves (given in Table 2 of the published catalog).
WISEHSPCAT Catalog
High Synchrotron Peaked blazars (HSPs) dominate the gamma-ray sky at energies
larger than a few GeV, however only a few hundred blazars of this type have
been catalogued so far. In this paper, the authors present the 2WHSP sample,
the largest and most complete list of HSP blazars available to date, which is
an expansion of the 1WHSP catalog (Arsioli et al. 2015, A&A, 579, A34) of
gamma-ray source candidates away from the Galactic Plane. They cross-matched
a number of multi-wavelength surveys (in the radio, infrared and X-ray bands)
and applied selection criteria based on the radio to IR, and IR to X-ray
spectral slopes. To ensure the selection of genuine HSPs, the authors
examined the spectral energy distribution (SED) of each candidate and
estimated the peak frequency of its synchrotron emission (nupeak) using the
Agenzia Spaziale Italiana Science Data Center (ASDC) SED tool, including only
sources with nupeak > 1015 Hz (equivalent to nupeak > 4 eV).
The authors have assembled the largest and most complete catalog of HSP
blazars to date, which includes 1691 sources. A number of population
properties, such as infrared colors, synchrotron peak, redshift
distributions, and gamma-ray spectral properties, have been used to
characterize the sample and maximize completeness. The authors also derived
the radio log N - log S distribution. This catalog has already been used to
provide seeds to discover new very high energy objects within Fermi-LAT data
and to look for the counterparts of neutrino and ultra-high energy cosmic ray
sources, showing its potential for the identification of promising
high-energy gamma-ray sources and multi-messenger targets.
This table comprises the 2WHSP catalog, a multi-frequency catalog of HSP. It
contains 1691 sources, 288 of which are newly identified HSPs, 540 are
previously known HSPs, 814 are HSP candidates, 45 are HSP blazars taken from
the 2FHL catalog, and 4 from TeVCat (http://tevcat.uchicago.edu).
XMMCTY2AGN Catalog
This table contains the results from a study of the multi-wavelength (from
the mid-infrared to the hard X-ray) properties of a sample of 255
spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS
survey. Most of them are obscured and the X-ray absorbing column density is
determined by either X-ray spectral analyses (for 45% of the sample), or from
hardness ratios. Spectral energy distributions (SEDs) were computed for all
sources in the sample. The average SEDs in the optical band are dominated by
the host-galaxy light, especially at low X-ray luminosities and redshifts.
There is also a trend between X-ray and mid-infrared luminosity: the AGN
contribution in the infrared is higher at higher X-ray luminosities. The
authors have calculated bolometric luminosities, bolometric corrections,
stellar masses and star formation rates (SFRs) for these sources using
multi-component modeling to properly disentangle the emission associated with
stellar light from that due to black hole accretion. For 90% of the sample,
they also have the morphological classifications obtained with an upgraded
version of the Zurich estimator of structural types (ZEST+). The authors find
that, on average, type-2 AGN have lower bolometric corrections than type-1
AGN. Moreover, they confirm that the morphologies of AGN host-galaxies
indicate that there is a preference for these type-2 AGN to be hosted in
bulge-dominated galaxies with stellar masses greater than 1010 solar masses.
For each source, this table contains the X-ray ID, spectroscopic redshift,
logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity,
bolometric correction, logarithm of the stellar mass, star formation rate,
absolute magnitude MU, absolute magnitude MV, absolute magnitude MJ
(Johnson-Kron-Cousin system), and the morphological class.
XRAYSELBLL Catalog
This table contains a catalog of 312 X-ray selected BL Lacertae objects
(XBLs), optically identified through the end of 2011. It contains the names
from different surveys, equatorial coordinates, redshifts, multi-frequency
flux values, and luminosities for each source. In the reference, the
different characteristics of these XBLs are statistically investigated
(redshift, radio/optical/X-ray luminosities, central black hole (BH) mass,
synchrotron peak frequency, broadband spectral indices, optical flux
variability). Their values were collected through an extensive bibliographic
and database search or calculated by the author. The redshifts range from
0.031 to 0.702 with a maximum of the distribution at z = 0.223. The 1.4-GHz
luminosities of XBLs log (nu * Lnu) ~ 39 - 42 (in units of erg s-1),
while the optical V and X-ray (0.1-2.4 keV) bands show log (nu * Lnu) ~ 43
- 46 (same units). The XBL hosts are elliptical galaxies with effective radii
reff = 3.26 - 25.40 kpc and ellipticities e = 0.04 - 0.52. Their R-band
absolute magnitudes MR range from -21.11 mag to -24.86 mag with a mean
value of -22.83 mag. The V - R indices of the hosts range from 0.61 to 1.52
and reveal a fourth-degree polynomial relationship with z that enabled the
author to evaluate the redshifts of five sources whose V - R indices were
determined from the observations, but whose redshifts values are either not
found or not confirmed. The XBL nuclei show a wider range of 7.31 mag for
MR, with the highest luminosity corresponding to MR = -27.24 mag. The
masses of the central BHs are found in the interval log MBH = 7.39 - 9.30
(in units of solar masses), with the maximum of the distribution at log
MBH/Msun = 8.30. The synchrotron peak frequencies are spread over the
range log nupeak = 14.56 - 19.18 Hz, with a peak of the distribution at log
nupeak = 16.60 Hz. The broad-band radio-to-optical (alpharo),
optical-to-X-ray (alphaox), and radio-to-X-ray (alpharx) spectral indices
are distributed in the intervals (0.17, 0.59), (0.56, 1.48), and (0.41,
0.75), respectively. In the optical energy range, the overall flux
variability increases, on average, towards shorter wavelengths: Delta(m) =
1.22, 1.50, and 1.82 through the R, V, B bands of the Johnson-Cousins system,
respectively. XBLs seem be optically less variable at intranight timescales
compared to radio-selected BL Lacs (RBLs).
XSHZAGNCXO Catalog
This table contains the results from an analysis of the largest high-redshift
(z > 3) X-ray-selected active galactic nucleus (AGN) sample to date,
combining the Chandra Cosmological Evolution Survey and Chandra
Multi-wavelength Project surveys and doubling the previous samples. The
sample comprises 209 X-ray-detected AGNs, over a wide range of rest-frame
2-10 keV luminosities log LX = 43.3 - 46.0 erg/s. X-ray hardness ratios
show that ~39 per cent of the sources are highly obscured, NH > 1022
cm-2, in agreement with the ~37 per cent of type-2 AGNs found in this
sample based on their optical classification. For ~26 per cent of objects,
there are mismatched optical and X-ray classifications. Utilizing the
1/Vmax method, the authors confirm that the comoving space density of all
luminosity ranges of AGNs decreases with redshift above z > 3 and up to z ~
7. With a significant sample of AGNs (N = 27) at z > 4, it is found that both
source number counts in the 0.5-2 keV band and comoving space density are
consistent with the expectation of a luminosity-dependent density evolution
(LDDE) model at all redshifts, while they exclude the luminosity and density
evolution (LADE) model. The measured comoving space density of type-1 and
type-2 AGNs shows a constant ratio between the two types at z > 3. These
results for both AGN types at these redshifts are consistent with the
expectations of LDDE model.
The high-redshift AGN sample used in this work has been selected from the
C-COSMOS X-ray catalog, combining the spectroscopic and photometric
information available from the identification catalogue of X-ray C-COSMOS
sources (Civano et al. 2011, ApJ, 741, 91; 2012, ApJS, 201, 30) and the ChaMP
(Chandra Multi-wavelength Project) X-ray catalog using only the 323 ChaMP
ObsIDs overlapping with Sloan Digital Sky Survey (SDSS; Richards et al. 2006,
AJ, 131, 2766) DR5 imaging.
ZCAT Catalog
The ZCAT database contains the CfA Redshift Catalog, which incorporates much
of the latest velocity data from the Whipple Observatory and other sources, as
well as velocities from earlier compilations such as the "Second Reference
Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy
Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of
Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes,
some UGC numbers, and increased "accuracy" in the velocity source information.
The data presented here have primarily been assembled for the purpose of
studying the large scale structure of the universe, and, as such, are nearly
complete in redshift information, but are not necessarily complete in such
categories as diameter, magnitude, and cross-references to other catalogues.
ZWCLUSTERS Catalog
The ZWCLUSTERS database is based upon the Catalogue of Zwicky Clusters
of Galaxies. The Zwicky clusters were identified by F. Zwicky in 560
POSS fields. They are rich clusters, each having at least 50 members
within 3 magnitudes of the brightest member.
