ACTEGSRCAT Catalog
This table contains a list of extragalactic radio sources detected in a 455
square-degree map of the southern sky made at a frequency of 148 GHz from the
Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157
sources with flux densities spanning two orders of magnitude from 15 to 1500
mJy. Comparison to other catalogs shows that 98% of the ACT detections
correspond to sources detected at lower radio frequencies. Three of the
sources appear to be associated with the brightest cluster galaxies of low
redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave
spectral indices and differential counts of the sources further bolster the
hypothesis that they are nearly all radio sources, and that their emission
is not dominated by re-emission from warm dust. In a bright (>50 mJy) 148
GHz-selected sample with complete cross-identifications from the Australia
Telescope 20-GHz survey, the authors of the study observe an average steepening
of the spectra between 5, 20, and 148 GHz with median spectral indices of
alpha5-20 = -0.07 +/- 0.06, alpha20-148 = -0.39 +/- 0.04, and
alpha5-148 = -0.20 +/- 0.03. When the measured spectral indices are
taken into account, the 148-GHz differential source counts are consistent with
previous measurements at 30 GHz in the context of a source count model
dominated by flat spectrum radio sources. Extrapolating with an appropriately
rescaled model for the radio source counts, the Poisson contribution to the
spatial power spectrum from synchrotron-dominated sources with flux density
less than 20 mJy is CSync = (2.8 +/- 0.3) x 10-6 microKelvin2.
ACTMADCOWS Catalog
Galaxy clusters are an important tool for cosmology, and their detection and
characterization are key goals for current and future surveys. Using data
from the Wide-field Infrared Survey Explorer (WISE), the Massive and Distant
Clusters of WISE Survey (MaDCoWS) located 2839 significant galaxy
overdensities at redshifts 0.7 <= z <= 1.5, which included extensive follow-up
imaging from the Spitzer Space Telescope to determine cluster richnesses.
Concurrently, the Atacama Cosmology Telescope (ACT) has produced large area
millimeter-wave maps in three frequency bands along with a large catalog of
Sunyaev-Zel'dovich (SZ)-selected clusters as part of its Data Release 5 (DR5).
The authors aimed to verify and characterize MaDCoWS clusters using
measurements of, or limits on, their thermal SZ effect signatures. They also
used these detections to establish the scaling relation between SZ mass and
the MaDCoWS-defined richness.
Using the maps and cluster catalog from DR5, the authors explore the scaling
between SZ mass and cluster richness. They do this by comparing cataloged
detections and extracting individual and stacked SZ signals from the MaDCoWS
cluster locations. The authors use complementary radio survey data from the
Very Large Array, submillimeter data from Herschel, and ACT 224GHz data to
assess the impact of contaminating sources on the SZ signals from both ACT
and MaDCoWS clusters. They use a hierarchical Bayesian model to fit the
mass-richness scaling relation, allowing for clusters to be drawn from two
populations: one, a Gaussian centered on the mass-richness relation, and the
other, a Gaussian centered on zero SZ signal.
This study found that MaDCoWS clusters have submillimeter contamination that
is consistent with a gray-body spectrum, while the ACT clusters are
consistent with no submillimeter emission on average. Additionally, the
intrinsic radio intensities of ACT clusters are lower than those of MaDCoWS
clusters, even when the ACT clusters are restricted to the same redshift
range as the MaDCoWS clusters. The authors found the best-fit ACT SZ mass
versus MaDCoWS richness scaling relation has a slope of p1=1.84-0.14+0.15,
where the slope is defined as M ~lambda15p1 and lambda15 is the
richness. They also found that the ACT SZ signals for a significant fraction
(~57%) of the MaDCoWS sample can statistically be described as being drawn
from a noise-like distribution, indicating that the candidates are possibly
dominated by low-mass and unvirialized systems that are below the mass limit
of the ACT sample. Further, the authors noted that a large portion of the
optically confirmed ACT clusters located in the same volume of the sky as
MaDCoWS were not selected by MaDCoWS, indicating that the MaDCoWS sample is
not complete with respect to SZ selection. Finally, the authors found that
the radio loud fraction of MaDCoWS clusters increases with richness, while
they found no evidence that the submillimeter emission of the MaDCoWS
clusters evolved with richness.
The authors concluded that the original MaDCoWS selection function is not
well defined and, as such, reiterated the MaDCoWS collaboration's
recommendation that the sample is suited for probing cluster and galaxy
evolution, but not cosmological analyses. They found a best-fit mass-richness
relation slope that agrees with the published MaDCoWS preliminary results.
Additionally, they concluded that, while the approximate level of infill of
the ACT and MaDCoWS cluster SZ signals (1-2%) is subdominant to other sources
of uncertainty for current generation experiments, characterizing and
removing this bias will be critical for next-generation experiments hoping to
constrain cluster masses at the sub-percent level.
ACTSOUTH Catalog
The ACTSOUTH catalog is a multi-frequency, multi-epoch catalog of
extragalactic sources, based on 150, 220 and 280 GHz observations carried out
in 2008, 2009 and 2010 using the Millimeter Bolometric Array Camera on the
Atacama Cosmology Telescope. The catalog contains 695 sources, found in a sky
area of ~600 square degrees. It is obtained by cross-matching sources found
in 11 sub-catalogs, one for each season and frequency band. Also include are
co-added data from ~150 and ~160 square degrees using 2 and 3 years of
overlapping observations. The authors divide the sources into two
populations, synchrotron and dusty emitters, based on their spectral behavior
in the 150 - 220 GHz frequency range. They find 374 synchrotron sources and
321 dusty source candidates. Cross-matching with catalogs from radio to X-ray
results in 264 synchrotron sources (71%) and 89 dusty sources (28%) with
counterparts, suggesting that 232 dusty candidates are not in existing
catalogs.
ACTSSRCAT Catalog
This table contains a catalog of 191 extragalactic sources detected by the
Atacama Cosmology Telescope (ACT) at 148 and/or 218 GHz in the 2008 Southern
survey. Flux densities span 14 -1700 mJy, and the authors use source spectral
indices derived using ACT-only data to divide their sources into two
subpopulations: 167 radio galaxies powered by central active galactic nuclei
(AGN) and 24 dusty star-forming galaxies (DSFGs). They cross-identify 97% of
their sources (166 of the AGN and 19 of the DSFGs) with those in currently
available catalogs. When combined with flux densities from the Australia
Telescope 20-GHz survey and follow-up observations with the Australia
Telescope Compact Array, the synchrotron-dominated population is seen to
exhibit a steepening of the slope of the spectral energy distribution from 20
to 148 GHz, with the trend continuing to 218 GHz. The ACT dust-dominated
source population has a median spectral index, alpha148-218GHz, of
3.7+0.62-0.86, and includes both local galaxies and sources with redshift
around 6. Dusty sources with no counterpart in existing catalogs likely
belong to a recently discovered subpopulation of DSFGs lensed by foreground
galaxies or galaxy groups.
The ACT experiment (Swetz et al., 2011, ApJS, 194, 41) is situated on the
slopes of Cerro Toco in the Atacama Desert of Chile at an elevation of 5190m.
ACT's latitude gives access to both the northern and southern celestial
hemispheres. Observations occurred simultaneously in three frequency bands,
at 148 GHz (2.0 mm), 218 GHz (1.4 mm) and 277 GHz (1.1 mm) with angular
resolutions of roughly 1.4, 1.0 and 0.9 arcminutes, respectively.
The ACT-detected source list contains 169 sources selected at 148 GHz with
S/N > 5, spanning two decades in flux density, from 14 to 1700 mJy. The 218
GHz map independently yielded 133 sources with S/N > 5. The combination of
these two independent source lists from which the present table was
constructed gives a total count of 191 sources, with 110 galaxies detected
with S/N > 5 at both frequencies.
ACTSZCLUST Catalog
The catalog of 4195 optically confirmed Sunyaev-Zel'dovich (SZ) selected
galaxy clusters were detected with signal-to-noise > 4 in 13,211 deg2 of
sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates
were selected by applying a multi-frequency matched filter to 98- and 150-GHz
maps constructed from ACT observations obtained from 2008-2018 and confirmed
using deep, wide-area optical surveys. The clusters span the redshift range
0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters,
and a total of 868 systems are new discoveries. Assuming an SZ-signal vs.
mass scaling relation calibrated from X-ray observations, the sample has a
90% completeness mass limit of M500c > 3.8 x 1014Msol, evaluated at
z=0.5, for clusters detected at signal-to-noise ratio > 5 in maps filtered at
an angular scale of 2.40. The survey has a large overlap with deep optical
weak-lensing surveys that are being used to calibrate the SZ-signal
mass-scaling relation, such as the Dark Energy Survey (4566 deg2), the
Hyper Suprime-Cam Subaru Strategic Program (469 deg2), and the Kilo Degree
Survey (825 deg2).
HESSCAT Catalog
H.E.S.S. is a system of Imaging Atmospheric Cherenkov Telescopes for the
investigation of cosmic gamma rays in the 100 GeV energy range. The name
H.E.S.S. stands for High Energy Stereoscopic System, and should also remind
us of Victor Hess, who received in 1936 the Nobel Prize in Physics for his
discovery of cosmic radiation. The instrument allows us to explore gamma-ray
sources with intensities at a level of a few thousandth parts of the flux of
the Crab nebula. H.E.S.S. is located in Namibia, near the Gamsberg, an area
well known for its excellent optical quality. The first of the four
telescopes of Phase I of the H.E.S.S. project went into operation in Summer
2002; all four were operational in December 2003, and were officially
inaugurated on September 28, 2004. In recognition of its scientific results,
H.E.S.S. was awarded the 2006 Descartes Prize for Research of the European
Commission.
IRAM30MLOG Catalog
This table contains the IRAM 30-m single-dish telescope observation log.
The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and
is operated as a French-German-Spanish collaboration. Its partner institutes
are the CNRS (Centre National de la Recherche Scientifique, France), the MPG
(Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico
Nacional, Spain). The principal activity of IRAM is the study of cold matter
(molecular gas and dust) in the solar system, in our Galaxy, and out to
cosmological distances, in order to determine its composition, density, mass,
temperature, and kinematics.
IRAM operates two observatories at millimeter wavelengths which are open to
the international astronomical community: the 30-m single-dish telescope on
Pico Veleta (2850 m), Spain, and the six-antenna interferometer on the Plateau
de Bure (2550 m) in France. Both sites are at high altitude to reduce the
absorption by water vapor. The observatories are supported by the IRAM
offices and laboratories in Granada and Grenoble.
The observation log included here concerns the 30-m single-dish telescope,
and summarizes the observations made there since September 30, 2009.
The observation log for the the six-antenna interferometer on the Plateau de
Bure in France is also available as the HEASARC database table
IRAMPDBLOG, and the observation log
for NOEMA (the NOrthern Extended Millimeter Array), the successor to the
Plateau de Bure observatory, is available as the HEASARC database table
IRAMNOELOG.
For more information on IRAM, see
the IRAM home page.
IRAMNOELOG Catalog
This table contains the IRAM NOEMA (NOrthern Extended Millimeter Array)
observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was
founded in 1979 and is operated as a French-German-Spanish collaboration. Its
partner institutes are the CNRS (Centre National de la Recherche
Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the
IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is
the study of cold matter (molecular gas and dust) in the solar system, in our
Galaxy, and out to cosmological distances, in order to determine its
composition, density, mass, temperature, and kinematics.
IRAM operates two observatories at millimeter wavelengths which are open to
the international astronomical community: the 30-m single-dish telescope on
Pico Veleta (2850 m), Spain, and the six-antenna interferometer on the Plateau
de Bure (2550 m) in France. Both sites are at high altitude to reduce the
absorption by water vapor. The observatories are supported by the IRAM
offices and laboratories in Granada and Grenoble.
The observation log included here concerns NOEMA, the NOrthern Extended
Millimeter Array, and summarizes the observations made there. NOEMA is the
successor to the Plateau de Bure observatory. During its history, the
observatory at the Plateau de Bure underwent several track extensions,
received additional antennas (all of 15-m diameter and of similar
construction to the first ones) and technical upgrades. From a three-antenna
interferometer with a maximum baseline of 288 meters in 1988, it has evolved
to a eight-antenna array with baselines up to 760 meters in 2016. With the
inauguration of the seventh antenna in September, 2014, the observatory
started its transformation into NOEMA. More information about NOEMA is
available at the IRAM web site.
The observation log for the 30-m telescope is available as the HEASARC
database table IRAM30MLOG, and the
observation log for the Plateau de Bure Interferometer is available as the
HEASARC database table IRAMPDBLOG.
For more information on IRAM, see
the IRAM home page.
IRAMPDBLOG Catalog
This table contains the IRAM Plateau de Bure Interferometer observation log.
The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and
is operated as a French-German-Spanish collaboration. Its partner institutes
are the CNRS (Centre National de la Recherche Scientifique, France), the MPG
(Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico
Nacional, Spain). The principal activity of IRAM is the study of cold matter
(molecular gas and dust) in the solar system, in our Galaxy, and out to
cosmological distances, in order to determine its composition, density, mass,
temperature, and kinematics.
IRAM operates two observatories at millimeter wavelengths which are open to
the international astronomical community: the 30-m single-dish telescope on
Pico Veleta (2850 m), Spain, and the six-antenna interferometer on the Plateau
de Bure (2550 m) in France. Both sites are at high altitude to reduce the
absorption by water vapor. The observatories are supported by the IRAM
offices and laboratories in Granada and Grenoble.
The observation log included here concerns the Plateau de Bure Interferometer
(PdBI) and summarizes the observations made there between December 1, 1990,
and March 31, 2017, inclusive. No observations were done by the PdBI during
the periods 1999-Sep-30 to 2000-Dec-03 and 2006-Sep-25 to 2007-Jan-18
(installation of the new receiver), notice.
The observation log for the 30-m telescope is available as the HEASARC
database table IRAM30MLOG, and the
observation log for NOEMA (the NOrthern Extended Millimeter Array), the
successor to the Plateau de Bure observatory, is available as the HEASARC
database table IRAMNOELOG.
For more information on IRAM, see
the IRAM home page.
SCUBAFEMOC Catalog
This table contains the SCUBA Legacy Catalogs, two comprehensive sets of
source catalogs using data at 850 and 450um of the various astronomical
objects obtained with the Submillimetre Common User Bolometer Array (SCUBA)
on the James Clerk Maxwell Telescope (JCMT). The Fundamental Map Data Set
contains data only where superior atmospheric opacity calibration data were
available. The Extended Map Data Set contains data regardless of the quality
of the opacity calibration. Each data set contains 1.2 degrees x 1.2 degrees
maps at locations where data existed in the JCMT archive, imaged using the
matrix inversion method. The Fundamental Data Set is composed of 1423 maps at
850um and 1357 maps at 450um. The Extended Data Set is composed of 1547 maps
at 850um. Neither data set includes high sensitivity, single-chop SCUBA maps
of "cosmological fields" nor solar system objects. Each data set was used to
determine a respective object catalog, consisting of objects identified
within the respective 850um maps using an automated identification algorithm.
The Fundamental and Extended Map Object Catalogs contain 5061 and 6118
objects, respectively. Objects are named based on their respective J2000.0
position of peak 850um intensity. The catalogs provide for each object the
respective maximum 850um intensity, estimates of total 850um flux and size,
and tentative identifications from the SIMBAD Database. Where possible, the
catalogs also provide for each object its maximum 450um intensity and total
450um flux and flux ratios.
Since the goal of this project was to make maps and then catalog objects
therein, all raw jiggle and scan data from SCUBA available in the JCMT
archive were downloaded from the CADC in 2006 May. (Photometry and
polarimetry data were ignored.) A full description of the instrumental
characteristics of SCUBA was made by Holland et al. (1999MNRAS.303..659H).
All maps are available at
http://www3.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/community/scubalegacy/
SPTMM87SD Catalog
This table contains the results of an 87 deg2 point-source survey centered
at RA = 5h30m, Dec = -55o (J2000.0) taken with the South Pole Telescope
at 1.4 and 2.0 mm wavelengths with arcminute resolution and milli-Jansky
(mJy) depth. Based on the ratio of flux in the two bands, the authors
separate the detected sources into two populations, one consistent with
synchrotron emission from active galactic nuclei (AGN) and the other
consistent with thermal emission from dust. In the reference paper, the
authors present source counts for each population from 11 to 640 mJy at 1.4
mm and from 4.4 to 800 mJy at 2.0 mm. The 2.0-mm counts are dominated by
synchrotron-dominated sources across the reported flux range; the 1.4-mm
counts are dominated by synchrotron-dominated sources above ~15 mJy and by
dust-dominated sources below that flux level. The authors detect 141
synchrotron-dominated sources and 47 dust-dominated sources at
signal-to-noise ratio S/N > 4.5 in at least one band. All of the most
significantly detected members of the synchrotron-dominated population are
associated with sources in previously published radio catalogs. Some of the
dust-dominated sources are associated with nearby (z << 1) galaxies whose
dust emission is also detected by the Infrared Astronomy Satellite (IRAS).
However, most of the bright, dust-dominated sources have no counterparts in
any existing catalogs. The authors argue that these sources represent the
rarest and brightest members of the population commonly referred to as
sub-millimeter galaxies (SMGs).
During the 2008 observing season, the 960-element South Pole Telescope (SPT)
camera included detectors sensitive to radiation within bands centered at
approximately 1.4 mm, 2.0 mm, and 3.2 mm (220 GHz, 150 GHz, and 95 GHz).
Result in this reference paper are based on 607 hr of observing time, using
only the 1.4-mm and 2.0-mm data from the 87 deg2 portion of the field that
was mapped with near-uniform coverage. Main-lobe beams were measured using
the brightest sources in the field and were adequately fit by two-dimensional
Gaussians with FWHM equal to 1.05 and 1.15 arcminutes at 1.4 mm and 2.0 mm,
respectively. The typical rms of the filtered 2.0-mm and 1.4-mm maps used for
source candidate identification (shown in Figures 1 and 2, respectively, of
the reference paper) is 1.3 mJy at 2.0 mm and 3.4 mJy at 1.4 mm. Detections
in both bands are listed in the final catalog as a single source if they are
offset <30 arcseconds between the two bands. For sources detected in both
bands, the authors adopt the position of the more significant detection. The
argue that they are far enough above the confusion limit that this simple and
intuitive method is adequate. For sources detected in only one band, the
authors use the flux in the cleaned map for the second band at the position
of the detection. This table lists all 3,496 sources above 3 sigma in either
map.
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.
SPTSZSPSC Catalog
This database table presents the catalog of emissive point-sources detected
in the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey, which is a
contiguous 2530 deg2 area surveyed between 2008-2011 in three bands
centered at 95, 150, and 220 GHz. The catalog contains 4845 sources measured
at a significance of 4.5 sigma or greater in at least one band, corresponding
to detections above approximately 9.8, 5.8, and 20.4 mJy in 95, 150, and 220
GHz, respectively. Spectral behavior in the SPT bands is used for source
classification into two populations based on the underlying physical
mechanisms of compact, emissive sources that are bright at millimeter
wavelengths: synchrotron radiation from active galactic nuclei and thermal
emission from dust. The latter population includes a component of
high-redshift sources often referred to as submillimeter galaxies (SMGs). In
the relatively bright flux ranges probed by the survey, these sources are
expected to be magnified by strong gravitational lensing. The survey also
contains sources consistent with protoclusters, groups of dusty galaxies at
high redshift undergoing collapse. The authors cross-match the SPT-SZ catalog
with external catalogs at radio, infrared, and X-ray wavelengths and identify
available redshift information. The catalog splits into 3980
synchrotron-dominated and 865 dust-dominated sources and determines a list of
506 SMGs. 10 sources are identified as stars.
The SPT is a 10-m telescope located at the Amundsen-Scott South Pole station
in Antarctica. At 150 GHz (2 mm), the SPT has arcminute angular resolution
and a 1 deg2 diffraction-limited field of view. The SPT was designed for
high-sensitivity millimeter/sub-millimeter observations of faint,
low-contrast sources, such as CMB anisotropies. The first survey with the
SPT, designated as the SPT-SZ survey, was completed in 2011 November and
covers a ~2500 deg2 region of the southern extragalactic sky in three
frequency bands, 95, 150, and 220 GHz, corresponding to wavelengths of 3.2,
2.0, and 1.4 mm. The fields were surveyed to depths of approximately 40, 18,
and 70 microK arcmin at 95, 150, and 220 GHz, respectively.
This study uses data from 19 fields observed by the SPT between 2008 and
2011. The fields are referred to using the J2000 coordinates of their
centers, Right Ascension in hours and Declination in degrees. Table 1 in the
reference paper lists the positions and effective areas of these fields.The
total effective area used for the catalog and analysis in this present work
is 2530 deg2. The catalog is an extension of two previous works: Vieira et
al. (2010, ApJ, 719, 763) and Mocanu et al. (2013, ApJ, 779, 61) and builds
on the same analysis pipeline, adding 1759 deg2 of newly analyzed data, and
additional data for two fields which were re-observed in 2010 and 2011.
SUBPFCLOG Catalog
This table contains the Subaru Prime Focus Camera (Suprime-Cam)
log of exposures having observation type = 'OBJECT' (those with 'BIAS',
'FLAT' and other types are not included) which have been made since April
2001. Note that from the version of Nov. 2005 on, the number of rows has
significantly increased because those data with worse position determination
(up to 30 arcsec error) are now included. The data currently extend to
November 2005 and it is anticipated that they will be regularly updated
Suprime-Cam is an 80-mega pixels (10240 x 8192) mosaic CCD camera, for
the wide-field prime focus of the 8.2m Subaru telescope. Suprime-Cam
covers a field of view 34' x 27', a unique facility among the 8-10m
class telescopes, with a resolution of 0.202 arcseconds per pixel. The focal
plane consists of ten high-resistivity 2kx2k CCDs developed by MIT
Lincoln Laboratory, which are cooled by a large Stirling-cycle cooler.
The CCD readout electronics was designed to be scalable, which allows
the multiple read-out of tens of CCDs. It takes 50 seconds to readout
entire arrays. A filter-exchange mechanism of the jukebox type is
designed that can hold up to ten large filters (205 x 170 x 15 mm3).
The wide-field corrector is basically a three-lens Wynne-type, but
has a new type of atmospheric dispersion corrector. The corrector
provides a flat focal plane and an un-vignetted field of view of 30'
in diameter. The achieved co-planarity of the focal array mosaic is
smaller than 30 um peak-to-peak, which realizes mostly the seeing
limited image over the entire field. The median seeing in the
I_c-band, measured over one year and a half, is 0.61 arcseconds. The PSF
anisotropy in Suprime-Cam images, estimated by stellar ellipticities,
is about 2% under this median seeing condition. At the time of its
commissioning, Suprime-Cam had the largest survey speed, which is
defined as the field of view multiplied by the primary mirror area of
the telescope, among those cameras built for sub-arcsecond imaging.
For more details, see: Miyazaki et al., Publ. Astron. Soc. Japan 54,
833-853, 2002 (2002PASJ...54..833M).
TEVCAT Catalog
TeVCat (http://tevcat.uchicago.edu/) is an online, interactive catalog for
very-high-energy (VHE: energies, E >~ 50 GeV) gamma-ray astronomy. As VHE
astronomy continues to grow, the usefulness of a one-stop clearing house for
information on new sources is increasingly evident. TeVCat is intended to be
such a resource. With sky maps, scientific information, visibility plotters
and linked references available at the website, it will help the wider
gamma-ray community stay up-to-date and informed on this exciting and rapidly
developing field.
This HEASARC database table provides the TeVCat list of VHE sources as well
as links to the TeV source resource pages on the TeVCat website. The catalog
and the website at the University of Chicago
are maintained by Scott Wakely and Deirdre Horan.
