- ID:
- ivo://CDS.VizieR/I/267
- Title:
- The APM-North Catalogue
- Short Name:
- I/267
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- ****************************************************************** This version is a preliminary adaptation of the APM, covering the Northern sky at high galactic latitudes only. ****************************************************************** The catalogue APMCAT-POSS1-1.0 is derived from the first epoch (1949-1958) Palomar Observatory-National Geographic Sky Survey (POSS). The catalog is based on digitised scans with the laser based Cambridge Automated Plate Measurement(APM) machine of both the blue O plates and red E plates. The plates are scanned with a pixel sampling 8microns which corresponds 0.49 arcsecs at the nominal plate scale of 61arcsec/mm (16.4 micron/arcsec). Further details about the survey material can be found in Minkowski and Abell 1963 and Lund and Dixon 1973.
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- ID:
- ivo://CDS.VizieR/J/ApJS/241/12
- Title:
- The Asteroseismic Target List (ATL) for TESS
- Short Name:
- J/ApJS/241/12
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the target list of solar-type stars to be observed in short-cadence (2 minute) for asteroseismology by the NASA Transiting Exoplanet Survey Satellite (TESS) during its 2 year nominal survey mission. The solar-like Asteroseismic Target List (ATL) is comprised of bright, cool main-sequence and subgiant stars and forms part of the larger target list of the TESS Asteroseismic Science Consortium. The ATL uses the Gaia Data Release 2 and the Extended Hipparcos Compilation (XHIP) to derive fundamental stellar properties, to calculate detection probabilities, and to produce a rank- ordered target list. We provide a detailed description of how the ATL was produced and calculate expected yields for solar-like oscillators based on the nominal photometric performance by TESS. We also provide a publicly available source code that can be used to reproduce the ATL, thereby enabling comparisons of asteroseismic results from TESS with predictions from synthetic stellar populations.
- ID:
- ivo://CDS.VizieR/J/ApJ/754/44
- Title:
- The AstraLux Large M-dwarf Survey
- Short Name:
- J/ApJ/754/44
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- These tables contain the results from a multiplicity survey of 701 M-type and 60 K-type stars (among which 182 new and 37 previously known companions were detected in 205 systems) using the Lucky Imaging cameras AstraLux Norte at the Calar Alto 2.2m and AstraLux Sur at the ESO NTT. Most of the targets have been observed during two or more epochs, and could be confirmed as physical companions through common proper motion, often with orbital motion being confirmed in addition. One table lists general properties of all the stars in the sample, another the observational parameters of each confirmed or suspected binary, a third lists the derived physical parameters of each confirmed or suspected binary, the fourth lists astrometric data points of all binary candidates for which multiple epochs have been collected (also including literature measurements for previously resolved binaries) and a final table lists observational properties of confirmed or suspected background stars.
- ID:
- ivo://CDS.VizieR/II/363
- Title:
- The band-merged unWISE Catalog
- Short Name:
- II/363
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the unWISE Catalog, containing the positions and fluxes of roughly 2 billion objects observed by the Wide-field Infrared Survey Explorer (WISE) over the full sky. The unWISE Catalog has two advantages over the existing WISE catalog (AllWISE): first, it is based on significantly deeper imaging, and second, it features improved modeling of crowded regions. The deeper imaging used in the unWISE Catalog comes from the coaddition of all publicly available 3-5um WISE imaging, including that from the ongoing NEOWISE-reactivation mission, thereby increasing the total exposure time by a factor of 5 relative to AllWISE. At these depths, even at high Galactic latitudes, many sources are blended with their neighbors; accordingly, the unWISE analysis simultaneously fits thousands of sources to obtain accurate photometry. Our new catalog detects sources roughly 0.7mag fainter than the AllWISE catalog at 5{sigma}, and more accurately models millions of faint sources in the Galactic plane, enabling a wealth of Galactic and extragalactic science. In particular, relative to AllWISE, unWISE doubles the number of galaxies detected between redshifts 0 and 1 and triples the number between redshifts 1 and 2, cataloging more than half a billion galaxies over the whole sky.
- ID:
- ivo://CDS.VizieR/J/ApJ/757/83
- Title:
- The Blanco Cosmology Survey (BCS)
- Short Name:
- J/ApJ/757/83
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Blanco Cosmology Survey (BCS) is a 60 night imaging survey of ~80deg^2^ of the southern sky located in two fields: (5hr,-55{deg}) and (23hr,-55{deg}). The survey was carried out between 2005 and 2008 in griz bands with the Mosaic2 imager on the Blanco 4m telescope. The primary aim of the BCS survey is to provide the data required to optically confirm and measure photometric redshifts for Sunyaev-Zel'dovich effect selected galaxy clusters from the South Pole Telescope and the Atacama Cosmology Telescope. We process and calibrate the BCS data, carrying out point-spread function-corrected model-fitting photometry for all detected objects. The median 10{sigma} galaxy (point-source) depths over the survey in griz are approximately 23.3 (23.9), 23.4 (24.0), 23.0 (23.6), and 21.3 (22.1), respectively. The astrometric accuracy relative to the USNO-B survey is ~45mas. We calibrate our absolute photometry using the stellar locus in grizJ bands, and thus our absolute photometric scale derives from the Two Micron All Sky Survey, which has ~2% accuracy. The scatter of stars about the stellar locus indicates a systematic floor in the relative stellar photometric scatter in griz that is ~1.9%, ~2.2%, ~2.7%, and ~2.7%, respectively. A simple cut in the AstrOmatic star-galaxy classifier spread_ model produces a star sample with good spatial uniformity. We use the resulting photometric catalogs to calibrate photometric redshifts for the survey and demonstrate scatter {delta}z/(1+z)=0.054 with an outlier fraction {eta}<5% to z~1. We highlight some selected science results to date and provide a full description of the released data products.
- ID:
- ivo://CDS.VizieR/J/ApJS/197/21
- Title:
- The Carnegie-Irvine Galaxy Survey (CGS). I.
- Short Name:
- J/ApJS/197/21
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Carnegie-Irvine Galaxy Survey (CGS) is a long-term program to investigate the photometric and spectroscopic properties of a statistically complete sample of 605 bright (B_T_<12.9mag), southern ({delta}<0{deg}) galaxies using the facilities at Las Campanas Observatory. This paper, the first in a series, outlines the scientific motivation of CGS, defines the sample, and describes the technical aspects of the optical broadband (BVRI) imaging component of the survey, including details of the observing program, data reduction procedures, and calibration strategy. The overall quality of the images is quite high, in terms of resolution (median seeing ~1"), field of view (8.9'x8.9'), and depth (median limiting surface brightness ~27.5, 26.9, 26.4, and 25.3mag/arcsec^2^ in the B, V, R, and I bands, respectively). We prepare a digital image atlas showing several different renditions of the data, including three-color composites, star-cleaned images, stacked images to enhance faint features, structure maps to highlight small-scale features, and color index maps suitable for studying the spatial variation of stellar content and dust. In anticipation of upcoming science analyses, we tabulate an extensive set of global properties for the galaxy sample. These include optical isophotal and photometric parameters derived from CGS itself, as well as published information on multiwavelength (ultraviolet, U-band, near-infrared, far-infrared) photometry, internal kinematics (central stellar velocity dispersions, disk rotational velocities), environment (distance to nearest neighbor, tidal parameter, group, or cluster membership), and HI content.
- ID:
- ivo://CDS.VizieR/J/ApJS/197/22
- Title:
- The Carnegie-Irvine Galaxy Survey (GGS). II.
- Short Name:
- J/ApJS/197/22
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Carnegie-Irvine Galaxy Survey (CGS) is a comprehensive investigation of the physical properties of a complete, representative sample of 605 bright (B_T_<=12.9mag) galaxies in the southern hemisphere. This contribution describes the isophotal analysis of the broadband (BVRI) optical imaging component of the project. We pay close attention to sky subtraction, which is particularly challenging for some of the large galaxies in our sample. Extensive crosschecks with internal and external data confirm that our calibration and sky subtraction techniques are robust with respect to the quoted measurement uncertainties. We present a uniform catalog of one-dimensional radial profiles of surface brightness and geometric parameters, as well as integrated colors and color gradients. We use the geometric parameters, in conjunction with the amplitude and phase of the m=2 Fourier mode, to identify bars and quantify their size and strength. Finally, we utilize the information encoded in the m=1 Fourier profiles to measure disk lopsidedness.
- ID:
- ivo://CDS.VizieR/J/ApJ/862/13
- Title:
- The Carnegie-Irvine Galaxy Survey. VI. Spirals
- Short Name:
- J/ApJ/862/13
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Carnegie-Irvine Galaxy Survey provides high-quality broadband optical images of a large sample of nearby galaxies for detailed study of their structure. To probe the physical nature and possible cosmological evolution of spiral arms, a common feature of many disk galaxies, it is important to quantify their main characteristics. We describe robust methods to measure the number of arms and their mean strength, length, and pitch angle. The arm strength depends only weakly on the adopted radii over which it is measured, and it is stronger in bluer bands than redder bands. The vast majority of clearly two-armed ("grand-design") spiral galaxies have a systematically higher relative amplitude of the m=2 Fourier mode in the main spiral region. We use both one-dimensional and two-dimensional Fourier decomposition to measure the pitch angle, finding reasonable agreement between these two techniques with a scatter of ~2{deg}. To understand the applicability and limitations of our methodology to imaging surveys of local and distant galaxies, we create mock images with properties resembling observations of local (z<~0.1) galaxies by the Sloan Digital Sky Survey and distant galaxies (0.1<~z<~1.1) observed with the Hubble Space Telescope. These simulations lay the foundation for forthcoming quantitative statistical studies of spiral structure to understand its formation mechanism, dependence on galaxy properties, and cosmological evolution.
- ID:
- ivo://CDS.VizieR/II/365
- Title:
- The CatWISE2020 catalog (updated version 28-Jan-2021)
- Short Name:
- II/365
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The CatWISE2020 Catalog consists of 1,890,715,640 sources over the entire sky selected from WISE and NEOWISE survey data at 3.4 and 4.6um (W1 and W2) collected from 2010 Jan 7 to 2018 Dec 13. This dataset adds two years to that used for the CatWISE Preliminary Catalog (Eisenhardt+ 2020ApJS..247...69E), bringing the total to six times as many exposures spanning over sixteen times as large a time baseline as the AllWISE catalog. The other major change from the CatWISE Preliminary Catalog is that the detection list for CatWISE2020 was generated using "crowdsource" software (Schlafly+ 2019ApJS..240...30S), while the Preliminary Catalog used the detection software used for AllWISE (II/328). These two factors result in roughly twice as many sources in CatWISE2020. The scatter with respect to Spitzer photometry at faint magnitudes in the COSMOS field, which is out of the Galactic plane and at low ecliptic latitude (corresponding to lower WISE coverage depth) is similar to that for the CatWISE Preliminary Catalog. The 90% completeness depth for CatWISE2020 is at roughly W1=17.7 and W2=17.5, about 1.7 mag deeper than in the Preliminary Catalog. From comparison to Gaia, CatWISE2020 motions are over a dozen times more accurate than those from AllWISE.
- ID:
- ivo://CDS.VizieR/II/317
- Title:
- The CFHTLS Survey (T0007 release)
- Short Name:
- II/317
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Canada and France joined a large fraction (~50%) of their dark and grey telescope time from mid-2003 to early 2009 for a large project, the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS). The data acquisition and calibration has been a major undertaking for the Canadian and French communities: more than 2300 hours over 5 years (an equivalent of 450 nights) have been devoted to the survey using the wide field optical imaging camera MegaCam, a 1{deg}x1{deg} field of view 340 Megapixel camera. The CFHTLS comprises 2 components: "CFHTLS Deep", 4 independent 1deg^2^ MegaCam pointing, and "CFHT Wide" comprising 171 MegaCam pointings covering ~155deg^2^ in 4 contiguous independent patches. All areas are located far from the galactic plane, and their central positions are: -------------------------------------------------- Field RA (J2000) Dec Galactic position -------------------------------------------------- W1 02:18 -07:00 172.468 -61.242 W2 08:54 -04:15 232.067 +24.743 W3 14:17:54 +54:30:31 098.850 +58.390 W4 22:13:18 +01:19 063.243 -42.511 D1 02:25:59 -04:29:40 171.993 -58.054 D2 10:00:28 +02:23:30 236.616 +42.227 D3 14:19:27 +52:40:56 096.227 +59.642 D4 22:15:31 -17:43:56 039.271 -52.925 -------------------------------------------------- This final release of the CFHTLS benefits greatly from vastly improved flat-fielding and photometric calibration techniques developed by the Supernovae Legacy Survey (SNLS) team and CFHT which allows us to significantly improve the precision of our photometric calibration compared to previous releases. The astrometric accuracy reaches 0.02arcsec internal and 0.2arcsec external. The set of filters used for the survey are close to the SDSS filter set; their characteristics and a comparison to SDSS can be found at http://www3.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/megapipe/docs/filters.html Please ee the documentation file "T0007-doc.pdf" for details concerning this T0007 release.