For a number of years there has been a great demand for a high-density catalog of accurate stellar positions and proper motions that maintains a consistent system of reference over the entire sky. The Smithsonian Astrophysical Observatory Star Catalog (SAO; SAO Staff 1966) has partially met those requirements, but its positions brought to current epochs now contain errors on the order of 1 second of arc, plus the proper motions in the SAO differ systematically with one another depending on their source catalogs. With the completion of the Second Cape Photographic Catalogue (CPC2; de Vegt et al. 1989), a photographic survey comparable in density to the AGK3 (Dieckvoss 1975) was finally available for the southern hemisphere. These two catalogs were used as a base and matched against the AGK2 (Schorr & Kohlschuetter 1951-58), Yale photographic zones (Yale Trans., Vols. 11-32), First Cape Photographic Catalogue (CPC1; Jackson & Stoy 1954, 55, 58; Stoy 1966), Sydney Southern Star Catalogue (King & Lomb 1983), Sydney Zone Catalogue -48 to -54 degrees (Eichhorn et al. 1983), 124 meridian circle catalogs, and catalogs of recent epochs, such as the Carlsberg Meridian Catalogue, La Palma (CAMC), USNO Zodiacal Zone Catalog (Douglass & Harrington 1990), and the Perth 83 Catalogue (Harwood [1990]) to obtain as many input positions as possible. All positions were then reduced to the system of the FK4 (Fricke & Kopff 1963) using a combination of the FK4, the FK4 Supplement as improved by H. Schwan of the Astronomisches Rechen-Institut in Heidelberg, and the International Reference Stars (IRS; Corbin 1991), then combined with the CPC2 and AGK3. The total number of input positions from which the ACRS was formed is 1,643,783. The original catalog is divided into two parts. Part 1 contains the stars having better observational histories and, therefore, more reliable positions and proper motions. This part constitutes 78 percent of the catalog; the mean errors of the proper motions are +/-0.47 arcsec per century and +/-0.46 arcsec per century in right ascension and declination, respectively. The stars in Part 2 have poor observational histories and consist mostly of objects for which only two catalog positions in one or both coordinates were available for computing the proper motions. Where accuracy is the primary consideration, only the stars in Part 1 should be used, while if the highest possible density is desired, the two parts should be combined. The ACRS was compiled at the U. S. Naval Observatory with the intention that it be used for new reductions of the Astrographic Catalogue (AC) plates. These plates are small in area (2 x 2 deg) and the IRS is not dense enough. Whereas the ACRS was compiled using the same techniques developed to produce the IRS, it became clear as the work progressed that the ACRS would have applications far beyond its original purpose. With accurate positions and proper motions rigorously reduced to both the FK4 and FK5 (Fricke et al. 1988) systems, it does more than simply replace the SAO. Rather, it provides the uniform system of reference stars that has been needed for many years by those who require densities greater than the IRS and with high accuracy over a wide range of epochs. It is intended that, as additional observations become available, stars will be migrated from Part 2 to Part 1, with the hope that eventually the ACRS will be complete in one part. Additional details concerning the compilation and properties of the ACRS can be found in Corbin & Urban (1989) except that the star counts and errors given here supersede the ones given in 1989. The HEASARC revised this database table in August, 2005, in order to add Galactic coordinates. This is a service provided by NASA HEASARC .

Note: in this dataset, the stars whose distances are 100,000 parsecs are associated with defective data. As it can't be modified at the source, users have to exclude it manually : but if you exclude these stars from all distance-related analyzes, everything works perfectly well."The database is a subset of the data in three major catalogs: the Hipparcos Catalog,the Yale Bright Star Catalog (5th Edition), and the Gliese Catalog of Nearby Stars (3rd Edition). Each of these catalogs contains information useful to amateur astronomers: The Hipparcos catalog is the largest collection of high-accuracy stellar positional data, particularly parallaxes, which makes it useful as a starting point for stellar distance data.The Yale Bright Star Catalog contains basic data on essentially all naked-eye stars, including much information (such as the traditional Bayer Greek letters and Flamsteed numbers) missing from many other catalogsThe Gliese catalog is the most comprehensive catalog of nearby stars (those within 75 light years of the Sun). It contains many fainter stars not found in Hipparcos.The name of the database comes from the three catalogs comprising its data: Hipparcos, Yale, and Gliese.This database contains ALL stars that are either brighter than a certain magnitude cutoff (magnitude +7.5 to +9.0) or within 50 parsecs (about 160 light years) from the Sun. The current version, v. 3.0, has no magnitude cutoff: any star in Hipparcos, Yale, or Gliese is represented."Source: http://www.astronexus.com/hyg and https://github.com/astronexus/HYG-DatabaseFields in the database: id: The database primary key.hip: The star's ID in the Hipparcos catalog, if known.hd: The star's ID in the Henry Draper catalog, if known.hr: The star's ID in the Harvard Revised catalog, which is the same as its number in the Yale Bright Star Catalog.gl: The star's ID in the third edition of the Gliese Catalog of Nearby Stars.bf: The Bayer / Flamsteed designation, primarily from the Fifth Edition of the Yale Bright Star Catalog. This is a combination of the two designations. The Flamsteed number, if present, is given first; then a three-letter abbreviation for the Bayer Greek letter; the Bayer superscript number, if present; and finally, the three-letter constellation abbreviation. Thus Alpha Andromedae has the field value "21Alp And", and Kappa1 Sculptoris (no Flamsteed number) has "Kap1Scl".ra, dec: The star's right ascension and declination, for epoch and equinox 2000.0.proper: A common name for the star, such as "Barnard's Star" or "Sirius". I have taken these names primarily from the Hipparcos project's web site, which lists representative names for the 150 brightest stars and many of the 150 closest stars. I have added a few names to this list. Most of the additions are designations from catalogs mostly now forgotten (e.g., Lalande, Groombridge, and Gould ["G."]) except for certain nearby stars which are still best known by these designations.dist: The star's distance in parsecs, the most common unit in astrometry. To convert parsecs to light years, multiply by 3.262. A value >= 10000000 indicates missing or dubious (e.g., negative) parallax data in Hipparcos.pmra, pmdec: The star's proper motion in right ascension and declination, in milliarcseconds per year.rv: The star's radial velocity in km/sec, where known.mag: The star's apparent visual magnitude.absmag: The star's absolute visual magnitude (its apparent magnitude from a distance of 10 parsecs).spect: The star's spectral type, if known.ci: The star's color index (blue magnitude - visual magnitude), where known.x,y,z: The Cartesian coordinates of the star, in a system based on the equatorial coordinates as seen from Earth. +X is in the direction of the vernal equinox (at epoch 2000), +Z towards the north celestial pole, and +Y in the direction of R.A. 6 hours, declination 0 degrees.vx,vy,vz: The Cartesian velocity components of the star, in the same coordinate system described immediately above. They are determined from the proper motion and the radial velocity (when known). The velocity unit is parsecs per year; these are small values (around 1 millionth of a parsec per year), but they enormously simplify calculations using parsecs as base units for celestial mapping.rarad, decrad, pmrarad, prdecrad: The positions in radians, and proper motions in radians per year.bayer: The Bayer designation as a distinct valueflam: The Flamsteed number as a distinct valuecon: The standard constellation abbreviationcomp, comp_primary, base: Identifies a star in a multiple star system. comp = ID of companion star, comp_primary = ID of primary star for this component, and base = catalog ID or name for this multi-star system. Currently only used for Gliese stars.lum: Star's luminosity as a multiple of Solar luminosity.var: Star's standard variable star designation, when known.var_min, var_max: Star's approximate magnitude range, for variables. This value is based on the Hp magnitudes for the range in the original Hipparcos catalog, adjusted to the V magnitude scale to match the "mag" field."

🇺🇸 미국 English The BSC5P database table contains data derived from the Bright Star Catalog, 5th Edition, preliminary, which is widely used as a source of basic astronomical and astrophysical data for stars brighter than magnitude 6.5. The database contains the identifications of included stars in several other widely-used catalogs, double- and multiple-star identifications, indication of variability and variable-star identifiers, equatorial positions for B1900.0 and J2000.0, galactic coordinates, UBVRI photoelectric photometric data when they exist, spectral types on the Morgan-Keenan (MK) classification system, proper motions (J2000.0), parallax, radial- and rotational-velocity data, and multiple-star information (number of components, separation, and magnitude differences) for known non-single stars. This table was created by the HEASARC in 1995 based upon a file obtained from either the ADC or the CDS. A number of revisions have been made by the HEASARC to this original version, e.g., celestial positions were added for the 14 non-stellar objects which have received HR numbers: HR 92, 95, 182, 1057, 1841, 2472, 2496, 3515, 3671, 6309, 6515, 7189, 7539 and 8296. In January 2014, the very incorrect position for HR 3671 = NGC 2808 was fixed (the Declination is -65 degrees not +65 degrees!), and smaller corrections were made to the positions of HR 2496, 3515 and 6515 so as to bring them in better agreement with the positions listed in SIMBAD and NED This is a service provided by NASA HEASARC .

This database is based on the electronic version of the SAO catalog from the Astronomical Data Center, which is itself based on an original binary version of the Smithsonian Astrophysical Observatory Star Catalog (SAO, SAO Staff 1966). Subsequent improvements by T. A. Nagy (1979) included the addition of cross-identifications from the Table of Correspondences SAO/HD/DM/GC (Morin 1973). As a prelude to creation of the 1984 version of the SAO, a new version of the SAO-HD-GC-DM Cross Index was prepared (Roman, Warren, and Schofield 1983). The 1984 version of the SAO contained the corrected and extended cross identifications, all errata published up to January 1984 and known to the ADC, numerous errors forwarded to the ADC by colleagues, and errors discovered at the ADC during the course of this work. Clayton A. Smith of the U. S. Naval Observatory provided J2000.0 positions and proper motions for the SAO stars. Published and unpublished errors discovered in the previous version (1984) have been corrected (up to May 1991). For this HEASARC representation, some parameters such as the RA and Dec in radians have been omitted. This online version of the SAO Catalog was created by the HEASARC in March 2001 based on ADC/CDS Catalog I/131A, which itself is originally derived from a character-coded machine-readable version of the Smithsonian Astrophysical Observatory Star Catalog (SAO, SAO Staff 1966) prepared by T.A. Nagy in 1979, and subsequently modified over the next decade or so. The first machine-readable version contained format modifications, cross identifications and other changes, and was the starting point of the version in this database. Additional changes were made to the SAO catalog over time (namely more cross identifications and corrections) which resulted in a new version in 1984. Finally, the most recent version of the catalog was published in 1989. It included J2000 positions for all the objects, and corrections to errors known as of May 1989. This is a service provided by NASA HEASARC .

The BSC5P database table contains data derived from the Bright Star Catalog, 5th Edition, preliminary, which is widely used as a source of basic astronomical and astrophysical data for stars brighter than magnitude 6.5. The database contains the identifications of included stars in several other widely-used catalogs, double- and multiple-star identifications, indication of variability and variable-star identifiers, equatorial positions for B1900.0 and J2000.0, galactic coordinates, UBVRI photoelectric photometric data when they exist, spectral types on the Morgan-Keenan (MK) classification system, proper motions (J2000.0), parallax, radial- and rotational-velocity data, and multiple-star information (number of components, separation, and magnitude differences) for known non-single stars. This table was created by the HEASARC in 1995 based upon a file obtained from either the ADC or the CDS. A number of revisions have been made by the HEASARC to this original version, e.g., celestial positions were added for the 14 non-stellar objects which have received HR numbers: HR 92, 95, 182, 1057, 1841, 2472, 2496, 3515, 3671, 6309, 6515, 7189, 7539 and 8296. In January 2014, the very incorrect position for HR 3671 = NGC 2808 was fixed (the Declination is -65 degrees not +65 degrees!), and smaller corrections were made to the positions of HR 2496, 3515 and 6515 so as to bring them in better agreement with the positions listed in SIMBAD and NED This is a service provided by NASA HEASARC .

This database is based on the electronic version of the SAO catalog from the Astronomical Data Center, which is itself based on an original binary version of the Smithsonian Astrophysical Observatory Star Catalog (SAO, SAO Staff 1966). Subsequent improvements by T. A. Nagy (1979) included the addition of cross-identifications from the Table of Correspondences SAO/HD/DM/GC (Morin 1973). As a prelude to creation of the 1984 version of the SAO, a new version of the SAO-HD-GC-DM Cross Index was prepared (Roman, Warren, and Schofield 1983). The 1984 version of the SAO contained the corrected and extended cross identifications, all errata published up to January 1984 and known to the ADC, numerous errors forwarded to the ADC by colleagues, and errors discovered at the ADC during the course of this work. Clayton A. Smith of the U. S. Naval Observatory provided J2000.0 positions and proper motions for the SAO stars. Published and unpublished errors discovered in the previous version (1984) have been corrected (up to May 1991). For this HEASARC representation, some parameters such as the RA and Dec in radians have been omitted. This online version of the SAO Catalog was created by the HEASARC in March 2001 based on ADC/CDS Catalog I/131A, which itself is originally derived from a character-coded machine-readable version of the Smithsonian Astrophysical Observatory Star Catalog (SAO, SAO Staff 1966) prepared by T.A. Nagy in 1979, and subsequently modified over the next decade or so. The first machine-readable version contained format modifications, cross identifications and other changes, and was the starting point of the version in this database. Additional changes were made to the SAO catalog over time (namely more cross identifications and corrections) which resulted in a new version in 1984. Finally, the most recent version of the catalog was published in 1989. It included J2000 positions for all the objects, and corrections to errors known as of May 1989. This is a service provided by NASA HEASARC .

"OpenNGC is a database containing positions and main data of NGC (New General Catalogue) and IC (Index Catalogue) objects. Unlike other similar databases which are released with license limitations, OpenNGC is released under CC-BY-SA-4.0 license, which allows the use for a wider range of cases.https://github.com/mattiaverga/OpenNGC Data SourcesOpenNGC has been built by merging data from: NASA/IPAC Extragalactic Database http://ned.ipac.caltech.edu/ This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.HyperLEDA database http://leda.univ-lyon1.fr We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr)SIMBAD Astronomical Database http://simbad.u-strasbg.fr/simbad/ This research has made use of the SIMBAD database, operated at CDS, Strasbourg, FranceHEASARC High Energy Astrophysics Science Archive Research Center http://heasarc.gsfc.nasa.gov/ We used several databases from HEASARC such as mwsc, lbn, plnebulae, lmcextobj and smcclustrs."

This database table contains a catalog of confirmed and suspected symbiotic stars. The list includes 188 symbiotic stars as well as 30 objects suspected of being symbiotic. For each star, basic observational material is presented: coordinates, V and K magnitudes, ultraviolet (UV), infrared (IR), X-ray and radio observations. Also listed are the spectral type of the cool component, the maximum ionization potential observed, references to finding charts, spectra, classifications and recent (as of 2000) papers discussing the physical parameters and nature of each object. This table does NOT contain the information on orbital photometric ephemerides and orbital elements of known symbiotic binaries, pulsational periods for symbiotic Miras, Hipparcos parallaxes and information about outbursts and flickering that is contained in the printed version of the catalog (see Tables 3-7 in the paper for this material). This table was created by the HEASARC in November 2005 based on 4 CDS tables (table1.dat, table1b.dat, table2.dat, table2b.dat) from the directory J/A+AS/146/407/. This is a service provided by NASA HEASARC .

The TC-STAR Spanish Baseline Female Speech Database was created within the scope of the TC-STAR project (IST- FP6-506738) funded by the European Commission.It contains the recordings of one female Spanish speaker recorded in a noise-reduced room simultaneously through a close talk microphone, a mid distance microphone and a laryngograph signal. It consists of the recordings and annotations of read text material of approximately 10 hours of speech for baseline applications (Text-to-Speech systems). This database is distributed on 10 DVDs. The database complies with the common specifications created in the TC-STAR project.The annotation of the database includes manual orthographic transcriptions, the automatic segmentation into phonemes and automatic generation of pitch marks. A certain percentage of phonetic segments and pitch marks has been manually checked. A pronunciation lexicon in SAMPA with POS, lemma and phonetic transcription of all the words prompted and spoken is also provided.Speech samples are stored as sequences of 24-bit 96 kHz with the least significant byte first (“lohi” or Intel format) as (signed) integers. Each prompted utterance is stored in a separate file. Each signal file is accompanied by an ASCII SAM label file which contains the relevant descriptive information.The TC-STAR Spanish Baseline Male Speech Database is also available via ELRA under reference ELRA-S0310.

This data is the gray scale, number and apparent magnitude data of stars observed by KAI-4021 on the ground. 1. StarMap1 refers to the data when the optical axis points to point to 101.636°for the right ascension, 31.054°for the declination. 2. StarMap2 refers to the data when the optical axis points to point to 106.778°for the right ascension, 31.068°for the declination. 3. StarMap3 refers to the data when the optical axis points to point to 112.501°for the right ascension, 31.069°for the declination. 4. StarMapi.track_num refers to the number of navigation stars in the image. 5. StarMapi.Mag refers to the apparent magnitude. 6. StarMapi.win_info refers to the 8*8 gray data of each star in the image. 7. StarMapi.ID_frm refers refers to the number of each star in our catalogue.

The Washington Double Star Catalog (WDS), maintained by the United States Naval Observatory (USNO), is the world's principal database of astrometric double and multiple star information. The WDS Catalog contains positions, discoverer designations, epochs, position angles, separations, magnitudes, spectral types, proper motions and when available, Durchmusterung numbers and notes for the components of close to 100,000 systems based on ~600,000 means. The current version at the HEASARC is updated weekly and is derived from the version available online at https://crf.usno.navy.mil/wds/ (and mirrored at http://www.astro.gsu.edu/wds/), the latter being potentially updated nightly. The Washington Visual Double Star Catalog (WDS) is the successor to the Index Catalogue of Visual Double Stars, 1961.0 (IDS; Jeffers & van den Bos, 1963). Three earlier double star catalogs in the 20th century, those by Burnham (BDS; 1906), Innes (SDS; 1927), and Aitken (ADS; 1932), each covered only a portion of the sky. Both the IDS and the WDS cover the entire sky, and the WDS is intended to contain all known visual double stars for which at least one differential measure has been published. The WDS is continually updated as published data become available. Prior to this, two major updates have been published (Worley & Douglass 1984, 1997). The Washington Double Star Catalog (WDS) has seen numerous changes since the last major release of the catalog. The application of many techniques and considerable industry over the past few years has yielded unprecedented gains in both the number of systems and the number of measures. This version of the WDS catalog was first created at the HEASARC in March 2002 based on the USNO online version (available at either https://crf.usno.navy.mil/wds/ or http://www.astro.gsu.edu/wds/), and is updated by the HEASARC on at least a weekly basis. The table schema was last revised in February 2005. This is a service provided by NASA HEASARC .

4 hours and 80 minutes of speech as spoken by 2 female speakers and 2 male speakers, covering both mimics and parallel voice conversion data.

The Galactic Plane Infrared Polarization Survey (GPIPS) covers 76 sq. deg. of the first Galactic quadrant midplane, 18<l<56 deg and -1<b<+1 deg, in H-band (1.6 micron) linear polarimetry to reveal the plane-of-the-sky orientation of the magnetic field in diffuse and denser atomic and molecular clouds. The Survey consists of 3234 overlapping 10x10 arcmin fields observed using the Mimir instrument on the 1.8 m Perkins telescope.The unique star data file (Clemens et al. 2020) collects all GPIPS photometry and polarimetry and all matching stellar data appropriate to each GPIPS star. The unique star file contains entries for 13,861,329 GPIPS stars.

The Extragalactic First Look Survey is composed of 4 square degrees of imaging with MIPS and IRAC centered at J1718+5930, with extensive ancillary data from ground-based optical and radio telescopes. As one of the first observations made with Spitzer after the completion of Science Verification at the end of 2003 November, the aim of this 67 hr survey was to characterize the extragalactic source populations observed with Spitzer down to sub-millijansky levels in the mid-infrared.

8 hours of speech as spoken by 2 female speakers and 2 male speakers for each language (English and Spanish).

The CSIRO 5-star Data Rating tool provides a self-assessment rating scheme against the social, technical and informational attributes of data. This tool provides implementations of the FORCE 11 FAIR data principles. The 5-star scheme aims to help users understand how mature some data or a service is. Lineage: Implementation of https://confluence.csiro.au/display/OZNOME/Data+ratings

Linear regression slope estimates by year and p-values for proportion of liver transplants caused by each disease etiology in general population, men, and women.

The data used in this paper is from the 16th issue of SDSS. SDSS-DR16 contains a total of 930,268 photometric images, with 1.2 billion observation sources and tens of millions of spectra. The data obtained in this paper is downloaded from the official website of SDSS. Specifically, the data is obtained through the SkyServerAPI structure by using SQL query statements in the subwebsite CasJobs. As the current SDSS photometric table PhotoObj can only classify all observed sources as point sources and surface sources, the target sources can be better classified as galaxies, stars and quasars through spectra. Therefore, we obtain calibrated sources in CasJobs by crossing SpecPhoto with the PhotoObj star list, and obtain target position information (right ascension and declination). Calibrated sources can tell them apart precisely and quickly. Each calibrated source is labeled with the parameter "Class" as "galaxy", "star", or "quasar". In this paper, observation day area 3462, 3478, 3530 and other 4 areas in SDSS-DR16 are selected as experimental data, because a large number of sources can be obtained in these areas to provide rich sample data for the experiment. For example, there are 9891 sources in the 3462-day area, including 2790 galactic sources, 2378 stellar sources and 4723 quasar sources. There are 3862 sources in the 3478 day area, including 1759 galactic sources, 577 stellar sources and 1526 quasar sources. FITS files are a commonly used data format in the astronomical community. By cross-matching the star list and FITS files in the local celestial region, we obtained images of 5 bands of u, g, r, i and z of 12499 galaxy sources, 16914 quasar sources and 16908 star sources as training and testing data.1.1 Image SynthesisSDSS photometric data includes photometric images of five bands u, g, r, i and z, and these photometric image data are respectively packaged in single-band format in FITS files. Images of different bands contain different information. Since the three bands g, r and i contain more feature information and less noise, Astronomical researchers typically use the g, r, and i bands corresponding to the R, G, and B channels of the image to synthesize photometric images. Generally, different bands cannot be directly synthesized. If three bands are directly synthesized, the image of different bands may not be aligned. Therefore, this paper adopts the RGB multi-band image synthesis software written by He Zhendong et al. to synthesize images in g, r and i bands. This method effectively avoids the problem that images in different bands cannot be aligned. The pixel of each photometry image in this paper is 2048×1489.1.2 Data tailoringThis paper first clipped the target image, image clipping can use image segmentation tools to solve this problem, this paper uses Python to achieve this process. In the process of clipping, we convert the right ascension and declination of the source in the star list into pixel coordinates on the photometric image through the coordinate conversion formula, and determine the specific position of the source through the pixel coordinates. The coordinates are regarded as the center point and clipping is carried out in the form of a rectangular box. We found that the input image size affects the experimental results. Therefore, according to the target size of the source, we selected three different cutting sizes, 40×40, 60×60 and 80×80 respectively. Through experiment and analysis, we find that convolutional neural network has better learning ability and higher accuracy for data with small image size. In the end, we chose to divide the surface source galaxies, point source quasars, and stars into 40×40 sizes.1.3 Division of training and test dataIn order to make the algorithm have more accurate recognition performance, we need enough image samples. The selection of training set, verification set and test set is an important factor affecting the final recognition accuracy. In this paper, the training set, verification set and test set are set according to the ratio of 8:1:1. The purpose of verification set is used to revise the algorithm, and the purpose of test set is used to evaluate the generalization ability of the final algorithm. Table 1 shows the specific data partitioning information. The total sample size is 34,000 source images, including 11543 galaxy sources, 11967 star sources, and 10490 quasar sources.1.4 Data preprocessingIn this experiment, the training set and test set can be used as the training and test input of the algorithm after data preprocessing. The data quantity and quality largely determine the recognition performance of the algorithm. The pre-processing of the training set and the test set are different. In the training set, we first perform vertical flip, horizontal flip and scale on the cropped image to enrich the data samples and enhance the generalization ability of the algorithm. Since the features in the celestial object source have the flip invariability, the labels of galaxies, stars and quasars will not change after rotation. In the test set, our preprocessing process is relatively simple compared with the training set. We carry out simple scaling processing on the input image and test input the obtained image.

The Washington Double Star Catalog (WDS), maintained by the United States Naval Observatory (USNO), is the world's principal database of astrometric double and multiple star information. The WDS Catalog contains positions, discoverer designations, epochs, position angles, separations, magnitudes, spectral types, proper motions and when available, Durchmusterung numbers and notes for the components of close to 100,000 systems based on ~600,000 means. The current version at the HEASARC is updated weekly and is derived from the version available online at https://crf.usno.navy.mil/wds/ (and mirrored at http://www.astro.gsu.edu/wds/), the latter being potentially updated nightly. The Washington Visual Double Star Catalog (WDS) is the successor to the Index Catalogue of Visual Double Stars, 1961.0 (IDS; Jeffers & van den Bos, 1963). Three earlier double star catalogs in the 20th century, those by Burnham (BDS; 1906), Innes (SDS; 1927), and Aitken (ADS; 1932), each covered only a portion of the sky. Both the IDS and the WDS cover the entire sky, and the WDS is intended to contain all known visual double stars for which at least one differential measure has been published. The WDS is continually updated as published data become available. Prior to this, two major updates have been published (Worley & Douglass 1984, 1997). The Washington Double Star Catalog (WDS) has seen numerous changes since the last major release of the catalog. The application of many techniques and considerable industry over the past few years has yielded unprecedented gains in both the number of systems and the number of measures. This version of the WDS catalog was first created at the HEASARC in March 2002 based on the USNO online version (available at either https://crf.usno.navy.mil/wds/ or http://www.astro.gsu.edu/wds/), and is updated by the HEASARC on at least a weekly basis. The table schema was last revised in February 2005. This is a service provided by NASA HEASARC .

The GSC-I catalog is an all-sky catalog of positions and magnitudes for approximately 19 million stars and other objects in the sixth to fifteenth magnitude range. The GSC is primarily based on an all-sky, single-epoch collection of Schmidt plates. For centers at +6 degrees and north, a 1982 epoch "Quick V" survey was obtained from the Palomar Observatory, while for southern fields, materials from the UK SERC J survey (epoch = 1975) and its equatorial extension (epoch = 1982) were used.