Search

Start Over Subject star
1. Allard, COND 2000
ID:
ivo://svo.cab/models/cond00
Title:
Allard, COND 2000
Short Name:
COND00
Date:
04 Sep 2019 08:27:24
Publisher:
SVO CAB
Description:
The COND00 Model grid of theoretical spectra (Lyon group)
2. Allard, DUSTY 2000
ID:
ivo://svo.cab/models/dusty00
Title:
Allard, DUSTY 2000
Short Name:
DUSTY00
Date:
04 Sep 2019 08:28:21
Publisher:
SVO CAB
Description:
The DUSTY00 Model grid of theoretical spectra (Lyon group)
3. Astrographic Catalog of Reference Stars
ID:
ivo://nasa.heasarc/acrs
Title:
Astrographic Catalog of Reference Stars
Short Name:
ACRS
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
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 .
4. ATMO 2020, CEQ
ID:
ivo://svo.cab/models/atmo2020/ceq
Title:
ATMO 2020, CEQ
Short Name:
ATMO-CEQ
Date:
27 Sep 2022 00:50:15
Publisher:
SVO CAB
Description:
A set of atmosphere models for cool T-Y brown dwarfs and giant exoplanets. Equilibrium chemistry. Valid temperature range: 200-2000K. Only for solar metallicity.
5. ATMO 2020, NEQ strong
ID:
ivo://svo.cab/models/atmo2020/neq_strong
Title:
ATMO 2020, NEQ strong
Short Name:
ATMO-NEQs
Date:
27 Sep 2022 13:17:57
Publisher:
SVO CAB
Description:
A set of atmosphere models for cool T-Y brown dwarfs and giant exoplanets. Non equilibrium chemistry (strong). Valid temperature range: 200-2000K. Only for solar metallicity.
6. ATMO 2020, NEQ weak
ID:
ivo://svo.cab/models/atmo2020/neq_weak
Title:
ATMO 2020, NEQ weak
Short Name:
ATMO-NEQw
Date:
27 Sep 2022 13:18:30
Publisher:
SVO CAB
Description:
A set of atmosphere models for cool T-Y brown dwarfs and giant exoplanets. Non equilibrium chemistry (weak). Valid temperature range: 200-2000K. Only for solar metallicity.
7. Be Stars Catalog
ID:
ivo://nasa.heasarc/bestars
Title:
Be Stars Catalog
Short Name:
Be
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
The BESTARS database tables contains a compilation of data concerning stars of type Be. For the purposes of this compilation, a Be star is defined as a non-supergiant B star which showed emission in one Balmer line at least once. Stars without published MK spectral types have been excluded, except for 132 stars from Bidelman and MacConnell (1973), who used the above definition but included no spectral types. There are 1,159 stars included in this list. This is a service provided by NASA HEASARC .
8. Black Body
ID:
ivo://svo.cab/models/bbody
Title:
Black Body
Short Name:
Black Body
Date:
04 Sep 2019 08:31:00
Publisher:
SVO CAB
Description:
Black Body flux. Teff from 10 to 200000 K
9. Bright Star Catalog
ID:
ivo://nasa.heasarc/bsc5p
Title:
Bright Star Catalog
Short Name:
BSC
Date:
10 May 2024
Publisher:
NASA/GSFC HEASARC
Description:
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 .
10. BT-COND
ID:
ivo://svo.cab/models/bt-cond
Title:
BT-COND
Short Name:
BT-COND
Date:
04 Sep 2019 08:31:00
Publisher:
SVO CAB
Description:
The BT-COND Model grid of theoretical spectra. Brown dwarfs/extrasolar planets atmosphere models without irradiation and no dust opacity (no dust settling) but updated abundances. Wavelengths have been converted to air wavelengths.