V/14               Estimated astrophysical parameters from uvby   (Philip+ 1980)

uvby estimated astrophysical parameters Philip A.G.D., Egret D. <Astron. Astrophys. Suppl. Ser. 40, 199 (1980)> =1980A&AS...40..199P 1980A&AS...40..199P
ADC_Keywords: Photometry, uvby, beta ; Effective temperatures ; Keywords: Four-color photometry ; Early-type stars ; Astrophysical parameters Description: Observed values of the Stroemgren uvby colors were collected from the literature. A computer program calculated the reddening for each star. This value was used to compute the unreddened value of (b-v), c1, and m1. These were then used to compute [c(1)], [m(1)], and [u-b] for the star. Except for the H beta index, the observed quantities are not included. Introduction: The stars were divided into groups by spectral types by means of the bracket quantities. Stars which deviated too greatly from the standard relations could not be dereddened. These include peculiar stars and high luminosity stars and are listed in reject.dat. Various discussions by Crawford were followed to deredden the other stars. The zero point of the [Fe/H] relation was changed from 0.4 to 0.2 on the basis of the study by Gustafsson and Nissen (1972A&A....19..261G 1972A&A....19..261G) and some corrections were made to the effective temperature scale in order to fit the new model by Kurucz (1979ApJS...40....1K 1979ApJS...40....1K). Otherwise, the derivations followed the methods of Philip, Miller, and Relyea (1976, Dudley Obs. Rep. No. 12, 1). File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file catalog.dat 131 9054 Estimated astrophysical parameter data codes.txt 80 1079 Description of the LID designation scheme -------------------------------------------------------------------------------- See also: II/57 : A Catalog of uvby Measurements (Hauck+ 1980) III/42 : Selected MK Spectral Types (Jaschek, 1978) Byte-per-byte Description of file: catalog.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 3- 12 A10 --- LID *Designation of the star (see "codes.txt" file) 13 A1 --- m_LID [1234DV] Multiplicity, variability or duplicity 15- 20 F6.3 mag (b-y)0 Dereddened Stroemgren index (b-y) 22- 27 F6.3 mag (c1)0 Dereddened Stroemgren index c1 = (u-v)-(v-b) 29- 34 F6.3 mag (m1)0 Dereddened Stroemgren index m1 = (v-b)-(b-y) 36- 41 F6.3 mag Hbeta ? Dereddened Stroemgren Hβ index 43- 48 F6.3 mag [c1] Extinction-independent Stroemgren index 50- 55 F6.3 mag [m1] Extinction-independent Stroemgren index 57- 62 F6.3 mag [u-b] Extinction-independent Stroemgren index 64- 69 F6.3 mag E(b-y) Derived color excess in (b-y) 71- 76 F6.3 mag dm1 Deviation of dereddened m1 index from ZAMS 78- 83 F6.3 mag dc1 ? Deviation of dereddened c1 index from ZAMS 85- 87 A3 --- SpG *Spectral group: B, A*, A, F, AM, AP 89- 97 A9 --- MKsp *Spectral classification of the star 99-103 F5.2 mag Mv ? Estimated visual absolute magnitude 106-109 F4.2 --- theta ? Estimated effective temperature (5040/T) 111-114 F4.2 [cm/s2] log.g ? Estimated gravity 116-119 F4.2 [Sun] [Fe/H] ? Estimated metallicity (relative to solar) 121-131 A11 --- Refs Bibliographical references to original data -------------------------------------------------------------------------------- Note on LID: Lausanne/Geneve coding system, see a full description in the "codes.txt" Note on SpG: The spectral group is one of B, A*, A, F, AM, AP Note on MKsp: Selected MK Spectral Types classification by Jaschek M. (Cat. III/42) --------------------------------------------------------------------------------
(End) Francois Ochsenbein [CDS] 15-Dec-1993, rev. 06-Nov-2006
The document above follows the rules of the Standard Description for Astronomical Catalogues; from this documentation it is possible to generate f77 program to load files into arrays or line by line