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V/58        [Fe/H], Vel, Orbits, F2-K5 Dwarfs 80pc from Sun (Marsakov+ 1988)
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The Catalogue of Metallicities, Velocity Components and Orbital Parameters for
F2-K5 Dwarfs in the Vicinity of 80 pc from the Sun
    Marsakov V.A., Shevelev Yu.G.
    <CDS Inf. Bull., 35, 129 (1988)>
    1988BICDS..35..129M
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ADC_Keywords: Abundances, [Fe/H] ; Space velocities ; Stars, late-type

Description:
   In this catalog, metallicities, distances, components of space velocities 
   and parameters of osculating orbits are calculated for 1065 F2-K5 dwarfs 
   with UBV photometric data, proper motions and radial velocities.
                                     
   The present sample is composed on the base of the Ochsenbein (1980) 
   catalogue and contains the stars of the V (IV-V) luminosity class, within 
   the colour range 0.35<B-V<1.10 (which corresponds to the spectral class 
   range F2-K5). 

   Sandage's (1969) Hyades sequence was used to determine the value   
   delta (U-B) for each star. The authors calibrated the ultraviolet excess 
   in terms of FE/H! separately for the four of the temperature index (B-V) 
   where delta(U-B) practically does not depend on the effective temperature. 
   Intervals in (B-V) correspond to the following division on spectral 
   class intervals: F2-F9, G0-G4, and G5-G9, K0-K5. Metallicity is calculated 
   from the formulae:                      
                FE/H!=-5.3*delta(U-B)+0.02     for stars F2-F9                  
                FE/H!=-5.1*delta(U-B)+0.13     for stars G0-G4                  
                FE/H!=-5.4*delta(U-B)+0.02     for stars G5-G9                  
                FE/H!=-4.7*delta(U-B)-0.04     for stars K0-K5                  
   These relations follow from the assumption that mean metallicity and 
   metallicity dispersion for stars of all spectral classes are the same.     

   Distances to the stars were calculated from spectral parallaxes. Absolute 
   magnitudes (M(V)) were obtained from the Sp,M(V)-relation for dwarfs 
   (Straizys, 1982). The sample includes only stars nearer than 80 pc because  
   reddening is negligible for them. the obtained distances together with 
   radial velocities and proper motions are used to calculate the components 
   of space velocities. The eccentricities, apogalactic and perigalactic 
   distances of the stars were calculated from the osculating orbit 
   approximation according to the galaxy model from the paper by 
   Eggen et al. (1962).                                          
                

File Summary:
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 FileName       Lrecl  Records   Explanations
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ReadMe             80        .   This file
desc.doc           80       78   Author's documentation
catalog.dat       115     1065   Catalog file
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Byte-by-byte Description of file: catalog.dat
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   Bytes Format  Units   Label    Explanations
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   1-  6  I6     ---     HD       ?HD number            
   7- 13  F7.2   deg     GLON     Galactic longitude       
  15- 20  F6.2   deg     GLAT     Galactic latitude       
  21- 25  F5.2   mag     V        Brightness in V filter                    
  28- 33  F6.3   mag     B-V      B-V color index          
  35- 40  F6.3   mag     U-B      U-B color index                
  41- 54  A14    ---     Sp       Spectral type     
  56- 60  F5.1   pc      R        Heliocentric distance                   
  62- 67  F6.1   km/s    Uvel     Velocity vector component in the direction 
                                    of the anticenter of the Galaxy 
  69- 74  F6.1   km/s    Vvel     Velocity component in the direction 
                                    of Galactic rotation    
  76- 81  F6.1   km/s    Wvel     Velocity component towards the north 
                                    Galactic pole         
  84- 88  F5.1   kpc     R1       Apogalactic distance of the Galactic orbit
  91- 95  F5.1   kpc     R2       Perigalactic distance of the Galactic orbit
  98-102  F5.3   ---     e        Eccentricity of the Galactic orbit
 104-109  F6.3   mag     E(U-B)   Ultraviolet excess      
 111-115  F5.2   ---     FE/H!    Metallicity 
                                   (FE/H!=LG(FE/H)(star)-LG(FE/H)(sun)) 
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References:       
    Eggen O.J., Lynden-Bell D., Sandage A.: 1962, ApJ, 136, 748            
    Ochsenbein F.: 1980, CDS Inf. Bull., 19, 74         
    Sandage A.: 1969, ApJ, 258, 1115.                                      
    Straizys V.: 1982, "Metal-Deficient Stars", Vilnius: Mokslas,P.206      
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(End)                                 James E. Gass [SSDOO/ADC]   9-Sep-1997