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J/A+AS/107/385      UV-excess objects Spacelab-1 survey IV.       (Tobin+, 1994)
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The Spacelab-1 Very Wide Field Survey of UV-excess objects. IV. The performance
of the instrument in combination with optical photometry as a means of
identifying stars with peculiar properties
       Tobin W., Viton M., Sivan J.-P.
      <Astron. Astrophys. Suppl. Ser. 107, 385 (1994)>
      =1994A&AS..107..385T      (SIMBAD/NED Reference)
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ADC_Keywords: Surveys; Ultraviolet; Photometry, ultraviolet; Stars, blue
Keywords: stars: fundamental parameters - Galaxy: stellar content -
          ultraviolet: stars - survey

Abstract:
   UV (195 nm) and Stroemgren uvby photometry of a 110 square degree field at 
   high southern galactic latitudes are analyzed through a comparison of i) 
   UV magnitudes for 57 stars of various types common to the published TD1 
   catalogue and the Very Wide Field Camera (VWFC); and ii) observed and 
   theoretical two-colour diagrams. The higher sensitivity of the VWFC 
   (=~0.5magnitude) and its more complete survey are exemplified by the 
   detection and UV measurement of a series of objects with moderate UV-excess
   in addition to detection of some very blue objects of various nature down 
   to fainter than 12th magnitude in the optical domain. A deeper survey with 
   a VWFC-type instrument could provide a complete sample for studies of the 
   group properties of faint blue stars. During the uvby reductions it was 
   found that the usual procedure of plotting residuals as functions of 
   declination, hour angle and airmass can be a powerful and diagnostic test 
   of photometer rigidity.

File Summary:
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 FileName    Lrecl    Records    Explanations
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ReadMe          80          .    This file
table1         131        109    Ultraviolet and Vuvby photometry for the
                                  completely-surveyed region indicated in Fig. 2
table1.tex      80        233    LaTeX version of table1
table4          93        139    Vuvby photometry for other stars
table4.tex      80        227    LaTeX version of table4
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Byte-by-byte Description of file: table1 table4
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   Bytes Format  Units   Label    Explanations
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   3-  6  A4     ---     WT       WT number
   8- 18  A11    ---     Name     Star name
  20- 24  F5.2   ---     y/V      []? Johnson V magnitude obtained by
                                      transformation of observations obtained
                                      with the Stroemgren y filter
      25  A1     ---   u_y/V      Uncertainty flag on y/V
  27- 31  F5.3   ---   e_y/V      []? Internal error on y/V (1)
  34- 39  F6.3   mag     (b-y)    []? (b-y) colour
  41- 45  F5.3   mag   e_(b-y)    []? Internal error on (b-y) (1)
  47- 52  F6.3   mag     m1       []? m1 colour index
  54- 58  F5.3   mag   e_m1       []? Internal error on m1 (1)
  60- 65  F6.3   mag     c1       []? c1 colour index
  67- 71  F5.3   mag   e_c1       []? Internal error on c1 (1)
  73- 74  I2     ---     nObs     []? Number of observations
  77- 80  F4.2   mag     m195     []? UV (195 nm) magnitude
  82- 85  F4.2   mag   e_m195     []? rms uncertainty on m195 (2)
      86  A1     --- n_e_m195     Note on e_m195 (3)
  90-149  A60    ---     Com.     Comments (3)
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Note (1): Single-star internal errors are reported for those stars for which any
           Stroemgren index exceeds 2.5 times the appropriate mean uncertainty
           reported in Table II
Note (2): The error given to m_195_ magnitudes is twice the one derived by the
           CAPELLA software, see Viton et al (1991)
Note (3): a uncertain error bar
          b VWFC image elongated, both HD 204779 and 204763 may contribute
          c CORAVEL data indicate possibly variable velocity
          d CORAVEL data indicate variable velocity
          e UV detection in fact due to WT026bis (Fig. 3, V=~12.5) which
             preliminary spectroscopy and CCD photometry has shown is a sdO
             star probably in binary association with a cooler companion
          f SAO 227683 excluded
          g SAO 227683 included
          h photometric and spectroscopic variable, suspected EB
            (see Prevot et al., 1993)
          + see Fig. 3 for finding .chart
          * see Viton et al. (1991)
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(End)                                           Patricia Bauer [CDS] 25-May-1994