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J/A+AS/136/95       V380 Ori emission line spectrum         (Rossi+ 1999)
On the nature of the Herbig Be star V380 Orionis
       Rossi C., Errico L., Friedjung M., Giovannelli F., Muratorio G.,
       Viotti R., Vittone A.
      <Astron. Astrophys. Suppl. Ser. 136, 95 (1999)>
      =1999A&AS..136...95R
ADC_Keywords: Stars, Be ; Spectroscopy ; Equivalent widths

Keywords: stars: emission line, Be - stars: individual: V380 Ori -
          stars: pre-main sequence - infrared: stars - ultraviolet: stars

Description:
    Table 3 presents the emission line spectrum of V380 Ori in the optical
    region observed at OHP in January 1995 with a mean resolution of
    10000. For the line blends the wavelength and flux (not reddening
    corrected) of each contributor are given. For the P-Cygni profiles the
    equivalent widths of the absorption component are also reported. We
    estimate an error of less than 10% for the strongest lines, 10% to 40%
    for the weakest lines.
Objects:
    ----------------------------------------------------------
       RA   (2000)   DE      Designation(s)
    ----------------------------------------------------------
    05 36 25.3   -06 42 57   V380 Ori
    ----------------------------------------------------------

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table3.dat        61      212  *The emission line spectrum of V380 Ori in
                                  January 1995 (OHP/AURELIE)
table3.tex        74      497   LaTeX version of table3
table3.ps         72      607   PostScript version of table3

Note on table3.dat: The hydrogen Balmer lines are not included in this table.



Byte-by-byte Description of file: table3.dat

   Bytes Format  Units          Label     Explanations

   1-  2  A2     ---            LineID    Identifier for successive lines (1)
       3  I1     ---            n_LineID  ? [1/6] Rank of the line (2)
   5- 11  F7.2   0.1nm         LambdaObs  Observed heliocentric wavelength
  13- 17  F5.2   10-13mW/m2/nm  Flux      ? Integrated emission line flux
  19- 23  F5.2   0.1nm          EW        ? Absorption line equivalent width
                                             (Negative values)
  25- 32  F8.3   0.1nm         LambdaLab  ? Laboratory wavelength
  34- 39  A6     ---            Ion       Ion of the contributor
  41- 43  A3     ---            n_Ion     Moore's multiplet number or
                                           Kurucz table (k)
  45- 48  I4     km/s           HRV       ? Heliocentric radial velocity
  50- 61  A12    ---            Rem       Remarks (3)

Note (1): When successive lines, they are preceded with the same identifier in
           the first column (from a to bh).
Note (2): For a set of lines, same n_LambdaObs, rank of the line.

Note (3): p: principal component
          b: blue shifted component
        pcy: P Cygni absorption component
         ca: narrow central/shell absorption
         is: interstellar absorption line
      contr: minor contributor to the line
        id?: uncertain identification


Acknowledgements: Corinne Rossi 

(End)                                         Patricia Bauer [CDS]   11-Jan-1999