J/A+AS/136/95 J/A+AS/136/95 V380 Ori emission line spectrum C Rossi L Errico M Friedjung F Giovannelli G Muratorio R Viotti A Vittone Astron. Astrophys. Suppl. Ser. 136 95 1999 1999A&AS..136...95R Equivalent widths Spectroscopy Stars, Be infrared: stars stars: emission-line, Be stars: individual (V380 Ori) stars: pre-main sequence ultraviolet: stars 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.

V380 Ori05 36 25.3-06 42 57

LineID Identifier for successive lines number=1 When successive lines, they are preceded with the same identifier in the first column (from a to bh). --- n_LineID [1/6] Rank of the line number=2 For a set of lines, same n_LambdaObs, rank of the line. --- LambdaObs Observed heliocentric wavelength 0.1nm Flux Integrated emission line flux 10-13mW/m2/nm EW Absorption line equivalent width (Negative values) 0.1nm LambdaLab Laboratory wavelength 0.1nm Ion Ion of the contributor --- n_Ion Moore's multiplet number or Kurucz table (k) --- HRV Heliocentric radial velocity km/s Rem Remarks number=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 --- table3.texLaTeX version of table3 table3.psPostScript version of table3 Patricia Bauer CDS 1999Jan11Corinne Rossi <ROSSIC@axrma.uniroma1.it> J_A+AS_136_95.xml