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. =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 60 212 *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