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 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:
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RA (2000) DE Designation(s)
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05 36 25.3 -06 42 57 V380 Ori
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File Summary:
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FileName Lrecl Records Explanations
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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
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Note on table3.dat: The hydrogen Balmer lines are not included in this table.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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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)
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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
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Acknowledgements: Corinne Rossi
(End) Patricia Bauer [CDS] 11-Jan-1999