J/A+AS/131/469 MWC 314 spectroscopy (Miroshnichenko+ 1998)
High resolution spectroscopy of the galactic candidate LBV MWC 314
Miroshnichenko A.S., Fremat Y., Houziaux L., Andrillat Y., Chentsov E.L.,
Klochkova V.G.
<Astron. Astrophys. Suppl. Ser. 131, 469 (1998)>
=1998A&AS..131..469M 1998A&AS..131..469M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, emission ; Equivalent widths ; Radial velocities ;
Spectroscopy
Keywords: stars: early-type; supergiants; abundances - stars: mass loss -
stars: individual: MWC 314
Abstract:
The results of high-resolution optical spectroscopy obtained for a
recently suggested LBV (luminous blue variable) candidate, MWC 314,
are presented. Photospheric lines mostly of N II and S II have been
found for the first time with a resolution of 0.4-0.8Å. They imply
a N/O overabundance previously reported for AG and HR Car since no O
II absorptions were detected. Nearly 400 emission lines have been
identified in the spectrum between 4190 and 8864Å many of which
appear double-peaked. No significant P Cygni type absorption
components have been found for the optically thick Balmer lines. This
suggests that the stellar wind of MWC 314 is non-spherical and the
circumstellar envelope is viewed not edge on. The systemic velocity
measured using the emission lines of ionized metals turned out to be
55km/s, which corresponds to a distance towards the object of
3.0±0.2kpc, according to the galactic rotation curve. Our analysis
of the characteristics of both photospheric and wind lines resulted in
an estimate of the object's Teff of nearly 25000K, which, however,
needs further improvement. The other stellar parameters were found to
be as follows:
Log(Lbol/L☉)=6.1±0.3, Rstar=60+30=10R☉.
Our study confirms that MWC 314 is one of the most luminous stars in
the Milky Way.
Objects:
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RA (2000) DE Designation(s)
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19 21 34.4 +14 52 52 MWC 314 = BD+14 3887
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 80 408 Emission lines identified in MWC 314 optical spectrum
table2.dat 35 63 Absorption lines identified in MWC 314 optical spectrum
table3.dat 28 60 Diffuse interstellar absorption features identified
tables.ps 72 1195 PostScript version of the tables
tables.tex 93 695 LaTeX version of the tables
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 0.1nm LambdaObs Observed wavelength
8 A1 --- n_LambdaObs [*:] Note on lines (1)
10- 36 A27 --- Ident Line identifications (2)
38- 42 F5.2 --- IPeak ? Peak Intensity for spectrum normalized
at the continuum
43 A1 --- u_IPeak Uncertainty flag on IPeak (3)
45 A1 --- l_EW Limit flag on EW
46- 51 F6.2 0.1nm EW ? Equivalent width
52 A1 --- u_EW Uncertainty flag on EW
53- 57 A5 --- n_EW Note on EW (4)
59- 60 I2 km/s RV ? Radial velocity
61 A1 --- u_RV Uncertainty flag on RV (3)
63 A1 --- l_IFlux Limit flag on IFlux
64- 72 F9.2 10-16mW/m2 IFlux ? Integrated flux
73- 79 A7 --- n_IFlux Note on IFlux (4)
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Note (1): *: double peaked lines for which wavelengths of their central
depressions are given.
Note (2): tellur: line is in a telluric region
J stands for the lines from the Johansson (1978PhS....18..217J 1978PhS....18..217J) list.
The lines with uncertain identification are marked with question mark.
Note (3): Weak lines measured with low accuracy are marked by colons.
Note (4): "p" refers to the preceding line,
"f" to the following line in a blend.
In these cases, equivalent width for the entire blend is given
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 0.1nm LambdaObs Observed wavelength
9- 18 A10 --- Ident Line identifications
20- 23 F4.2 --- IPeak ? Peak intensity for spectrum normalized at
the continuum
24 A1 --- u_IPeak Uncertainty flag on IPeak (1)
25 A1 --- l_EW Limit flag on EW
26- 29 F4.2 0.1nm EW ? Equivalent width
30- 31 A2 --- n_EW Note on EW (2)
33- 34 I2 km/s RV ? Radial velocity
35 A1 --- u_RV Uncertainty flag on RV (1)
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Note (1): Weak lines measured with low accuracy are marked by colons.
Note (2): "f" to the following line in a blend, in this case, equivalent width
for the entire blend is given
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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- 7 F7.2 0.1nm LambdaObs Observed wavelength
8 A1 --- n_LambdaObs [a] a: Na I
10- 13 F4.2 --- IPeak Peak Intensity for spectrum normalized
at the continuum
14 A1 --- u_IPeak Uncertainty flag on IPeak (1)
16 A1 --- l_EW Limit flag on EW
17- 20 F4.2 0.1nm EW ? Equivalent width
21 A1 --- u_EW Uncertainty flag on EW (1)
22- 23 A2 --- n_EW Note on EW (2)
25- 27 I3 km/s RV ? Radial velocity
28 A1 --- u_RV Uncertainty flag on EW (1)
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Note (1): Weak lines measured with low accuracy are marked by colons.
Note (2): "f" to the following line in a blend. In this case, equivalent width
for the entire blend is given
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Table 4: Unidentified lines in the optical spectrum MWC 314
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LambdaObs Identifications Peak intensity Equivalent width
0.1nm 0.1nm
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4675.69 1.13 0.10
5328.50 Fe I (15) 1.12
5397.83 Fe I (15) 1.07
5587.00 Fe I (686) 1.07
8514.60 1.07 0.31
8914.20 1.19 1.08
8927.40 1.73 2.45
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Acknowledgements: Yves Fremat
(End) Patricia Bauer [CDS] 03-Sep-1998