Time-dependent spectral-feature variations of stars displaying the B[e] phenomenon - II. MWC 342

Free Access

Issue		A&A Volume 554, June 2013


Article Number		A143
Number of page(s)		26
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201117437
Published online		18 June 2013

Online material

	Fig. 1 Line identification of MWC 342. Two diffuse interstellar bands (DIB) identified by MC99 was also seen.
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	Fig. 5 Relative flux of the Hα red peak.
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	Fig. 6 Relative flux of the Hα violet peak (asterisks). The circles denote the value for the bump, if it is present.
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	Fig. 11 Hα width at the relative height 0.1 (0 – continuum; 1 – Hα line intensity). The error bars are in the size of the symbols.
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	Fig. 13 Radial velocity of the Hα line centre in the wings.
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	Fig. 14 Variations of He i 6678 Å line profile during three nights in July 2005, April 2007, and two nights in September 2009.
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	Fig. 18 Equivalent width of metal lines.
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	Fig. 20 Radial velocity of [O i]. The line at λ = 6300 Å (upper panel) and 6364 Å (bottom panel).
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	Fig. 22 All the spectra from the Hα region. The spectrum showing the inverse P Cygni profile of the He i 6678 Å is displayed by the green line. The details of the Hα wings and He i 6678 Å are shown on the top of the figure.
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	Fig. 24 Ratio of the equivalent width of metal lines and equivalent width of Hα.
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Appendix A: List of observations and table of measurements.

Table A.1

List of observations and measured values of the Hα line.

Table A.2

List of observations and measured values of equivalent width of iron lines.

Table A.3

List of observations and measured values of oxygen and silicon lines.

© ESO, 2013

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