Optical spectroscopic variability of Herbig Ae/Be stars

Free Access

Issue		A&A Volume 529, May 2011


Article Number		A34
Number of page(s)		43
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201015821
Published online		28 March 2011

Online material

Appendix A: Tables with multi-epoch line EWs and fluxes

Table A.1

Equivalent widths, Hα widths at 10% of peak intensity and Hα profile types on different observing Julian Dates.

Table A.2

Line fluxes on several observing Julian Dates for a subsample of the stars.

Appendix B: Mean spectra and relative variability distributions

Fig. B.1

For each star and observing campaign, the mean spectra and relative variability distributions are plotted on the left side. The HeI5876, NaID, [OI]6300 and Hα regions are enlarged on the right side, for a better visualization. The mean spectrum is given by I_i,k, and the relative variability by σ_k/I_rel,k, being σ_k = [(I_i,k − I_rel,k)²]^1/2. The subindex k refers to each spectral bin and the subindex i to each one of the N spectra per observing campaign. The relative variability plots provide information on the strength and wavelength position of the changes in the line intensity (Johns & Basri 1995).

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	Fig. B.2 Individual spectra taken within a time span of hours (i.e. during the same night) for the five objects monitored on this timescale.
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© ESO, 2011

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