Accretion-related properties of Herbig Ae/Be stars - Comparison with T Tauris

I. Mendigutía; A. Mora; B. Montesinos; C. Eiroa; G. Meeus; B. Merín; R. D. Oudmaijer

doi:10.1051/0004-6361/201219110

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Volume 543 (July 2012)

A&A, 543 (2012) A59

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Issue		A&A Volume 543, July 2012


Article Number		A59
Number of page(s)		21
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201219110
Published online		27 June 2012

Online material

Appendix A: Tables with photometry and SEDs

Table A.1

Ultraviolet, optical and near-IR photometry.

Table A.2

Mid-infrared photometry.

Table A.3

Sub-mm and mm photometry for a sub-sample of stars.

	Fig. A.1 SEDs of the stars in the sample. Triangles are photometric upper limits. For each panel, the best fit is the black-solid line and the models fitting with are the grey-solid lines, where n is the number of datapoints per star (see Robitaille et al. 2007). The best stellar (de-redenned) photosphere is indicated with a dashed line.
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	Fig. A.1 continued.
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	Fig. A.1 continued.
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	Fig. A.1 continued.
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	Fig. A.1 continued.
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	Fig. A.2 Subsample of stars with fluxes available at λ ≥ 0.35 mm (log ν [GHz] ≤ 2.9, see Table A.3). The best graybody fits yielding the indicated values for t_D and β are shown. Fluxes at λ ≤ 2.0 mm (log ν [GHz] ≥ 2.1) are weighted stronger in the fits.
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	Fig. A.2 continued.
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© ESO, 2012

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