The VLTI/MIDI survey of massive young stellar objects - Sounding the inner regions around intermediate- and high-mass young stars using mid-infrared interferometry

Paul A. Boley; Hendrik Linz; Roy van Boekel; Thomas Henning; Markus Feldt; Lex Kaper; Christoph Leinert; André Müller; Ilaria Pascucci; Massimo Robberto; Bringfried Stecklum; L. B. F. M.  Waters; Hans Zinnecker

doi:10.1051/0004-6361/201321539

Home

All issues

Volume 558 (October 2013)

A&A, 558 (2013) A24

Online Material

Free Access

Issue		A&A Volume 558, October 2013


Article Number		A24
Number of page(s)		33
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201321539
Published online		27 September 2013

Online material

Appendix A: Online material

Table A.1

Observation log.

	Fig. A.1 Measured correlated flux spectra (solid black line and error bars) for AFGL 2136, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.2 Measured correlated flux spectra (solid black line and error bars) for AFGL 4176, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.3 Measured correlated flux spectra (solid black line and error bars) for G305.20+0.21, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.4 Measured correlated flux spectra (solid black line and error bars) for IRAS 13481-6124, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.5 Measured correlated flux spectra (solid black line and error bars) for IRAS 17216-3801, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.6 Measured correlated flux spectra (solid black line and error bars) for M8E-IR, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.7 Measured correlated flux spectra for M17 SW IRS1, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation.
Open with DEXTER

	Fig. A.8 Measured correlated flux spectra (solid black line and error bars) for M17 UC1, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.9 Measured correlated flux spectra (solid black line and error bars) for Mon R2 IRS2, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.10 Measured correlated flux spectra for Mon R2 IRS3 A, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points.
Open with DEXTER

	Fig. A.11 Measured correlated flux spectra (solid black line and error bars) for Mon R2 IRS3 B, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.12 Measured correlated flux spectra for MWC 300, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation.
Open with DEXTER

	Fig. A.13 Measured correlated flux spectra (solid black line and error bars) for NGC 2264 IRS1, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.14 Measured correlated flux spectra for R CrA, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation.
Open with DEXTER

	Fig. A.15 Measured correlated flux spectra (solid black line and error bars) for R Mon, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.16 Measured correlated flux spectra (solid black line and error bars) for S255 IRS3, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation. The dashed blue line shows a continuum fit to the red points, and the solid blue line shows the best fit to the absorption spectrum (see Sect. 4.3).
Open with DEXTER

	Fig. A.17 Measured correlated flux spectra for V921 Sco, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation.
Open with DEXTER

	Fig. A.18 Measured correlated flux spectra for V1028 Cen, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation.
Open with DEXTER

	Fig. A.19 Measured correlated flux spectra for VY Mon, in order of increasing projected baseline. The caption shows the projected baseline and position angle of each observation.
Open with DEXTER

© ESO, 2013

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.