Spectro-interferometry of the Be Star $ Sco: Near-infrared Continuum and Gas Emission Region Sizes in 2007

R. Millan-Gabet, J.~D. Monnier, Y. Touhami, D. Gies, E. Hesselbach, E. Pedretti, N. Thureau, M. Zhao, T. ten Brummelaar, CHARA Group

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13 Citations (Scopus)


We present near-infrared H- and K-band spectro-interferometric observations of the gaseous disk around the primary Be star in the ? Sco binary system, obtained in 2007 (between periastron passages in 2000 and 2011). Observations using the CHARA/MIRC instrument at H band resolve an elongated disk with a Gaussian FWHM 1.18 × 0.91 mas. Using the Keck Interferometer (KI), the source of the K-band continuum emission is only marginally spatially resolved, and consequently we estimate a relatively uncertain K-band continuum disk FWHM of 0.7 ? 0.3 mas. Line emission on the other hand, He I ?2.0583 ?m and Br? ?2.1657 ?m, is clearly detected, with ~10% lower visibilities than those of the continuum. When taking into account the continuum/line flux ratio this translates into much larger sizes for the line emission regions: 2.2 ? 0.4 mas and 1.9 ? 0.3 mas for He I and Br?, respectively. Our KI data also reveal a relatively flat spectral differential phase response, ruling out significant off-center emission. We expect that these new measurements will help constrain dynamical models being actively developed in order to explain the disk formation process in the ? Sco system and Be stars in general.
Original languageEnglish
Pages (from-to)544-549
Number of pages6
JournalAstrophysical Journal
Issue number1
Publication statusPublished - 12 Oct 2010


  • stars: emission-line, Be, stars: individual: $ Sco, techniques: high angular resolution


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