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

doi:10.1088/0004-637X/723/1/544

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

School of Engineering & Physical Sciences

Research output: Contribution to journal › Article › peer-review

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Abstract

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 language	English
Pages (from-to)	544-549
Number of pages	6
Journal	Astrophysical Journal
Volume	723
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/723/1/544
Publication status	Published - 12 Oct 2010

Keywords

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

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10.1088/0004-637X/723/1/544

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@article{c560a81884a642eeba2d5538301dbe6a,

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

abstract = "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.",

keywords = "stars: emission-line, Be, stars: individual: $ Sco, techniques: high angular resolution",

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

year = "2010",

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doi = "10.1088/0004-637X/723/1/544",

language = "English",

volume = "723",

pages = "544--549",

journal = "Astrophysical Journal",

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TY - JOUR

T1 - Spectro-interferometry of the Be Star $ Sco: Near-infrared Continuum and Gas Emission Region Sizes in 2007

AU - Millan-Gabet, R.

AU - Monnier, J.~D.

AU - Touhami, Y.

AU - Gies, D.

AU - Hesselbach, E.

AU - Pedretti, E.

AU - Thureau, N.

AU - Zhao, M.

AU - ten Brummelaar, T.

AU - Group, CHARA

PY - 2010/10/12

Y1 - 2010/10/12

N2 - 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.

AB - 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.

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

U2 - 10.1088/0004-637X/723/1/544

DO - 10.1088/0004-637X/723/1/544

M3 - Article

SN - 0004-637X

VL - 723

SP - 544

EP - 549

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

ER -

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

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