INFRARED SPECTROGRAPH CHARACTERIZATION OF A DEBRIS DISK AROUND AN M-TYPE STAR IN NGC 2547

Journal Article · Mon Jul 20 04:00:00 EDT 2009 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/700/1/454; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21313872

Teixeira, Paula S; Lada, Charles J ^[1]; Wood, Kenneth; Robitaille, Thomas P ^[2]

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1. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
2. School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS (United Kingdom)

We present 5 to 15 {mu}m Spitzer Infrared Spectrograph (IRS) low-resolution spectral data of a candidate debris disk around an M4.5 star identified as a likely member of the {approx}40 Myr old cluster NGC 2547. The IRS spectrum shows a silicate emission feature, indicating the presence of warm, small, (sub)micron-sized dust grains in the disk. Of the 15 previously known candidate debris disks around M-type stars, the one we discuss in this paper is the first to have an observed mid-infrared spectrum and is also the first to have measured silicate emission. We combined the IRS data with ancillary data (optical, JHK{sub s} , and Spitzer InfraRed Array Camera and 24 {mu}m data) to build the spectral energy distribution (SED) of the source. Monte Carlo radiation transfer modeling of the SED characterized the dust disk as being very flat (h {sub 100} = 2 AU) and extending inward within at least 0.13 AU of the central star. Our analysis shows that the disk is collisionally dominated and is likely a debris disk.

• OSTI ID: 21313872
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 700; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
DUSTS
EMISSION
ENERGY SPECTRA
INFRARED SPECTRA
MONTE CARLO METHOD
SILICATES
SIMULATION
STARS