2009/05/15 by Paula S. Teixeira, P. S. Teixeira, Charles J. Lada +6
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Debris #Debris disk #Galaxy #Infrared #Physics #Planetary system #Spectral energy distribution #Spectral line #Spectrograph #Stars #Stellar, planetary, and galactic studies #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/700/1/454
published as Astrophys.J.700:454-459,2009 · Accepted for publication in ApJ. The paper has 19 pages, 4 figures, and one table
arxiv created 2009/05/15 · openalex publication_date 2009/07/02 · arxiv updated 2014/11/18 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present 5 to 15 μm 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 ∼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 s , and Spitzer InfraRed Array Camera and 24 μm 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 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.