IRAC and MIPS Observations of IC 1805

Details IRAC and MIPS Observations of IC 1805 IRAC and MIPS Observations of IC 1805

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop20052w&link_type=abstract

Spitzer Proposal ID #20052

Physics

Scientific paper

To date, solar-type stars (M < 1 Msun) have been a main focus of Spitzer observations aimed at understanding the initial phases of disk evolution - as disks transition from the accretion phase (3-10 Myr) to the very early debris disk phase (10-30 Myr). By comparison, disks in comparable evolutionary phases surrounding intermediate mass stars have received only modest attention. Because accretion disks (ADs) are more massive (5-10x) and shorter-lived (~10x) among stars with M > 2 Msun, the initial conditions (timescale, surface density) for planet formation should be significantly different. How do these differences manifest themselves as disks surrounding these stars evolve from the AD to early debris disk phases? Could short AD lifetimes inhibit giant planet formation via core accretion? Or might giant planets form quickly via gravitational instability, and produce relatively high optical depth disks with large holes interior to the planet? We propose an IRAC and MIPS study of the young (1-3 Myr) cluster IC 1805. This region contains one of the richest known (N~400) populations of 2-8 Msun young stars - a sample large enough to track the early evolution of disks. Our goals are to (a) determine the fraction of stars as a function of time and mass having IR SEDs consistent with optically thick ADs to provide thereby robust estimates of AD lifetimes as a function of mass for 2-8 Msun stars; (b) use IRAC colors and MIPS-24 measurements to (i) diagnose the fraction of flared and flat ADs and thus constrain dust settling timescales; (ii) search for 'transition disks' which lack evidence for small grains in their inner disk but have robust 24 um excesses indicative of a significant grain population beyond several AU; (c) use the 3.6-24 um SEDs to constrain the radial distribution of dust among a potentially large sample of debris disks and to provide insight into the physical processes that sculpt the solid matter distribution.

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