160 micron Photometry of A star Power Laws

Details 160 micron Photometry of A star Power Laws 160 micron Photometry of A star Power Laws

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50302r&link_type=abstract

Spitzer Proposal ID #50302

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Scientific paper

We propose 160 um imaging for a sample of 4 planetary debris disks around main-sequence A stars, with MIPS 24 and 70 um excess, and for which the 5-35 um IRS data are best fit by power-laws of slopes ranging from 1.1 to 2.4. By extending our observations out to 160 um, we may find evidence for substantial reservoirs of colder material that considerably outweighs the warmer material seen shortward of 70 um. Other debris disks do not show evidence for such SEDs, nor for such large amounts of cold material. It is not clear whether this difference is due to the greater luminosity of the A stars, their higher mass and light/mass ratio, or their naturally younger ages, but we may be able to explore this interesting question. The result of these measurements will be an SED that extends over a factor of 10 in wavelength and as much as a factor of 100 in radial distance from the star. This broad range of spectral coverage can be used to test models of the structure and evolution of debris disks and their underlying planetary systems.

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