Spitzer Observations of a Newly-Discovered Nearly Edge-On Disk About HD 32297

Details Spitzer Observations of a Newly-Discovered Nearly Edge-On Disk About HD 32297 Spitzer Observations of a Newly-Discovered Nearly Edge-On Disk About HD 32297

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop..255s&link_type=abstract

Spitzer Proposal ID #255

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We request 1.1 hours of Spitzer Director's Discretionary time to obtain IRAC and MIPS imaging photometry and IRS low resolution spectroscopy of a newly discovered, nearly edge-on, debris disk around HD 32297. The disk, discovered in our currently executing HST/NICMOS GO 10177 coronagraphic survey program, extends at least 3.3" (400 AU) from the star along its major axis and has a 1.1 micron flux density of F(1.1 micron) = 4.81 +/- 0.57 mJy beyond 0.3". Although providing crucial information on the disk morphology and dust scattering efficiency, our scattered light image cannot unambiguously inform on the physical properties of the dust in this potentially planet-forming environment. Thermal emission from the disk was detected at 25 + 60 microns with IRAS, but these measures alone permit only a very rudimentary thermal model of the system, leaving many degeneracies that allow a large range of particle sizes and disk masses. No other IR photometry is available, and indeed this object has been largely ignored in the past at all wavelengths. To further elucidate the physical characteristics of the disk and its constituent grains, we propose to obtain photometry and spectra from 3.6 - 160 microns with the Spitzer Space Telescope. This will allow us to develop a well-sampled spectral energy distribution (SED) for both the star and the disk emission, including mid-IR spectral coverage sufficient to characterize mineralogical features that will place strong constraints on the dust constituents. In addition, the large angular extent of the disk makes it one of the few known systems that can be spatially resolved in thermal emission with Spitzer (at wavelengths < 24 micron). Given the 1.1 microns scattering fraction of f(disk)/f(star) = 0.33% (from our NICMOS observations), an IRAS F(60 micron) = 1.12 Jy, and a 25 + 60 microns fractional dust emission excess luminosity of L(ir)/L(star) ~ 0.27%, this object is easy to observe with Spitzer and will consume minimal resources. As one of only a small handful of disks resolved i

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