Identifying the cm-wave continuum emitters in rho Oph W.

Details Identifying the cm-wave continuum emitters in rho Oph W. Identifying the cm-wave continuum emitters in rho Oph W.

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009atnf.prop.2338c&link_type=abstract

ATNF proposal C1845, Semester: April, 2009

Physics

Galactic, Atca

Scientific paper

The young stars in the rho Oph molecular cloud are not hot enough to form a conspicuous HII region. Only faint radiation from the Rayleigh-Jeans tail of ~10-100K dust is expected at wavelengths longwards of ~3mm. Yet we have found with the Cosmic Background Imager (CBI, 6arcmin uniform beam) that the rho Oph W photo-dissociation region (PDR) is surprisingly bright at cm wavelengths. The centimetric emission mechanism probably involves spinning dust, or electric dipole radiation from spinning very small dust grains (VSGs). Spinning dust holds the promise of a new window on VSG and PDR physics. ATCA can resolve the cm-wave continuum in rho Oph W and provide the first well-sampled 6cm - 0.7cm radio spectra and images of PDRs. Models of VSG emission both at cm-waves and in the infrared will bring constraints on physical conditions in the solid and gas states.

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