UV processing of ices across the Rosette molecular cloud

Details UV processing of ices across the Rosette molecular cloud UV processing of ices across the Rosette molecular cloud

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50146k&link_type=abstract

Spitzer Proposal ID #50146

Physics

Scientific paper

During star-formation, materials in the general cloud medium are subjected to numerous chemical and physical processes that are driven mostly by thermal and energetic radiation. In part because of Spitzer, significant progress has been made towards understanding the various effects of these radiation processes on the ices and organics as they form and cycle through the dense and diffuse regions of molecular clouds and subsequently become incorporated into (proto)stellar environments (i.e planets, comets, etc.). However, to date the majority of the focus has been directed at clouds (such as Taurus-Auriga) that are NOT analogous to the molecular cloud from which the solar nebula originated. Rather, the Sun formed in a high mass star-forming cloud where a number of supernova events occurred, resulting in intense UV radiation throughout the cloud complex, such as the Rosette Nebula. We propose to take low resolution spectra from 5 to 22 microns along the line of sight toward 13 sources in 8 embedded clusters in the Rosette molecular cloud. The clusters are all deeply embedded, indicative of a similar formation time but have a range of luminosities and are spread out across the cloud at different distances from the neighboring HII region, NGC 2244. We will also take high resolution spectra from 10 to 20 microns toward the 5 brightest and most embedded sources to examine the CO_2 line profile in detail. This will allow us to determine the mixture of different ices and thereby the temperature and radiation processing history in each region. These observations will reveal how the ice composition in each cluster envelope varies with environment, both locally from the embedded sources and globally due to the heating and UV radiation from NGC 2244. Differences in gas phase chemistry have already been observed at millimeter wavelengths and we will use these mid-infrared data to obtain a more complete picture of the chemistry.

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