Physical/chemical structure and kinematics of an extremely filamentary Infrared Dark Cloud

Details Physical/chemical structure and kinematics of an extremely filamentary Infrared Dark Cloud Physical/chemical structure and kinematics of an extremely filamentary Infrared Dark Cloud

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.194h&link_type=abstract

The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole

Astronomy and Astrophysics

Astronomy

Scientific paper

The study of Infrared Dark Clouds (IRDCs) holds great importance for understanding high-mass stars and stellar cluster formation. Early studies have shown IRDCs are typically cold (T<25K), dense (n(H_2) ˜ 10^5 cm-3, N(H_2) ˜ 1022 cm-2), and massive (10^2-10^5 M&sun;). Discovered in the 1990s during mid-IR mapping of the Galaxy with MSX and ISO, IRDCs were observed as high extinction features seen in silhouette against the diffuse mid-IR galactic background. Recent results from the Herschel Space Observatory have shown that IRDCs contain within them the very earliest stages of star formation. Here we focus on IRDC G035.39-00.33, selected because of its extremely filamentary morphology, extended quiescent regions with high mass surface density, and narrow line-widths. These properties all signify that this cloud is in the early stages of its formation. We present preliminary results on the comparison of high-density tracers such as N_2H^+ and N_2D^+ with low-density tracers such as C18O, in order to understand the kinematics, as well as the physical and chemical properties of the filament as a whole.

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