Dust, Ice and Gas in Time (DIGIT) Herschel program first results: A full PACS-SED scan of the gas line emission in protostar DK Cha

DK Cha is an intermediate-mass star in transition from an embedded configuration to a star plus disk stage. We aim to study the composition and energetics of the circumstellar material during this pivotal stage. Using the Range Scan mode of PACS on the Herschel Space Observatory, we obtained a spect...

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Bibliographic Details
Published in:arXiv.org 2010-05
Main Authors: van Kempen, T A, Green, J D, Evans, N J, van Dishoeck, E F, Kristensen, L E, Herczeg, G J, Merin, B, J -E Lee, Joergensen, J K J, Bouwman, J, Acke, B, Adamkovics, M, Augereau, J C, Bergin, E, Blake, G A, Brown, J M, Carr, J S, J -H Chen, Cieza, L, Dominik, C, Dullemond, C P, Dunham, M M, Glassgold, A, Güdel, M, Harvey, P M, Henning, Th, Hogerheijde, M R, Jaffe, D, Kim, H J, Knez, C, Lacy, J H, Maret, S, Meeus, G, Meijerink, R, Mulders, G D, Mundy, L, Najita, J, Olofsson, J, Pontoppidan, K M, Salyk, C, Sturm, B, Visser, R, L B F M Waters, Waelkens, C, Yıldız, U A
Format: Article
Language:English
Subjects:
Continuum radiation
Deposition
Emission
Far infrared radiation
Outflow
Space telescopes
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Summary:DK Cha is an intermediate-mass star in transition from an embedded configuration to a star plus disk stage. We aim to study the composition and energetics of the circumstellar material during this pivotal stage. Using the Range Scan mode of PACS on the Herschel Space Observatory, we obtained a spectrum of DK Cha from 55 to 210 micron as part of the DIGIT Key Program. Almost 50 molecular and atomic lines were detected, many more than the 7 lines detected in ISO-LWS. Nearly the entire ladder of CO from J=14-13 to 38-37 (E_u/k = 4080 K), water from levels as excited as E_u/k = 843 K, and OH lines up to E_u/k = 290 K were detected. The continuum emission in our PACS SED scan matches the flux expected from a model consisting of a star, a surrounding disk of 0.03 Solar mass, and an envelope of a similar mass, supporting the suggestion that the object is emerging from its main accretion stage. Molecular, atomic, and ionic emission lines in the far-infrared reveal the outflow's influence on the envelope. The inferred hot gas can be photon-heated, but some emission could be due to C-shocks in the walls of the outflow cavity.
ISSN:2331-8422
DOI:10.48550/arxiv.1005.2548