Universität zu Köln

Okada, Yoko ORCID: 0000-0002-6838-6435, Guesten, Rolf, Requena-Torres, Miguel Angel, Roellig, Markus, Stutzki, Juergen, Graf, Urs Ulrich and Hughes, Annie (2019). Velocity profiles of [C-II], [C-I], CO, and [O-I] and physical conditions in four star-forming regions in the Large Magellanic Cloud. Astron. Astrophys., 621. LES ULIS CEDEX A: EDP SCIENCES S A. ISSN 1432-0746

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Abstract

Aims. The aim of our study is to investigate the physical properties of the star-forming interstellar medium (ISM) in the Large Magellanic Cloud (LMC) by separating the origin of the emission lines spatially and spectrally. The LMC provides a unique local template to bridge studies in the Galaxy and high redshift galaxies because of its low metallicity and proximity, enabling us to study the detailed physics of the ISM in spatially resolved individual star-forming regions. Following Okada et al. (Okada, Y., Requena-Torres, M. A., Gusten, R., et al. 2015, A&A, 580, A54), we investigate different phases of the ISM traced by carbon-bearing species in four star-forming regions in the LMC, and model the physical properties using the KOSMA-tau PDR model. Methods. We mapped 3-13 arcmin(2) areas in 30 Dor, N158, N160, and N159 along the molecular ridge of the LMC in [C II] 158 mu m with GREAT on board SOFIA. We also observed the same area with CO(2-1) to (6-5), (CO)-C-13(2-1) and (3-2), [C I] P-3(1)-P-3(0) and P-3(2)-P-3(1) with APEX. For selected positions in N159 and 30 Dor, we observed [O I] 145 mu m and [O I] 63 mu m with upGREAT. All spectra are velocity resolved. Results. In all four star-forming regions, the line profiles of CO, (CO)-C-13, and [C I] emission are similar, being reproduced by a combination of Gaussian profiles defined by CO(3-2), whereas [C II] typically shows wider line profiles or an additional velocity component. At several positions in N159 and 30 Dor, we observed the velocity-resolved [O I] 145 and 63 mu m lines for the first time. At some positions, the [O I] line profiles match those of CO, at other positions they are more similar to the [C II] profiles. We interpret the different line profiles of CO, [C II] and [O I] as contributions from spatially separated clouds and/or clouds in different physical phases, which give different line ratios depending on their physical properties. We modeled the emission from the CO, [C I], [C II], and [O I] lines and the far-infrared continuum emission using the latest KOSMA-tau PDR model, which treats the dust-related physics consistently and computes the dust continuum SED together with the line emission of the chemical species. We find that the line and continuum emissions are not well-reproduced by a single clump ensemble. Toward the CO peak at N159 W, we propose a scenario that the CO, [C II], and [O I] 63 mu m emission are weaker than expected because of mutual shielding among clumps.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Okada, Yoko UNSPECIFIED orcid.org/0000-0002-6838-6435 UNSPECIFIED Guesten, Rolf UNSPECIFIED UNSPECIFIED UNSPECIFIED Requena-Torres, Miguel Angel UNSPECIFIED UNSPECIFIED UNSPECIFIED Roellig, Markus UNSPECIFIED UNSPECIFIED UNSPECIFIED Stutzki, Juergen UNSPECIFIED UNSPECIFIED UNSPECIFIED Graf, Urs Ulrich UNSPECIFIED UNSPECIFIED UNSPECIFIED Hughes, Annie UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-159418
DOI:	10.1051/0004-6361/201833398
Journal or Publication Title:	Astron. Astrophys.
Volume:	621
Date:	2019
Publisher:	EDP SCIENCES S A
Place of Publication:	LES ULIS CEDEX A
ISSN:	1432-0746
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language COMPACT HII-REGIONS; N159/N160 COMPLEX; LINE EMISSION; SELF-ABSORPTION; 1ST DETECTION; 30 DORADUS; METALLICITY; SPITZER; CARBON; DENSE Multiple languages Astronomy & Astrophysics Multiple languages
Refereed:	Yes
URI:	http://kups.ub.uni-koeln.de/id/eprint/15941