Universität zu Köln

Schneider, N., Roellig, M., Polehampton, E. T., Comeron, F., Djupvik, A. A., Makai, Z., Buchbender, C., Simon, R., Bontemps, S., Guesten, R., White, G., Okada, Y., Parikka, A. and Rothbart, N. (2021). Globules and pillars in Cygnus X III. Herschel and upGREAT/SOFIA far-infrared spectroscopy of the globule IRAS 20319+3958 in Cygnus X. Astron. Astrophys., 653. LES ULIS CEDEX A: EDP SCIENCES S A. ISSN 1432-0746

Full text not available from this repository.

Abstract

IRAS 20319+3958 in Cygnus X South is a rare example of a free-floating globule (mass similar to 240 M-circle dot, length similar to 1.5 pc) with an internal H II region created by the stellar feedback of embedded intermediate-mass stars, in particular, one Herbig Be star. In Schneider et al. 2012, (A&A, 542, L18) and Djupvik et al. 2017, (A&A, 599, A37), we proposed that the emission of the far-infrared (FIR) lines of [C II] at 158 mu m and [O I] at 145 mu m in the globule head are mostly due to an internal photodissociation region (PDR). Here, we present a Herschel/HIFI [C II] 158 mu m map of the whole globule and a large set of other FIR lines (mid-to high-J CO lines observed with Herschel/PACS and SPIRE, the [O I] 63 mu m line and the (CO)-C-12 16 -> 15 line observed with upGREAT on SOFIA), covering the globule head and partly a position in the tail. The [C II] map revealed that the whole globule is probably rotating. Highly collimated, high-velocity [C II] emission is detected close to the Herbig Be star. We performed a PDR analysis using the KOSMA-tau PDR code for one position in the head and one in the tail. The observed FIR lines in the head can be reproduced with a two-component model: an extended, non-clumpy outer PDR shell and a clumpy, dense, and thin inner PDR layer, representing the interface between the H II region cavity and the external PDR. The modelled internal UV field of similar to 2500 G(degrees) is similar to what we obtained from the Herschel FIR fluxes, but lower than what we estimated from the census of the embedded stars. External illumination from the similar to 30 pc distant Cyg OB2 cluster, producing an UV field of similar to 150-600 G(degrees) as an upper limit, is responsible for most of the [C II] emission. For the tail, we modelled the emission with a non-clumpy component, exposed to a UV-field of around 140 G(degrees).

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Schneider, N. UNSPECIFIED UNSPECIFIED UNSPECIFIED Roellig, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Polehampton, E. T. UNSPECIFIED UNSPECIFIED UNSPECIFIED Comeron, F. UNSPECIFIED UNSPECIFIED UNSPECIFIED Djupvik, A. A. UNSPECIFIED UNSPECIFIED UNSPECIFIED Makai, Z. UNSPECIFIED UNSPECIFIED UNSPECIFIED Buchbender, C. UNSPECIFIED UNSPECIFIED UNSPECIFIED Simon, R. UNSPECIFIED UNSPECIFIED UNSPECIFIED Bontemps, S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Guesten, R. UNSPECIFIED UNSPECIFIED UNSPECIFIED White, G. UNSPECIFIED UNSPECIFIED UNSPECIFIED Okada, Y. UNSPECIFIED UNSPECIFIED UNSPECIFIED Parikka, A. UNSPECIFIED UNSPECIFIED UNSPECIFIED Rothbart, N. UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-601962
DOI:	10.1051/0004-6361/202140824
Journal or Publication Title:	Astron. Astrophys.
Volume:	653
Date:	2021
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 STAR-FORMATION; COMETARY GLOBULES; EMISSION; REGIONS; LINE; PHOTOEVAPORATION; FILAMENT; NEBULA; CLOUDS; SPECTROMETER Multiple languages Astronomy & Astrophysics Multiple languages
URI:	http://kups.ub.uni-koeln.de/id/eprint/60196