Volume 599, March 2017
|Number of page(s)||13|
|Published online||20 February 2017|
Disentangling the ISM phases of the dwarf galaxy NGC 4214 using [C ii] SOFIA/GREAT observations⋆
1 Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Überle-Straße 2, 69120 Heidelberg, Germany
2 University of Cincinnati, Clermont College, MCGP Department, Batavia, OH 45103, USA
3 School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UK
4 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
5 I. Physikalisches Institut der Universität zu Köln, Zülpicher Straβ<e 77, 50937 Köln, Germany
6 Laboratoire AIM, CEA Saclay, Orme des Merisiers, Bât. 709, 91191 Gif-sur-Yvette, France
7 Department of Astronomy, The University of Tokyo, Bunkyo-ku, 113-0033 Tokyo, Japan
8 Physics Department, New Mexico Tech, 801 Leroy Place, Socorro, NM 87801, USA
Received: 19 July 2016
Accepted: 2 November 2016
Context. The [C ii] 158 μm fine structure line is one of the dominant cooling lines in the interstellar medium (ISM) and is an important tracer of star formation. Recent velocity-resolved studies with Herschel/HIFI and SOFIA/GREAT showed that the [C ii] line can constrain the properties of the ISM phases in star-forming regions. The [C ii] line as a tracer of star formation is particularly important in low-metallicity environments where CO emission is weak because of the presence of large amounts of CO-dark gas.
Aims. The nearby irregular dwarf galaxy NGC 4214 offers an excellent opportunity to study an actively star-forming ISM at low metallicity. We analyzed the spectrally resolved [C ii] line profiles in three distinct regions at different evolutionary stages of NGC 4214 with respect to ancillary H i and CO data in order to study the origin of the [C ii] line.
Methods. We used SOFIA/GREAT [C ii] 158 μm observations, H i data from THINGS, and CO(2 → 1) data from HERACLES to decompose the spectrally resolved [C ii] line profiles into components associated with neutral atomic and molecular gas. We use this decomposition to infer gas masses traced by [C ii] under different ISM conditions.
Results. Averaged over all regions, we associate about 46% of the [C ii] emission with the H i emission. However, we can assign only ~9% of the total [C ii] emission to the cold neutral medium (CNM). We found that about 79% of the total molecular hydrogen mass is not traced by CO emission.
Conclusions. On average, the fraction of CO-dark gas dominates the molecular gas mass budget. The fraction seems to depend on the evolutionary stage of the regions: it is highest in the region covering a super star cluster in NGC 4214, while it is lower in a more compact, more metal-rich region.
Key words: galaxies: dwarf / galaxies: star formation / galaxies: individual: NGC 4214 / ISM: lines and bands
Reduced SOFIA/GREAT data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/599/A9
© ESO, 2017
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