Volume 518, July-August 2010
Herschel: the first science highlights
|Number of page(s)||4|
|Published online||16 July 2010|
Letter to the Editor
The effects of star formation on the low-metallicity ISM: NGC 4214 mapped with Herschel/PACS spectroscopy *
Laboratoire AIM, CEA/DSM - CNRS - Université Paris Diderot, Irfu/Service d'Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France e-mail: email@example.com
2 Max-Planck-Institut fuer extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
Accepted: 29 April 2010
We present Herschel/PACS spectroscopic maps of the dwarf galaxy NC4214 observed in 6 far infrared fine-structure lines: [C ii] 158 μm, [O iii] 88 μm, [O i] 63 μm, [O i] 146 μm, [N ii] 122 μm, and [N ii] 205 μm. The maps are sampled to the full telescope spatial resolution and reveal unprecedented detail on ~ 150 pc size scales. We detect [C ii] emission over the whole mapped area, [O iii] being the most luminous FIR line. The ratio of [O iii]/[C ii] peaks at about 2 toward the sites of massive star formation, higher than ratios seen in dusty starburst galaxies. The [C ii]/CO ratios are 20 000 to 70 000 toward the 2 massive clusters, which are at least an order of magnitude larger than spiral or dusty starbursts, and cannot be reconciled with single-slab PDR models. Toward the 2 massive star-forming regions, we find that L[CII] is 0.5 to 0.8% of the LTIR. All of the lines together contribute up to 2% of LTIR. These extreme findings are a consequence of the lower metallicity and young, massive-star formation commonly found in dwarf galaxies. These conditions promote large-scale photodissociation into the molecular reservoir, which is evident in the FIR line ratios. This illustrates the necessity to move to multiphase models applicable to star-forming clusters or galaxies as a whole.
Key words: galaxies: ISM / galaxies: individual: NGC 4214 / ISM: line and bands / photon-dominated region (PDR) / galaxies: dwarf
© ESO, 2010
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