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Reference: Herrera-Camus, R., Bolatto, A., Smith, J. D. et al., (2016). The ionized gas in nearby galaxies as traced by the [NII] 122 and 205 μm transitions. The Astrophysical Journal, 826 (2), 1-17.Citable link to this page:

 

The ionized gas in nearby galaxies as traced by the [NII] 122 and 205 μm transitions

Abstract: The [N ii] 122 and 205 μm transitions are powerful tracers of the ionized gas in the interstellar medium. By combining data from 21 galaxies selected from the Herschel KINGFISH and Beyond the Peak surveys, we have compiled 141 spatially resolved regions with a typical size of ∼1 kpc, with observations of both [N ii] far-infrared lines. We measure [N ii] 122/205 line ratios in the ∼0.6-6 range, which corresponds to electron gas densities of n e ∼ 1-300 cm-3, with a median value of n e = 30 cm-3. Variations in the electron density within individual galaxies can be as high as a factor of ∼50, frequently with strong radial gradients. We find that n e increases as a function of infrared color, dust-weighted mean starlight intensity, and star-formation rate (SFR) surface density (ΣSFR). As the intensity of the [N ii] transitions is related to the ionizing photon flux, we investigate their reliability as tracers of the SFR. We derive relations between the [N ii] emission and SFR in the low-density limit and in the case of a log-normal distribution of densities. The scatter in the correlation between [N ii] surface brightness and ΣSFR can be understood as a property of the n e distribution. For regions with n e close to or higher than the [N ii] line critical densities, the low-density limit [N ii]-based SFR calibration systematically underestimates the SFR because the [N ii] emission is collisionally quenched. Finally, we investigate the relation between [N ii] emission, SFR, and n e by comparing our observations to predictions from the MAPPINGS-III code.

Publication status:PublishedPeer Review status:Peer reviewedVersion:Publisher's VersionDate of acceptance:2016-05-10Notes:© 2016. The American Astronomical Society. All rights reserved. This is the publisher's version of the article. The final version is available online from American Astronomical Society at: 10.3847/0004-637X/826/2/175Notes:For the full funder list, see: 10.3847/0004-637X/826/2/175

Bibliographic Details

Publisher: American Astronomical Society

Publisher Website: https://aas.org/

Journal: The Astrophysical Journalsee more from them

Publication Website: http://iopscience.iop.org/journal/0004-637X

Volume: 826

Issue Date: 2016-07-29

pages:1-17Identifiers

Doi: https://doi.org/10.3847/0004-637X/826/2/175

Eissn: 1538-4357

Issn: 0004-637X

Uuid: uuid:f761fefb-7489-435b-9cd1-2f3205f5dbc6

Urn: uri:f761fefb-7489-435b-9cd1-2f3205f5dbc6

Pubs-id: pubs:641041 Item Description

Type: journal-article;

Version: Publisher's VersionKeywords: galaxies ISM - galaxies star formation - ISM structure

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Autor: Herrera-Camus, R. - - - Bolatto, A. - - - Smith, J. D. - - - Draine, B. - - - Pellegrini, E. - - - Wolfire, M. - - - Croxall, K.

Fuente: https://ora.ox.ac.uk/objects/uuid:f761fefb-7489-435b-9cd1-2f3205f5dbc6



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