Journal
ASTROPHYSICAL JOURNAL
Volume 861, Issue 2, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/1538-4357/aac0f6
Keywords
galaxies: active; galaxies: general; galaxies: ISM; galaxies: Seyfert; galaxies: star formation; galaxies: starburst
Categories
Funding
- US ONR
- NHSC
- Spanish Ministerio de Economia y Competitividad [FIS2012-39162-C06-01, ESP2015-65597-C4-1-R]
- NASA [ADAP NNX15AE56G]
- ERC Advanced Grant [695671]
- Science and Technology Facilities Council (STFC)
- BMVIT (Austria)
- ESA-PRODEX (Belgium)
- CEA/CNES (France)
- DLR (Germany)
- ASI/INAF (Italy)
- CICYT/MCYT (Spain)
- Alfred P. Sloan Foundation
- National Aeronautics and Space Administration
- National Science Foundation
- U.S. Department of Energy
- Japanese Monbukagakusho
- Max Planck Society
- STFC [ST/M001172/1, ST/M007650/1, ST/K00106X/1, ST/N002717/1] Funding Source: UKRI
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We use the Herschel/PACS spectrometer to study the global and spatially resolved far-infrared (FIR) fine-structure line emission in a sample of 52 galaxies that constitute the SHINING survey. These galaxies include star-forming, active-galactic nuclei (AGNs), and luminous infrared galaxies (LIRGs). We find an increasing number of galaxies (and kiloparsec-size regions within galaxies) with low line-to-FIR continuum ratios as a function of increasing FIR luminosity (L-FIR), dust infrared color, L-FIR to molecular gas mass ratio (L-FIR/M-mol), and FIR surface brightness (Sigma(FIR)). The correlations between the [C II]/FIR or [O I]/FIR ratios with Sigma(FIR) are remarkably tight (similar to 0.3 dex scatter over almost four orders of magnitude in Sigma(FIR)). We observe that galaxies with L-FIR/M-mol greater than or similar to 80 L-circle dot M-circle dot(-1) and Sigma(FIR) greater than or similar to 10(11) L-circle dot kpc(-2) tend to have weak fine-structure line-to-FIR continuum ratios, and that LIRGs with infrared sizes greater than or similar to 1 kpc have line-to-FIR ratios comparable to those observed in typical star-forming galaxies. We analyze the physical mechanisms driving these trends in Paper II. The combined analysis of the [C II], [N II] 122 mu m, and [O III] 88 mu m lines reveals that the fraction of the [C II] line emission that arises from neutral gas increases from 60% to 90% in the most active star-forming regions and that the emission originating in the ionized gas is associated with low-ionization, diffuse gas rather than with dense gas in H II regions. Finally, we report the global and spatially resolved line fluxes of the SHINING galaxies to enable the comparison and planning of future local and high-z studies.
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