[C i](1-0) and [C i](2-1) in resolved local galaxies
We present resolved [C i] line intensities of 18 nearby galaxies observed with the SPIRE FTS spectrometer on the Herschel Space Observatory. We use these data along with resolved CO line intensities from J up = 1 to 7 to interpret what phase of the interstellar medium the [C i] lines trace within ty...
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| Main Authors: | , , |
|---|---|
| Format: | Article (Journal) |
| Language: | English |
| Published: |
2019 December 13
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| In: |
The astrophysical journal
Year: 2019, Volume: 887, Issue: 1 |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/ab4196 |
| Online Access: | Verlag, Volltext: https://doi.org/10.3847/1538-4357/ab4196
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| Author Notes: | Alison F. Crocker, Eric Pellegrini, J.-D. T. Smith, Bruce T. Draine, Christine D. Wilson, Mark Wolfire, Lee Armus, Elias Brinks, Daniel A. Dale, Brent Groves, Rodrigo Herrera-Camus, Leslie K. Hunt, Robert C. Kennicutt, Eric J. Murphy, Karin Sandstrom, Eva Schinnerer, Dimitra Rigopoulou, Erik Rosolowsky, Paul van der Werf |
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| 245 | 1 | 0 | |a [C i](1-0) and [C i](2-1) in resolved local galaxies |c Alison F. Crocker, Eric Pellegrini, J.-D. T. Smith, Bruce T. Draine, Christine D. Wilson, Mark Wolfire, Lee Armus, Elias Brinks, Daniel A. Dale, Brent Groves, Rodrigo Herrera-Camus, Leslie K. Hunt, Robert C. Kennicutt, Eric J. Murphy, Karin Sandstrom, Eva Schinnerer, Dimitra Rigopoulou, Erik Rosolowsky, Paul van der Werf |
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| 520 | |a We present resolved [C i] line intensities of 18 nearby galaxies observed with the SPIRE FTS spectrometer on the Herschel Space Observatory. We use these data along with resolved CO line intensities from J up = 1 to 7 to interpret what phase of the interstellar medium the [C i] lines trace within typical local galaxies. A tight, linear relation is found between the intensities of the CO(4-3) and [C i](2-1) lines; we hypothesize this is due to the similar upper level temperature of these two lines. We modeled the [C i] and CO line emission using large-velocity gradient models combined with an empirical template. According to this modeling, the [C i](1-0) line is clearly dominated by the low-excitation component. We determine [C i] to molecular mass conversion factors for both the [C i](1-0) and [C i](2-1) lines, with mean values of α [C i](1−0) = 7.3 M ⊙ K−1 km−1 s pc−2 and α [C i](2−1) = 34 M ⊙ K−1 km−1 s pc−2 with logarithmic root-mean-square spreads of 0.20 and 0.32 dex, respectively. The similar spread of to (derived using the CO(2-1) line) suggests that [C i](1-0) may be just as good a tracer of cold molecular gas as CO(2-1) in galaxies of this type. On the other hand, the wider spread of α [C i](2−1) and the tight relation found between [C i](2-1) and CO(4-3) suggest that much of the [C i](2-1) emission may originate in warmer molecular gas. | ||
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