[CI](1-0) and [CI](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...
| Main Authors: | , , , , , , , , , , , , , , , , , , |
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| Format: | Journal article |
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American Astronomical Society
2019
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| _version_ | 1826273227688640512 |
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| author | Alison F Crocker Eric Pellegrini J-DT 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 |
| author_facet | Alison F Crocker Eric Pellegrini J-DT 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 |
| author_sort | Alison F Crocker |
| collection | OXFORD |
| description | 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 o K-1 km-1 s pc-2 and α [C i](2-1) = 34 M o 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 α [C I](1-0) to αCO (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. |
| first_indexed | 2024-03-06T22:24:59Z |
| format | Journal article |
| id | oxford-uuid:5660223c-ffd1-4c74-a3ac-ea5f52611111 |
| institution | University of Oxford |
| last_indexed | 2024-03-06T22:24:59Z |
| publishDate | 2019 |
| publisher | American Astronomical Society |
| record_format | dspace |
| spelling | oxford-uuid:5660223c-ffd1-4c74-a3ac-ea5f526111112022-03-26T16:49:52Z[CI](1-0) and [CI](2-1) in Resolved Local GalaxiesJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:5660223c-ffd1-4c74-a3ac-ea5f52611111Symplectic ElementsAmerican Astronomical Society2019Alison F CrockerEric PellegriniJ-DT SmithBruce T DraineChristine D WilsonMark WolfireLee ArmusElias BrinksDaniel A DaleBrent GrovesRodrigo Herrera-CamusLeslie K HuntRobert C KennicuttEric J MurphyKarin SandstromEva SchinnererDimitra RigopoulouErik RosolowskyPaul van der WerfWe 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 o K-1 km-1 s pc-2 and α [C i](2-1) = 34 M o 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 α [C I](1-0) to αCO (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. |
| spellingShingle | Alison F Crocker Eric Pellegrini J-DT 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 [CI](1-0) and [CI](2-1) in Resolved Local Galaxies |
| title | [CI](1-0) and [CI](2-1) in Resolved Local Galaxies |
| title_full | [CI](1-0) and [CI](2-1) in Resolved Local Galaxies |
| title_fullStr | [CI](1-0) and [CI](2-1) in Resolved Local Galaxies |
| title_full_unstemmed | [CI](1-0) and [CI](2-1) in Resolved Local Galaxies |
| title_short | [CI](1-0) and [CI](2-1) in Resolved Local Galaxies |
| title_sort | ci 1 0 and ci 2 1 in resolved local galaxies |
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