Modeling CO emission from hydrodynamic simulations of nearby spirals, starbursting mergers, and high-redshift galaxies. Bournaud, F., Daddi, E., Weiß, A., Renaud, F., Mastropietro, C., & Teyssier, R. Astronomy and Astrophysics, 575:A56, March, 2015. ![Modeling CO emission from hydrodynamic simulations of nearby spirals, starbursting mergers, and high-redshift galaxies [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex We model the intensity of emission lines from the CO molecule, based on hydrodynamic simulations of spirals, mergers, and high-redshift galaxies with very high resolutions (3 pc and 103 M⊙) and detailed models for the phase-space structure of the interstellar gas including shock heating, stellar feedback processes, and galactic winds. The simulations are analyzed with a large velocity gradient (LVG) model to compute the local emission in various molecular lines in each resolution element, radiation transfer, opacity effect, and the intensity emerging from galaxies to generate synthetic spectra for various transitions of the CO molecule. This model reproduces the known properties of CO spectra and CO-to-H2 conversion factors in nearby spirals and starbursting major mergers. The high excitation of CO lines in mergers is dominated by an excess of high-density gas, and the high turbulent velocities and compression that create this dense gas excess result in broad linewidths and low CO intensity-to-H2 mass ratios. When applied to high-redshift gas-rich disks galaxies, the same model predicts that their CO-to-H2 conversion factor is almost as high as in nearby spirals, and much higher than in starbursting mergers. High-redshift disk galaxies contain giant star-forming clumps that host a high-excitation component associated to gas warmed by the spatially concentrated stellar feedback sources, although CO(1-0) to CO(3-2) emission is dominated overall by low-excitation gas around the densest clumps. These results generally highlight a strong dependence of CO excitation and the CO-to-H2 conversion factor on galaxy type, even at similar star formation rates or densities. The underlying processes are driven by the interstellar medium structure and turbulence and its response to stellar feedback, which depend on global galaxy structure and in turn affect the CO emission properties.
@article{bournaud_modeling_2015,
title = {Modeling {CO} emission from hydrodynamic simulations of nearby spirals, starbursting mergers, and high-redshift galaxies},
volume = {575},
issn = {0004-6361},
url = {http://adsabs.harvard.edu/abs/2015A%26A...575A..56B},
doi = {10.1051/0004-6361/201425078},
abstract = {We model the intensity of emission lines from the CO molecule, based on
hydrodynamic simulations of spirals, mergers, and high-redshift galaxies
with very high resolutions (3 pc and 103 M⊙)
and detailed models for the phase-space structure of the interstellar
gas including shock heating, stellar feedback processes, and galactic
winds. The simulations are analyzed with a large velocity gradient (LVG)
model to compute the local emission in various molecular lines in each
resolution element, radiation transfer, opacity effect, and the
intensity emerging from galaxies to generate synthetic spectra for
various transitions of the CO molecule. This model reproduces the known
properties of CO spectra and CO-to-H2 conversion factors in
nearby spirals and starbursting major mergers. The high excitation of CO
lines in mergers is dominated by an excess of high-density gas, and the
high turbulent velocities and compression that create this dense gas
excess result in broad linewidths and low CO intensity-to-H2
mass ratios. When applied to high-redshift gas-rich disks galaxies, the
same model predicts that their CO-to-H2 conversion factor is
almost as high as in nearby spirals, and much higher than in
starbursting mergers. High-redshift disk galaxies contain giant
star-forming clumps that host a high-excitation component associated to
gas warmed by the spatially concentrated stellar feedback sources,
although CO(1-0) to CO(3-2) emission is dominated overall by
low-excitation gas around the densest clumps. These results generally
highlight a strong dependence of CO excitation and the
CO-to-H2 conversion factor on galaxy type, even at similar
star formation rates or densities. The underlying processes are driven
by the interstellar medium structure and turbulence and its response to
stellar feedback, which depend on global galaxy structure and in turn
affect the CO emission properties.},
urldate = {2021-03-24},
journal = {Astronomy and Astrophysics},
author = {Bournaud, F. and Daddi, E. and Weiß, A. and Renaud, F. and Mastropietro, C. and Teyssier, R.},
month = mar,
year = {2015},
keywords = {galaxies: ISM, galaxies: star formation},
pages = {A56},
}
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The simulations are analyzed with a large velocity gradient (LVG) model to compute the local emission in various molecular lines in each resolution element, radiation transfer, opacity effect, and the intensity emerging from galaxies to generate synthetic spectra for various transitions of the CO molecule. This model reproduces the known properties of CO spectra and CO-to-H2 conversion factors in nearby spirals and starbursting major mergers. The high excitation of CO lines in mergers is dominated by an excess of high-density gas, and the high turbulent velocities and compression that create this dense gas excess result in broad linewidths and low CO intensity-to-H2 mass ratios. When applied to high-redshift gas-rich disks galaxies, the same model predicts that their CO-to-H2 conversion factor is almost as high as in nearby spirals, and much higher than in starbursting mergers. High-redshift disk galaxies contain giant star-forming clumps that host a high-excitation component associated to gas warmed by the spatially concentrated stellar feedback sources, although CO(1-0) to CO(3-2) emission is dominated overall by low-excitation gas around the densest clumps. These results generally highlight a strong dependence of CO excitation and the CO-to-H2 conversion factor on galaxy type, even at similar star formation rates or densities. The underlying processes are driven by the interstellar medium structure and turbulence and its response to stellar feedback, which depend on global galaxy structure and in turn affect the CO emission properties.","urldate":"2021-03-24","journal":"Astronomy and Astrophysics","author":[{"propositions":[],"lastnames":["Bournaud"],"firstnames":["F."],"suffixes":[]},{"propositions":[],"lastnames":["Daddi"],"firstnames":["E."],"suffixes":[]},{"propositions":[],"lastnames":["Weiß"],"firstnames":["A."],"suffixes":[]},{"propositions":[],"lastnames":["Renaud"],"firstnames":["F."],"suffixes":[]},{"propositions":[],"lastnames":["Mastropietro"],"firstnames":["C."],"suffixes":[]},{"propositions":[],"lastnames":["Teyssier"],"firstnames":["R."],"suffixes":[]}],"month":"March","year":"2015","keywords":"galaxies: ISM, galaxies: star formation","pages":"A56","bibtex":"@article{bournaud_modeling_2015,\n\ttitle = {Modeling {CO} emission from hydrodynamic simulations of nearby spirals, starbursting mergers, and high-redshift galaxies},\n\tvolume = {575},\n\tissn = {0004-6361},\n\turl = {http://adsabs.harvard.edu/abs/2015A%26A...575A..56B},\n\tdoi = {10.1051/0004-6361/201425078},\n\tabstract = {We model the intensity of emission lines from the CO molecule, based on \nhydrodynamic simulations of spirals, mergers, and high-redshift galaxies\nwith very high resolutions (3 pc and 103 M⊙)\nand detailed models for the phase-space structure of the interstellar\ngas including shock heating, stellar feedback processes, and galactic\nwinds. The simulations are analyzed with a large velocity gradient (LVG)\nmodel to compute the local emission in various molecular lines in each\nresolution element, radiation transfer, opacity effect, and the\nintensity emerging from galaxies to generate synthetic spectra for\nvarious transitions of the CO molecule. This model reproduces the known\nproperties of CO spectra and CO-to-H2 conversion factors in\nnearby spirals and starbursting major mergers. The high excitation of CO\nlines in mergers is dominated by an excess of high-density gas, and the\nhigh turbulent velocities and compression that create this dense gas\nexcess result in broad linewidths and low CO intensity-to-H2\nmass ratios. When applied to high-redshift gas-rich disks galaxies, the\nsame model predicts that their CO-to-H2 conversion factor is\nalmost as high as in nearby spirals, and much higher than in\nstarbursting mergers. High-redshift disk galaxies contain giant\nstar-forming clumps that host a high-excitation component associated to\ngas warmed by the spatially concentrated stellar feedback sources,\nalthough CO(1-0) to CO(3-2) emission is dominated overall by\nlow-excitation gas around the densest clumps. These results generally\nhighlight a strong dependence of CO excitation and the\nCO-to-H2 conversion factor on galaxy type, even at similar\nstar formation rates or densities. The underlying processes are driven\nby the interstellar medium structure and turbulence and its response to\nstellar feedback, which depend on global galaxy structure and in turn\naffect the CO emission properties.},\n\turldate = {2021-03-24},\n\tjournal = {Astronomy and Astrophysics},\n\tauthor = {Bournaud, F. and Daddi, E. and Weiß, A. and Renaud, F. and Mastropietro, C. and Teyssier, R.},\n\tmonth = mar,\n\tyear = {2015},\n\tkeywords = {galaxies: ISM, galaxies: star formation},\n\tpages = {A56},\n}\n\n","author_short":["Bournaud, F.","Daddi, E.","Weiß, A.","Renaud, F.","Mastropietro, C.","Teyssier, R."],"key":"bournaud_modeling_2015","id":"bournaud_modeling_2015","bibbaseid":"bournaud-daddi-wei-renaud-mastropietro-teyssier-modelingcoemissionfromhydrodynamicsimulationsofnearbyspiralsstarburstingmergersandhighredshiftgalaxies-2015","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2015A%26A...575A..56B"},"keyword":["galaxies: ISM","galaxies: star formation"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["galaxies: ism","galaxies: star formation"],"search_terms":["modeling","emission","hydrodynamic","simulations","nearby","spirals","starbursting","mergers","high","redshift","galaxies","bournaud","daddi","weiß","renaud","mastropietro","teyssier"],"title":"Modeling CO emission from hydrodynamic simulations of nearby spirals, starbursting mergers, and high-redshift galaxies","year":2015}