Hostname: page-component-745bb68f8f-cphqk Total loading time: 0 Render date: 2025-01-10T04:01:42.273Z Has data issue: false hasContentIssue false
  • English
  • Français

Large reservoirs of turbulent diffuse gas around high-z starburst galaxies

Published online by Cambridge University Press:  04 June 2020

E. Falgarone Open the ORCID record for E. Falgarone [Opens in a new window] ,
A. Vidal-Garca ,
B. Godard ,
M. A. Zwaan ,
C. Herrera ,
R. J. Ivison ,
E. Bergin ,
P. M. Andreani ,
A. Omont  and
F. Walter
E. Falgarone
Affiliation:
Laboratoire de Physique de l’ENS, ENS, Université PSL, CNRS, Sorbonne Université, Université de Paris, 24 rue Lhomond, 75005 Paris, France email: [email protected]
A. Vidal-Garca
Affiliation:
Laboratoire de Physique de l’ENS, ENS, Université PSL, CNRS, Sorbonne Université, Université de Paris, 24 rue Lhomond, 75005 Paris, France email: [email protected]
B. Godard
Affiliation:
Laboratoire de Physique de l’ENS, ENS, Université PSL, CNRS, Sorbonne Université, Université de Paris, 24 rue Lhomond, 75005 Paris, France email: [email protected] LERMA, Observatoire de Paris, CNRS, 61 avenue de l’Observatoire, 75014 Paris, France
M. A. Zwaan
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
C. Herrera
Affiliation:
IRAM, 300 rue de la Piscine, Domaine universitaire, 38406 Saint Martin d’Hères, France
R. J. Ivison
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
E. Bergin
Affiliation:
University of Michigan, 311 West Hall, 1085 S. University Ave, Ann Arbor, MI 48109, USA
P. M. Andreani
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
A. Omont
Affiliation:
UMPC Université Paris 6 & Institut d’Astrophysique de Paris, CNRS, 75014 Paris, France
F. Walter
Affiliation:
Max Planck Institute für Astronomie, Heidelberg, Germany
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Starburst galaxies at z ∼ 2 – 4 are among the most intensely star-forming galaxies in the universe. The way they accrete their gas to form stars at such high rates is still a controversial issue. ALMA has detected the CH+ (J = 1-0) line in emission and/or absorption in all the gravitationally lensed starburst galaxies targeted so far at z ∼ 3. Its unique spectroscopic and chemical properties enable CH+ to highlight the sites of most intense dissipation of mechanical energy. The absorption lines reveal highly turbulent, massive reservoirs of low-density molecular gas. The broad emission lines, arising in myriad UV-irradiated molecular shocks, reveal powerful galactic winds. The CH+ lines therefore probe the fate of prodigious energy releases, due to infall and/or outflows, and primarily stored in turbulence before being radiated by cool molecular gas. The turbulent reservoirs act as mass and energy buffers over the duration of the starburst phase.

Keywords

galaxies: starburstgalaxies: high-redshiftgalaxies: ISMgalaxies: formationintergalactic mediumturbulenceshock waves
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S352: Uncovering Early Galaxy Evolution in the ALMA and JWST Era , June 2019 , pp. 200 - 204
Copyright
© International Astronomical Union 2020

References

Douglas, A. E. & Herzberg, G. 1941, ApJ, 94, 38110.1086/144342CrossRefGoogle Scholar
Eales, S., Dunne, L., Clements, D., et al. 2010, PASP, 122, 49910.1086/653086CrossRefGoogle Scholar
Falgarone, E., Zwaan, M.A., Godard, B., et al. 2017, Nature, 548, 43010.1038/nature23298CrossRefGoogle Scholar
Gerin, M., Neufeld, D. A., & Goicoechea, J. R. 2016, ARAA, 54, 18110.1146/annurev-astro-081915-023409CrossRefGoogle Scholar
Godard, B., Falgarone, E., & Pineau des Forêts, G. 2014, A&A, 570, A27Google Scholar
Godard, B., Pineau des Forêts, G.Lesaffre, P., et al. 2019, A&A, 622, A100Google Scholar
Ivison, R. J., Swinbank, A. M., Swinyard, B., et al. 2010, A&A, 518, L35Google Scholar
Kennicutt, Jr Robert C. 1998, ApJ, 498, 541CrossRefGoogle Scholar
Madau, P. & Dickinson, M. 2014, ARAA, 52, 41510.1146/annurev-astro-081811-125615CrossRefGoogle Scholar
Oliver, S. J., Wang, L., Smith, A. J., et al. 2010, A&A, 518, L21Google Scholar
Schaye, J., Crain, R. A., Bower, R. G., et al. 2015, MNRAS, 446, 521CrossRefGoogle Scholar
Veilleux, S., Cecil, G., & Bland-Hawthorn, J. 2005, ARAA, 43, 769CrossRefGoogle Scholar
Verhamme, A., Schaerer, D., & Maselli, A. 2006, A&A 460, 397Google Scholar
Zabl, J., Bouché, N. F., Schroetter, L., et al. 2019, MNRAS, 485, 196110.1093/mnras/stz392CrossRefGoogle Scholar
Zhang, Z.-Y., Ivison, R. J., George, R. D., et al. 2018, MNRAS, 481, 59CrossRefGoogle Scholar