Determining the Halo Mass Scale Where Galaxies Lose Their Gas

Gregory Rudnick, Pascale Jablonka, John Moustakas, Alfonso Aragón-Salamanca, Dennis F Zaritsky, Yara L. Jaffé, Gabriella De Lucia, Vandana Desai, Claire Halliday, Dennis Just, Bo Milvang-Jensen, Bianca Poggianti

Research output: Contribution to journalArticle

5 Citations (Scopus)

Abstract

A major question in galaxy formation is how the gas supply that fuels activity in galaxies is modulated by their environment. We use spectroscopy of a set of well-characterized clusters and groups at 0.4 < z < 0.8 from the ESO Distant Cluster Survey and compare it to identically selected field galaxies. Our spectroscopy allows us to isolate galaxies that are dominated by old stellar populations. Here we study a stellar-mass-limited sample (log(M/M) > 10.4) of these old galaxies with weak [O ii] emission. We use line ratios and compare to studies of local early-type galaxies to conclude that this gas is likely excited by post-AGB stars and hence represents a diffuse gas component in the galaxies. For cluster and group galaxies the fraction with EW([O ii]) > 5 Å is f [O II] = 0.08+0.03 -0.02 and f [O II] = 0.06+0.07 -0.04, respectively. For field galaxies we find f [O II] = 0.27+0.07 -0.06, representing a 2.8σ difference between the [O ii] fractions for old galaxies between the different environments. We conclude that a population of old galaxies in all environments has ionized gas that likely stems from stellar mass loss. In the field galaxies also experience gas accretion from the cosmic web, and in groups and clusters these galaxies have had their gas accretion shut off by their environment. Additionally, galaxies with emission preferentially avoid the virialized region of the cluster in position-velocity space. We discuss the implications of our results, among which is that gas accretion shutoff is likely effective at group halo masses (log M/M > 12.8) and that there are likely multiple gas removal processes happening in dense environments.

Original languageEnglish (US)
Article number181
JournalAstrophysical Journal
Volume850
Issue number2
DOIs
StatePublished - Dec 1 2017

Fingerprint

halos
galaxies
gases
gas
accretion
gas supply
galactic clusters
asymptotic giant branch stars
galactic evolution
ionized gases
spectroscopy
stellar mass
stems

Keywords

  • galaxies: evolution
  • galaxies: groups: general
  • galaxies: ISM

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Rudnick, G., Jablonka, P., Moustakas, J., Aragón-Salamanca, A., Zaritsky, D. F., Jaffé, Y. L., ... Poggianti, B. (2017). Determining the Halo Mass Scale Where Galaxies Lose Their Gas. Astrophysical Journal, 850(2), [181]. https://doi.org/10.3847/1538-4357/aa866c

Determining the Halo Mass Scale Where Galaxies Lose Their Gas. / Rudnick, Gregory; Jablonka, Pascale; Moustakas, John; Aragón-Salamanca, Alfonso; Zaritsky, Dennis F; Jaffé, Yara L.; Lucia, Gabriella De; Desai, Vandana; Halliday, Claire; Just, Dennis; Milvang-Jensen, Bo; Poggianti, Bianca.

In: Astrophysical Journal, Vol. 850, No. 2, 181, 01.12.2017.

Research output: Contribution to journalArticle

Rudnick, G, Jablonka, P, Moustakas, J, Aragón-Salamanca, A, Zaritsky, DF, Jaffé, YL, Lucia, GD, Desai, V, Halliday, C, Just, D, Milvang-Jensen, B & Poggianti, B 2017, 'Determining the Halo Mass Scale Where Galaxies Lose Their Gas', Astrophysical Journal, vol. 850, no. 2, 181. https://doi.org/10.3847/1538-4357/aa866c
Rudnick G, Jablonka P, Moustakas J, Aragón-Salamanca A, Zaritsky DF, Jaffé YL et al. Determining the Halo Mass Scale Where Galaxies Lose Their Gas. Astrophysical Journal. 2017 Dec 1;850(2). 181. https://doi.org/10.3847/1538-4357/aa866c
Rudnick, Gregory ; Jablonka, Pascale ; Moustakas, John ; Aragón-Salamanca, Alfonso ; Zaritsky, Dennis F ; Jaffé, Yara L. ; Lucia, Gabriella De ; Desai, Vandana ; Halliday, Claire ; Just, Dennis ; Milvang-Jensen, Bo ; Poggianti, Bianca. / Determining the Halo Mass Scale Where Galaxies Lose Their Gas. In: Astrophysical Journal. 2017 ; Vol. 850, No. 2.
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