Skip navigation
  • INAF logo
  • Home
  • Communities
    & Collections
  • Research outputs
  • Researchers
  • Organization units
  • Projects
  • Explore by
    • Research outputs
    • Researchers
    • Organization units
    • Projects
  • Login:
    • My DSpace
    • Receive email
      updates
    • Edit Account details
  • Italian
  • English

  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/29090
Title: Determining the Halo Mass Scale Where Galaxies Lose Their Gas
Authors: Rudnick, Gregory
Jablonka, Pascale
Moustakas, John
Aragón-Salamanca, Alfonso
Zaritsky, Dennis
Jaffé, Yara L.
DE LUCIA, GABRIELLA 
Desai, Vandana
Halliday, Claire
Just, Dennis
Milvang-Jensen, Bo
POGGIANTI, Bianca Maria 
Issue Date: 2017
Journal: THE ASTROPHYSICAL JOURNAL 
Number: 850
Issue: 2
First Page: 181
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}<SUB>* </SUB>/{M}<SUB>☉ </SUB>)> 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 <SUB>[O II] </SUB> = {0.08}<SUB>-0.02</SUB><SUP>+0.03</SUP> and f <SUB>[O II] </SUB> = {0.06}<SUB>-0.04</SUB><SUP>+0.07</SUP>, respectively. For field galaxies we find f <SUB>[O II] </SUB> = {0.27}<SUB>-0.06</SUB><SUP>+0.07</SUP>, 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 }}<SUB>☉ </SUB> > 12.8) and that there are likely multiple gas removal processes happening in dense environments. <P />Based on observations obtained at the European Southern Observatory using the ESO Very Large Telescope on Cerro Paranal through ESO program 166.A-0162.
URI: http://hdl.handle.net/20.500.12386/29090
URL: https://iopscience.iop.org/article/10.3847/1538-4357/aa866c
ISSN: 0004-637X
DOI: 10.3847/1538-4357/aa866c
Bibcode ADS: 2017ApJ...850..181R
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

Files in This Item:
File Description SizeFormat
1709.03691.pdfpreprint1.16 MBAdobe PDFView/Open
Rudnick_2017_ApJ_850_181.pdfpdf editoriale1.71 MBAdobe PDFView/Open
Show full item record

Page view(s)

41
checked on Oct 1, 2023

Download(s)

24
checked on Oct 1, 2023

Google ScholarTM

Check

Altmetric

Altmetric


Items in DSpace are published in Open Access, unless otherwise indicated.


Explore by
  • Communities
    & Collections
  • Research outputs
  • Researchers
  • Organization units
  • Projects

Informazioni e guide per autori

https://openaccess-info.inaf.it: tutte le informazioni sull'accesso aperto in INAF

Come si inserisce un prodotto: le guide a OA@INAF

La Policy INAF sull'accesso aperto

Documenti e modelli scaricabili

Feedback
Built with DSpace-CRIS - Extension maintained and optimized by Logo 4SCIENCE