Molecular disk properties in early-type galaxies

X. Xu, D. Narayanan, Christopher K Walker

Research output: Contribution to journalArticle

7 Citations (Scopus)

Abstract

We study the simulated CO emission from elliptical galaxies formed in the mergers of gas-rich disk galaxies. The cold gas not consumed in the merger-driven starburst quickly resettles into a disk-like configuration. By analyzing a variety of arbitrary merger orbits that produce a range of fast- to slow-rotating remnants, we find that molecular disk formation is a fairly common consequence of gas-rich galaxy mergers. Hence, if a molecular disk is observed in an early-type merger remnant, it is likely the result of a "wet merger" rather than a "dry merger."We compare the physical properties from our simulated disks (e.g., size and mass) and find reasonably good agreement with recent observations. Finally, we discuss the detectability of these disks as an aid to future observations.

Original languageEnglish (US)
JournalAstrophysical Journal Letters
Volume721
Issue number2 PART 2
DOIs
StatePublished - Oct 1 2010

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merger
galaxies
cold gas
disk galaxies
elliptical galaxies
gas
gases
physical properties
orbits
aid
physical property
configurations

Keywords

  • Galaxies: elliptical and lenticular, cD
  • Galaxies: evolution
  • Galaxies: kinematics and dynamics
  • ISM: molecules

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Molecular disk properties in early-type galaxies. / Xu, X.; Narayanan, D.; Walker, Christopher K.

In: Astrophysical Journal Letters, Vol. 721, No. 2 PART 2, 01.10.2010.

Research output: Contribution to journalArticle

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AB - We study the simulated CO emission from elliptical galaxies formed in the mergers of gas-rich disk galaxies. The cold gas not consumed in the merger-driven starburst quickly resettles into a disk-like configuration. By analyzing a variety of arbitrary merger orbits that produce a range of fast- to slow-rotating remnants, we find that molecular disk formation is a fairly common consequence of gas-rich galaxy mergers. Hence, if a molecular disk is observed in an early-type merger remnant, it is likely the result of a "wet merger" rather than a "dry merger."We compare the physical properties from our simulated disks (e.g., size and mass) and find reasonably good agreement with recent observations. Finally, we discuss the detectability of these disks as an aid to future observations.

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KW - Galaxies: kinematics and dynamics

KW - ISM: molecules

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