Cold gas in group-dominant elliptical galaxies ^⋆,⋆⋆

¹ Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-50 Cambridge, MA 02138, USA
e-mail: eosullivan@cfa.harvard.edu
² Observatoire de Paris, LERMA (CNRS UMR 8112), 61 Av. de l’Observatoire, 75014 Paris, France
³ Department of Physics and Astronomy, University of Victoria, Victoria, BC, V8W 2Y2, Canada
⁴ Department of Physics, Presidency University, 86/1 College Street, 700073 Kolkata, India
⁵ School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK

Received: 19 August 2014
Accepted: 2 November 2014

Abstract

We present IRAM 30 m telescope observations of the CO(1–0) and (2–1) lines in a sample of 11 group-dominant elliptical galaxies selected from the CLoGS nearby groups sample. Our observations confirm the presence of molecular gas in 4 of the 11 galaxies at >4σ significance, and combining these with data from the literature we find a detection rate of 43 ± 14%, comparable to the detection rate for nearby radio galaxies, suggesting that group-dominant ellipticals may be more likely to contain molecular gas than their non-central counterparts. Those group-dominant galaxies which are detected typically contain ~ 2 × 10⁸ M_⊙ of molecular gas, and although most have low star formation rates (<1  M_⊙ yr^-1) they have short depletion times, indicating that the gas must be replenished on timescales ~10⁸ yr. Almost all of the galaxies contain active nuclei, and we note while the data suggest that CO may be more common in the most radio-loud galaxies, the mass of molecular gas required to power the active nuclei through accretion is small compared to the masses observed. We consider possible origin mechanisms for the gas, through cooling of stellar ejecta within the galaxies, group-scale cooling flows, and gas-rich mergers, and find probable examples of each type within our sample, confirming that a variety of processes act to drive the build up of molecular gas in group-dominant ellipticals.