Cold gas in a complete sample of group-dominant early-type galaxies

O’Sullivan, Ewan; Combes, F.; Salomé, P.; David, L. P.; Babul, Arif; Vrtilek, J. M.; Lim, Jeremy; Olivares, Valeria; Raychaudhury, Somak; Schellenberger, G.

doi:10.1051/0004-6361/201833580

Cited by 42 publications

(41 citation statements)

References 131 publications

(189 reference statements)

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“…Davis et al [218] use a combination of the ATLAS3D and MASSIVE samples to show that gas-rich mergers are an important source of molecular gas in these galaxies. The observations of smaller samples of BGGs find some of the same trends, and show that BGGs of X-ray bright, cool core groups are not the CO-richest systems [219,220]. BGGs of X-ray fainter groups can contain more CO (and HI), and it is more often located in disks, rather than filaments.…”

Section: Multiwavelength Observationsmentioning

confidence: 69%

“…The BGGs of X-ray bright cool core groups generally seem to contain only a few ×10 6 or ×10 7 M of molecular gas [220], which makes them challenging targets, even for ALMA. However, being nearer than typical cool core clusters, groups offer an opportunity to study individual molecular cloud associations within the cool core, rather than the overall filamentary structures.…”

Section: Multiwavelength Observationsmentioning

confidence: 99%

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Feedback from Active Galactic Nuclei in Galaxy Groups

et al. 2021

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The co-evolution between supermassive black holes and their environment is most directly traced by the hot atmospheres of dark matter halos. The cooling of the hot atmosphere supplies the central regions with fresh gas, igniting active galactic nuclei (AGN) with long duty cycles. Outflows from the central engine tightly couple with the surrounding gaseous medium and provide the dominant heating source preventing runaway cooling by carving cavities and driving shocks across the medium. The AGN feedback loop is a key feature of all modern galaxy evolution models. Here, we review our knowledge of the AGN feedback process in the specific context of galaxy groups. Galaxy groups are uniquely suited to constrain the mechanisms governing the cooling–heating balance. Unlike in more massive halos, the energy that is supplied by the central AGN to the hot intragroup medium can exceed the gravitational binding energy of halo gas particles. We report on the state-of-the-art in observations of the feedback phenomenon and in theoretical models of the heating-cooling balance in galaxy groups. We also describe how our knowledge of the AGN feedback process impacts galaxy evolution models and large-scale baryon distributions. Finally, we discuss how new instrumentation will answer key open questions on the topic.

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Section: Multiwavelength Observationsmentioning

confidence: 69%

Section: Multiwavelength Observationsmentioning

confidence: 99%

Feedback from Active Galactic Nuclei in Galaxy Groups

et al. 2021

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“…This is known to be an important mechanism for the central galaxies in galaxy clusters and groups, and ALMA observations have begun to resolve this process in a variety of systems in recent years (e.g. Russell et al 2016;Vantyghem et al 2017;O'Sullivan et al 2018;Tremblay et al 2018). However, the importance of halo cooling in isolated systems is less well understood.…”

Section: Discussionmentioning

confidence: 99%

The MASSIVE survey – XI. What drives the molecular gas properties of early-type galaxies

Davis

Greene

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In this paper we study the molecular gas content of a representative sample of 67 of the most massive early-type galaxies in the local universe, drawn uniformly from the MASSIVE survey. We present new IRAM-30m telescope observations of 30 of these galaxies, allowing us to probe the molecular gas content of the entire sample to a fixed molecular-to-stellar mass fraction of 0.1%. The total detection rate in this representative sample is 25 +5.9 −4.4 %, and by combining the MASSIVE and ATLAS 3D molecular gas surveys we find a joint detection rate of 22.4 +2.4 −2.1 %. This detection rate seems to be independent of galaxy mass, size, position on the fundamental plane, and local environment. We show here for the first time that true slow rotators can host molecular gas reservoirs, but the rate at which they do so is significantly lower than for fast-rotators. Objects with a higher velocity dispersion at fixed mass (a higher kinematic bulge fraction) are less likely to have detectable molecular gas, and where gas does exist, have lower molecular gas fractions. In addition, satellite galaxies in dense environments have ≈0.6 dex lower molecular gas-to-stellar mass ratios than isolated objects. In order to interpret these results we created a toy model, which we use to constrain the origin of the gas in these systems. We are able to derive an independent estimate of the gas-rich merger rate in the low-redshift universe. These gas rich mergers appear to dominate the supply of gas to ETGs, but stellar mass loss, hot halo cooling and transformation of spiral galaxies also play a secondary role.

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“…There is no H I detection for NGC 5153. A recent molecular gas study of dominant early type galaxies in groups also shows no detection of CO in NGC 5153 (O'Sullivan et al 2018). This suggests gas depletion in NGC 5153.…”

Section: E N V I Ro N M E N T a N D H I M O R P H O L O G Ymentioning

confidence: 93%

WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351

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Staveley‐Smith

Westmeier

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present an H i study of the galaxy group LGG 351 using Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY) early science data observed with the Australian Square Kilometre Array Pathfinder (ASKAP). LGG 351 resides behind the M 83 group at a velocity range (cz) of ∼3500–4800 km s−1 within the rich Hydra-Centaurus overdensity region. We detect 40 sources with the discovery of a tidally interacting galaxy pair and two new H i sources that are not presented in previous optical catalogues. 23 out of 40 sources have new redshifts derived from the new H i data. This study is the largest WALLABY sub-sample to date and also allows us to further validate the performance of ASKAP and the data reduction pipeline askapsoft. Extended H i emission is seen in six galaxies indicating interaction within the group, although no H i debris is found. We also detect H i in a known ultra-faint dwarf galaxy (dw 1328−29), which demonstrates that it is not a satellite of the M 83 group as previously thought. In conjunction with multiwavelength data, we find that our galaxies follow the atomic gas fraction and baryonic Tully–Fisher scaling relations derived from the GALEX Arecibo SDSS Survey. In addition, majority of our galaxies fall within the star formation main sequence indicating inefficiency of gas removal processes in this loose galaxy group.

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Cold gas in a complete sample of group-dominant early-type galaxies

Cited by 42 publications

References 131 publications

Feedback from Active Galactic Nuclei in Galaxy Groups

Feedback from Active Galactic Nuclei in Galaxy Groups

The MASSIVE survey – XI. What drives the molecular gas properties of early-type galaxies

WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351

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