The ATLAS3D project - IV. The molecular gas content of early-type galaxies★

Young, Lisa M.; Bureau, Martin; Davis, Timothy A.; Combes, F.; McDermid, Richard M.; Alatalo, Katherine; Blitz, Leo; Bois, Maxime; Bournaud, F.; Cappellari, Michele; Davies, Roger L.; Zeeuw, P. T. de; Emsellem, Éric; Khochfar, Sadegh; Krajnović, Davor; Küntschner, H.; Lablanche, Pierre Yves; Morganti, Raffaella; Naab, Thorsten; Oosterloo, Tom; Sarzi, Marc; Scott, Nicholas; Serra, P.; Weijmans, Anne-Marie

doi:10.1111/j.1365-2966.2011.18561.x

Cited by 363 publications

(334 citation statements)

References 84 publications

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“…Mergers between the BCG and donor galaxies are likely rare due to the dearth of gas-rich galaxies at the centres of rich clusters (eg. Young et al 2011) and because the cluster's high velocity dispersion decreases the merger rate. Ram pressure stripping by the ICM of a gas rich galaxy that passes close to the BCG seems similarly unlikely.…”

Section: Origin Of the Molecular Gasmentioning

confidence: 99%

“…Molecular gas is much more tightly bound to its host galaxy than atomic gas and is retained on all but the most eccentric orbits within a cluster (eg. Young et al 2011). Observations of Virgo cluster members have shown that galaxies with strong HI deficiencies have minimal molecular gas deficiencies (Kenney & Young 1989;di Serego Alighieri et al 2007;Grossi et al 2009).…”

Section: Origin Of the Molecular Gasmentioning

confidence: 99%

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ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

Russell

McNamara

Fabian

et al. 2016

Mon. Not. R. Astron. Soc.

105

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We present ALMA observations of the CO(1-0) and CO(3-2) line emission tracing filaments of cold molecular gas in the central galaxy of the cluster PKS 0745-191. The total molecular gas mass of 4.6±0.3×10 9 M , assuming a Galactic X CO factor, is divided roughly equally between three filaments each extending radially 3 − 5 kpc from the galaxy centre. The emission peak is located in the SE filament ∼ 1 arcsec (2 kpc) from the nucleus. The velocities of the molecular clouds in the filaments are low, lying within ±100 km s −1 of the galaxy's systemic velocity. Their FWHMs are less than 150 km s −1 , which is significantly below the stellar velocity dispersion. Although the molecular mass of each filament is comparable to a rich spiral galaxy, such low velocities show that the filaments are transient and the clouds would disperse on < 10 7 yr timescales unless supported, likely by the indirect effect of magnetic fields. The velocity structure is inconsistent with a merger origin or gravitational free-fall of cooling gas in this massive central galaxy. If the molecular clouds originated in gas cooling even a few kpc from their current locations their velocities would exceed those observed. Instead, the projection of the N and SE filaments underneath X-ray cavities suggests they formed in the updraft behind bubbles buoyantly rising through the cluster atmosphere. Direct uplift of the dense gas by the radio bubbles appears to require an implausibly high coupling efficiency. The filaments are coincident with low temperature X-ray gas, bright optical line emission and dust lanes indicating that the molecular gas could have formed from lifted warmer gas that cooled in situ.

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Section: Origin Of the Molecular Gasmentioning

confidence: 99%

Section: Origin Of the Molecular Gasmentioning

confidence: 99%

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

Russell

McNamara

Fabian

et al. 2016

Mon. Not. R. Astron. Soc.

105

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“…Earlier work has focused on the ATLAS 3D sample (e.g., Emsellem et al 2011;Krajnović et al 2011;Young et al 2011;Cappellari et al 2013), a volume-limited sample ( < D 42 Mpc) of all nearby early-type galaxies with < -M 21.5 K mag. Using the ATLAS 3D galaxies, there has been suggestive evidence that galaxies with net rotation (i.e., fast rotators) have lower L X than slow rotators at a given stellar mass.…”

Section: Introductionmentioning

confidence: 99%

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Goulding

Greene

et al. 2016

ApJ

114

156

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Studies of the physical properties of local elliptical galaxies are shedding new light on galaxy formation. Here we present the hot-gas properties of 33 early-type systems within the MASSIVE galaxy survey that have archival Chandra X-ray observations, and we use these data to derive X-ray luminosities (L X,gas ) and plasma temperatures (T gas ) for the diffuse gas components. We combine this with the ATLAS 3D survey to investigate the X-ray-optical properties of a statistically significant sample of early-type galaxies across a wide range of environments. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, we deduce that all early types (independent of galaxy mass, environment, and rotational support) follow a universal scaling law such that µL T X,gas gas 4.5 . We further demonstrate that the scatter in L X,gas around both K-band luminosity (L K ) and the galaxy stellar velocity dispersion (s e ) is primarily driven by T gas , with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the gas origin directly to either stellar mass or galaxy potential. Indeed, our data require a steeper relation between L L , K X,gas , and s e than predicted by standard mass-loss models. Finally, we find that T gas is set by the galaxy potential inside the optical effective radius. We conclude that within the innermost 10-30 kpc region, early types maintain pressure-supported hot gas, with a minimum T gas set by the virial temperature, but the majority show evidence for additional heating.

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“…Yet, there are signs of possible low-level SF within the stellar body. For instance, NGC 4203 contains 2.5×10 7 M of H 2 in the centre (Welch & Sage 2003;Young et al 2011). Hubble Space Telescope observations show nuclear dust structures in the very centre of the galaxy (300 pc radius; Erwin & Sparke 2003).…”

Section: Introductionmentioning

confidence: 99%

Star formation in the outer regions of the early-type galaxy NGC 4203

Yıldız¹,

Serra

Oosterloo

et al. 2015

Monthly Notices of the Royal Astronomical Society

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NGC 4203 is a nearby early-type galaxy surrounded by a very large, low-column-density H i disc. In this paper we study the star formation efficiency in the gas disc of NGC 4203 by using the UV, deep optical imaging and infrared data. We confirm that the H i disc consists of two distinct components: an inner star forming ring with radius from ∼1 to ∼3 R e f f , and an outer disc. The outer H i disc is 9 times more massive than the inner H i ring. At the location of the inner H i ring we detect spiral-like structure both in the deep g − r image and in the 8 µm Spitzer-IRAC image, extending in radius up to ∼ 3 R e f f . These two gas components have a different star formation efficiency likely due to the different metallicity and dust content. The inner component has a star formation efficiency very similar to the inner regions of late-type galaxies. Although the outer component has a very low star formation efficiency, it is similar to that of the outer regions of spiral galaxies and dwarfs. We suggest that these differences can be explained with different gas origins for the two components such as stellar mass loss for the inner H i ring and accretion from the inter galactic medium (IGM) for the outer H i disc. The low level star formation efficiency in the outer H i disc is not enough to change the morphology of NGC 4203, making the depletion time of the H i gas much too long.

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The ATLAS3D project - IV. The molecular gas content of early-type galaxies★

Cited by 363 publications

References 84 publications

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Star formation in the outer regions of the early-type galaxy NGC 4203

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