Cold gas accretion in galaxies

Sancisi, R.; Fraternali, Filippo; Oosterloo, Tom; Hulst, J. M. van der

doi:10.1007/s00159-008-0010-0

Cited by 579 publications

(731 citation statements)

References 120 publications

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“…5, left panels). Although not as spectacular as in IZw18, elongated extraplanar features are quite common in disk galaxies (e.g., NGC925, Pisano et al 1998, and the many other examples given in the review by Sancisi et al 2008). Extraplanar gas is also found in our own galaxy, where the existence of gas clouds falling in is long known (Oort 1966;Blitz et al 1999;van Woerden et al 2004;Wakker et al 2007Wakker et al , 2008.…”

Section: Neutral Gas Observationsmentioning

confidence: 83%

“…The scatter of the relationships with stellar mass and Hubble type is significant, so that neither the mass nor the Hubble type fully determines the gas fraction of a galaxy (Kannappan 2004;Kannappan et al 2013;Wang et al 2011). Sancisi et al (2008) summarize radio observations of HI cloud complexes, tails and filaments in and around local galaxies, suggesting ongoing minor mergers and recent arrival of external gas. The HI image of the dwarf galaxy IZw18 in Fig.…”

Section: Neutral Gas Observationsmentioning

confidence: 93%

“…The existence of HVCs agrees qualitatively with theoretical expectations; however, they pose an observational problem common to many other galaxies. Their mass infall rate is estimated to be ∼ 0.1-0.2 M year −1 which is one order of magnitude too small to maintain the MW SFR of ∼ 1-2 M year −1 (Sancisi et al 2008;Fraternali 2014), and thus inconsistent with the MW being in a stationary state sustained by HVCs (Sect. 2.1).…”

Section: Neutral Gas Observationsmentioning

confidence: 99%

“…This poses a problem. Several possibilities have been explored (e.g., Sancisi et al 2008;Joung et al 2012) but the issue has not been settled yet. Details of the interaction between a cold metal-poor gas stream and a galaxy disk remain to be modeled.…”

Section: What We Understand and What We Do Not And Pathways To Follmentioning

confidence: 99%

“…We limit ourselves to the global picture, leaving aside details about star-formation processes Gnedin et al 2014), stellar and active galactic nucleus (AGN) feedback (Silich et al 2010;Hopkins et al 2013a;Trujillo-Gomez et al 2013), secular evolution (Binney 2013;Kormendy 2013), dense cluster environments (Santini 2011;Kravtsov and Borgani 2012), and the growth of black holes (BH) through cosmic gas accretion (Husemann et al 2011;Chen et al 2013). Other recent reviews covering cosmic gas accretion from different perspectives are in Sancisi et al (2008), Fig. 1 Zoom into a simulated halo at z = 2 with halo mass M halo 10 12 M (from Schaye et al 2010).…”

Section: Introductionmentioning

confidence: 99%

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Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

171

130

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Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

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Section: Neutral Gas Observationsmentioning

confidence: 83%

Section: Neutral Gas Observationsmentioning

confidence: 93%

Section: Neutral Gas Observationsmentioning

confidence: 99%

Section: What We Understand and What We Do Not And Pathways To Follmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

171

130

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On the Origin of Gaseous Galaxy Halos – Low‐Column Density Gas in the Milky Way Halo

Bekhti

Winkel

Richter

et al. 2011

Reviews in Modern Astronomy

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Recent observations show that spiral galaxies are surrounded by extended gaseous halos as predicted by the hierarchical structure formation scenario. The origin and nature of extraplanar gas is often unclear since the halo is continuously fueled by different circulation processes as part of the on-going formation and evolution of galaxies (e.g., outflows, galaxy merging, and gas accretion from the intergalactic medium). We use the Milky Way as a laboratory to study neutral and mildly ionised gas located in the inner and outer halo. Using spectral line absorption and emission measurements in different wavelength regimes we obtain detailed information on the physical conditions and the distribution of the gas. Such studies are crucial for our understanding of the complex interplay between galaxies and their gaseous environment as part of the formation and evolution of galaxies. Our analysis suggests that the column-density distribution and physical properties of gas in the Milky Way halo are very similar to that around other disk galaxies at low and high redshifts.

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Cool gas accretion, thermal evaporation, and quenching of star formation in elliptical galaxies

Nipoti¹

2009

Astron Nachr

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The most evident features of colour-magnitude diagrams of galaxies are the red sequence of quiescent galaxies, extending up to the brightest elliptical galaxies, and the blue cloud of star-forming galaxies, which is truncated at a luminosity L ∼ L * . The truncation of the blue cloud indicates that in the most massive systems star formation must be quenched. For this to happen the virial-temperature galactic gas must be kept hot and any accreted cold gas must be heated. The elimination of accreted cold gas can be due to thermal evaporation by the hot interstellar medium, which in turn is prevented from cooling by feedback from active galactic nuclei. Need for quenching of star formation in galaxiesColour-magnitude diagrams of galaxies are dominated by the red sequence of quiescent galaxies and the blue cloud of star-forming galaxies (Blanton et al. 2003;Baldry et al. 2004), with a green valley in between, in which a minority of galaxies lie (Driver et al. 2006). While the red sequence extends up to the bright end of the galaxy distribution, the blue cloud is truncated at a luminosity L ∼ L * , so there are not very massive blue, star-forming galaxies. Such a feature can be reproduced in galaxy formation models only assuming that star formation is effectively quenched in the galaxies with the deepest potential wells (e.g. Bower et al. 2006;Croton et al. 2006;Cattaneo et al. 2008). What are the processes responsible for this quenching is still matter of debate.For star formation to cease in a galactic system, it is necessary that (1) hot (virial-temperature) gas does not cool efficiently and (2) accreted cool gas is heated before it can form stars (Binney 2004). Task (1) can be accomplished by feedback from Active Galactic Nuclei (AGN). Though the details of how AGN feedback works are controversial, empirical evidence that this mechanism is effective comes from studies of cool cores in galaxy clusters (Birzan et al. 2004;McNamara & Nulsen 2007), suggesting that also in massive galaxies virial-temperature gas is kept hot by the intermittent jets of the central radio source (Binney 2004;Nipoti & Binney 2005). Other mechanisms, such as gravitational heating by clumpy accretion (Dekel & Birnboim 2008;Khochfar & Ostriker 2008), can contribute to prevent virial-temperature gas from cooling, but non-gravitational heating is necessary to drive gas out of the galaxy potenCorresponding author: carlo.nipoti@unibo.it tial well and thus explain, for instance, why the intracluster medium is metal-enriched (Renzini 1997). Task (2) is not less important than task (1), because there is growing evidence that cold gas accretion is a common phenomenon during the galaxy lifetimes: the strongest evidence for accretion comes from observation of late-type galaxies (Sancisi et al. 2008), but cold gas structures are observed also around early-type galaxies (Morganti et al. 2006). Nevertheless, not so much attention has been devoted to finding the mechanism responsible for eliminating recently accreted cool gas. Here I briefly review the pr...

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Cold gas accretion in galaxies

Cited by 579 publications

References 120 publications

Star formation sustained by gas accretion

Star formation sustained by gas accretion

On the Origin of Gaseous Galaxy Halos – Low‐Column Density Gas in the Milky Way Halo

Cool gas accretion, thermal evaporation, and quenching of star formation in elliptical galaxies

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