The impact of feedback on cosmological gas accretion

Nelson, Dylan; Genel, Shy; Vogelsberger, Mark; Springel, Volker; Sijacki, Debora; Torrey, Paul; Hernquist, Lars

doi:10.1093/mnras/stv017

Cited by 164 publications

(168 citation statements)

References 92 publications

(122 reference statements)

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“…The central regions of the clusters are usually characterised by decoupled motions of dark matter and gas. This region is very close to the central galaxy and the properties of the gas flow are influenced by the dynamics of infalling satellites and by the effect of feedback and cooling on the gas accretion mode (Kereš et al 2005;Dekel & Birnboim 2006;Ocvirk et al 2008;Dekel et al 2009;van de Voort et al 2011;Nelson et al 2015). On the other hand at the outskirts of the clusters the dark matter radial velocity is well coupled to the gas accretion velocity at all redshifts.…”

Section: Growth Of the Icm Mass Profile And Its Effect On Icm Metallimentioning

confidence: 99%

Rhapsody-G simulations – II. Baryonic growth and metal enrichment in massive galaxy clusters

Martizzi

Hahn

et al. 2016

Mon. Not. R. Astron. Soc.

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We study the evolution of the stellar component and the metallicity of both the intracluster medium and of stars in massive (M vir « 6ˆ10 14 M d {h) simulated galaxy clusters from the Rhapsody-G suite in detail and compare them to observational results. The simulations were performed with the AMR code RAMSES and include the effect of AGN feedback at the sub-grid level. AGN feedback is required to produce realistic galaxy and cluster properties and plays a role in mixing material in the central regions and regulating star formation in the central galaxy. In both our low and high resolution runs with fiducial stellar yields, we find that stellar and ICM metallicities are a factor of two lower than in observations. We find that cool core clusters exhibit steeper metallicity gradients than non-cool core clusters, in qualitative agreement with observations. We verify that the ICM metallicities measured in the simulation can be explained by a simple "regulator" model in which the metallicity is set by a balance of stellar yield and gas accretion. It is plausible that a combination of higher resolution and higher metal yield in AMR simulation would allow the metallicity of simulated clusters to match observed values; however this hypothesis needs to be tested with future simulations. Comparison to recent literature highlights that results concerning the metallicity of clusters and cluster galaxies might depend sensitively on the scheme chosen to solve the hydrodynamics.

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Section: Growth Of the Icm Mass Profile And Its Effect On Icm Metallimentioning

confidence: 99%

Rhapsody-G simulations – II. Baryonic growth and metal enrichment in massive galaxy clusters

Martizzi

Hahn

et al. 2016

Mon. Not. R. Astron. Soc.

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“…In addition to accretion, feedback driven by star formation may change the nature and properties of the gas in the CGM Nelson et al 2015Nelson et al , 2016Kauffmann et al 2016;Liang et al 2016). Massive young stars inject energy and/or momentum into outflows (Veilleux et al 2005;Heckman et al 2011;Borthakur et al 2014;Heckman et al 2015;Heckman & Borthakur 2016) that may travel into the CGM, enriching it with metals, shock-heating the cooler CGM clouds, and possibly even expelling/unbinding the CGM (Borthakur et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The Properties of the Circumgalactic Medium in Red and Blue Galaxies: Results From the Cos-Gass+cos-Halos Surveys

Borthakur

Heckman

Tumlinson

et al. 2016

ApJ

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We use the combined data from the COS-GASS and COS-Halos surveys to characterize the Circum-Galactic Medium (CGM) surrounding typical low-redshift galaxies in the mass range  *~-M M 10 9.5 11.5, and over a range of impact parameters extending to just beyond the halo virial radius (R vir ). We find the radial scale length of the distributions of the equivalent widths of the Lyαand Si III absorbers to be ∼1 and ∼0.4R vir , respectively. The radial distribution of equivalent widths is relatively uniform for the blue galaxies, but highly patchy (i.e., it has a low covering fraction) for the red galaxies. We also find that the Lyαand Si III equivalent widths show significant positive correlations with the specific star formation rate (sSFR) of the galaxy. We find a surprising lack of correlations between the halo mass (virial velocity) and either the velocity dispersions or velocity offsets of the Lyαlines. The ratio of the velocity offset to the velocity dispersion for the Lyαabsorbers has a mean value of ∼4, suggesting that a given line of sight is intersecting a dynamically coherent structure in the CGM, rather than a sea of orbiting clouds. The kinematic properties of the CGM are similar in the blue and red galaxies, although we find that a significantly larger fraction of the blue galaxies have large Lyαvelocity offsets (>200 km s −1 ). We show that-if the CGM clouds represent future fuel for star formation-our new results could imply a large drop in the sSFR across the galaxy mass-range we probe.

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“…Agertz et al 2011;Brook et al 2011;De Rossi et al 2012;Padilla et al 2014;Nelson et al 2015). In particular, SN feedback plays a critical role in determining the fraction of disc components, as well as mergers and interactions (e.g Domínguez-Tenreiro et al 1998;Scannapieco et al 2009;Guedes et al 2011;Sales et al 2012;Lagos et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Angular momentum evolution for galaxies in a Λ-CDM scenario

Pedrosa

Tissera

2015

A&A

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Context. Galaxy formation in the current cosmological paradigm is a very complex process in which inflows, outflows, interactions, and mergers are common events. These processes can redistribute the angular momentum content of baryons. Recent observational results suggest that disc formed conserving angular momentum while elliptical galaxies, although they lose angular momentum, determine a correlation between the specific angular momentum of the galaxy and the stellar mass. These observations provide stringent constraints for galaxy formation models in a hierarchical clustering scenario. Aims. We aim to analyse the specific angular momentum content of the disc and bulge components as a function of virial mass, stellar mass, and redshift. We also estimate the size of the simulated galaxies and compare them with observations. Methods. We use cosmological hydrodynamical simulations that include an effective, physically motivated supernova feedback which is able to regulate the star formation in haloes of different masses. We analyse the morphology and formation history of a sample of galaxies in a cosmological simulation by performing a bulge-disc decomposition of the analysed systems and their progenitors. We estimate the angular momentum content of the stellar and gaseous discs, stellar bulges, and total baryons. Results. In agreement with recent observational findings, our simulated galaxies have disc and spheroid components whose specific angular momentum content determine correlations with the stellar and dark matter masses with the same slope, although the spheroidal components are offset by a fixed fraction. The average angular momentum efficiency for the simulated discs is η ∼ 1, while for bulges it is η ∼ 0.10−0.20. For the simulated sample, the correlations found for the specific angular momentum content as a function of virial mass or stellar mass are found not to evolve significantly with redshift (up to z ∼ 2). Both dynamical components seem to move along the correlations as they evolve. The total specific angular momentum of galaxies occupy different positions filling the gap between pure rotational-dominated and dispersion-dominated systems. The scaling relations derived from the simulated galaxies determine a similar relation with the virial radius, which is in agreement with recent observations.

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The impact of feedback on cosmological gas accretion

Cited by 164 publications

References 92 publications

Rhapsody-G simulations – II. Baryonic growth and metal enrichment in massive galaxy clusters

Rhapsody-G simulations – II. Baryonic growth and metal enrichment in massive galaxy clusters

The Properties of the Circumgalactic Medium in Red and Blue Galaxies: Results From the Cos-Gass+cos-Halos Surveys

Angular momentum evolution for galaxies in a Λ-CDM scenario

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