The Temperature of Hot Gas in Galaxies and Clusters: Baryons Dancing to the Tune of Dark Matter

Hansen, Steen H.; Macciò, Andrea V.; Romano-Díaz, Emilio; Hoffman, Yehuda; Brüggen, M.; Scannapieco, Evan; Stinson, Greg

doi:10.1088/0004-637x/734/1/62

Cited by 11 publications

(12 citation statements)

References 43 publications

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“…The temperature profiles observed in Fig. 4 (first column, third row) are consistent with gas in hydrostatic equilibrium and are therefore the direct consequence of the gas and total mass distribution in the cluster (see Hansen et al 2011). For gas in pure hydrostatic equilibrium, the pressure obeys where ρ is the gas density, G is the gravitational constant, r is the spherical radius and M tot (< r ) is the total mass (gas, stars, DM and BHs) within r .…”

Section: Resultssupporting

confidence: 57%

How active galactic nucleus feedback and metal cooling shape cluster entropy profiles

Dubois

Devriendt

Teyssier

et al. 2011

Monthly Notices of the Royal Astronomical Society

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Observed clusters of galaxies essentially come in two flavours: non‐cool‐core clusters characterized by an isothermal temperature profile and a central entropy floor, and cool‐core clusters where temperature and entropy in the central region are increasing with radius. Using cosmological resimulations of a galaxy cluster, we study the evolution of its intracluster medium (ICM) gas properties, and through them we assess the effect of different (subgrid) modelling of the physical processes at play, namely gas cooling, star formation, feedback from supernovae and active galactic nuclei (AGNs). More specifically, we show that AGN feedback plays a major role in the pre‐heating of the protocluster as it prevents a high concentration of mass from collecting in the centre of the future galaxy cluster at early times. However, AGN activity during the cluster’s later evolution is also required to regulate the mass flow into its core and prevent runaway star formation in the central galaxy. Whereas the energy deposited by supernovae alone is insufficient to prevent an overcooling catastrophe, supernovae are responsible for spreading a large amount of metals at high redshift, enhancing the cooling efficiency of the ICM gas. As the AGN energy release depends on the accretion rate of gas on to its central black hole engine, the AGNs respond to this supernova‐enhanced gas accretion by injecting more energy into the surrounding gas, and as a result increase the amount of early pre‐heating. We demonstrate that the interaction between an AGN jet and the ICM gas that regulates the growth of the AGN’s black hole can naturally produce cool‐core clusters if we neglect metals. However, as soon as metals are allowed to contribute to the radiative cooling, only the non‐cool‐core solution is produced.

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Section: Resultssupporting

confidence: 57%

How active galactic nucleus feedback and metal cooling shape cluster entropy profiles

Dubois

Devriendt

Teyssier

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…Sommer-Larsen 2006;Johansson et al 2009;Rasmussen & Ponman 2009;Hansen et al 2011) and observations (e.g. Owen & Warwick 2009, Anderson et al 2013).…”

Section: Discussionmentioning

confidence: 99%

From discs to bulges: effect of mergers on the morphology of galaxies

Kannan¹,

Macciò²,

Fontanot³

et al. 2015

Mon. Not. R. Astron. Soc.

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We study the effect of mergers on the morphology of galaxies by means of the simulated merger tree approach first proposed by Moster et al. This method combines N-body cosmological simulations and semi-analytic techniques to extract realistic initial conditions for galaxy mergers. These are then evolved using high resolution hydrodynamical simulations, which include dark matter, stars, cold gas in the disc and hot gas in the halo. We show that the satellite mass accretion is not as effective as previously thought, as there is substantial stellar stripping before the final merger. The fraction of stellar disc mass transferred to the bulge is quite low, even in the case of a major merger, mainly due to the dispersion of part of the stellar disc mass into the halo. We confirm the findings of Hopkins et al., that a gas rich disc is able to survive major mergers more efficiently. The enhanced star formation associated with the merger is not localised to the bulge of galaxy, but a substantial fraction takes place in the disc too. The inclusion of the hot gas reservoir in the galaxy model contributes to reducing the efficiency of bulge formation. Overall, our findings suggest that mergers are not as efficient as previously thought in transforming discs into bulges. This possibly alleviates some of the tensions between observations of bulgeless galaxies and the hierarchical scenario for structure formation.

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“…The velocity, in turn, depends only on the depth of the potential well of the group/cluster, which is dominated by dark matter (DM), and to first order this is also true of the temperature of the ICM (e.g. Voit et al 2002; Hansen et al 2011). Therefore, we expect our results to be insensitive to uncertain subgrid processes such as star formation and feedback.…”

Section: Simulations and Analysismentioning

confidence: 99%

The competition between confinement and ram pressure and its implications for galaxies in groups and clusters

Bahé

McCarthy

Crain

et al. 2012

Monthly Notices of the Royal Astronomical Society

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Ram pressure stripping of the hot gas that surrounds normal galaxies as they fall into groups and clusters (also referred to as ‘strangulation’ or ‘starvation’) is generally thought to shut down star formation on a time‐scale of a few Gyr. However, it has recently been suggested, on the basis of X‐ray–optical scaling relations of galaxies in the field and the group/cluster environment, that confinement pressure by the intracluster medium can actually lead to an increase in the mass of hot gas surrounding these galaxies. We investigate the competition between pressure confinement and ram pressure stripping for satellite galaxies in orbit about galaxy groups and clusters using simple analytic models and detailed cosmological hydrodynamic simulations. It is found that, independent of host mass, ram pressure is generally dominant over confinement pressure – only ∼16 per cent of galaxies find themselves in the reverse situation. Furthermore, these galaxies have, on average, less hot gas than ram‐pressure‐dominated ones, contrary to simple expectations. This is explained by the fact that the small number of galaxies which are confinement dominated are typically at first or second apocentre and have therefore already been maximally affected by ram pressure stripping around first pericentre. Our results are shown to be insensitive to host halo mass; we argue that the same is true for uncertain subgrid processes, such as feedback.

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The Temperature of Hot Gas in Galaxies and Clusters: Baryons Dancing to the Tune of Dark Matter

Cited by 11 publications

References 43 publications

How active galactic nucleus feedback and metal cooling shape cluster entropy profiles

How active galactic nucleus feedback and metal cooling shape cluster entropy profiles

From discs to bulges: effect of mergers on the morphology of galaxies

The competition between confinement and ram pressure and its implications for galaxies in groups and clusters

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