On the onset of galactic winds in quiescent star forming galaxies

Dubois, Yohan; Teyssier, Romain

doi:10.1051/0004-6361:20078326

Cited by 281 publications

(377 citation statements)

References 79 publications

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“…We employ three different SN feedback models implemented in ramses: (i) a thermal feedback (simulation 'T'), (ii) a kinetic feedback (simulation 'K') and (iii) a delayed cooling model (simulation 'D'). We use a weak "thermal" SN feedback which releases only internal energy in the neighboring cells (Dubois & Teyssier 2008). The kinetic SN feedback (Dubois & Teyssier 2008) is modeled to reproduce a Sedov blast wave, where energy, mass and momentum are deposited in the neighboring gas cells.…”

Section: Sn Feedbackmentioning

confidence: 99%

“…We use a weak "thermal" SN feedback which releases only internal energy in the neighboring cells (Dubois & Teyssier 2008). The kinetic SN feedback (Dubois & Teyssier 2008) is modeled to reproduce a Sedov blast wave, where energy, mass and momentum are deposited in the neighboring gas cells. The third model is called delayed cooling (Stinson et al 2006;Teyssier et al 2013).…”

Section: Sn Feedbackmentioning

confidence: 99%

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Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Habouzit

Volonteri²,

Dubois³

2017

Monthly Notices of the Royal Astronomical Society

239

223

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Massive black holes (BHs) inhabit local galaxies, including the Milky Way and some dwarf galaxies. BH formation, occurring at early cosmic times, must account for the properties of BHs in today's galaxies, notably why some galaxies host a BH, and others do not. We investigate the formation, distribution and growth of BH 'seeds' by using the adaptive mesh refinement code Ramses. We develop an implementation of BH formation in dense, low-metallicity environments, as advocated by models invoking the collapse of the first generation of stars, or of dense nuclear star clusters. The seed masses are computed one-by-one on-the-fly, based on the star formation rate and the stellar initial mass function. This self-consistent method to seed BHs allows us to study the distribution of BHs in a cosmological context and their evolution over cosmic time. We find that all high-mass galaxies tend to host a BH, whereas low-mass counterparts have a lower probability of hosting a BH. After the end of the epoch of BH formation, this probability is modulated by the growth of the galaxy. The simulated BHs connect to low-redshift observational samples, and span a similar range in accretion properties as Lyman-Break Analogs. The growth of BHs in low-mass galaxies is stunted by strong supernova feedback. The properties of BHs in dwarf galaxies thus remain a testbed for BH formation. Simulations with strong supernova feedback, which is able to quench BH accretion in shallow potential wells, produce galaxies and BHs in better agreement with observational constraints.

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Section: Sn Feedbackmentioning

confidence: 99%

Section: Sn Feedbackmentioning

confidence: 99%

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Habouzit

Volonteri²,

Dubois³

2017

Monthly Notices of the Royal Astronomical Society

239

223

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“…Stellar particles are seeded locally from a Poisson process. Supernova feedback is implemented based on the model of Dubois & Teyssier (2008), in which each newly formed star particle releases a fraction η = 0.1 of its mass and metals with a yield of y = 0.1 into its surrounding cells through supernovae (SNe) after 10 Myr (this implies that 1 per cent of the time integrated global star formation rate is returned as metals to the ISM). In addition, each supernova injects an energy of 10 51 erg into the surrounding ISM which regulates the star formation efficiency at galaxy scale halo masses.…”

Section: Modelling Cooling Star Formation Stellar Feedback and Chemmentioning

confidence: 99%

Rhapsody-G simulations I: the cool cores, hot gas and stellar content of massive galaxy clusters

Hahn

Martizzi

et al. 2017

Mon. Not. R. Astron. Soc.

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We present the Rhapsody-G suite of cosmological hydrodynamic AMR zoom simulations of ten massive galaxy clusters at the M vir ∼ 10 15 M scale. These simulations include cooling and sub-resolution models for star formation and stellar and supermassive black hole feedback. The sample is selected to capture the whole gamut of assembly histories that produce clusters of similar final mass. We present an overview of the successes and shortcomings of such simulations in reproducing both the stellar properties of galaxies as well as properties of the hot plasma in clusters. In our simulations, a long-lived cool-core/non-cool core dichotomy arises naturally, and the emergence of non-cool cores is related to low angular momentum major mergers. Nevertheless, the cool-core clusters exhibit a low central entropy compared to observations, which cannot be alleviated by thermal AGN feedback. For cluster scaling relations we find that the simulations match well the M 500 − Y 500 scaling of Planck SZ clusters but deviate somewhat from the observed X-ray luminosity and temperature scaling relations in the sense of being slightly too bright and too cool at fixed mass, respectively. Stars are produced at an efficiency consistent with abundance matching constraints and central galaxies have star formation rates consistent with recent observations. While our simulations thus match various key properties remarkably well, we conclude that the shortcomings strongly suggest an important role for non-thermal processes (through feedback or otherwise) or thermal conduction in shaping the intra-cluster medium.

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“…A few studies have proposed numerical schemes for efficient thermal feedback in smoothed particle hydrodynamics (SPH) simulations (e.g., Kay, Thomas & Theuns 2003;Dalla Vecchia & Schaye 2012). Depositing the SN energy in the kinetic form is a more popular implementation in the literature, which has been shown to have significant feedback effects (e.g., Navarro & White 1993;Cen & Ostriker 2000;Kawata 2001;Dubois & Teyssier 2008;Oppenheimer et al 2012). Some other approaches of numerical SN feedback are: consider that a part of the neighbouring gas undergoes adiabatic evolution by turning off radiative cooling temporarily (e.g., Mori et al 1997;Thacker & Couchman 2000;Brook et al 2005;Stinson et al 2006;Piontek & Steinmetz 2011); distribute SN energy to hot and cold gas phases separately (e.g., Marri & White 2003;Scannapieco et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Galactic outflow and diffuse gas properties at z ≥ 1 using different baryonic feedback models

Barai

Monaco

Murante

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We measure and quantify properties of galactic outflows and diffuse gas at z 1 in cosmological hydrodynamical simulations performed using the GADGET-3 code containing novel baryonic feedback models. Our sub-resolution model, MUPPI, implements supernova feedback using fully local gas properties, where the wind velocity and mass loading are not given as input. We find the following trends at z = 2 by analysing central galaxies having a stellar mass higher than 10 9 M ⊙ . The outflow velocity and mass outflow rate (Ṁ out ) exhibit positive correlations with galaxy mass and with the star formation rate (SFR). However, most of the relations present a large scatter. The outflow mass loading factor (η) is between 0.2 − 10, with an average η ∼ 1. The comparison Effective model generates a constant outflow velocity as expected from the input fixed wind kick speed, and a negative correlation of η with halo mass as opposed to the fixed input η. The shape of the outflows is bi-polar in 95% of the MUPPI galaxies. The MUPPI model produces colder galaxy cores and flatter gas metallicity radial profiles than the Effective model. The number fraction of galaxies where outflow is detected decreases at lower redshifts, but remains more than 80% over z = 1 − 5. High SF activity at z ∼ 2 − 4 drives strong outflows, causing the positive and steep correlations of velocity andṀ out with SFR. The outflow velocity correlation with SFR becomes flatter at z = 1, and η displays a negative correlation with halo mass in massive galaxies. Our study demonstrates that both the MUPPI and Effective models produce significant outflows at ∼ 1/10 of the virial radius; at the same time shows that the properties of outflows generated can be different from the input speed and mass loading in the Effective model. Our MUPPI model, using local properties of gas in the sub-resolution recipe, is able to develop galactic outflows whose properties correlate with global galaxy properties, and consistent with observations.

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On the onset of galactic winds in quiescent star forming galaxies

Cited by 281 publications

References 79 publications

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Rhapsody-G simulations I: the cool cores, hot gas and stellar content of massive galaxy clusters

Galactic outflow and diffuse gas properties at z ≥ 1 using different baryonic feedback models

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