Outflows in Infrared‐Luminous Starbursts at
                    <i>z</i>
                    &lt; 0.5. II. Analysis and Discussion

Rupke, David S. N.; Veilleux, Sylvain; Sanders, D. B.

doi:10.1086/432889

Cited by 529 publications

(701 citation statements)

References 80 publications

(175 reference statements)

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“…Lower-mass galaxies were more efficient at producing outflows, in terms of both their higher mass loading factors and the higher fractions of disk gas that was ejected. Indeed, the scaling of the mass loading factor with circular velocity calculated from our simulations is consistent with previous observations (Rupke et al 2005;Arribas et al 2014;Chisholm et al 2015). In contrast, the gas that was ejected from the disk tends to have similar v v circ , recycling times, and reaccreted fractions across all halo masses.…”

Section: Discussionsupporting

confidence: 90%

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

Christensen

Davé

Governato

et al. 2016

ApJ

212

250

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We examine the scalings of galactic outflows with halo mass across a suite of 20 high-resolution cosmological zoom galaxy simulations covering halo masses in the range - . These simulations self-consistently generate outflows from the available supernova energy in a manner that successfully reproduces key galaxy observables, including the stellar mass-halo mass, Tully-Fisher, and mass-metallicity relations. We quantify the importance of ejective feedback to setting the stellar mass relative to the efficiency of gas accretion and star formation. Ejective feedback is increasingly important as galaxy mass decreases; we find an effective mass loading factor that scales asv circ 2.2 , with an amplitude and shape that are invariant with redshift. These scalings are consistent with analytic models for energy-driven wind, based solely on the halo potential. Recycling is common: about half of the outflow mass across all galaxy masses is later reaccreted. The recycling timescale is typically ∼1 Gyr, virtually independent of halo mass. Recycled material is reaccreted farther out in the disk and with typically ∼2-3 times more angular momentum. These results elucidate and quantify how the baryon cycle plausibly regulates star formation and alters the angular momentum distribution of disk material across the halo mass range where most cosmic star formation occurs.

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Section: Discussionsupporting

confidence: 90%

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

Christensen

Davé

Governato

et al. 2016

ApJ

212

250

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“…There is now considerable observational evidence for ejection of interstellar gas due to star formation activity (Shapley et al 2003;Rupke et al 2005;Weiner et al 2009;Martin et al 2012;Rubin et al 2013). While the overall impact of such processes is still debated, observations of rapidly Figure S2.…”

Section: S17 Supernova Feedbackmentioning

confidence: 99%

Galaxy formation in the Planck cosmology – I. Matching the observed evolution of star formation rates, colours and stellar masses

Henriques

White

Thomas

et al. 2015

Monthly Notices of the Royal Astronomical Society

615

747

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We have updated the Munich galaxy formation model to the Planck first-year cosmology, while modifying the treatment of baryonic processes to reproduce recent data on the abundance and passive fractions of galaxies from z = 3 down to z = 0. Matching these more extensive and more precise observational results requires us to delay the reincorporation of wind ejecta, to lower the surface density threshold for turning cold gas into stars, to eliminate ram-pressure stripping in haloes less massive than ∼ 10 14 M ⊙ , and to modify our model for radio mode feedback. These changes cure the most obvious failings of our previous models, namely the overly early formation of low-mass galaxies and the overly large fraction of them that are passive at late times. The new model is calibrated to reproduce the observed evolution both of the stellar mass function and of the distribution of star formation rate at each stellar mass. Massive galaxies (log M * / M ⊙ 11.0) assemble most of their mass before z = 1 and are predominantly old and passive at z = 0, while lower mass galaxies assemble later and, for log M * / M ⊙ 9.5, are still predominantly blue and star forming at z = 0. This phenomenological but physically based model allows the observations to be interpreted in terms of the efficiency of the various processes that control the formation and evolution of galaxies as a function of their stellar mass, gas content, environment and time.

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“…Such powerful outbursts are well observed in high-surface density galaxies over a wide range of masses and redshifts (e.g., Martin 1999;Pettini et al 2001;Heckman 2002;Veilleux et al 2005), including the ultraluminous infrared galaxies that host as much as half of the z 1 star formation in the universe (Rupke et al 2005). Their impact is extensive: they are believed to set the correlation between galaxy stellar mass and interstellar medium metallicity, (e.g., Tremonti et al 2004;Kewley & Ellison 2008;Mannucci et al 2010), they enrich the intergalactic medium with metals (e.g., Pichon et al 2003;Ferrara et al 2005;Martin et al 2010;Peeples et al 2014;Turner et al 2015), and they help determine the number density of faint galaxies (e.g., Scannapieco et al 2002;Benson et al 2003).…”

Section: Introductionmentioning

confidence: 99%

“…Moreover, the observation of the multiphase ISM is difficult: the hot phases of the outflow have only been detected in a few instances (e.g., Heckman et al 1990;Veilleux et al 2014;Wang et al 2014), and the cold phases of gas are often difficult to interpret. Nevertheless, the kinematics of neutral, atomic outflows has been studied in many cases through the absorption line as well as emission line measurements of Lyα, Hα, and Hβ, as Rupke et al 2005;Weiner et al 2009;Erb et al 2012;Kornei et al 2013;Arrigoni Battaia et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The Launching of Cold Clouds by Galaxy Outflows. Ii. The Role of Thermal Conduction

Brüggen

Scannapieco

2016

ApJ

132

123

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We explore the impact of electron thermal conduction on the evolution of radiatively cooled cold clouds embedded in flows of hot and fast material as it occurs in outflowing galaxies. Performing a parameter study of threedimensional adaptive mesh refinement hydrodynamical simulations, we show that electron thermal conduction causes cold clouds to evaporate, but it can also extend their lifetimes by compressing them into dense filaments. We distinguish between low column-density clouds, which are disrupted on very short times, and high-column density clouds with much longer disruption times that are set by a balance between impinging thermal energy and evaporation. We provide fits to the cloud lifetimes and velocities that can be used in galaxy-scale simulations of outflows in which the evolution of individual clouds cannot be modeled with the required resolution. Moreover, we show that the clouds are only accelerated to a small fraction of the ambient velocity because compression by evaporation causes the clouds to present a small cross-section to the ambient flow. This means that either magnetic fields must suppress thermal conduction, or that the cold clouds observed in galaxy outflows are not formed of cold material carried out from the galaxy.

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Outflows in Infrared‐Luminous Starbursts at z < 0.5. II. Analysis and Discussion

Cited by 529 publications

References 80 publications

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

Galaxy formation in the Planck cosmology – I. Matching the observed evolution of star formation rates, colours and stellar masses

The Launching of Cold Clouds by Galaxy Outflows. Ii. The Role of Thermal Conduction

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