Breathing Fire: How Stellar Feedback Drives Radial Migration, Rapid Size Fluctuations, and Population Gradients in Low-Mass Galaxies

El-Badry, Kareem; Wetzel, Andrew; Geha, Marla; Hopkins, Philip F.; Kereš, Dušan; Chan, T. K.; Faucher-Giguère, Claude-André

doi:10.3847/0004-637x/820/2/131

Cited by 285 publications

(336 citation statements)

References 98 publications

Supporting

Mentioning

309

Contrasting

Order By: Relevance

“…Several of these mechanisms may play a role in preferentially stalling disk formation in low mass galaxies. Feedback through stellar winds and supernovae can effectively blow out gas and dynamically heat stars in low mass dwarf galaxies ( 10 9.5 M ; e.g, Wheeler et al 2015;El-Badry et al 2016). We note that we find no trend between V rot /σ g and SF R at fixed mass among the galaxies studied in this sample (9.2 < log M * /M < 11), indicating that such feedback mechanisms may only assume a secondary role in disturbing the gas kinematics in these galaxies.…”

Section: Discussionmentioning

confidence: 99%

KINEMATIC DOWNSIZING AT z ∼ 2

Simons

Kassin

Trump

et al. 2016

ApJ

View full text Add to dashboard Cite

We present results from a survey of the internal kinematics of 49 star-forming galaxies at z ∼ 2 in the CANDELS fields with the Keck/MOSFIRE spectrograph (SIGMA, Survey in the near-Infrared of Galaxies with Multiple position Angles). Kinematics (rotation velocity V rot and integrated gas velocity dispersion σ g ) are measured from nebular emission lines which trace the hot ionized gas surrounding star-forming regions. We find that by z ∼ 2, massive star-forming galaxies (log M * /M 10.2) have assembled primitive disks: their kinematics are dominated by rotation, they are consistent with a marginally stable disk model, and they form a Tully-Fisher relation. These massive galaxies have values of V rot /σ g which are factors of 2-5 lower than local well-ordered galaxies at similar masses. Such results are consistent with findings by other studies. We find that low mass galaxies (log M * /M 10.2) at this epoch are still in the early stages of disk assembly: their kinematics are often supported by gas velocity dispersion and they fall from the Tully-Fisher relation to significantly low values of V rot . This "kinematic downsizing" implies that the process(es) responsible for disrupting disks at z ∼ 2 have a stronger effect and/or are more active in low mass systems. In conclusion, we find that the period of rapid stellar mass growth at z ∼ 2 is coincident with the nascent assembly of low mass disks and the assembly and settling of high mass disks.

show abstract

Section: Discussionmentioning

confidence: 99%

KINEMATIC DOWNSIZING AT z ∼ 2

Simons

Kassin

Trump

et al. 2016

ApJ

View full text Add to dashboard Cite

show abstract

“…Within the Local Group, modeling of the orbit and star-formation history of Leo I suggest that it experienced a small burst of star formation at pericentric passage prior to being quenched, consistent with being initiated by ram pressure Boylan-Kolchin et al 2013;Weisz et al 2014). This increase in star formation, driven by interaction with the host CGM, can inject energy into the ISM of the satellite, puffing up the system and thereby making it more susceptible to stripping (Stinson et al 2007;El-Badry et al 2016, but see also Emerick et al 2016). High-resolution hydrodynamic simulations of Milky Way-or Local Group-like environments should provide a robust means for studying the possible importance of feedback in increasing the efficiency of stripping (e.g.…”

Section: The Efficacy Of Stripping: Refining Our Analysismentioning

confidence: 99%

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Fillingham

Cooper

Pace

et al. 2016

Mon. Not. R. Astron. Soc.

121

123

View full text Add to dashboard Cite

Recent studies of galaxies in the local Universe, including those in the Local Group, find that the efficiency of environmental (or satellite) quenching increases dramatically at satellite stellar masses below ∼ 10 8 M . This suggest a physical scale where quenching transitions from a slow "starvation" mode to a rapid "stripping" mode at low masses. We investigate the plausibility of this scenario using observed HI surface density profiles for a sample of 66 nearby galaxies as inputs to analytic calculations of ram-pressure and turbulent viscous stripping. Across a broad range of host properties, we find that stripping becomes increasingly effective at M * 10 8−9 M , reproducing the critical mass scale observed. However, for canonical values of the circumgalactic medium density (n halo < 10 −3.5 cm −3 ), we find that stripping is not fully effective; infalling satellites are, on average, stripped of only 40 − 60% of their cold gas reservoir, which is insufficient to match observations. By including a host halo gas distribution that is clumpy and therefore contains regions of higher density, we are able to reproduce the observed HI gas fractions (and thus the high quenched fraction and short quenching timescale) of Local Group satellites, suggesting that a host halo with clumpy gas may be crucial for quenching low-mass systems in Local Group-like (and more massive) host halos.

show abstract

“…Instead, metals propelled by bursts of stellar feedback cycle through the galaxy and halo throughout all of cosmic history. This behavior is critical to explain observed kinematics of stars, sizes, and dark matter cores in these galaxies Chan et al 2015;El-Badry et al 2016). Once ejected from the galaxy into the CGM, the metals can cool gradually and recycle into the galaxy, or be re-heated through the next superwind outflow.…”

Section: Dwarf Starburstsmentioning

confidence: 99%

Metal flows of the circumgalactic medium, and the metal budget in galactic haloes

Muratov

Kereš

Faucher-Giguère

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

178

161

View full text Add to dashboard Cite

We present an analysis of the flow of metals through the circumgalactic medium (CGM) in the Feedback in Realistic Environments (FIRE) simulations of galaxy formation, ranging from isolated dwarfs to L * galaxies. We find that nearly all metals produced in high-redshift galaxies are carried out in winds that reach 0.25R vir . When measured at 0.25R vir the metallicity of outflows is slightly higher than the interstellar medium (ISM) metallicity. Many metals thus reside in the CGM. Cooling and recycling from this reservoir determine the metal budget in the ISM. The outflowing metal flux decreases by a factor of ∼ 2 − 5 between 0.25R vir and R vir . Furthermore, outflow metallicity is typically lower at R vir owing to dilution of the remaining outflow by metal-poor material swept up from the CGM. The inflow metallicity at R vir is generally low, but outflow and inflow metallicities are similar in the inner halo. At low redshift, massive galaxies no longer generate outflows that reach the CGM, causing a divergence in CGM and ISM metallicity. Dwarf galaxies continue to generate outflows, although they preferentially retain metal ejecta. In all but the least massive galaxy considered, a majority of the metals are within the halo at z = 0. We measure the fraction of metals in CGM, ISM and stars, and quantify the thermal state of CGM metals in each halo. The total amount of metals in the low-redshift CGM of two simulated L * galaxies is consistent with estimates from the COS halos survey, while for the other two it appears to be lower.

show abstract

Breathing Fire: How Stellar Feedback Drives Radial Migration, Rapid Size Fluctuations, and Population Gradients in Low-Mass Galaxies

Cited by 285 publications

References 98 publications

KINEMATIC DOWNSIZING AT z ∼ 2

KINEMATIC DOWNSIZING AT z ∼ 2

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Metal flows of the circumgalactic medium, and the metal budget in galactic haloes

Contact Info

Product

Resources

About