Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

Chisholm, John; Tremonti, C.; Leitherer, Claus; Chen, Yanmei; Wofford, Aida; Lundgren, Britt

doi:10.1088/0004-637x/811/2/149

Cited by 163 publications

(234 citation statements)

References 154 publications

(333 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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“…From an HST UV spectroscopic study of the wind velocities of starburst galaxies, Chisholm et al (2015) conclude that galaxies with stellar masses greater than about 3 × 10 10 M ⊙ do not lose interstellar gas via winds, but at lower masses some gas is removed. This stellar mass cut-off for gas lost through winds is consistent with expectations based on binding energy arguments (Dekel & Woo 2003).…”

Section: Low Mass Galaxiesmentioning

confidence: 99%

Diffuse X-Ray-emitting Gas in Major Mergers

Smith

Campbell

Struck

et al. 2018

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Using archived data from the Chandra X-ray telescope, we have extracted the diffuse Xray emission from 49 equal-mass interacting/merging galaxy pairs in a merger sequence, from widely separated pairs to merger remnants. After removal of contributions from unresolved point sources, we compared the diffuse thermal X-ray luminosity from hot gas (L X (gas)) with the global star formation rate (SFR). After correction for absorption within the target galaxy, we do not see strong trend of L X (gas)/SFR with SFR or merger stage for galaxies with SFR > 1 M ⊙ yr −1 . For these galaxies, the median L X (gas)/SFR is 5.5 × 10 39 ((erg s −1 )/M ⊙ yr −1 )), similar to that of normal spiral galaxies. These results suggest that stellar feedback in star forming galaxies reaches an approximately steady state condition, in which a relatively constant fraction of about 2% of the total energy output from supernovae and stellar winds is converted into X-ray flux. Three late-stage merger remnants with low SFRs and high K band luminosities (L K ) have enhanced L X (gas)/SFR; their UV/IR/optical colors suggest that they are post-starburst galaxies, perhaps in the process of becoming ellipticals. Systems with L K < 10 10 L ⊙ have lower L X (gas)/SFR ratios than the other galaxies in our sample, perhaps due to lower gravitational fields or lower metallicities. We see no relation between L X (gas)/SFR and Seyfert activity in this sample, suggesting that feedback from active galactic nuclei is not a major contributor to the hot gas in our sample galaxies.

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“…For this sample we have access to both nebular line redshifts and stellar redshifts. The stellar redshift was measured by fitting linear combinations of Starburst99 (Leitherer et al 1999(Leitherer et al , 2010 simple stellar population models to each spectrum, while simultaneously fitting for reddening, following the methodology of Chisholm et al (2015). These fits were made using a linear combination of 10 single-aged, fully theoretical Starburst99 models, and 5 different stellar continuum metallicities (0.01, 0,2, 0.4, 1.0, and 2.0 Z ).…”

Section: Input M Egasaura Mage Spectramentioning

confidence: 99%

The Magellan Evolution of Galaxies Spectroscopic and Ultraviolet Reference Atlas (MegaSaura). II. Stacked Spectra

Rigby

Bayliss

Chisholm

et al. 2018

ApJ

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We stack the rest-frame ultraviolet spectra of N = 14 highly magnified gravitationally lensed galaxies at redshifts 1.6 < z < 3.6. The resulting new composite spans 900 < λ rest < 3000Å, with a peak signal-to-noise ratio of 103 per spectral resolution element (∼100 km s −1 ). It is the highest signalto-noise ratio, highest spectral resolution composite spectrum of z ∼ 2-3 galaxies yet published. The composite reveals numerous weak nebular emission lines and stellar photospheric absorption lines that can serve as new physical diagnostics, particularly at high redshift with the James Webb Space Telescope (JWST ). We report equivalent widths to aid in proposing for and interpreting JWST spectra. We examine the velocity profiles of strong absorption features in the composite, and in a matched composite of z ∼ 0 COS/HST galaxy spectra. We find remarkable similarity in the velocity profiles at z ∼ 0 and z ∼ 2, suggesting that similar physical processes control the outflows across cosmic time. While the maximum outflow velocity depends strongly on ionization potential, the absorptionweighted mean velocity does not. As such, the bulk of the high-ionization absorption traces the low-ionization gas, with an additional blueshifted absorption tail extending to at least −2000 km s −1 . We interpret this tail as arising from the stellar wind and photospheres of massive stars. Starburst99 models are able to replicate this high-velocity absorption tail. However, these theoretical models poorly reproduce several of the photospheric absorption features, indicating that improvements are needed to match observational constraints on the massive stellar content of star-forming galaxies at z ∼ 2. We publicly release our composite spectra.

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Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

Cited by 163 publications

References 154 publications

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

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

Diffuse X-Ray-emitting Gas in Major Mergers

The Magellan Evolution of Galaxies Spectroscopic and Ultraviolet Reference Atlas (MegaSaura). II. Stacked Spectra

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