EVIDENCE FOR UBIQUITOUS COLLIMATED GALACTIC-SCALE OUTFLOWS ALONG THE STAR-FORMING SEQUENCE AT z ∼ 0.5

By K. Rubin, J. Xavier Prochaska, D. Koo, A. Phillips, Crystal L. Martin, L. Winstrom. 2013

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We analyze Mg ii λλ2796, 2803 and Fe ii λλ2586, 2600 absorption profiles in individual spectra of 105 galaxies at 0.3 < z < 1.4. The galaxies, drawn from redshift surveys of the GOODS fields and the Extended Groth Strip, sample the range in star formation rates (SFRs) occupied by the star-forming sequence with stellar masses log M*/M☉ ≳ 9.6 down to SFR ≳ 2 M☉ yr−1 at 0.3 < z < 0.7. Using the Doppler shifts of Mg ii and Fe ii absorption as tracers of cool gas kinematics, we detect large-scale winds in 66 ± 5% of the galaxies. Hubble Space Telescope Advanced Camera for Surveys imaging and our spectral analysis indicate that the outflow detection rate depends primarily on galaxy orientation: winds are detected in ∼89% of galaxies having inclinations (i) <30° (face-on), while the wind detection rate is ∼45% in objects having i > 50° (edge-on). Combined with the comparatively weak dependence of wind detection rate on intrinsic galaxy properties, this implies that biconical outflows are ubiquitous in normal, star-forming galaxies at z ∼ 0.5. We find that wind velocity is correlated with galaxy M* at 3.4σ significance, while outflow equivalent width is correlated with SFR at 3.5σ significance, suggesting hosts with higher SFR launch more material and/or generate a larger velocity spread for the absorbing clouds. Assuming the gas is driven into halos with isothermal density profiles, the wind velocities (∼200–400 km s−1) permit escape from the halo potentials only for the lowest-M* systems in the sample. However, the gas carries sufficient energy to reach distances ≳ 50 kpc, and may therefore be a viable source of material for the massive, cool circumgalactic medium around bright galaxies at z ∼ 0.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/090c36b4393e42ce3c5ff0e2295b0567fa4a57f1

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Citations in the corpus

Gusty, gaseous flows of FIRE: Galactic winds in cosmological simulations with explicit stellar feedback (2015, background): “…of kinematically distinct material from the rest frame of the host galaxy via Doppler shifted emission (e.g. Martin 1998) and absorption lines (e.g. Heckman et al. 2000; Grimes et al. 2009; Weiner et al. 2009; Steidel et al. 2010; Bouché et al. 2012; Martin et al. 2012; Rubin et al. 2014).”
THE SYSTEMATIC PROPERTIES OF THE WARM PHASE OF STARBURST-DRIVEN GALACTIC WINDS (2015, background): “There have also been a number of investigations of intermediate redshift (z ∼ 0.5 to 1.5) star-forming galaxies (e.g. Weiner et al. 2009; Erb et al. 2012; Kornei et al. 2012; Martin 2012; Rubin et al. 2014; Bordoloi et al. 2014).”
Neutral hydrogen in galaxy haloes at the peak of the cosmic star formation history (2014, background): “…with observations that the covering fraction of LLSs around DLAs (likely spanning a broad range of halo masses ∼ 1010.5 − 1013 M , e.g. Font-Ribera et al. 2012; Barnes & Haehnelt 2014) is similar to that around LBGs within an impact parameter ∼ 100 proper kpc at z ∼ 2 (Rubin et al. 2014a).”
ON THE INTERPLAY BETWEEN STAR FORMATION AND FEEDBACK IN GALAXY FORMATION SIMULATIONS (2014, methodology): “…velocities as a function of galaxy circular velocity for the three simulations, together with data derived from Na I D absorption measurements from Schwartz & Martin (2004) and Rupke et al. (2005), as well as from Mg II absorption lines from a sample of galaxies at 0.3< z< 1.4 (Rubin et al. 2014).”
First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback (2019, background): “…detection of outflow signatures along the minor axes of galaxies is a common conclusion at low-z (Heckman et al. 2000) based on SDSS (Chen et al. 2010; Concas et al. 2017; Bae & Woo 2018) and also towards z ∼ 1 (Martin et al. 2012; Kornei et al. 2012; Bordoloi et al. 2014b; Rubin et al. 2014).”
The Circumgalactic Medium (2017, methodology): “…method is commonly used in optical and near-UV lines such as Ca ii, Na i, Mg ii, and Fe ii (Martin 2005; Kornei et al. 2012; Bordoloi et al. 2011; Rubin et al. 2014) to study outflows from galaxies out to z ∼ 1, in UV lines for low-redshift star-forming galaxies (Henry et al. 2015; Heckman et…”
Cool outflows in galaxies and their implications (2020, methodology): “(39) is used to derive the total Mg abundance in the gas phase, and a dust depletion corrections BMg = −0.5 dex is used in galaxies with near-solar abundances (Rubin et al. 2014).”
Bimodality of low-redshift circumgalactic O VI in non-equilibrium EAGLE zoom simulations (2016, background): “…blue-shifted, low-ion absorption wings extending to at most a few hundred km s−1 from the galaxy, almost always at velocities unable to escape the gravitational potential of the halo (e.g. Bouché et al. 2012; Martin et al. 2012; Rubin et al. 2014; Chisholm et al. 2015; Nielsen et al. 2015).”
THE COS-HALOS SURVEY: ORIGINS OF THE HIGHLY IONIZED CIRCUMGALACTIC MEDIUM OF STAR-FORMING GALAXIES (2016, background): “Shocks and Radiatively Cooling Gas Behind Fast Winds Galaxy-scale winds are a natural model to address for the CGM, especially given their observed ubiquity in star-forming galaxies (e.g. Martin et al. 2012; Rubin et al. 2014) and their potential to scale with SFR/R2 (Borthakur et al. 2013).”
Theoretical Challenges in Galaxy Formation (2016, background): “…than the star formation rate) are ubiquitous, not only in the nearby Universe (e.g. Heckman, Armus & Miley 1990; Heckman et al. 2000; Martin 1999; Rubin et al. 2014; Veilleux, Cecil & Bland-Hawthorn 2005) but also at higher redshift at the cosmic peak of conversion of gas into stars (Martin et…”