THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z ∼ 1.4 AND ∼1

By K. Rubin, B. Weiner, D. Koo, Crystal L. Martin, J. Xavier Prochaska, A. Coil, J. Newman. 2009

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We present an analysis of the Mg ii λλ2796, 2803 and Fe ii λλ2586, 2600 absorption line profiles in co-added spectra of 468 galaxies at 0.7 < z < 1.5. The galaxy sample, drawn from the Team Keck Treasury Redshift Survey of the GOODS-N field, has a range in stellar mass (M*) comparable to that of the sample at z ∼ 1.4 analyzed in a similar manner by Weiner et al. (W09), but extends to lower redshifts and has specific star formation rates which are lower by ∼0.6 dex. We identify outflows of cool gas from the Doppler shift of the Mg ii absorption lines and find that the equivalent width (EW) of absorption due to outflowing gas increases on average with M* and star formation rate (SFR). We attribute the large EWs measured in spectra of the more massive, higher-SFR galaxies to optically thick absorbing clouds having large velocity widths. The outflows have hydrogen column densities N(H) ≳ 1019.4 cm−2 and extend to velocities of ∼500 km s-1. While galaxies with SFR>10 M☉ yr−1 host strong outflows in both this and the W09 sample, we do not detect outflows in lower-SFR (i.e., log M*/M☉ ≲ 10.5) galaxies at lower redshifts. Using a simple galaxy evolution model that assumes exponentially declining SFRs, we infer that strong outflows persist in galaxies with log M*/M☉ > 10.5 as they age between z = 1.4 and z ∼ 1, presumably because of their high absolute SFRs. Finally, our spectral analysis, combined with high-resolution Hubble Space Telescope/Advanced Camera for Surveys imaging, weakly suggests that outflow absorption strength increases with galaxy SFR surface density.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/f36cd0aa2c64b0ef0deb3970df0d7c7c4456cfec

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Citations in the corpus

PROBING THE INTERGALACTIC MEDIUM/GALAXY CONNECTION. V. ON THE ORIGIN OF Lyα AND O vi ABSORPTION AT z < 0.2 (2011, result): “This hypothesis, however, is apparently not supported by current research on galactic-scale winds (e.g. Weiner et al. 2009; Rubin et al. 2010). has a density and/or temperature that is not favorable for O+5 ions.”
First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback (2019, background): “Observational probes for the incidence and properties of outflows extend from z ∼ 0, including analyses of SDSS (Chen et al. 2010) through z ∼ 0.5 − 1 (Rubin et al. 2010, 2011) to the peak epoch of cosmic star formation at z ∼ 2− 3 in both absorption (Steidel et al. 2010) and emission, focusing on…”
The DEEP3 Galaxy Redshift Survey: the impact of environment on the size evolution of massive early-type galaxies at intermediate redshift (2011, background): “…galaxies suggests that low-luminosity AGN may not play a dominant role in galactic feedback (Rupke, Veilleux & Sanders 2005; Weiner et al. 2009; Rubin et al. 2010, 2011; Coil et al. 2011, but see also Hainline et al. C© 2011 The Authors, MNRAS 419, 3018–3027 Monthly Notices of the Royal…”
Cosmic ray driven outflows in global galaxy disc models (2013, background): “Thus our model may help explain why star-forming galaxies show evidence for substantial amounts of multiphase gas in their haloes (e.g. Chen et al. 2010; Rubin et al. 2010; Tumlinson et al. 2011).”
Cool outflows in galaxies and their implications (2020, background): “Fits with two separate velocity components for each line are generally used to mitigate these effects (Rubin et al. 2010; Coil et al. 2011).”
EVIDENCE FOR UBIQUITOUS COLLIMATED GALACTIC-SCALE OUTFLOWS ALONG THE STAR-FORMING SEQUENCE AT z ∼ 0.5 (2013, background): “We note that the more standard assumption that the wind is distributed in a spherical shell having radius R ≈ D would result in Aflow ≈ 4πR2, or 314 kpc2, and a mass flux of ∼ 7 M⊙ yr−1 (e.g., Weiner et al. 2009; Rubin et al. 2010; Martin et al. 2012).”
THE RADIAL AND AZIMUTHAL PROFILES OF Mg ii ABSORPTION AROUND 0.5 < z < 0.9 zCOSMOS GALAXIES OF DIFFERENT COLORS, MASSES, AND ENVIRONMENTS (2011, background): “…systems originate due to cool gas entrained in outflows from star-forming galaxies (Bouché et al. 2006; Bouché 2008; Ménard et al. 2009; Nestor et al. 2010), which is also supported by the blueshifts of Mg II absorption in the spectra of individual galaxies (Weiner et al. 2009; Rubin et al. 2010).”
DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 < z < 1.4 (2012, background): “…the broader width of the strong emission feature at λ2326 to a blend of various C II] transitions; in our picture, the Fe II λ2328 feature, which Rubin et al. (2010a) suggested contributed to this emission complex, does not contribute because its upper level cannot be populated by a permitted…”
TRACING OUTFLOWS AND ACCRETION: A BIMODAL AZIMUTHAL DEPENDENCE OF Mg ii ABSORPTION (2012, unknown): “…& Bouché 2009; Weiner et al. 2009; Chelouche & Bowen 2010; Nestor et al. 2011; Noterdaeme et al. 2010; Bordoloi et al. 2011; Coil et al. 2011; Rubin et al. 2010; Ménard & Fukugita 2012; Martin et al. 2012) and accretion onto host galaxies (Steidel et al. 2002; Chen et al. 2010a; Chen et al.…”
The ESO UVES advanced data products quasar sample: II. Cosmological evolution of the neutral gas mass density (2013, background): “Outflows are ubiquitous in almost all distant star-forming galaxies (Weiner et al. 2009; Rubin et al. 2010; Steidel et al. 2010; Kacprzak et al. 2011; Bordoloi et al. 2011) and their rates arimilar to or higher than the SFR (e.g., Kornei et al. 2012).”