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

By D. Rupke, Sylvain Veilleux, D. C. U. O. Maryland, College Park, Institute for Astronomy, U. Hawaii. 2005

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We have performed an absorption-line survey of outflowing gas in 78 starburst-dominated, infrared-luminous galaxies. This is the largest study of superwinds at z ≲ 3. Superwinds are found in almost all infrared-luminous galaxies, and changes in detection rate with SFR—winds are found twice as often in ultraluminous infrared galaxies (ULIRGs) as in less-luminous galaxies—reflect different wind geometries. The maximum velocities we measure are 600 km s-1, though most of the outflowing gas has lower velocities (100-200 km s-1). (One galaxy has velocities exceeding 1000 km s-1.) Velocities in LINERs are higher than in H II galaxies, and outflowing ionized gas often has higher velocities than the neutral gas. Wind properties (velocity, mass, momentum, and energy) scale with galaxy properties (SFR, luminosity, and galaxy mass), consistent with ram-pressure driving of the wind. Wind properties increase strongly with increasing galactic mass, contrary to expectation. These correlations flatten at high SFR (≳10-100 M☉ yr-1), luminosities, and masses. This saturation is due to a lack of gas remaining in the wind's path, a common neutral gas terminal velocity, and/or a decrease in the efficiency of thermalization of the supernovae energy. It means that mass entrainment efficiency, rather than remaining constant, declines in galaxies with SFR > 10 M☉ yr-1 and MK < -24. Half of our sample consists of ULIRGs, which host as much as half of the star formation in the universe at z ≳ 1. The powerful, ubiquitous winds we observe in these galaxies imply that superwinds in massive galaxies at redshifts above unity play an important role in the evolution of galaxies and the intergalactic medium.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

• THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z ∼ 1.4 AND ∼1 (2009, background): “As in previous work (e.g., Martin 1999; Rupke et al. 2005b; Martin 2005), we find that Ṁ is on the same order as the SFR of the sample (∼1–30 M yr−1).”
• GALAXY-WIDE SHOCKS IN LATE-MERGER STAGE LUMINOUS INFRARED GALAXIES (2011, background): “…HI 96822 2 Research School of Astronomy and Astrophysics, AustralianN tional University, Cotter Rd., Weston ACT 2611, Australia galaxies move along the Toomre & Toomre (1972) merger sequence the IR luminosity is generally found to increase along with galactic wind activity (Rupke et al. 2005).”
• THE STRUCTURE AND KINEMATICS OF THE CIRCUMGALACTIC MEDIUM FROM FAR-ULTRAVIOLET SPECTRA OF z ≃ 2–3 GALAXIES (2010, background): “…is interesting in light of recent studies relating outflow velocity to galaxy properties in local starbursts; for example, both Martin (2005) and Rupke et al. (2005) find evidence for correlations of outflow speed with SFR and dynamical mass (represented by the circular velocity), in the sense…”
• Cool outflows in galaxies and their implications (2020, background): “Once N(Na I) has been derived, the column density of hydrogen, N(H), can be estimated from N(Na I) given a metallicity and ionization fraction (Rupke et al. 2005b): N(H) = N(Na I) X−1Na0 10 −(ANa+BNa), (39) where XNa0 ≡ N(Na I) / N(Na) is the fraction of Na that is neutral Na I, ANa ≡…”
• Metallicity gradients in local field star-forming galaxies: insights on inflows, outflows, and the coevolution of gas, stars and metals (2015, background): “Mass loading factors of about 0.1–1 were also found inz < 0.5 luminous and ultra-luminous infrared galaxies, and nearby mergers (Rupke et al. 2005b; Rupke & Veilleux 2013).”
• DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 < z < 1.4 (2012, background): “In particular, we would not discount models that predict Vmax ∝ Vesc (Murray et al. 2005; Zhang & Thompson 2010); their results are supported by observations of small samples of local starbursts observed at much higher resolution and S/N ratio (Martin 2005; Rupke et al. 2005).”
• Feedback in simulations of disc-galaxy major mergers (2005, background): “Correlations between mergers and AGN (Veilleux et al. 1995; Wyithe & Loeb 2003) and mergers and outflows (Martin 1999, 2005; Rupke et al. 2005, 2002) provide evidence for this scenario.”
• The cosmic baryon cycle and galaxy mass assembly in the FIRE simulations (2016, background): “E-mail: anglesd@northwestern.edu bursts to high redshift galaxies (Martin 2005; Rupke et al. 2005; Veilleux et al. 2005; Weiner et al. 2009; Steidel et al. 2010; Martin et al. 2012; Newman et al. 2012; Heckman et al. 2015).”
• THE IMPACT OF COLD GAS ACCRETION ABOVE A MASS FLOOR ON GALAXY SCALING RELATIONS (2009, methodology): “For a marginally unstable disk with Toomre Q parameter Q ∼ 1, it can be shown (Martin & Kennicutt 2001; Krumholz & Thompson 2007) that Equation 7 is equivalent to the traditional Kennicutt-Schmidt (KS) relation (Schmidt 1959; Kennicutt 1998), which relates the surface densities of gas and SFR via ΣS”
• The SAMI Galaxy Survey: shocks and outflows in a normal star-forming galaxy (2014, background): “Studies of blue-shifted absorption by neutral gas entrained in outflows have reached sample sizes on the order of tens to a hundred and provided constraints on the mass, momentum, and energy of outflows (Heckman et al. 2000; Rupke et al. 2005b,c; Rubin et al. 2013, and references therein).”
• The origin of the galaxy mass-metallicity relation and implications for galactic outflows (2007, background): “Interestingly, recent observations of local galactic outflows indicate momentum-driven wind scalings (Martin 2005; Rupke et al. 2005), providing an intriguing connection between rare local outflows and the more ubiquitous and generally stronger outflows at z & 2.”
• 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).”
• THE SYSTEMATIC PROPERTIES OF THE WARM PHASE OF STARBURST-DRIVEN GALACTIC WINDS (2015, background): “…of the optically-selected sam- Systematic Properties of Galactic Winds 3 ple in Chen et al. (2010), the previous analyses of comparably large samples of low-redshift galaxies have focused on dusty far-IR-selected galaxies (e.g. Heckman et al. 2000; Rupke et al. 2005; Martin 2005; Sato et al. 2009).”
• SPITZER QUASAR AND ULIRG EVOLUTION STUDY (QUEST). IV. COMPARISON OF 1 Jy ULTRALUMINOUS INFRARED GALAXIES WITH PALOMAR-GREEN QUASARS (2009, background): “Optical spectral types, which are referred to extensively in this paper, are taken from Veilleux et al. 1999a and Rupke et al. 2005a for the 1 Jy sample, and Veilleux et al. 1995 for the 5 RBGS objects.”