ABSORPTION-LINE PROBES OF THE PREVALENCE AND PROPERTIES OF OUTFLOWS IN PRESENT-DAY STAR-FORMING GALAXIES

By Yan-Mei Chen, Christy A. Tremonti, T. Heckman, G. Kauffmann, B. Weiner, J. Brinchmann, Jing Wang. 2010

164 citations recorded by the source corpus.

We analyze star-forming galaxies drawn from SDSS DR7 to show how the interstellar medium (ISM) Na i λλ5890, 5896 (Na D) absorption lines depend on galaxy physical properties, and to look for evidence of galactic winds. We combine the spectra of galaxies with similar geometry/physical parameters to create composite spectra with signal-to-noise ∼300. The stellar continuum is modeled using stellar population synthesis models, and the continuum-normalized spectrum is fit with two Na i absorption components. We find that (1) ISM Na D absorption lines with equivalent widths EW > 0.8 Å are only prevalent in disk galaxies with specific properties—large extinction (AV), high star formation rates (SFR), high SFR per unit area (ΣSFR), or high stellar mass (M*); (2) the ISM Na D absorption lines can be separated into two components: a quiescent disk-like component at the galaxy systemic velocity and an outflow component; (3) the disk-like component is much stronger in the edge-on systems, and the outflow component covers a wide angle but is stronger within 60° of the disk rotation axis; (4) the EW and covering factor of the disk component correlate strongly with dust attenuation, highlighting the importance that dust shielding may play in the survival of Na i; (5) the EW of the outflow component depends primarily on ΣSFR and secondarily on AV; and (6) the outflow velocity varies from ∼120 to 160 km s−1 but shows little hint of a correlation with galaxy physical properties over the modest dynamic range that our sample probes (1.2 dex in log ΣSFR and 1 dex in log M*).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3f96d66ab9dc35271c79793a0badc8a53db53e19

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Citations in the corpus

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 S”
IMPROVED AND QUALITY-ASSESSED EMISSION AND ABSORPTION LINE MEASUREMENTS IN SLOAN DIGITAL SKY SURVEY GALAXIES (2011, background): “…such as the typical “bump” at 4640Å associated to the presence of WolfRayet stars (e.g., Brinchmann, Kunth & Durret 2008) or a systematic mismatch in the NaD region around 5900Å due to the presence of neutral material entrained in galactic outflows (e.g., Sato et al. 2009, Chen et al. 2010).”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, methodology): “…of local galactic winds (see the review by Veilleux et al. 2005), the largest census of galactic winds in the local universe was undertaken by Chen et al. (2010) based on using SDSS galaxy spectra to measure the interstellar absorption feature produced by neutral Na atoms that trace the…”
THE SINS/zC-SINF SURVEY of z ∼ 2 GALAXY KINEMATICS: OUTFLOW PROPERTIES (2012, background): “And indeed, winds are only detected in compact star forming dwarfs and/or starbursts above ∼0.1 M⊙yr −1kpc−2(Heckman et al. 1990; Veilleux et al. 2005; Chen et al. 2010), see also Murray et al. (2011).”
FAST MOLECULAR OUTFLOWS IN LUMINOUS GALAXY MERGERS: EVIDENCE FOR QUASAR FEEDBACK FROM HERSCHEL (2013, background): “The velocities of local neutral gas outflows traced by Na I show a tendency to become more negative with increasing host galaxy stellar velocity dispersions and stellar masses (e.g., Rupke et al. 2002, 2005bc; Martin 2005; Chen et al. 2010).”
FIRE-2 simulations: physics versus numerics in galaxy formation (2017, background): “…galaxy SFR (Aguirre et al. 2001; Pettini et al. 2003; Songaila 2005; Martin et al. 2010; Oppenheimer & Davé 2006), and indeed such winds are ubiquitously observed (Martin 1999, 2006; Heckman et al. 2000; Newman et al. 2012; Sato et al. 2009; Chen et al. 2010; Steidel et al. 2010; Coil et al. 2011).”
Stellar Feedback in Galaxies and the Origin of Galaxy-scale Winds (2011, background): “…mass-loading factors of several times the SFR are also estimated in even relatively massive local galaxies and massive star-forming regions at z ∼ 2–3 (Martin 1999, 2006; Heckman et al. 2000; Sato et al. 2009; Chen et al. 2010; Steidel et al. 2010; Coil et al. 2011; Newman et al., in preparation).”
Shaping the galaxy stellar mass function with supernova- and AGN-driven winds (2012, background): “Chen et al. (2010) found weak (yet noisy) positive correlations between outflow velocity and star formation rate density or galaxy stellar mass, respectively.”
EVIDENCE FOR UBIQUITOUS COLLIMATED GALACTIC-SCALE OUTFLOWS ALONG THE STAR-FORMING SEQUENCE AT z ∼ 0.5 (2013, methodology): “Indeed, the first evidence for such a relationship was presented in Chen et al. (2010), who reported a positive correlation between ΣSFR and the EW of Na I absorption tracing outflows.”
The SAMI Galaxy Survey: shocks and outflows in a normal star-forming galaxy (2014, background): “Stacking spectra of galaxies of similar properties is sometimes necessary to detect outflow signatures, at the expense of probing mean outflow properties of pre-defined populations (e.g., Chen et al. 2010).”
THE SYSTEMATIC PROPERTIES OF THE WARM PHASE OF STARBURST-DRIVEN GALACTIC WINDS (2015, background): “Compared to most studies of higher-redshift UV-selected galaxies, our individual spectra are higher in S/N and the sample spans much wider ranges in star-formation rates (SFR), galaxy stellar masses (M∗), circular ve- Systematic Properties of Galactic Winds 13 locities (vcir), metallicities, specifi”
The baryonic assembly of dark matter haloes (2011, background): “Observations show that powerful superwinds are ubiquitous in galaxies with star formation rates per unit area SFR ≥ 0.1 M yr−1 kpc−2 (e.g. Heckman 2002), with outflows from other galaxies being significantly weaker (e.g. Chen et al. 2010).”
Galaxies on FIRE (Feedback In Realistic Environments): stellar feedback explains cosmologically inefficient star formation (2013, background): “Such winds have been observed ubiquitously in local and high-redshift starforming galaxies (Martin 1999, 2006; Heckman et al. 2000; Newman et al. 2012; Sato et al. 2009; Chen et al. 2010; Steidel et al. 2010; Coil et al. 2011).”
The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows (2015, background): “Observations reveal that gas is ejected from the disc at velocities of a few 100 km s−1 with mass loading factors (ratio of outflowing to star-forming gas) of order unity and above (see, e.g. Chen et al. 2010; Martin et al. 2012; Newman et al. 2012; Martin et al. 2013).”
THE MULTIPHASE STRUCTURE AND POWER SOURCES OF GALACTIC WINDS IN MAJOR MERGERS (2013, unknown): “Systems with star formation rate (SFR) ∼ 1 M yr−1 show Ω/4π ∼ 0.1 (Chen et al. 2010; Bouché et al. 2012), nearby LIRGs (SFR = 7− 70 M yr−1) have Ω/4π ∼ 0.4 (Rupke et al. 2005c), and nearby ULIRGs (SFR & 70 M yr−1) have Ω/4π ∼ 0.8 (Rupke et al. 2002, 2005c; Martin 2005).”
Metallicity gradients in local field star-forming galaxies: insights on inflows, outflows, and the coevolution of gas, stars and metals (2015, background): “…winds, are found to be ubiquitously in galaxies at lower redshifts with high enough star-formation surface density (Heckman 2002), with the wind velocities showing indication of correlating with both the SFR and host galaxy mass (Rupke et al. 2005a,b; Veilleux et al. 2005; Chen et al. 2010).”
DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 < z < 1.4 (2012, background): “…filling in Na I λλ5890, 96 has long been attributed to the high gas densities in regions with a significant neutral sodium fraction; the large pathlength of scattered photons produces a high probability of absorption by a dust grain (Heckman et al. 2000; Martin 2005, 2006; Chen et al. 2010).”