On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies

• Published in: The Astrophysical journal 2022-09, Vol.936 (2), p.171
• Main Authors: Rubin, Kate H. R., Juarez, Christian, Cooksey, Kathy L., Werk, Jessica K., Prochaska, J. Xavier, O’Meara, John M., Burchett, Joseph N., Rickards Vaught, Ryan J., Kulkarni, Varsha P., Straka, Lorrie A.
• Format: Article
• Language: English
• Subjects: Absorbers; Astrophysics; Circumgalactic medium; Cold flow; Emission spectra; Emissions; Galaxies; Interstellar matter; Interstellar medium; Kinematics; Milky Way; Modelling; Quasar absorption line spectroscopy; Quasar-galaxy pairs; Quasars; Red shift; Sky surveys (astronomy); Spectroscopy; Spectrum analysis; Star & galaxy formation; Star formation; Stars; Stars & galaxies
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ac7b88

We use medium-resolution Keck/Echellette Spectrograph and Imager spectroscopy of bright quasars to study cool gas traced by Ca ii λλ 3934, 3969 and Na i λλ 5891, 5897 absorption in the interstellar/circumgalactic media of 21 foreground star-forming galaxies at redshifts 0.03 < z < 0.20 with stellar masses 7.4 ≤ log M * / M ⊙ ≤ 10.6. The quasar–galaxy pairs were drawn from a unique sample of Sloan Digital Sky Survey quasar spectra with intervening nebular emission, and thus have exceptionally close impact parameters ( R ⊥ < 13 kpc). The strength of this line emission implies that the galaxies’ star formation rates (SFRs) span a broad range, with several lying well above the star-forming sequence. We use Voigt profile modeling to derive column densities and component velocities for each absorber, finding that column densities N (Ca ii ) > 10 12.5 cm −2 ( N (Na i ) > 10 12.0 cm −2 ) occur with an incidence f C (Ca ii ) = 0.63 +0.10 −0.11 ( f C (Na i ) = 0.57 +0.10 −0.11 ). We find no evidence for a dependence of f C or the rest-frame equivalent widths W r (Ca ii K) or W r (Na i 5891) on R ⊥ or M * . Instead, W r (Ca ii K) is correlated with local SFR at >3 σ significance, suggesting that Ca ii traces star formation-driven outflows. While most of the absorbers have velocities within ±50 km s −1 of the host redshift, their velocity widths (characterized by Δ v 90 ) are universally 30–177 km s −1 larger than that implied by tilted-ring modeling of the velocities of interstellar material. These kinematics must trace galactic fountain flows and demonstrate that they persist at R ⊥ > 5 kpc. Finally, we assess the relationship between dust reddening and W r (Ca ii K) ( W r (Na i 5891)), finding that 33% (24%) of the absorbers are inconsistent with the best-fit Milky Way E ( B −V)- W r relations at >3 σ significance.