English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We use medium-resolution Keck/Echellette Spectrograph and Imager spectroscopyof bright quasars to study cool gas traced by CaII 3934,3969 and NaI 5891,5897absorption in the interstellar/circumgalactic media of 21 foregroundstar-forming galaxies at redshifts 0.03 < z < 0.20 with stellar masses 7.4 <log M_*/M_sun < 10.6. The quasar-galaxy pairs were drawn from a unique sampleof Sloan Digital Sky Survey quasar spectra with intervening nebular emission,and thus have exceptionally close impact parameters (R_perp < 13 kpc). Thestrength of this line emission implies that the galaxies' star formation rates(SFRs) span a broad range, with several lying well above the star-formingsequence. We use Voigt profile modeling to derive column densities andcomponent velocities for each absorber, finding that column densities N(CaII) >10^12.5 cm^-2 (N(NaI) > 10^12.0 cm^-2) occur with an incidence f_C(CaII) =0.63^+0.10_-0.11 (f_C(NaI) = 0.57^+0.10_-0.11). We find no evidence for adependence of f_C or the rest-frame equivalent widths W_r(CaII K) or W_r(NaI5891) on R_perp or M_*. Instead, W_r(CaII K) is correlated with local SFR at>3sigma significance, suggesting that CaII traces star formation-drivenoutflows. While most of the absorbers have velocities within +/-50 km/s of thehost redshift, their velocity widths (characterized by Delta v_90) areuniversally 30-177 km/s larger than that implied by tilted-ring modeling of thevelocities of interstellar material. These kinematics must trace galacticfountain flows and demonstrate that they persist at R_perp > 5 kpc. Finally, weassess the relationship between dust reddening and W_r(CaII K) (W_r(NaI 5891)),finding that 33% (24%) of the absorbers are inconsistent with the best-fitMilky Way E(B-V)-W_r relations at >3sigma significance.

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