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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The relative distribution of molecular gas and star formation in galaxiesgives insight into the physical processes and timescales of the cycle betweengas and stars. In this work, we track the relative spatial configuration of COand H$\alpha$ emission at high resolution in each of our galaxy targets, anduse these measurements to quantify the distributions of regions in differentevolutionary stages of star formation: from molecular gas without starformation traced by H$\alpha$ to star-forming gas, and to HII regions. Thelarge sample, drawn from the Physics at High Angular resolution in NearbyGalaxieS ALMA and narrowband H$\alpha$ (PHANGS-ALMA and PHANGS-H$\alpha$)surveys, spans a wide range of stellar mass and morphological types, allowingus to investigate the dependencies of the gas-star formation cycle on globalgalaxy properties. At a resolution of 150 pc, the incidence of regions indifferent stages shows a dependence on stellar mass and Hubble type of galaxiesover the radial range probed. Massive and/or earlier-type galaxies exhibit asignificant reservoir of molecular gas without star formation traced byH$\alpha$, while lower-mass galaxies harbor substantial HII regions that mayhave dispersed their birth clouds or formed from low-mass, more isolatedclouds. Galactic structures add a further layer of complexity to relativedistribution of CO and H$\alpha$ emission. Trends between galaxy properties anddistributions of gas traced by CO and H$\alpha$ are visible only when theobserved spatial scale is $\ll$ 500 pc, reflecting the critical resolutionrequirement to distinguish stages of star formation process.

The Gas-Star Formation Cycle in Nearby Star-forming Galaxies II. Resolved Distributions of CO and H$\alpha$ Emission for 49 PHANGS Galaxies