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

Star formation depends critically on cooling mechanisms in the interstellarmedium (ISM); however, thermal properties of gas in galaxies at the peak epochof star formation (z ~ 2) remain poorly understood. A limiting factor inunderstanding the multiphase ISM is the lack of multiple tracers detected inthe same galaxies, such as Polycyclic Aromatic Hydrocarbon (PAH) emission, atracer of a critical photoelectric heating mechanism in interstellar gas, and[C II] 158{\mu}m fine-structure emission, a principal coolant. We present ALMABand 9 observations targeting [C II] in six z ~ 2 star-forming galaxies withstrong Spitzer IRS detections of PAH emission. All six galaxies are detected indust continuum and marginally resolved. We compare the properties of PAH and [CII] emission, and constrain their relationship as a function of total infraredluminosity (LIR) and IR surface density. [C II] emission is detected in onegalaxy at high signal-to-noise (34{\sigma}), and we place a secure upper limiton a second source. The rest of our sample are not detected in [C II] likelydue to redshift uncertainties and narrow ALMA bandpass windows. Our results areconsistent with the deficit in [C II]/LIR and PAH/LIR observed in theliterature. However, the ratio of [C II] to PAH emission at z ~ 2 is possiblymuch lower than what is observed in nearby dusty star-forming galaxies. Thiscould be the result of enhanced cooling via [O I] at high-z, hotter gas anddust temperatures, and/or a reduction in the photoelectric efficiency, in whichthe coupling between interstellar radiation and gas heating is diminished.

Measuring the Heating and Cooling of the Interstellar Medium at High redshift: PAH and [C II] Observations of the Same Star Forming Galaxies at z~2