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

We present the first Herschel spectroscopic detections of the [OI]63 and[CII]158 micron fine-structure transitions, and a single para-H2O line from the35 x 15 kpc^2 shocked intergalactic filament in Stephan's Quintet. The filamentis believed to have been formed when a high-speed intruder to the groupcollided with clumpy intergroup gas. Observations with the PACS spectrometerprovide evidence for broad (> 1000 km s^-1) luminous [CII] line profiles, aswell as fainter [OI]63micron emission. SPIRE FTS observations reveal wateremission from the p-H2O (111-000) transition at several positions in thefilament, but no other molecular lines. The H2O line is narrow, and may beassociated with denser intermediate-velocity gas experiencing the strongestshock-heating. The [CII]/PAH{tot) and [CII]/FIR ratios are too large to beexplained by normal photo-electric heating in PDRs. HII region excitation orX-ray/Cosmic Ray heating can also be ruled out. The observations lead to theconclusion that a large fraction the molecular gas is diffuse and warm. Wepropose that the [CII], [OI] and warm H2 line emission is powered by aturbulent cascade in which kinetic energy from the galaxy collision with theIGM is dissipated to small scales and low-velocities, via shocks and turbulenteddies. Low-velocity magnetic shocks can help explain both the [CII]/[OI]ratio, and the relatively high [CII]/H2 ratios observed. The discovery that[CII] emission can be enhanced, in large-scale turbulent regions in collisionalenvironments has implications for the interpretation of [CII] emission inhigh-z galaxies.

Shock-Enhanced C+ Emission and the Detection of H2O from Stephan's Quintet's Group-Wide Shock using Herschel