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 a deep Chandra observation to examine the structure of the hotintra-group medium of the compact group of galaxies Stephan's Quintet. Thegroup is thought to be undergoing a strong dynamical interaction as aninterloper, NGC 7318b, passes through the group core at ~850 km/s. A brightridge of X-ray and radio continuum emission has been interpreted as the resultof shock heating, with support from observations at other wavelengths. We findthat gas in this ridge has a similar temperature (~0.6 keV) and abundance (~0.3solar) to the surrounding diffuse emission, and that a hard emission componentis consistent with that expected from high-mass X-ray binaries associated withstar-formation in the ridge. The cooling rate of gas in the ridge is consistentwith the current star formation rate, suggesting that radiative cooling isdriving the observed star formation. The lack of a high-temperature gascomponent is used to place constraints on the nature of the interaction andshock, and we find that an oblique shock heating a pre-existing filament of HImay be the most likely explanation of the X-ray gas in the ridge. The mass ofhot gas in the ridge is only ~2 per cent of the total mass of hot gas in thegroup, which is roughly equal to the deficit in observed HI mass compared topredictions. The hot gas component is too extended to have been heated by thecurrent interaction, strongly suggesting that it must have been heated duringprevious dynamical encounters.

A Chandra X-ray view of Stephan's Quintet: Shocks and Star-formation