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

The presence of luminous hot X-ray coronae in the dark matter halos ofmassive spiral galaxies is a basic prediction of galaxy formation models.However, observational evidence for such coronae is very scarce, with the firstfew examples having only been detected recently. In this paper, we study thelarge-scale diffuse X-ray emission associated with the massive spiral galaxyNGC266. Using ROSAT and Chandra X-ray observations we argue that the diffuseemission extends to at least ~70 kpc, whereas the bulk of the stellar light isconfined to within ~25 kpc. Based on X-ray hardness ratios, we find that mostof the diffuse emission is released at energies <1.2 keV, which indicates thatthis emission originates from hot X-ray gas. Adopting a realistic gastemperature and metallicity, we derive that in the (0.05-0.15)r_200 region(where r_200 is the virial radius) the bolometric X-ray luminosity of the hotgas is (4.3 +/- 0.8) x 10^40 erg/s and the gas mass is (9.1 +/- 0.9) x 10^9M_sun. These values are comparable to those observed for the two otherwell-studied X-ray coronae in spiral galaxies, suggesting that the physicalproperties of such coronae are similar. This detection offers an excellentopportunity for comparison of observations with detailed galaxy formationsimulations.

Detection of a luminous hot X-ray corona around the massive spiral galaxy NGC266