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 Suzaku spectra of X-ray emission in the fields just off the LMCX-3 sight line. OVII, OVIII, and NeIX emission lines are clearly detected,suggesting the presence of an optically thin thermal plasma with an averagetemperature of 2.4E6. This temperature is significantly higher than thatinferred from existing X-ray absorption line data obtained with Chandra gratingobservations of LMC X-3, strongly suggesting that the gas is not isothermal. Wethen jointly analyze these data to characterize the spatial and temperaturedistributions of the gas. Assuming a vertical exponential Galactic disk model,we estimate the gas temperature and density at the Galactic plane and theirscale heights as 3.6(2.9, 4.7)E6 K and 1.4(0.3, 3.4)E-3 cm^{-3} and 1.4(0.2,5.2) kpc and $2.8(1.0, 6.4)$ kpc, respectively. This characterization canaccount for all the \ovi line absorption, as observed in a FUSE spectrum of LMCX-3, but only predicts less than one tenth of the OVI line emission intensitytypically detected at high Galactic latitudes. The bulk of the OVI emissionmost likely arises at interfaces between cool and hot gases.

X-ray and UV spectroscopy of Galactic diffuse hot gas along the LMC X--3 sight line