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

Suzaku performed observations of 3 regions in and around the Shapleysupercluster: a region located between A3558 and A3556, at ~0.9 times thevirial radii of both clusters, and two other regions at 1{\deg}and 4{\deg}awayfrom the first pointing. The 4{\deg}-offset observation was used to evaluatethe Galactic foreground emission. We did not detect significant redshiftedOxygen emission lines (O VII and O VIII) in the spectra of all three pointings,after subtracting the contribution of foreground and background emission. Anupper limit for the redshifted O VIII Ka line intensity of the warm-hotintergalactic medium (WHIM) is 1.5 \times 10^-7 photons s^-1 cm^-2 arcmin^-2,which corresponds to an overdensity of ~380 (Z/0.1 Z_solar)^{-1/2} (L/3Mpc)^{-1/2}, assuming T=3\times10^6 K. We found excess continuum emission inthe 1{\deg}-offset and on-filament regions, represented by thermal models withkT ~1 keV and ~2 keV, respectively. The redshifts of both 0 and that of thesupercluster (0.048) are consistent with the observed spectra. The ~1 keVemission can be also fitted with Ne-rich Galactic (zero redshift) thin thermalemission. Radial intensity profile of 2 keV component suggests contributionfrom A3558 and A3556, but with significant steepening of the intensity slope inthe outer region of A3558. Finally, we summarized the previous Suzaku searchfor the WHIM and discussed the feasibility of constraining the WHIM. Anoverdensity of < 400 can be detectable using O VII and O VIII emission lines ina range of 1.4\times10^6 K < T < 5\times10^6 K or a continuum emission in arelatively high temperature range T > 5\times10^6 K with the Suzaku XIS. Thenon detection with Suzaku suggests that typical line-of-sight averageoverdensity is < 400.

Search for X-Ray Emission Associated with the Shapley Supercluster with Suzaku