The [AN] Isotropy of the X-Ray Sky release_pkxpx7czm5ci3jh6jn4gnw5hxm

Abstract

In this presentation we show how the study of the isotropy of the X-ray sky contributes to our understanding of the structure of the universe at moderate redshifts (1≲z&lt;&lt;z<jats:sub>recombination</jats:sub>). Actually, the <jats:underline>an</jats:underline>isotropy of the sky flux provides the information, much as the microwave sky anisotropy does for earlier epochs. [See reports in this volume.] Though we are currently unable to make measurements with the precision and small solid angles typically achieved in the microwave, comparatively crude limits from the X-ray fluctuations place limits on the largest scale structure of the universe. We first outline the measurements of the X-ray sky and its anisotropies made with the <jats:underline>HEAO 1</jats:underline> A-2 experiment. Detailed presentations are found elsewhere [Shafer 1982; Marshall <jats:underline>et al.</jats:underline> 1980; Piccinotti <jats:underline>et. al.</jats:underline> 1982; Iwan <jats:underline>et al.</jats:underline> 1982; Shafer <jats:underline>et al.</jats:underline> in prep.]. We then show how the anisotropies place limits on the origin of the X-ray sky and on any large scale structure of the universe, following the example of previous analyses which used earlier anisotropy estimates [see <jats:underline>e.g.</jats:underline> Fabian and Rees 1978; Rees 1980; Fabian 1981].
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