scholarly journals X-ray sources as tracers of the large-scale structure in the universe

2001 ◽  
Author(s):  
X. Barcons
1983 ◽  
Vol 104 ◽  
pp. 333-343
Author(s):  
R. A. Shafer ◽  
A. C. Fabian

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<<zrecombination). Actually, the anisotropy 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 HEAO 1 A-2 experiment. Detailed presentations are found elsewhere [Shafer 1982; Marshall et al. 1980; Piccinotti et. al. 1982; Iwan et al. 1982; Shafer et al. 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 e.g. Fabian and Rees 1978; Rees 1980; Fabian 1981].


2011 ◽  
Vol 54 (10) ◽  
pp. 983-1005 ◽  
Author(s):  
Vladimir N Lukash ◽  
Elena V Mikheeva ◽  
A M Malinovsky

Physics Today ◽  
1981 ◽  
Vol 34 (8) ◽  
pp. 62-63 ◽  
Author(s):  
P. J. E. Peebles ◽  
Simon D. M. White

1978 ◽  
Vol 79 ◽  
pp. 409-421 ◽  
Author(s):  
Ya B. Zeldovich

The God-father of psychoanalysis Professor Sigmund Freud taught us that the behaviour of adults depends on their early childhood experiences. in the same spirit, the problem of cosmological analysis is to derive the observed present day situation and structure of the Universe from certain plausible assumptions about its early behaviour. Perhaps the most important single statement about the large scale structure is that there is no structure at all on the largest scale − 1000 Mpc and more. On this scale the Universe is rather uniform, structureless and isotropically expanding - just according to the simplified pictures of Einstein-Friedmann……. Humason, Hubble…. Robertson, Walker. On the other hand there is a lot of structure on the scale of 100 or 50 Mpc and less. There are clusters and superclusters of galaxies.


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