Confrontation of Cosmological Theories with Observational by Michał Heller, Zbigniew Klimek, Konrad Rudnicki (auth.), M.

By Michał Heller, Zbigniew Klimek, Konrad Rudnicki (auth.), M. S. Longair (eds.)

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In VIew of recent interest in dIfferential counts, I will here compare the observed dIfferential counts wIth the predictions of Lemaitre models. The results are summarized on FIgure 2 where I present the varIation wIth flux density of the ratIo of the differentIal count n(S) to the count noocS- 2 5 expected from the Euclidean model. The observed points are taken from the review paper by Kellermann (1972). 02 and z. = 2. This curve reproduces the observed feature at hIgh flux densities. However, when the contrIbutIOn from sources with dIfferent radIO luminosIties are added, the narrow feature extendIng one decade (from 5 to 50 flux units) is washed out by the large dIspersIOn in the radio lumInosity of the sources.

46<~~~~"~\~~tti;',','''' f - (0 ~ I +3 Abell a Virgo --- Abell II • ••••••• Abellll',IV,V Groups ---- I +2 LOG E (keV) ' -. ::·.. :.... :,. " -'. I 0 ••••••••••••••,. , . )\:. - 23 -I tv 0 1il t'" bO 0 '" INTERGALACTIC GAS 27 classes III to V, only to avoid the lack of isotropy in the background that would be observed If these objects were strong X-ray sources. One sees that a substantIal fraction of the observed background might be due to clusters of galaxIes, rangmg from 100% at 1 keY, through 10% at 10 keY, to 100% at 100 keY and 1 MeV.

1967} when the preponderance of quasars WIth redshifts near 2 was reported (BurbIdge and BurbIdge, 42 V PETROSIAN 1967). At that tIme two anomalies seemed to be present in the redshlft dlstributlOn of quasars. 95. Shklovsky (1967) and Kardashev (1968) attempted to explam this feature as absorption of quasar hght by intervening galaxIes dunng the quasi-statIc period. A long quasi-static period was necessary to explain the narrow feature. 95 feature. 95. We shall not dISCUSS thIS effect here. The other anomaly was the presence of a mlld hump in the redshift distnbution of quasars at z'" 2 (with a rapid cutoff beyond It) WhIch prompted us to consider a Lemaitre model with fairly short quasi-statIc period.

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