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The physical properties of the intergalactic gas in rich clusters of galaxies
Astronomy Reports, 2010We perform a statistical analysis of the properties of 170 rich clusters of galaxies. We confirm the existence of correlations between the X-ray luminosity and temperature of the cluster intergalactic medium (IGM) and between the velocity dispersion of the galaxies and the X-ray luminosity of the IGM.
I. B. Kuvshinova, I. K. Rozgacheva
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A first glimpse of possibly primordial intergalactic gas
Physics Today, 2012Before the first stars, there were presumably no nuclei heavier than lithium. But pristine gas without a trace of stellar contamination has been elusive.
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Quasars: Their Evolution, Absorption Lines and the Intergalactic Gas
Transactions of the International Astronomical Union, 1988For many years now it has been known that the number vs. magnitude counts of quasars is the prima facie evidence of a cosmological evolution of this class of objects. Down to an apparent magnitude B - 19 the number of quasars increases by almost a factor 8 per magnitude Interval, compared to a factor 4 obtained in an Euclidean universe filled with a ...
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Coma cluster gives up secrets of intergalactic gas
Nature Astronomy, 2019Extremely deep observations of the Coma galaxy cluster with the Chandra X-ray Observatory have found that the gas between galaxies, where the vast majority of the baryons lie, is far less viscous than expected.
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On the sources of the thermal energy of the intergalactic gas in clusters of galaxies
Astrophysics, 1984Possible mechanisms of heating of the intergalactic gas in clusters are discussed. It is shown that the energy released in the form of cosmic rays in supernova explosions in the early stages of evolution of the galaxies is sufficiently great to be an important source of the observed high temperature of the gas in the clusters.
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On Intergalactic Gas as a Possible Absorber of Extragalactic Radio Noise
Nature, 1964IT has recently been pointed out by Smith1 that most of the background radiation at low frequencies (< 10 Mc/s) is probably of extragalactic origin. The intensity of this radiation increases with decreasing frequency until about 3 Mc/s where it turns over sharply1–3. This turnover is probably due to absorption by ionized hydrogen, the required emission
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KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Astrophysical Journal, 2022Michele Fumagalli +2 more
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