Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.103..301v&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 103, no. 2, Aug. 1984, p. 301-319.
Astronomy and Astrophysics
Astronomy
11
Cosmic Dust, Galactic Clusters, Infrared Astronomy, Interstellar Radiation, Absorptivity, Gas Temperature, Spatial Distribution
Scientific paper
The observations of the reddening of the distant galaxies and the weak diffuse radiation in the clusters of galaxies can be interpreted as a consequence of the presence of dust grains in the intergalactic medium. When allowance is made for the destruction of the grains in collision with particles of the hot gas, its lifetime is about 10 to the 7th - 10 to the 8th yr at a gas concentration ng approximately 0.001 per cu cm. The detection of the infrared (IR) emission from the galaxy clusters might be the test for the proof of the presence of dust grains in the intergalactic medium. In this paper the estimates of the expected intensities and fluxes of IR emission for the spectral region 50-300 microns are presented for two galaxy clusters in Coma and Perseus. The parameters of the hot gas spatial distribution are chosen from X-ray observations. Having assumed that intergalactic dust can be ejected only from the galaxies, such a model for intergalactic dust grains which explains very well the interstellar dust effects is used. It is shown that the dust temperature, which is determined from the general energetic balance of the dust grains, can achieve some scores of degrees of Kelvin. Two models of the dust spatial distribution are considered. It is found that the maximum of IR flux for the Coma cluster lies near lambda = 100 microns and the same for the Perseus cluster near lambda approximately 50-70 microns. The total fluxes of IR emission from these clusters are about 10 to the 5th - 10 to the 6th Jy and can be detected by modern observational methods.
Khersonskii V. K.
Voshchinnikov Nikolai V.
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