We study the counts of resolved SZE (Sunyaev-Zel'dovich effect) clusters expected from an interferometric survey in different cosmological models under different conditions. The self-similar universal gas model an...We study the counts of resolved SZE (Sunyaev-Zel'dovich effect) clusters expected from an interferometric survey in different cosmological models under different conditions. The self-similar universal gas model and Press-Schechter mass function are used. We take the observing frequency to be 90 GHz, and consider two dish diameters, 1.2 m and 2.5 m. We calculate the number density of the galaxy clusters dN/(dΩdz) at a high flux limit S<SUB>v</SUB><SUP>lim</SUP>=100 mJy and at a relative low S<SUB>v</SUB><SUP>lim</SUP> =10 mJy. The total numbers of SZE clusters N in two low-Ω<SUB>0</SUB> models are compared. The results show that the influence of the resolved effect depends not only on D, but also on S<SUB>v</SUB><SUP>lim</SUP>: at a given D, the effect is more significant for a high than for a low S<SUB>v</SUB><SUP>lim</SUP>. Also, the resolved effect for a flat universe is more impressive than that for an open universe. For D = 1.2 m and S<SUB>v</SUB><SUP>lim</SUP> =10 mJy, the resolved effect is very weak. Considering the designed interferometers which will be used to survey SZE clusters, we find that the resolved effect is insignificant when estimating the expected yield of the SZE cluster surveys.展开更多
文摘We study the counts of resolved SZE (Sunyaev-Zel'dovich effect) clusters expected from an interferometric survey in different cosmological models under different conditions. The self-similar universal gas model and Press-Schechter mass function are used. We take the observing frequency to be 90 GHz, and consider two dish diameters, 1.2 m and 2.5 m. We calculate the number density of the galaxy clusters dN/(dΩdz) at a high flux limit S<SUB>v</SUB><SUP>lim</SUP>=100 mJy and at a relative low S<SUB>v</SUB><SUP>lim</SUP> =10 mJy. The total numbers of SZE clusters N in two low-Ω<SUB>0</SUB> models are compared. The results show that the influence of the resolved effect depends not only on D, but also on S<SUB>v</SUB><SUP>lim</SUP>: at a given D, the effect is more significant for a high than for a low S<SUB>v</SUB><SUP>lim</SUP>. Also, the resolved effect for a flat universe is more impressive than that for an open universe. For D = 1.2 m and S<SUB>v</SUB><SUP>lim</SUP> =10 mJy, the resolved effect is very weak. Considering the designed interferometers which will be used to survey SZE clusters, we find that the resolved effect is insignificant when estimating the expected yield of the SZE cluster surveys.
