摘要
By phenomenologically describing the high-redshift star formation history, i.e., ,ρ.（z） oc [（1 ＋z）/4.5]-% and semi-analytically calculating the fractions of high-redshift Pop I/II and Pop II! stars, we investigate the contributions from both high-redshfit Pop I/II and Pop II/stars to the observed near-infrared （3 μm 〈// 〈 5 μm） excess in the cosmic infrared background emission. In order to account for the observational level of the near-infrared excess, the power-law index or of the assumed star formation history is constrained to within the range of 0 ≤a≤1. Such a constraint is obtained under the condition that the viral temperature of dark matter halos belongs to the range of 500 K ≤ Tvir≤ 104 K.
By phenomenologically describing the high-redshift star formation history, i.e., ρ*(z)∝[(1+z)/4.5]-α , and semi-analytically calculating the fractions of high-redshift Pop Ⅰ/Ⅱ and Pop Ⅲ stars, we investigate the contributions from both high-redshfit Pop Ⅰ/Ⅱ and Pop Ⅲ stars to the observed near-infrared (3μm<λ<5μm) excess in the cosmic infrared background emission. In order to account for the observational level of the near-infrared excess, the power-law index α of the assumed star formation history is constrained to within the range of 0≤α≤1. Such a constraint is obtained under the condition that the viral temperature of dark matter halos belongs to the range of 500K≤Tvir≤104K.
基金
supported by the National Natural Science Foundation of China (Grant No.11103004)
the Foundation for the Authors of National Excellent Doctoral Dissertations of China (Grant No.201225)
