The Cosmic Evolution Survey (COSMOS) allows for the first time a highly significant census of environments and structures up to redshift one, as well as a full morphological description of the galaxy population. In this paper we present a study aimed to constrain the evolution, in the redshift range 0.2 < z < 1.2, of the mass content of different morphological types and its dependence on the environmental density. We use a deep multicolor catalog, covering an area of ~0.7 square degrees inside the COSMOS field, with accurate photometric redshifts (i < 26.5 and dz/(z+1) ~ 0.035). We estimate galaxy stellar masses by fitting the multi-color photometry to a grid of composite stellar population models. We quantitatively describe the galaxy morphology by fitting PSF convolved Sersic profiles to the galaxy surface brightness distributions down to F814 = 24 mag for a sample of 41300 objects.
We confirm an evolution of the morphological mix with redshift: the higher the redshift the more disk-dominated galaxies become important. We find that the morphological mix is a function of the local comoving density: the morphology density relation extends up to the highest redshift explored.
The stellar mass function of disk-dominated galaxies is consistent with being constant with redshift. Conversely, the stellar mass function of bulge-dominated systems shows a decline in normalization with redshift. Such different behaviors of late-types and early-types stellar mass functions naturally set the redshift evolution of the transition mass. ABRIDGED
A cosmological model describing the early inflation, the intermediate decelerating expansion, and the late accelerating expansion by a quadratic equation of state
我们发展了一个基于二次状态方程p/c^2=-（α+1）{ρ^2}/{ρ_P}+αρ-（α+1）ρ_Λ（其中ρ_P是普朗克密度，ρ_Λ是宇宙学密度）的宇宙学模型，它以广义Chaubergin气体模型的精神“统一”了真空能量和暗能量.对于$ρ\rightarrow ρ_P$，它降低到p=-ρ c ^2，导致早期加速膨胀（早期暴胀）阶段，密度等于普朗克密度ρ_P（真空能量）。对于$ρ_Λ\llρ\ll ρ_P$，我们恢复了描述辐射（α=1/3）或无压物质（α=0）的标准线性状态方程p=αρc^2，并导致减速膨胀的中间阶段。对于$ρ\rightarrow ρ_Λ$，我们得到p=-ρc^2，导致后期加速膨胀（后期暴胀）阶段，其恒定密度等于宇宙学密度ρ_Λ（暗能量）。我们发现早期宇宙（真空能量+ α流体）和晚期宇宙（α流体+暗能量）之间存在一个很好的对称性。在我们的模型中，它们分别由两个指数为n=+1和n=-1的多方状态方程描述。此外，普朗克密度ρ_P在早期宇宙中所起的作用与宇宙学密度ρ_Λ在晚期宇宙中所起的作用相似。它们代表了基本的密度上限和下限，相差122个数量级。这个二次状态方程导致了一个完全的分析模型，描述了宇宙从早期的膨胀（普朗克时代）到晚期的加速膨胀（德西特时代）的演化。这两个阶段由减速代数展开（α-era）连接。这个模型在t=0时不存在任何奇点，并且永远存在于过去。它允许基于精华…
Focus Point on Tensions in Cosmology from Early to Late Universe: Part II: New Directions in the Light of Observations from the Most Modern Astronomical Facilities
Dipartimento di Fisica E. Pancini, Universit di Napoli Federico II（那不勒斯费德里科二世大学物理系）；INFN, Sezione di Napoli（意大利国家核物理研究所那不勒斯分部）；Scuola Superiore Meridionale（南方高等学院）；School of Mathematical and Physical Sciences, University of Sheffield（谢菲尔德大学数学与物理科学学院）；Center for Cosmology and Astrophysics, Alikhanian National Laboratory and Yerevan State University（阿利哈尼安国立实验室与埃里温州立大学宇宙学与天体物理中心）
