Merging Rates of the First Objects and the Formation of First Mini-Filaments in Models with Massive Neutrinos
Hyunmi Song, Jounghun Lee
备注：
Accepted for publication in ApJ, mistakes in the calculation of the merging rates corrected, feasibility study of constraining neutrino mass with high-z quasar luminosity function presented, discussion improved, 7 figures
We study the effect of massive neutrinos on the formation and evolution of the first filaments containing the first star-forming halos of mass M~10^{6}M_sun at z~20. With the help of the extended Press-Schechter formalism, we evaluate analytically the rates of merging of the first star-forming halos into zero-dimensional larger halos and one-dimensional first filaments. It is shown that as the neutrino mass fraction f_ν increases, the halo-to-filament merging rate increases while the halo-to-halo merging rate decreases sharply. For f_ν<=0.04, the halo-to-filament merging rate is negligibly low at all filament mass scales, while for f_ν>=0.07 the halo-to-filament merging rate exceeds 0.1 at the characteristic filament mass scale of ~10^{9}M_sun. The distribution of the redshifts at which the first filaments ultimately collapse along their longest axes is derived and found to have a sharp maximum at z~8. We also investigate the formation and evolution of the second generation filaments which contain the first galaxies of mass 10^{9}M_sun at z=8 as the parent of the first generation filaments. A similar trend is found: For f_ν>= 0.07 the rate of clustering of the first galaxies into the second-generation filaments exceeds 0.3 at the characteristic mass scale of ~10^{11}M_sun. The longest-axis collapse of these second-generation filaments are found to occur at z~3. The implications of our results on the formation of massive high-z galaxies and the early metal enrichment of the intergalactic media by supernova-driven outflows, and possibility of constraining the neutrino mass from the mass distribution of the high-z central blackholes are discussed.
Mapping Dark Matter in Merging Clusters with Weak Lensing for CSST: Morphology and Filament Recovery
National Astronomical Observatories (NAOC), Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Science（中国科学院大学天文与空间科学学院）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；South-Western Institute for Astronomy Research (SWIFAR), Yunnan University（云南大学西南天文研究所）；Yunnan Key Laboratory of Survey Science,Yunnan University（云南大学云南省测绘科学重点实验室）；Shanghai Astronomical Observatory (SHAO)（中国科学院上海天文台）；Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences（中国科学院射电天文与技术重点实验室）
Revealing the intricacies of radio galaxies and filaments in the merging galaxy cluster Abell 2255. II. Properties of filaments using multi-frequency radio data
Università di Bologna（博洛尼亚大学）；INAF - Istituto di Radioastronomia di Bologna（意大利国家天体物理研究所波洛尼亚射电天文台）；Leiden University（莱顿大学）；ASTRON, The Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；University of Minnesota（明尼苏达大学）；Universität Hamburg（汉堡大学）；Durham University（杜伦大学）
Revealing the intricacies of radio galaxies and filaments in the merging galaxy cluster Abell 2255. I. Insights from deep LOFAR-VLBI sub-arcsecond resolution images
Study of Polarized Emission in Radio Halos and Filaments in the SKA Telescopes Era
Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）；Sapienza—University of Rome（罗马第一大学）；University of Bologna（博洛尼亚大学）；Université Côte d'Azur（蔚蓝海岸大学）；University of Cagliari（卡利亚里大学）
