Establishing HI mass vs. stellar mass and halo mass scaling relations using an abundance matching method  

作　　者：Yi Lu Xiaohu Yang Chengze Liu Haojie Xu Antonios Katsianis Hong Guo Xiaoju Xu Yizhou Gu 

机构地区：[1]Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China [2]Tsung-Dao Lee Institute,and Shanghai Key Laboratory for Particle Physics and Cosmology,Shanghai Jiao Tong University,Shanghai 200240,China [3]Department of Astronomy,School of Physics and Astronomy,Shanghai Jiao Tong University,Shanghai 200240,China [4]School of Physics and Astronomy,Sun Yat-sen University,Zhuhai Campus,Zhuhai 519082,China

出　　处：《Science China(Physics,Mechanics & Astronomy)》2024年第11期149-163,共15页中国科学：物理学、力学、天文学（英文版）

基　　金：supported by the National Key R&D Program of China(Grant Nos.2023YFA1607800,and 2023YFA1607804);the National Natural Science Foundation of China (Grant Nos.11833005,11890692,and12141302);the Fundamental Research Funds for the Central Universities,111 Project (Grant No.B20019);Shanghai Natural Science Foundation(Grant No.19ZR1466800);the science research grants from the China Manned Space Project (Grant Nos.CMS-CSST-2021-A02;CMS-CSST-2021-A03)。

摘　　要：We combined data from the Sloan Digital Sky Survey(SDSS) and the Arecibo Legacy Fast ALFA Survey(ALFALFA) to establish the HI mass vs. stellar mass and halo mass scaling relations using an abundance matching method that is free of the Malmquist bias. To enable abundance matching, a cross-match between the SDSS DR7 galaxy group sample and the ALFALFA HI sources provides a catalog of 16520 HI-galaxy pairs within 14270 galaxy groups(halos). By applying the observational completeness reductions for both optical and HI observations, we used the remaining 8180 ALFALFA matched sources to construct the model constraints. Taking into account the dependence of HI mass on both the galaxy and group properties, we establish two sets of scaling relations: one with a combination of stellar mass,(g-r) color and halo mass, and the other with stellar mass,specific star-formation rate(sSFR), and halo mass. We demonstrate that our models can reproduce the HI mass component as both stellar mass and halo mass. Additional tests showed that the conditional HI mass distributions as a function of the cosmic web type and the satellite fractions were well recovered.

关 键 词：galaxy groups neutral hydrogen HALOS STATISTICAL 

分 类 号：P15[天文地球—天文学]