论文标题
宇宙网（PAC）周围的光度对象在光谱调查中描述。 iii。借助宇宙红移调查，准确测量星系恒星质量功能
Photometric Objects Around Cosmic Webs (PAC) Delineated in a Spectroscopic Survey. III. Accurate Measurement of Galaxy Stellar Mass Function with the Aid of Cosmological Redshift Surveys
论文作者
论文摘要
我们提出了一种新的方法，可以根据我们该系列的第一篇论文（论文I）中开发的宇宙网（PAC）方法的光度对象准确测量星系恒星质量函数（GSMF）。该方法使我们能够测量GSMF到较低的质量端，而PAC中使用的光谱样品无法访问。与纸I相比，GSMF的当前测量是直接的，并且独立于模型。我们在红移范围内测量GSMFS <0.2 $，$ 0.2 <z_s <0.4 $和$ 0.5 <z_s <0.7 $降低到恒星质量$ $ m _*= 10^{8.2} $，$ 10^{10.6} $ 10^{10.6} $和$ 10^{10^{10.6} desi} m _ =口号数字天空调查的调查和光谱样品（即Main，Lowz和CMASS样本）。我们的结果表明，GSMF从$ z_s = 0.6 $到$ z_s = 0.1 $ for $ m _*> 10> 10> 10^{10.6} m _ {\ odot} $，并且在$ m _*\ od od of to to to y to $ _ {9.5} m _ {\ ody palax in to $ m _********} $ to thaty to that to that to than palaxies to $ z_s = 0.1 $。我们在整个$ m _*$的整个范围内为本地GSMF提供了准确的双schechter拟合，并在三个红移处提供了我们的测量表，可以用来测试星系形成的理论。我们的方法可以将GSMF准确地测量到恒星质量限制，而光谱样品已经高度不完整（例如$ \ sim 10^{ - 3} $）进行目标选择。
We present a novel method to accurately measure the galaxy stellar mass function (GSMF) based upon the Photometric objects Around Cosmic webs (PAC) method developed in our first paper (Paper I) of the series. The method allows us to measure the GSMF to a lower mass end that is not accessible to the spectroscopic sample used in the PAC. Compared with Paper I, the current measurement of GSMF is direct and model independent. We measure the GSMFs in the redshift ranges of $z_s<0.2$, $0.2<z_s<0.4$ and $0.5<z_s<0.7$ down to the stellar mass $M_*=10^{8.2}$, $10^{10.6}$ and $10^{10.6}M_{\odot}$, using the data from the DESI Legacy Imaging Surveys and the spectroscopic samples of Slogan Digital Sky Survey (i.e. Main, LOWZ and CMASS samples). Our results show that there is no evolution of GSMF from $z_s=0.6$ to $z_s=0.1 $ for $M_*>10^{10.6} M_{\odot}$, and that there is a clear up-turn at $M_*\approx 10^{9.5} M_{\odot}$ towards smaller galaxies in the local GMSF at $z_s=0.1$. We provide an accurate double Schechter fit to the local GSMF for the entire range of $M_*$ and a table of our measurements at the three redshifts, which can used to test theories of galaxy formation. Our method can achieve an accurate measurement of GSMF to the stellar mass limit where the spectroscopic sample is already highly incomplete (e.g. $\sim 10^{-3}$) for its target selection.
