论文标题
通过GAMA DR4，SDSS DR12和Reflex II数据组合对光环质量函数的经验测量
An empirical measurement of the Halo Mass Function from the combination of GAMA DR4, SDSS DR12, and REFLEX II data
论文作者
论文摘要
我们从质量范围10^12.7M_SOL到10^15.5M_SOL的质量范围内的GAMA GALAXY组目录构建了Halo质量函数（HMF），并与LambDACDM的期望找到了很好的一致性。与以前的研究相比，该结果扩展了HMF现在通过数量级测量的质量范围。我们将GAMA DR4 HMF与SDSS DR12和Reflex II调查的类似数据相结合，并适合四参数Murray-Robotham-Power（MRP）功能，在Z〜0.1时有效，屈服：Log10的密度归一化：log10（Phi MPC^3）= -3.96 [+0.55，MOSS-MOSS-MOSS-MOSS-MASS A FROIN-MASS A TROIN-ANF TRING-MOSS-MOSS A TRENT-AN-A. log10（m/m_sol）= 14.13 [+0.43，-0.40]，低质量法律斜率：alpha = -1.68 [+0.21，-0.24]，高质量软化参数为：beta = 0.63 [+0.25，-0.11]。如果我们从Planck 2018 Cosmology对Omega_m的约束折叠，我们能够进一步减少这些不确定性，但这取决于可以将幂律趋势从10^12.7m_sol推断到零质量的假设。在整个过程中，我们强调了改进HMF测量所需的努力：改进了不依赖校准来模拟的光环质量估计值；减少了降低的光环质量不确定性，以减轻由HMF低质量斜率陡峭而产生的强大爱丁顿偏差。以及更深入的区域光谱调查。对于我们的光环质量极限为10^12.7 m_sol，我们直接解决（“看到”）41 +/- 5％的总质量密度，即omega_ [M> 12.7] = 0.128 +/- 0.016，打开了直接构建3D暗质量质量映射在MPC分辨率下的门的门。
We construct the halo mass function (HMF) from the GAMA galaxy group catalogue over the mass range 10^12.7M_sol to 10^15.5M_sol, and find good agreement with the expectation from LambdaCDM. In comparison to previous studies, this result extends the mass range over which the HMF has now been measured over by an order of magnitude. We combine the GAMA DR4 HMF with similar data from the SDSS DR12 and REFLEX II surveys, and fit a four-parameter Murray-Robotham-Power (MRP) function, valid at z~0.1, yielding: a density normalisation of: log10 (phi Mpc^3)=-3.96[+0.55,-0.82], a high mass turn-over of: log10(M/M_sol)=14.13[+0.43,-0.40], a low mass power law slope of: alpha=-1.68[+0.21,-0.24] , and a high mass softening parameter of: beta= 0.63[+0.25,-0.11]. If we fold in the constraint on Omega_M from Planck 2018 Cosmology, we are able to reduce these uncertainties further, but this relies on the assumption that the power-law trend can be extrapolated from 10^12.7M_sol to zero mass. Throughout, we highlight the effort needed to improve on our HMF measurement: improved halo mass estimates that do not rely on calibration to simulations; reduced halo mass uncertainties needed to mitigate the strong Eddington Bias that arises from the steepness of the HMF low mass slope; and deeper wider area spectroscopic surveys. To our halo mass limit of 10^12.7 M_sol, we are directly resolving (`seeing') 41+/-5 per cent of the total mass density, i.e. Omega_[M>12.7]=0.128+/-0.016, opening the door for the direct construction of 3D dark matter mass maps at Mpc resolution.
