论文标题
迈向温暖的暗物质光环质量函数的一般参数化
Towards a general parametrization of the warm dark matter halo mass function
论文作者
论文摘要
恒星流中通量异常统计和扰动的研究可能会限制包括无菌中微子在内的温暖暗物质模型（WDM）。产生这些约束需要相对于冷暗物质（CDM）等效的wdm质量函数的参数化。 We use five WDM models with half-mode masses, $M_\mathrm{hm}=[1.3,35]\times10^{8}$~$M_{\odot}$, spread across simulations of the Local Group, lensing ellipticals and the $z=2$ universe, to generate such a parametrization: we fit parameters to a functional form for the WDM-to-CDM halo质量函数比率，$ n_ \ mathrm {wdm}（m_ {x}）/n_ \ mathrm {cdm}（m_ {x}）$，of（$ 1+（$ 1+）（αm_\ mathrm {hm}/m_}/m_ {x}}）^β）^β）^β）^β$。对于$ m_ {x} \ equiv $中央光环的病毒质量，我们获得$α= 2.3 $，$β= 0.8 $，$γ= -1.0 $，并且这种拟合度比扩展的新闻编组形式主义预测的更陡。对于$ m_ {x} \ equiv $ subhalos的质量，我们获得$α= 4.2 $，$β= 2.5 $和$γ= -0.2 $;在这两个质量定义中，散点都是$ \ sim20 $〜每〜Cent。第二个拟合通常低估了$ z = 2 $ wdm subhaloes的相对丰度在数百分之级的水平上。我们警告说，鲁棒的约束将需要定制模拟和对光环质量的仔细定义，尤其是对于质量$ <10^{8} m _ {\ odot} $的Subhalos。
Studies of flux anomalies statistics and perturbations in stellar streams have the potential to constrain models of warm dark matter (WDM), including sterile neutrinos. Producing these constraints requires a parametrization of the WDM mass function relative to that of the cold dark matter (CDM) equivalent. We use five WDM models with half-mode masses, $M_\mathrm{hm}=[1.3,35]\times10^{8}$~$M_{\odot}$, spread across simulations of the Local Group, lensing ellipticals and the $z=2$ universe, to generate such a parametrization: we fit parameters to a functional form for the WDM-to-CDM halo mass function ratio, $n_\mathrm{WDM}(M_{X})/n_\mathrm{CDM}(M_{X})$, of ($1+(αM_\mathrm{hm}/M_{X})^β)^γ$. For $M_{X}\equiv$ virial mass of central halos we obtain $α=2.3$, $β=0.8$, and $γ=-1.0$, and this fit is steeper than the extended Press-Schechter formalism predicts. For $M_{X}\equiv$ mass of subhalos we instead obtain $α=4.2$, $β=2.5$ and $γ=-0.2$; in both mass definitions the scatter is $\sim20$~per~cent. The second fit typically underestimates the relative abundance of $z=2$ WDM subhaloes at the tens of per cent level. We caution that robust constraints will require bespoke simulations and a careful definition of halo mass, particularly for subhalos of mass $<10^{8}M_{\odot}$.
