论文标题
在高红移时对M*-SFR关系进行建模：在固有散点测量中驱动偏见的无缠绕因子
Modelling the M*-SFR relation at high redshift: untangling factors driving biases in the intrinsic scatter measurement
论文作者
论文摘要
我们提出了一种自我传播m $ _ {*} $和sfr（$ψ$）的方法，不确定性在截距，坡度和固有散射估算中，用于恒星形成星系的主要模型，其中$ψ=α=α +β$ m $ m $ m $ _ {*} + \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ n n} $ n} $ 0. 0，从$ z \ sim5 $的Nircam过滤器中设置的简单理想化模型，我们测试方法并与文献中的方法进行比较。通过将$ψ$估计为基于粉尘校正的MUV来简化$ψ$估计，可以帮助减少模板集对斜率和截距估计值的影响，但要起到偏向固有的散射估计值的作用。我们发现，仅宽带通量不能限制发射线的贡献，这意味着如果没有中等频段的约束，则需要在排放线上的强大先验。因此，在高红移时，发射线贡献了较高的宽带通量的较高分数，光度法拟合对短（$ \ sim $ 10 MYR）的时间表对$ψ$变化敏感。以恒定（或上升）星形成历史记录（SFH）施加的年龄的先验，不允许人们在高红移时研究$σ$对M $ _ {*} $的可能依赖性。延迟的指数SFHS的先验较少，但在短时间内不考虑$ψ$变化，如果$σ$由于恒星形成的随机性而增加，则问题。与以前的历史相结合的具有当前恒星形成的简单SFH是合适的。我们表明，对于假设点源的简单曝光时间计算，灰尘含量较低，我们应该能够获得对log（m/m $ _ {\ odot} $）$ \ sim $ 8 at $ z \ sim5 $的无偏估计（m/m $ _ {\ odot} $），同时允许james webb space the，同时允许使用Star Choration的站点。
We present a method to self-consistently propagate M$_{*}$ and SFR ($Ψ$) uncertainties onto intercept, slope and intrinsic scatter estimates for a simple model of the main sequence of star forming galaxies where $Ψ= α+ β$M$_{*} + \mathcal{N}(0,σ)$. From simple idealised models set up with broad-band photometry from NIRCam filters at $z\sim5$, we test the method and compare to methods in the literature. Simplifying the $Ψ$ estimate by basing it on dust-corrected MUV can help to reduce the impact of template set degeneracies on slope and intercept estimates, but act to bias the intrinsic scatter estimate. We find that broad-band fluxes alone cannot constrain the contribution from emission lines, implying that strong priors on the emission-line contribution are required if no medium-band constraints are available. Therefore at high redshifts, where emission lines contribute a higher fraction of the broad-band flux, photometric fitting is sensitive to $Ψ$ variations on short ($\sim$ 10 Myr) timescales. Priors on age imposed with a constant (or rising) star formation history (SFH) do not allow one to investigate a possible dependence of $σ$ on M$_{*}$ at high redshifts. Delayed exponential SFHs have less constrained priors, but do not account for $Ψ$ variations on short timescales, a problem if $σ$ increases due to stochasticity of star formation. A simple SFH with current star formation decoupled from the previous history is appropriate. We show that, for simple exposure-time calculations assuming point sources, with low levels of dust, we should be able to obtain unbiased estimates of the main sequence down to log(M/M$_{\odot}$) $\sim$ 8 at $z\sim5$ with the James Webb Space Telescope while allowing for stochasticity of star formation.
