B波段星系光度函数的近似贝叶斯测量
Measurement of the B-band Galaxy Luminosity Function with Approximate Bayesian Computation
摘要：
星系光度函数（LF）是研究星系形成、演化和宇宙学的重要观测量。在这项工作中，我们提出了一种新的技术，前向模型宽场宽带星系调查使用快速图像模拟器UFig和测量LF的星系在B波段。我们使用近似贝叶斯计算（ABC）来约束模拟的星系种群模型参数，并匹配CFHTLS的数据。我们定义了一些模拟和调查数据之间的距离度量。通过探索参数空间的星系人口模型，通过ABC找到一组参数，使这些距离度量最小化，我们得到的约束的LF的蓝色和红色星系的红移的函数。我们发现，对于蓝星系和红星系，$\mathrm{M^*}$在红移$\mathrm{z = 1}$和$\mathrm{z = 0.1}$之间分别衰减$Δ\mathrm{M}^*_{\mathrm{0.1-1.0,b}} = 0.68 \pm 0.52$和$Δ\mathrm{M}^*_{\mathrm{0.1-1.0,r}} = 0.54 \pm 0.48$量级.我们还发现，蓝星系的$ϕ^*$在红移$\mathrm{z = 0.1}$和$\mathrm{z=1}$之间大致保持不变，而红星系的$ϕ^*$则减少了$\sim 35\%$。我们比较我们的结果与其他测量，发现在所有红移良好的协议，蓝色和红色星系。为了进一步检验我们的结果，我们比较了观测数据和模拟数据的红移分布。我们使用的光谱红移分布从VIMOS公共河外红移巡天（VIPERS），我们应用相同的选择在我们的模拟颜色和幅度。我们发现一个很好的协议之间的调查和模拟的红移分布。我们为LF的参数提供最佳拟合值和不确定性。这项工作提供了良好的前景，测量其他星系人口的性质作为红移的函数，使用ABC。
英文摘要：
The galaxy Luminosity Function (LF) is a key observable for galaxy formation, evolution studies and for cosmology. In this work, we propose a novel technique to forward model wide-field broad-band galaxy surveys using the fast image simulator UFig and measure the LF of galaxies in the B-band. We use Approximate Bayesian Computation (ABC) to constrain the galaxy population model parameters of the simulations and match data from CFHTLS. We define a number of distance metrics between the simulated and the survey data. By exploring the parameter space of the galaxy population model through ABC to find the set of parameters that minimize these distance metrics, we obtain constraints on the LFs of blue and red galaxies as a function of redshift. We find that $\mathrm{M^*}$ fades by $Δ\mathrm{M}^*_{\mathrm{0.1-1.0,b}} = 0.68 \pm 0.52$ and $Δ\mathrm{M}^*_{\mathrm{0.1-1.0,r}} = 0.54 \pm 0.48$ magnitudes between redshift $\mathrm{z = 1}$ and $\mathrm{z = 0.1}$ for blue and red galaxies, respectively. We also find that $ϕ^*$ for blue galaxies stays roughly constant between redshift $\mathrm{z = 0.1}$ and $\mathrm{z=1}$, while for red galaxies it decreases by $\sim 35\%$. We compare our results to other measurements, finding good agreement at all redshifts, for both blue and red galaxies. To further test our results, we compare the redshift distributions for survey and simulated data. We use the spectroscopic redshift distribution from the VIMOS Public Extragalactic Redshift Survey (VIPERS) and we apply the same selection in colours and magnitudes on our simulations. We find a good agreement between the survey and the simulated redshift distributions. We provide best-fit values and uncertainties for the parameters of the LF. This work offers excellent prospects for measuring other galaxy population properties as a function of redshift using ABC.
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