论文标题
PPXF中具有光度法的全光谱拟合：恒星种群与动态质量，非参数恒星形成历史和金属性，用于3200 lega-c星系，在RedShift Z〜0.8
Full spectrum fitting with photometry in pPXF: stellar population versus dynamical masses, non-parametric star formation history and metallicity for 3200 LEGA-C galaxies at redshift z~0.8
论文作者
论文摘要
我介绍了PPXF方法的一些改进，该方法测量了星系的恒星和气体运动学，星形形成历史（SFH）和化学组成。我描述了PPXF使用的新优化算法以及我同时拟合光谱和光度法所做的更改。我将更新的PPXF方法应用于3200个星系的样本，红移$ 0.6 <z <1 $（中位$ z = 0.76 $，使用LEGA-C SUPERATION（DR3）和28- Bands Phote的光谱，使用光谱的光谱，$ M_ \ AST> 3 \ ast> 3 \ times10^{10} $ m $ _ \ odot $）我将新的JAM动力学模型的质量与PPXF恒星总体$ M_ \ AST $进行比较，并显示后者比以前的估计更可靠。我在PPXF和两个光度源中使用了三种不同的恒星种群合成（SPS）模型。我证实了星系的全球年龄和金属性$ [m/h] $的主要趋势，其恒星速度分散$σ_\ ast $（或中央密度），但我也发现$ [m/h] $取决于固定$σ_\ ast $的年龄。 SFHS揭示了从星形形成到淬火星系的急剧过渡，该星系具有$ \ lg（σ_\ ast/\ mathrm {km \，s^{ - 1}}）> 2.3 $，或平均质量密度在1 kpc $ \ lg（σ_1^{σ_1^{\ rm jam} {\ rm jam}/\ math kpc^{ - 2}}）> 9.9 $，或使用$ [m/h]> -0.1 $，或带有刻有sersic索引$ \ lg n _ {\ rm ser}> 0.5 $。但是，由于$ m_ \ ast $的函数，过渡更加顺畅。对于两个SPS模型和两个光度源，这些结果是一致的，但是它们与第三SPS模型显着差异，这证明了比较模型假设的重要性。 PPXF软件可从https://pypi.org/project/ppxf/获得。
I introduce some improvements to the pPXF method, which measures the stellar and gas kinematics, star formation history (SFH) and chemical composition of galaxies. I describe the new optimization algorithm that pPXF uses and the changes I made to fit both spectra and photometry simultaneously. I apply the updated pPXF method to a sample of 3200 galaxies at redshift $0.6<z<1$ (median $z=0.76$, stellar mass $M_\ast>3\times10^{10}$ M$_\odot$), using spectroscopy from the LEGA-C survey (DR3) and 28-bands photometry from two different sources. I compare the masses from new JAM dynamical models with the pPXF stellar population $M_\ast$ and show the latter are more reliable than previous estimates. I use three different stellar population synthesis (SPS) models in pPXF and both photometric sources. I confirm the main trend of the galaxies' global ages and metallicity $[M/H]$ with stellar velocity dispersion $σ_\ast$ (or central density), but I also find that $[M/H]$ depends on age at fixed $σ_\ast$. The SFHs reveal a sharp transition from star formation to quenching for galaxies with $\lg(σ_\ast/\mathrm{km\, s^{-1}})>2.3$, or average mass density within 1 kpc $\lg(Σ_1^{\rm JAM}/\mathrm{M_\odot kpc^{-2}})>9.9$, or with $[M/H]>-0.1$, or with Sersic index $\lg n_{\rm Ser}>0.5$. However, the transition is smoother as a function of $M_\ast$. These results are consistent for two SPS models and both photometric sources, but they differ significantly from the third SPS model, which demonstrates the importance of comparing model assumptions. The pPXF software is available from https://pypi.org/project/ppxf/.
