论文标题
从经典cepheids的银河系的旋转曲线，质量分布和暗物质含量
The Rotation Curve, Mass Distribution and Dark Matter Content of the Milky Way from Classical Cepheids
论文作者
论文摘要
随着大型恒星调查项目数量的越来越多，研究银河系的优质示踪剂的质量和数量正在迅速增长，其中之一就是经典的头皮。经典的头孢虫是高精度的标准蜡烛，具有非常低的典型不确定性（$ <$ 3％），可通过中红外时期luminosition提供。在这项工作中已经分析了大约3500个从Ogle，ASAS-SN，GAIA，WISE和ZTF调查数据确定的经典头，其空间分布显示出明显的银河经符号。采用了两种运动学方法来测量$ 4 \ sillsim r _ {\ rm gc} \ lyseSim 19 $ kpc的银河旋转曲线。旋转曲线的轻度下降是通过适当的运动（PM）方法和3维速度矢量（3DV）方法得出的。以3DV方法对具有最准确的6D相位空间坐标的最大经典头齿样本进行了建模，并且发现所得的旋转曲线在相对较小的梯度下下降（$ -1.33 \ pm0.1 $）$ -1.33 \ pm0.1 $）$与PM方法的结果相比，较高的旋转速度（（（$ 232.5 \ pm0.83 $）$ {\ rm km \，s^{ - 1}} $）在3DV方法中的太阳位置得出。病毒质量和局部暗物质密度是从3DV方法估算的，这是更可靠的方法，$ m _ {\ rm vir} =（0.822 \ pm0.052）\ times 10^{12} {12} \，m_ \ odot $ and $ p $ and $ρ_{ cm^{ - 3}} $。
With the increasing numbers of large stellar survey projects, the quality and quantity of excellent tracers to study the Milky Way is rapidly growing, one of which is the classical Cepheids. Classical Cepheids are high precision standard candles with very low typical uncertainties ($<$ 3%) available via the mid-infrared period-luminosity relation. About 3500 classical Cepheids identified from OGLE, ASAS-SN, Gaia, WISE and ZTF survey data have been analyzed in this work, and their spatial distributions show a clear signature of Galactic warp. Two kinematical methods are adopted to measure the Galactic rotation curve in the Galactocentric distance range of $4\lesssim R_{\rm GC} \lesssim 19$ kpc. Gently declining rotation curves are derived by both the proper motion (PM) method and 3-dimensional velocity vector (3DV) method. The largest sample of classical Cepheids with most accurate 6D phase-space coordinates available to date are modeled in the 3DV method, and the resulting rotation curve is found to decline at the relatively smaller gradient of ($-1.33\pm0.1$) ${\rm km\,s^{-1}\,kpc^{-1}}$. Comparing to results from the PM method, a higher rotation velocity (($232.5\pm0.83$) ${\rm km\,s^{-1}}$) is derived at the position of Sun in the 3DV method. The virial mass and local dark matter density are estimated from the 3DV method which is the more reliable method, $M_{\rm vir} = (0.822\pm0.052)\times 10^{12}\,M_\odot$ and $ρ_{\rm DM,\odot} = 0.33\pm0.03$ GeV ${\rm cm^{-3}}$, respectively.
