折射引力下DiskMass巡天星系的动力学
Dynamics of DiskMass Survey galaxies in refracted gravity
摘要：
我们测试如果折射重力（RG）可以描述动态的磁盘星系，而不诉诸暗物质。RG是经典的引力理论，其中标准泊松方程由引力介电常数$ε$（局部质量密度的普适单调函数）修改。本文利用银河质量巡天（DMS）中30个星系的自转曲线和垂直速度色散来确定$ε$。RG描述了与SPS模型一致的质轻比的运动学剖面，以及与观测一致的盘厚度，一旦考虑观测偏差。我们的结果依赖于设置每个星系的$ε$的三个自由参数。然而，我们表明，这些参数的差异，从星系到星系可以归因于统计波动。我们采用一种近似的方法来找到一组参数，可以适当地描述整个样品的运动学，并建议$ε$的普遍性。最后，我们表明，RG模型的个别旋转曲线只能部分描述径向加速度关系（RAR）。显然，RG模型低估了在低牛顿加速度下观察到的0.1-0.3 dex的加速度。另一个问题是强相关性，在远超过5 $σ$，RAR模型的残差和三个径向依赖的星系属性之间，而DMS数据显示一个相当不太重要的相关性，在超过4 $σ$，只有其中两个。这些相关性可能导致RG模型的非零内禀散射，这与观测到的不同于DMS的星系样本的内禀散射不一致，这与0。需要进一步的研究来评估RAR中的这些差异是否源于DMS样本，这可能对于推导RAR并不理想，或者它们是否是RG的真正失败。
英文摘要：
We test if Refracted Gravity (RG) can describe the dynamics of disk galaxies without resorting to dark matter. RG is a classical theory of gravity where the standard Poisson equation is modified by the gravitational permittivity, $ε$, a universal monotonic function of the local mass density. We use the rotation curves and the vertical velocity dispersions of 30 galaxies in the DiskMass Survey (DMS) to determine $ε$. RG describes the kinematic profiles with mass-to-light ratios consistent with SPS models, and disk thicknesses in agreement with observations, once observational biases are considered. Our results rely on setting the three free parameters of $ε$ for each galaxy. However, we show that the differences of these parameters from galaxy to galaxy could be ascribed to statistical fluctuations. We adopt an approximate method to find a single set of parameters that may properly describe the kinematics of the entire sample and suggest the universality of $ε$. Finally, we show that the RG models of the individual rotation curves can only partly describe the radial acceleration relation (RAR). Evidently, the RG models underestimate the observed accelerations of 0.1-0.3 dex at low Newtonian accelerations. Another problem is the strong correlation, at much more than 5$σ$, between the residuals of the RAR models and three radially-dependent properties of galaxies, whereas the DMS data show a considerably less significant correlation, at more than 4$σ$, for only two of them. These correlations might originate the non-null intrinsic scatter of the RG models, at odds with the observed intrinsic scatter of galaxy samples different from DMS, which is consistent with 0. Further studies are required to assess if these discrepancies in the RAR originate from the DMS sample, which might not be ideal for deriving the RAR, or if they are genuine failures of RG.
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