arXiv 2301.040422023-01-10astro-ph.GA

模拟银河系扁平子系统天体的垂直分布

Modeling the vertical distribution of the Milky Way's flat subsystem objects

Igor' I. Nikiforov, Vadim A. Usik, Angelina V. Veselova

备注：: 21 pages, 9 figures, 7 tables. Accepted for publication in Research in Astronomy and Astrophysics
DOI：: 10.1088/1674-4527/aca887

摘要：

本文是一个初始阶段的考虑联合建模的银河系平坦的子系统的垂直结构和银河系的磁盘的平均表面的一般问题，考虑到自然和测量分散。我们近似的平均表面的银河系的磁盘与多项式模型，并确定其参数最小化的平方偏差的对象沿法线的模型表面。所开发的方法使我们能够同时识别银河系翘曲的重要细节，并估计太阳相对于银河系盘的平均（非平坦）表面的偏移量$z_\odot$，以及数据覆盖的盘的任意区域的对象系统的垂直尺度。该方法适用于经典造父变星的数据。显着的平均磁盘表面模型的局部极值被发现：在第一银河象限的最小值和最大值在第二。第三象限的一个众所周知的曲速已经被证实。发现模型的最优阶为$n_\text{o}=4$。$z_\odot = 28.1 \pm \left.6.1\right|_{\text{stat.}}\left.{}\pm1.3\right|_{\text{cal.}}$ pc的局部（靠近太阳，$n_\text{o}=0$）估计与非局部（$n_\text{o}=4$）$z_\odot = 27.1 \pm \left.8.8\right|_{\text{stat.}}\left.{}^{+1.3}_{-1.2}\right|_{\text{cal.}}$ pc接近，表明该方法消除了翘曲对$z_\odot$估计的影响.然而，造父变星$σ_ρ = 132.0 \pm \left.3.7\right|_{\text{stat.}}\left.{}^{+6.3}_{-5.9}\right|_{\text{cal.}}$ pc的垂直标准差的非局部估计与局部$σ_ρ = \left.76.5 \pm 4.4\right|_{\text{stat.}}\left.{}^{+3.6}_{-3.4}\right|_{\text{cal.}}$ pc有很大不同，这意味着需要在太阳附近之外引入更复杂的模型。

英文摘要：

This paper is an initial stage of consideration of the general problem of joint modeling of the vertical structure of a Galactic flat subsystem and the average surface of the disk of the Galaxy, taking into account the natural and measurement dispersions. We approximate the average surface of the Galactic disk with a polynomial model and determine its parameters by minimizing the squared deviations of objects along the normal to the model surface. The developed method allows us to simultaneously identify significant details of the Galactic warping and estimate the offset $z_\odot$ of the Sun relative to the average (non-flat) surface of the Galactic disk and the vertical scale of the object system for an arbitrary area of the disk covered by data. The method is applied to data on classical Cepheids. Significant local extremes of the average disk surface model were found: the minimum in the first Galactic quadrant and the maximum in the second. A well-known warp in the third quadrant has been confirmed. The optimal order of the model was found to be $n_\text{o}=4$. The local (near the Sun, $n_\text{o}=0$) estimate of $z_\odot = 28.1 \pm \left.6.1\right|_{\text{stat.}}\left.{}\pm1.3\right|_{\text{cal.}}$ pc is close to the non-local ($n_\text{o}=4$) $z_\odot = 27.1 \pm \left.8.8\right|_{\text{stat.}}\left.{}^{+1.3}_{-1.2}\right|_{\text{cal.}}$ pc, which suggests that the proposed method eliminates the influence of warping on the $z_\odot$ estimate. However, the non-local estimate of the vertical standard deviation of Cepheids $σ_ρ = 132.0 \pm \left.3.7\right|_{\text{stat.}}\left.{}^{+6.3}_{-5.9}\right|_{\text{cal.}}$ pc differs significantly from the local $σ_ρ = \left.76.5 \pm 4.4\right|_{\text{stat.}}\left.{}^{+3.6}_{-3.4}\right|_{\text{cal.}}$ pc, which means the need to introduce more complex models outside the Sun's vicinity.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

摘要：

英文摘要：

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