论文标题
在太阳700 pc内的银河尘埃层的性质上
On the Properties of the Galactic Dust Layer within 700 pc of the Sun
论文作者
论文摘要
我们将空间恒星颜色变化与空间灰尘分布的3D模型进行比较，以完善银河太阳街中灰尘层的特性。我们使用93992团块巨头的完整样品，并在空间圆柱体中与Gaia DR2目录的分支巨头混合，在太阳周围的半径为700 pc，延伸至| Z | = 1800 PC。这些恒星在GAIA DR2 GRP和WISE W3频段中的准确数据允许使用空间GRP-W3颜色变化来计算模型参数和样品的两个特征，即DEDEDDENDED的颜色模式（GRP-W3）0（GRP-W3）0的巨型团块和与该模式的线性变化与coorcorcorcor | z | | | | | |。结果，已经获得了Gontcharov（2009b）首先提出的三维模型的改进版本。与上一个版本一样，该模型沿着银河赤道和古尔德皮带中的两个尘埃层，它们以18 \ pm2摄氏度的角度在太阳附近相交。与先前版本的模型形成鲜明对比的是，在新版本中，中间平面是一个相对于太阳的椭圆形的椭圆形。两种防尘层都发现了170 \ pm40 pc的比例高度。绝对幅度MW3 = -1.70 \ PM0.02和DERDEDDEN的颜色（GRP-W3）0 =（1.43 \ PM0.01）的模式，（0.020 \ pm0.007）| Z |，其中Z以KPC表示为Z，已计算出kpc的巨型团团附近的巨型团块。所考虑的数量的分散体允许相对于根据模型计算出的平均红色粉尘介质的天然小规模密度波动。这些波动为变红的不确定性做出了重大贡献。
We compare the spatial stellar color variations with our 3D model of the spatial dust distribution to refine the properties of the dust layer in Galactic solar neighborhoods. We use a complete sample of 93992 clump giants with an admixture of branch giants from the Gaia DR2 catalogue in a spatial cylinder with a radius of 700 pc around the Sun extending to |Z|=1800 pc. Accurate data of these stars in the Gaia DR2 GRP and WISE W3 bands have allowed the spatial GRP-W3 color variations to be used to calculate the model parameters and two characteristics of the sample, the mode of the dereddened color (GRP-W3)0 of the giant clump and the linear change of this mode with coordinate |Z|. As a result, an improved version of the three-dimensional model first proposed by Gontcharov (2009b) has been obtained. As in the previous version, the model suggests two dust layers, along the Galactic equator and in the Gould Belt, that intersect near the Sun at an angle of 18\pm2 degs. In contrast to the previous version of the model with a midplane of the Gould Belt dust layer in the form of a circle with the center at the Sun, in the new version this midplane is an ellipse decentered relative to the Sun. A scale height of 170\pm40 pc has been found for both dust layers. The modes of the absolute magnitude MW3=-1.70\pm0.02 and the dereddened color (GRP-W3)0=(1.43\pm0.01)-(0.020\pm0.007)|Z|, where Z is expressed in kpc, have been calculated for the giant clump near the Sun. The dispersions of the quantities under consideration have allowed the natural small-scale density fluctuations of the dust medium relative to the mean reddening calculated from the model to be characterized. These fluctuations make a major contribution to the uncertainty in the reddening.
