We investigate how well the intrinsic shape of early-type galaxies can be recovered when both photometric and two-dimensional stellar kinematic observations are available. We simulate these observations with galaxy models that are representative of observed oblate fast-rotator to triaxial slow-rotator early-type galaxies. By fitting realistic triaxial dynamical models to these simulated observations, we recover the intrinsic shape (and mass-to-light ratio), without making additional (ad-hoc) assumptions on the orientation.
For (near) axisymmetric galaxies the dynamical modelling can strongly exclude triaxiality, but the regular kinematics do not further tighten the constraint on the intrinsic flattening significantly, so that the inclination is nearly unconstrained above the photometric lower limit even with two-dimensional stellar kinematics. Triaxial galaxies can have additional complexity in both the observed photometry and kinematics, such as twists and (central) kinematically decoupled components, which allows the intrinsic shape to be accurately recovered. For galaxies that are very round or show no significant rotation, recovery of the shape is degenerate, unless additional constraints such as from a thin disk are available.
Intrinsic Axis Ratio Distribution of Early-type Galaxies From Sloan Digital Sky Survey
利用Sloan数字巡天数据Release 5研究了早型星系的内禀轴比分布。我们在$0.05 \leq z \leq 0.06$建立了一个3,922个目视检查的早期类型星系的体积有限的样本，仔细考虑由星系等照度线的大小和光度引起的采样偏差。我们试图去项目所观察到的ARD成三维类型（扁圆，扁长，和三轴），这是在三轴性方面进行分类。我们证实，没有线性组合的$randomly$分布轴比的三种类型可以重现所观察到的ARD。然而，使用高斯本征分布，我们发现了与扁圆、长轴和三轴（两个轴比中的三轴）的优选平均轴比的数据的合理拟合，其中扁圆、长轴和三轴类型的分数为\textrm{O:P:T} =0.29^{ \pm 0.09}：0.26^{ \pm 0.11}：0.45^{ \pm 0.13} $. We have also found that the luminous sample ($-23.3 < M_r \leq-21.2 $) tends to have more triaxials than the less luminous ($-21.2 < M_r <-19.3 $）样品确实。扁圆星系在亮度较低的星系中相对较多。有趣的是，两个光度类别中三轴类型的轴比的偏好非常相似。我们没有发现任何显着的影响，本地星系数密度的ARD。我们发现，结果可能会受到严重影响的数据选择和类型分类方案的细节。…
Fraction of the radial velocity stable stars in the early observations of the Grid Giant Star Survey
GGSS是一个部分填充的全天空巡天，用于识别具有低水平RV变化的K巨星。我们研究了网格巨星巡天早期阶段获得的径向速度（RV）变化的直方图（GGSS，Bizyaev等人，2006年）。这部分的巡天是在每颗恒星的观测数量非常有限的情况下进行的，精度也很粗略。我们应用蒙特卡罗模拟来推断样本中RV稳定星的一部分。我们的乐观估计是，20%的所有考虑的K-巨星的RV-可变性低于30 m s $^{-1}$。不同的假设，我们的恒星的内在RV-可变性给出了12 - 20%的RV-稳定的K-巨星在研究的样本。
Evidence for Intrinsic Redshifts in Normal Spiral Galaxies
利用Tully-Fisher关系（TFR）确定了正常旋涡星系的反常红移。在这个分析中发现了三个红移异常：（1）发现晚型旋涡星系相对于早型旋涡星系有明显的超额红移;（2）发现与ScI星系形态相似的星系团相对于哈勃常数为72 km s ~（-1）Mpc ~（-1）的红移有系统的超额红移;（3）个别星系，对，和组被确定为强烈偏离光滑哈勃流的预测。这些红移偏差明显大于可以解释的特殊运动和TFR的错误。它的结论是，在此分析中确定的红移异常与以前的大的非宇宙学（本征）红移的索赔是一致的。
Modelling the Interstellar Medium of Low Surface Brightness Galaxies: Constraining Internal Extinction, Disk Color Gradients, and Intrinsic Rotation Curve Shapes
