我们利用我们先前发表的VLT/FORS 2吸收线光谱的空间信息，测量了25个场早型星系的平均恒星速度和速度色散分布，中位红移z=0.97（全范围0.6<z<1.2）。这提供了第一个详细的研究早期类型的星系旋转在这些红移。从HST成像的表面亮度分布，我们计算两个积分扁圆轴对称的Jeans方程模型所观察到的运动学。适合每个星系的旋转支持度和质量与光的比率M/L_牛仔裤的数据产量。S 0和Sa星系通常是旋转支撑的，而椭圆星系旋转速度较慢或根本不旋转。直到M（B）=-19.5（校正光度演化），我们没有发现在z=1（63+/-11%）和现在（61+/-5%）之间旋转的早期型（E+ S 0）星系的演化证据。我们解释这作为证据很少或没有变化的领域S 0分数红移。我们比较了M/L_Jeans和M/L_vir，它们是由维里定理和全局平均量推导出来的，并假设同源演化。有很好的协议，非旋转（主要是E）星系。然而，对于旋转支撑星系（主要是S 0），M/L_Jeans平均比M/L_vir高约40%。我们讨论了可能的解释和影响的M/L之间的z=1和本和它的依赖于质量的演变。
英文摘要：
We use the spatial information of our previously published VLT/FORS2 absorption line spectroscopy to measure mean stellar velocity and velocity dispersion profiles of 25 field early-type galaxies at a median redshift z=0.97 (full range 0.6<z<1.2). This provides the first detailed study of early-type galaxy rotation at these redshifts. From surface brightness profiles from HST imaging we calculate two-integral oblate axisymmetric Jeans equation models for the observed kinematics. Fits to the data yield for each galaxy the degree of rotational support and the mass-to-light ratio M/L_Jeans. S0 and Sa galaxies are generally rotationally supported, whereas elliptical galaxies rotate less rapidly or not at all. Down to M(B)=-19.5 (corrected for luminosity evolution), we find no evidence for evolution in the fraction of rotating early-type (E+S0) galaxies between z=1 (63+/-11%) and the present (61+/-5%). We interpret this as evidence for little or no change in the field S0 fraction with redshift. We compare M/L_Jeans with M/L_vir inferred from the virial theorem and globally averaged quantities and assuming homologous evolution. There is good agreement for non-rotating (mostly E) galaxies. However, for rotationally supported galaxies (mostly S0) M/L_Jeans is on average ~40% higher than M/L_vir. We discuss possible explanations and the implications for the evolution of M/L between z=1 and the present and its dependence on mass.
IRCS/Subaru Observations of Water in the Inner Coma of Comet 73P-B/Schwassmann-Wachmann 3: Spatially Resolved Rotational Temperatures and Ortho-Para Ratios
A spatially resolved plerionic X-ray nebula around PSR B0540-69
本文报道了大麦云星云中一颗50毫秒脉冲星PSR B 0540 -69的高分辨率Chandra X射线观测。我们使用相位分辨成像来分解扩展的X射线发射，正如预期的同步加速器星云，从脉冲星的点状发射。脉冲X射线发射的图像显示了观测结果中定义明确的点扩散函数，而分辨出的星云具有与蟹状星云非常相似的形态和大小，包括PSR B 0540 -69中喷流特征的证据。斑驳的外壳，最有可能代表超新星爆炸波的膨胀，让人想起在无线电中看到的。根据形态、大小和能量，PSR B 0540 -69无疑是一个类似于蟹状星云的星系，但位于我们的邻近星系。
