The Atlas3D project - XV. Benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, Fundamental Plane and Mass Plane
Michele Cappellari, Nicholas Scott, Katherine Alatalo, Leo Blitz, Maxime Bois, Frederic Bournaud, M. Bureau, Alison F. Crocker, Roger L. Davies, Timothy A. Davi… 展开作者
Michele Cappellari, Nicholas Scott, Katherine Alatalo, Leo Blitz, Maxime Bois, Frederic Bournaud, M. Bureau, Alison F. Crocker, Roger L. Davies, Timothy A. Davis, P. T. de Zeeuw, Pierre-Alain Duc, Eric Emsellem, Sadegh Khochfar, Davor Krajnovic, Harald Kuntschner, Richard M. McDermid, Raffaella Morganti, Thorsten Naab, Tom Oosterloo, Marc Sarzi, Paolo Serra, Anne-Marie Weijmans, Lisa M. Young
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35 pages, 18 figures, LaTeX. Accepted for publication in MNRAS. Includes a new data table and figures of all dynamical models. More information about our Atlas3D project is available at http://purl.org/atlas3d
We study the volume-limited and nearly mass selected (stellar mass M>6*10^9 Msun) Atlas3D sample of 260 early-type galaxies. We construct detailed axisymmetric dynamical models (JAM), which allow for orbital anisotropy, include a dark matter halo, and reproduce in detail both the galaxy images and the high-quality integral-field stellar kinematics. We derive accurate total M/L and dark matter fractions f_DM, within a sphere of radius r=Re. We also measure the stellar M/L and derive a median dark matter fraction f_DM=13%. We find that the thin two-dimensional subset spanned by galaxies in the (M_JAM,sigma_e,R_e) coordinates system, which we call the Mass Plane (MP) has an observed rms scatter of 19% and an intrinsic one of 11%. The MP satisfies the scalar virial relation M_JAM sigma_e^2 R_e within our tight errors. However, the details of how both Re and sigma_e are determined are critical in defining the precise deviation from the virial exponents. We revisit the (M/L)-sigma_e relation, which describes most of the deviations between the MP and the FP. The best-fitting relation is (M/L) sigma_e^0.72 (r-band). It provides an upper limit to any systematic increase of the IMF mass normalization with sigma_e. We study of the link between sigma_e and the galaxies circular velocity V_circ within 1Re (where stars dominate) and find the relation max(V_circ)~1.76*sigma_e, which has an observed scatter of 7%. The accurate parameters described in this paper are used in the companion Paper XX of this series to explore the variation of global galaxy properties, including the IMF, on the projections of the MP. [Abridged]
Shape Evolution of Massive Early-Type Galaxies: Confirmation of Increased Disk Prevalence at z>1
利用高分辨率K波段VLT/HAWK-I 0.25平方度成像研究了大质量早型星系自z1以来的结构演化。质量选定的样本，完成下降到日志（M/M_太阳）~10.7，使“典型的”L* 星系包括在所有的红移，从预先存在的光度红移调查。然后，我们将样本分成不同的红移切片，并根据其特定的恒星形成率将其分类为晚型或早型星系。在红移范围0.6<z 1的约400个早型星系的轴比测量值<1.8 are accurate to 0.1 or better. The projected axis-ratio distributions are then compared with lower redshift samples. We find strong evidence for evolution of the population properties: early-type galaxies at z>平均比z<1时平坦，并且在固定质量下的中值投影轴比随红移而减小。然而，我们也发现，在z<~2的所有历元中，质量最大的早型星系（log（M/M_sun）>11.3）是最圆的，其中明显缺乏投影平坦的星系。合并是一个合理的机制，可以解释这两个结果：在所有的时代，合并是需要的早期类型的星系增长超过log（M/M_sun）~11.3，和所有早期类型随着时间的推移逐渐和部分松动的盘状特征。
Reconstructing galaxy fundamental distributions and scaling relations from photometric redshift surveys. Applications to the SDSS early-type sample
与光度红移而不是光谱红移相关的噪声距离估计导致对光度的错误估计，并产生相关的对大小的错误估计。我们考虑一个来自SDSS DR 6的早期星系样本，它的光谱和光度信息都是可用的，并应用V_max方法的推广来校正这些偏差。我们表明，我们的技术恢复真正的红移，幅度和大小分布，以及真正的大小-光度关系。我们发现，仅使用10%的光谱信息随机分布在我们的目录是足够的重建是准确的约3%，当光度红移误差为dz = 0.038。然后，我们解决的问题，我们的方法扩展到深红移目录，只有光度信息。除了这里概述的具体应用外，当至少涉及一个距离依赖量时，我们的技术会影响更广泛的研究。这对下一代的调查特别重要，其中一些调查只有光度信息。
A Universal CMB $B$-Mode Spectrum from Early Causal Tensor Sources
Seoul National University（首尔大学）；Stanford University（斯坦福大学）；Fermi National Accelerator Laboratory（费米国家加速器实验室）；University of Chicago（芝加哥大学）；University of Notre Dame（圣母大学）
