The GALEX Arecibo SDSS Survey – IV. Baryonic mass–velocity–size relations of massive galaxies
The GALEX Arecibo SDSS Survey – IV. Baryonic mass–velocity–size relations of massive galaxies
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DOI：
10.1111/j.1365-2966.2011.20012.x
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发表时间：
2011-10
影响因子：
4.8
通讯作者：
B. Catinella;G. Kauffmann;D. Schiminovich;J. Lemonias;C. Scannapieco;Jing Wang;S. Fabello;C. Hummels;S. Moran;R. Wu;A. Cooper;R. Giovanelli;M. Haynes;T. Heckman;A. Saintonge
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作者：
B. Catinella;G. Kauffmann;D. Schiminovich;J. Lemonias;C. Scannapieco;Jing Wang;S. Fabello;C. Hummels;S. Moran;R. Wu;A. Cooper;R. Giovanelli;M. Haynes;T. Heckman;A. Saintonge
作为正在进行的GALEX Arecibo SDSS调查的一部分，我们提出了一个均匀的和有代表性的样本的500个大质量星系的动力学标度关系，这些星系仅根据恒星质量（> 10 10 M）和红移（0.025 < z < 0.05）进行选择。我们比较重子Tully-Fisher（BTF）和Faber-Jackson（BFJ）的关系为这个样本，并研究星系如何分散周围的最佳拟合修剪的磁盘为主和膨胀为主的系统的子集。的BFJ关系是显着分散比BTF的关系时，适用于其最大的样本（BTF，只有星系与喜检测），并没有受到困扰的BTF的倾斜问题。以盘为主的富含气体的星系系统性地偏离了由球体定义的BFJ关系。我们表明，通过应用一个简单的校正，仅取决于星系的浓度指数的恒星速度色散，我们能够使磁盘和球状体到相同的动力学关系-换句话说，我们得到一个广义的BFJ关系，适用于我们的样本中的所有星系，无论形态，倾斜或气体含量，并具有小于0.1德克斯的散射。我们比较了这项工作中使用的三个动力学指标的速度-大小关系，即，旋转速度，观测和浓度校正的恒星色散。我们发现，磁盘和球状体的恒星色散的大小关系的偏移，而偏移被删除时，校正色散代替。广义的BFJ关系代表了全球暗物质和星系重子含量之间的基本相关性，这是服从所有（大质量）系统，无论形态。
We present dynamical scaling relations for a homogeneous and representative sample of �500 massive galaxies, selected only by stellar mass (> 10 10 M⊙) and redshift (0.025 < z < 0.05) as part of the ongoing GALEX Arecibo SDSS Survey. We compare baryonic Tully-Fisher (BTF) and Faber-Jackson (BFJ) relations for this sample, and investigate how galaxies scatter around the best fits obtained for pruned subsets of disk-dominated and bulge-dominated systems. The BFJ relation is significantly less scattered than the BTF when the relations are applied to their maximum samples (for the BTF, only galaxies with Hi detections), and is not affected by the inclination problems that plague the BTF. Disk-dominated, gas-rich galaxies systematically deviate from the BFJ relation defined by the spheroids. We demonstrate that by applying a simple correction to the stellar velocity dispersions that depends only on the concentration index of the galaxy, we are able to bring disks and spheroids onto the same dynamical relation — in other words, we obtain a generalized BFJ relation that holds for all the galaxies in our sample, regardless of morphology, inclination or gas content, and has a scatter smaller than 0.1 dex. We compare the velocity-size relation for the three dynamical indicators used in this work, i.e., rotational velocity, observed and concentration-corrected stellar dispersion. We find that disks and spheroids are offset in the stellar dispersion-size relation, and that the offset is removed when corrected dispersions are used instead. The generalized BFJ relation represents a fundamental correlation between the global dark matter and baryonic content of galaxies, which is obeyed by all (massive) systems regardless of morphology.