THE SAMI GALAXY SURVEY: TOWARD A UNIFIED DYNAMICAL SCALING RELATION FOR GALAXIES OF ALL TYPES-猫眼课题宝

DOI：

10.1088/2041-8205/795/2/l37

发表时间：

2014-10

期刊：

The Astrophysical Journal Letters

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

L. Cortese;L. Fogarty;I. Ho;K. Bekki;J. Bland-Hawthorn;M. Colless;W. Couch;S. Croom;K. Glazebrook;J. Mould;Nicholas Scott;R. Sharp;C. Tonini;J. Allen;J. Bloom;J. Bryant;J. Bryant;M. Cluver;R. Davies;M. Drinkwater;M. Goodwin;A. Green;L. Kewley;I. S. Kostantopoulos;J. Lawrence;S. Mahajan;S. Mahajan;A. Medling;M. Owers;S. Richards;S. Richards;S. Sweet;O. I. Wong

我们利用悉尼-AAO多目标积分场星系调查的第一批数据，研究了附近星系的综合样本中气体和恒星的运动学与恒星质量之间的关系。我们发现，样本中的所有235个天体，无论它们的形态如何，都建立在一种紧密的关系上，将恒星质量(M*)与由S0.5参数量化的内部速度联系在一起，S0.5参数结合了色散(σ)和自转速度(VROT)对星系动力学支持的贡献()。我们的结果与用于估算σ和VROT的重子分量无关，因为恒星和气体的S0.5非常一致。与规范的M*对VROT和M*对σ关系相比，这是一个显著的改进。不仅不需要样本修剪，而且可以同时使用恒星运动学和气体运动学，因为一旦VROT和σ结合起来，就考虑了不对称漂移的影响。我们的发现说明了气体和恒星的色散和自转速度的组合如何为我们提供了一个对至少在恒星质量范围8.5&lt；log(M*/M☉)&lt；11范围内所有形态的星系有效的单一动力学标度关系。这种关系似乎更一般，至少和任何其他动力学标度关系一样紧密，这是研究星系运动学和重子含量之间联系的独特工具，与理论模型的比较没有那么有偏见。

We take advantage of the first data from the Sydney-AAO Multi-object Integral field Galaxy Survey to investigate the relation between the kinematics of gas and stars, and stellar mass in a comprehensive sample of nearby galaxies. We find that all 235 objects in our sample, regardless of their morphology, lie on a tight relation linking stellar mass (M*) to internal velocity quantified by the S0.5 parameter, which combines the contribution of both dispersion (σ) and rotational velocity (Vrot) to the dynamical support of a galaxy (). Our results are independent of the baryonic component from which σ and Vrot are estimated, as the S0.5 of stars and gas agree remarkably well. This represents a significant improvement compared to the canonical M* versus Vrot and M* versus σ relations. Not only is no sample pruning necessary, but also stellar and gas kinematics can be used simultaneously, as the effect of asymmetric drift is taken into account once Vrot and σ are combined. Our findings illustrate how the combination of dispersion and rotational velocities for both gas and stars can provide us with a single dynamical scaling relation valid for galaxies of all morphologies across at least the stellar mass range 8.5 <log (M*/M☉) < 11. Such relation appears to be more general and at least as tight as any other dynamical scaling relation, representing a unique tool for investigating the link between galaxy kinematics and baryonic content, and a less biased comparison with theoretical models.

THE SAMI GALAXY SURVEY: TOWARD A UNIFIED DYNAMICAL SCALING RELATION FOR GALAXIES OF ALL TYPES

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