A Break in Spiral Galaxy Scaling Relations at the Upper Limit of Galaxy Mass
A Break in Spiral Galaxy Scaling Relations at the Upper Limit of Galaxy Mass
复制标题
星系质量上限处螺旋星系标度关系的突破
DOI：
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发表时间：
2019
影响因子：
4.9
通讯作者：
J. Mazzarella
中科院分区：
文献类型：
--
作者：
P. Ogle;T. Jarrett;L. Lanz;M. Cluver;K. Alatalo;P. Appleton;J. Mazzarella
超级螺旋星系是宇宙中最大的恒星形成盘星系。我们用南非大型望远镜（SALT）测量了23个大质量螺旋的旋转曲线，发现了一个很宽的快速旋转速度范围（240-570 km s−1），表明封闭的动力学质量为（0.6−4）× 1012 M。质量为log M星/ M> 11.5的超级螺旋星系打破了为低质量星系建立的重子塔利-费舍尔关系（BTFR）。BTFR的幂律指数在转速超过340 km s−1时从3.75 ± 0.11变为0.25 ± 0.41。超级螺线也有很高的比角动量，打破了Fall关系。这些结果表明，超级螺旋星系的暗物质晕的质量不足，其质量仅限于log M星/ M < 11.8的恒星。大多数巨大的椭圆星系也遵守这个基本的限制，这对应于一个临界的暗晕质量log M halo / M 12.7。一旦一个晕达到这个质量，它的气体就不能在动力学时间内冷却和坍缩。超级螺旋体在质量为log M halo / M 13.6的晕中幸存下来，继续从它们在晕达到临界质量之前捕获的冷重子中形成恒星。BTFR中观察到的高质量断裂与修正牛顿动力学理论不一致。
Super spirals are the most massive star-forming disk galaxies in the universe. We measured rotation curves for 23 massive spirals with the Southern African Large Telescope (SALT) and found a wide range of fast rotation speeds (240–570 km s−1), indicating enclosed dynamical masses of (0.6−4) × 1012M⊙. Super spirals with mass in stars log M stars / M ⊙ > 11.5 break from the baryonic Tully–Fisher relation (BTFR) established for lower-mass galaxies. The BTFR power-law index breaks from 3.75 ± 0.11 to 0.25 ± 0.41 above a rotation speed of ∼340 km s−1. Super spirals also have very high specific angular momenta that break from the Fall relation. These results indicate that super spirals are undermassive for their dark matter halos, limited to a mass in stars of log M stars / M ⊙ < 11.8 . Most giant elliptical galaxies also obey this fundamental limit, which corresponds to a critical dark halo mass of log M halo / M ⊙ ≃ 12.7 . Once a halo reaches this mass, its gas can no longer cool and collapse in a dynamical time. Super spirals survive today in halos as massive as log M halo / M ⊙ ≃ 13.6 , continuing to form stars from the cold baryons they captured before their halos reached critical mass. The observed high-mass break in the BTFR is inconsistent with the Modified Newtonian Dynamics theory.
影响因子：
4.8
作者：
Kung-Yi Su;P. Hopkins;C. Hayward;Xiangcheng Ma;C. Faucher-Giguère;D. Kerevs;Matthew E. Orr;V. Robles
通讯作者：
Kung-Yi Su;P. Hopkins;C. Hayward;Xiangcheng Ma;C. Faucher-Giguère;D. Kerevs;Matthew E. Orr;V. Robles
DOI：
10.1088/0004-637x/782/2/90
发表时间：
2014-01
期刊：
The Astrophysical Journal
影响因子：
--
作者：
M. Cluver;M. Cluver;T. Jarrett;A. Hopkins;S. Driver;S. Driver;J. Liske;M. Gunawardhana;M. Gunawardhana;M. Gunawardhana;E. Taylor;A. Robotham;M. Alpaslan;I. Baldry;Michael J. I. Brown;J. Peacock;C. Popescu;R. Tuffs;A. Bauer;J. Bland-Hawthorn;M. Colless;B. Holwerda;M. Lara-López;K. Leschinski;Á. López-Sánchez;Á. López-Sánchez;P. Norberg;M. Owers;Lingyu Wang;S. Wilkins
通讯作者：
M. Cluver;M. Cluver;T. Jarrett;A. Hopkins;S. Driver;S. Driver;J. Liske;M. Gunawardhana;M. Gunawardhana;M. Gunawardhana;E. Taylor;A. Robotham;M. Alpaslan;I. Baldry;Michael J. I. Brown;J. Peacock;C. Popescu;R. Tuffs;A. Bauer;J. Bland-Hawthorn;M. Colless;B. Holwerda;M. Lara-López;K. Leschinski;Á. López-Sánchez;Á. López-Sánchez;P. Norberg;M. Owers;Lingyu Wang;S. Wilkins
影响因子：
8.7
作者：
Komatsu, E.;Smith, K. M.;Wright, E. L.
通讯作者：
Wright, E. L.