A unified model for the maximum mass scales of molecular clouds, stellar clusters and high-redshift clumps
A unified model for the maximum mass scales of molecular clouds, stellar clusters and high-redshift clumps
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分子云、星团和高红移团块最大质量尺度的统一模型
DOI：
10.1093/mnras/stx790
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发表时间：
2017
影响因子：
4.8
通讯作者：
Kruijssen
中科院分区：
文献类型：
--
作者：
Reina-Campos;Kruijssen
我们提出了一个简单的，自洽的模型来预测作为银河系环境的函数的巨分子云（GMCs），星团和高红移团块的最大质量。最近的研究提出，这些最大质量是由剪切运动和离心力决定的，但我们表明，这一想法与在一个重要的局部宇宙环境范围内观察到的低质量不一致，例如低表面密度星系和星系外围。相反，我们认为来自年轻恒星的反馈可以在剪切限制区域的全球崩溃完成之前破坏云。我们开发了一个剪切反馈混合模型，依赖于三个可观察的量：气体表面密度，epicyclic频率和Toomre参数。该模型在四个星系环境中进行了测试：银河系，本星系群M31，旋涡星系M83和高红移星系zC406690。我们证明，我们的模型同时再现了所观察到的最大质量的GMC，团块和集群在这些环境中的每一个。我们发现M31和银河系中的云和星系团在半径分别超过8.4和4 kpc时受到反馈限制，而M83和zC 406690中的质量在所有半径处都受到剪切限制。在zC406690中，最大的星系团质量由于动力学摩擦而进一步下降。这些结果表明，最大质量的变化，从被剪切限制的反馈限制的星系变得不那么丰富的气体，并向低剪切演化。这就解释了为什么高红移团块的质量比本宇宙中的GMC更大。
We present a simple, self-consistent model to predict the maximum masses of giant molecular clouds (GMCs), stellar clusters and high-redshift clumps as a function of the galactic environment. Recent works have proposed that these maximum masses are set by shearing motions and centrifugal forces, but we show that this idea is inconsistent with the low masses observed across an important range of local-Universe environments, such as low-surface density galaxies and galaxy outskirts. Instead, we propose that feedback from young stars can disrupt clouds before the global collapse of the shear-limited area is completed. We develop a shear–feedback hybrid model that depends on three observable quantities: the gas surface density, the epicylic frequency and the Toomre parameter. The model is tested in four galactic environments: the Milky Way, the Local Group galaxy M31, the spiral galaxy M83 and the high-redshift galaxy zC406690. We demonstrate that our model simultaneously reproduces the observed maximum masses of GMCs, clumps and clusters in each of these environments. We find that clouds and clusters in M31 and in the Milky Way are feedback-limited beyond radii of 8.4 and 4 kpc, respectively, whereas the masses in M83 and zC406690 are shear-limited at all radii. In zC406690, the maximum cluster masses decrease further due to their inspiral by dynamical friction. These results illustrate that the maximum masses change from being shear-limited to being feedback-limited as galaxies become less gas rich and evolve towards low shear. This explains why high-redshift clumps are more massive than GMCs in the local Universe.
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DOI：
--
发表时间：
2016
期刊：
影响因子：
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作者：
J. Henshaw;S. Longmore;J. Kruijssen;J. Kruijssen
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DOI：
10.1088/0004-6256/145/5/137
发表时间：
2013-02
期刊：
The Astronomical Journal
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通讯作者：
I. Konstantopoulos;L. Smith;A. Adamo;E. Silva-Villa;J. Gallagher;N. Bastian;J. Ryon;M. Westmoquette;E. Zackrisson;S. Larsen;D. Weisz;J. C. C. A. A. Observatory-J.-C.-C.-A.-A.-Observatory-2248073539;The Pennsylvania State University;Space Telescope Science Institute;E. S. Agency;M. F. Astronomy;Universit'e Laval;U. Wisconsin--Madison-U.-Wisconsin--Madison-1387898181;Excellence Cluster Universe;Liverpool John Moore's University;E. Observatory;S. University;R. Nijmegen;U. Washington
影响因子：
4.8
作者：
J. Kruijssen;S. Longmore;B. Elmegreen;N. Murray;J. Bally;L. Testi;R. C. K. J. E. Garching;E. Garchi
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J. Kruijssen;S. Longmore;B. Elmegreen;N. Murray;J. Bally;L. Testi;R. C. K. J. E. Garching;E. Garchi
DOI：
10.1088/0004-637x/768/1/74
发表时间：
2012-11
期刊：
The Astrophysical Journal
影响因子：
--
作者：
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L. Tacconi;R. Neri;R. Genzel;F. Combes;A. Bolatto;M. Cooper;S. Wuyts;F. Bournaud;A. Burkert-
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DOI：
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发表时间：
2014
期刊：
影响因子：
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