SImulator of GAlaxy Millimetre/submillimetre Emission (sígame): CO emission from massive z = 2 main-sequence galaxies
SImulator of GAlaxy Millimetre/submillimetre Emission (sígame): CO emission from massive z = 2 main-sequence galaxies
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GAlaxy 毫米/亚毫米发射模拟器 (sígame)：来自大质量 z = 2 个主序星系的 CO 发射
DOI：
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发表时间：
2015
期刊：
影响因子：
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通讯作者：
A. Zirm
中科院分区：
文献类型：
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作者：
K. Olsen;T. Greve;C. Brinch;J. Sommer;J. Rasmussen;S. Toft;A. Zirm
我们推出了 SIGAME（GAlaxy 毫米/亚毫米发射模拟器），这是一种新的数字代码，旨在模拟星系的 12CO 旋转线发射光谱。使用子网格物理配方对平滑粒子流体动力学 (SPH) 模拟的输出进行后处理，分子气相从热且部分电离的 SPH 气体中凝结出来。气体受到远紫外辐射场和宇宙射线电离率的影响，这些辐射场和宇宙射线电离率与当地恒星形成率体积密度成比例。 CO 线的水平布居和辐射传输通过 3-D 辐射传输代码 LIME 求解。我们已将 SIGAME 应用于 z=2 处的三个盘状星系的宇宙学 SPH 模拟，其中恒星质量在 ~(0.5-2)x10^11 Msun 范围内，恒星形成率 ~40-140 Msun/yr。全球 CO 光度和线比与 z~2 至 J=3-2（包括 J=3-2）处盘状星系的观测结果一致，但低于现有的少数 J=5-4 观测结果。我们星系中央 5 kpc 区域的 CO 3-2/1-0 和 7-6/1-0 亮温比分别为 ~0.55-0.65 和 ~0.02-0.08，而在盘中更远的地方，比率下降到更静态的值 ~0.5 和 =3，CO 到 H2 转换因子 [~=3.6 Msun*pc^2/(K km/s)]。
We present SIGAME (SImulator of GAlaxy Millimetre/submillimetre Emission), a new numerical code designed to simulate the 12CO rotational line emission spectrum of galaxies. Using sub-grid physics recipes to post-process the outputs of smoothed particle hydrodynamics (SPH) simulations, a molecular gas phase is condensed out of the hot and partly ionized SPH gas. The gas is subjected to far-UV radiation fields and cosmic ray ionization rates which are set to scale with the local star formation rate volume density. Level populations and radiative transport of the CO lines are solved with the 3-D radiative transfer code LIME. We have applied SIGAME to cosmological SPH simulations of three disc galaxies at z=2 with stellar masses in the range ~(0.5-2)x10^11 Msun and star formation rates ~40-140 Msun/yr. Global CO luminosities and line ratios are in agreement with observations of disc galaxies at z~2 up to and including J=3-2 but falling short of the few existing J=5-4 observations. The central 5 kpc regions of our galaxies have CO 3-2/1-0 and 7-6/1-0 brightness temperature ratios of ~0.55-0.65 and ~0.02-0.08, respectively, while further out in the disc the ratios drop to more quiescent values of ~0.5 and =3 and CO-to-H2 conversion factors [~=3.6 Msun*pc^2/(K km/s)].
DOI：
10.1088/0004-637x/768/1/74
发表时间：
2012-11
期刊：
The Astrophysical Journal
影响因子：
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作者：
L. Tacconi;R. Neri;R. Genzel;F. Combes;A. Bolatto;M. Cooper;S. Wuyts;F. Bournaud;A. Burkert-
通讯作者：
L. Tacconi;R. Neri;R. Genzel;F. Combes;A. Bolatto;M. Cooper;S. Wuyts;F. Bournaud;A. Burkert-