A VIRTUAL SKY WITH EXTRAGALACTIC H i AND CO LINES FOR THE SQUARE KILOMETRE ARRAY AND THE ATACAMA LARGE MILLIMETER/SUBMILLIMETER ARRAY
A VIRTUAL SKY WITH EXTRAGALACTIC H i AND CO LINES FOR THE SQUARE KILOMETRE ARRAY AND THE ATACAMA LARGE MILLIMETER/SUBMILLIMETER ARRAY
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DOI：
10.1088/0004-637x/703/2/1890
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发表时间：
2009-10
期刊：
影响因子：
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通讯作者：
D. Obreschkow;H. Klöckner;I. Heywood;F. Levrier;Steve Rawlings
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作者：
D. Obreschkow;H. Klöckner;I. Heywood;F. Levrier;Steve Rawlings
我们给出了银河系以外星系中原子H -发射线和分子气体的前10个12C16O旋转发射线的天空模拟。模拟的天空场运动直径为500 h−1 Mpc；因此，实际的视场取决于（用户定义的）最大红移zmax；例如，当zmax = 10时，视场产生~ 4 × 4 deg2。对于所有星系，我们估计了H - i和co -发射线的线通量、线轮廓和角大小。对于冷氢质量超过108 M☉的星系样本是完整的。这个天空模拟建立在Λ冷暗物质（ΛCDM）宇宙学中星系宇宙演化的半解析模型之上。进化的CDM分布采用了Millennium Simulation，这是一个边长为500 h−1 Mpc的立方盒中的n体CDM模拟。这个边长限制了我们的天空模拟的相干尺度：它足够长，可以提取星系功率谱中的重子声学振荡，但第一个声学峰值的位置和振幅将不完全确定。这种天空模拟对未来望远镜的设计和操作有切实的帮助，比如平方公里阵列、大型毫米望远镜和阿塔卡马大型毫米/亚毫米阵列。本文提出的结果仅限于模拟天空的图形表示和对H i和CO的峰值通量密度限制和总通量限制调查的基本dN/dz分析。一个关键的预测是，在红移z > 2时，H i将比无演化模型预测的更难探测到。未来对这一预测的验证或证伪将使我们能够对半解析模型进行限定。
We present a sky simulation of the atomic H i-emission line and the first 10 12C16O rotational emission lines of molecular gas in galaxies beyond the Milky Way. The simulated sky field has a comoving diameter of 500 h−1 Mpc; hence, the actual field of view depends on the (user-defined) maximal redshift zmax; e.g., for zmax = 10, the field of view yields ∼4 × 4 deg2. For all galaxies, we estimate the line fluxes, line profiles, and angular sizes of the H i and CO-emission lines. The galaxy sample is complete for galaxies with cold hydrogen masses above 108 M☉. This sky simulation builds on a semi-analytic model of the cosmic evolution of galaxies in a Λ cold dark matter (ΛCDM) cosmology. The evolving CDM distribution was adopted from the Millennium Simulation, an N-body CDM simulation in a cubic box with a side length of 500 h−1 Mpc. This side length limits the coherence scale of our sky simulation: it is long enough to allow the extraction of the baryon acoustic oscillations in the galaxy power spectrum, yet the position and amplitude of the first acoustic peak will be imperfectly defined. This sky simulation is a tangible aid to the design and operation of future telescopes, such as the Square Kilometre Array, Large Millimeter Telescope, and Atacama Large Millimeter/Submillimeter Array. The results presented in this paper have been restricted to a graphical representation of the simulated sky and fundamental dN/dz analyses for peak flux density limited and total flux limited surveys of H i and CO. A key prediction is that H i will be harder to detect at redshifts z ≳ 2 than predicted by a no-evolution model. The future verification or falsification of this prediction will allow us to qualify the semi-analytic models.