Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph
Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph
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DOI：
10.1093/pasj/pst019
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发表时间：
2012-06
影响因子：
2.3
通讯作者：
M. Takada;R. Ellis;M. Chiba;J. Greene;H. Aihara;N. Arimoto;K. Bundy;J. Cohen;O. Dor'e
中科院分区：
文献类型：
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作者：
M. Takada;R. Ellis;M. Chiba;J. Greene;H. Aihara;N. Arimoto;K. Bundy;J. Cohen;O. Dor'e
斯巴鲁Prime Focus摄谱仪（PFS）是一款大规模多路复用光纤馈电光学和近红外三臂摄谱仪（N_fiber=2400，380<lambda<1260 nm，1.3度直径FoV），为测量天文学提供了独特的机会。在这里，我们总结了科学的情况下可行的调查斯巴鲁300夜。我们描述了通过测量在红移0.8<z<2.4范围内共动体积为9.3（Gpc/h）^3的发射线星系来限制暗能量性质的计划。在6个红移仓中的每一个中，宇宙学距离将通过BAO测量到3%的精度，而红移空间扭曲将用于限制结构增长到6%的精度。在GA计划中，银河系和M31中恒星的径向速度和化学丰度将用于推断螺旋星系过去的组装历史及其暗物质晕的结构。将获得银河系厚盘、晕和潮汐流中10^6颗恒星的数据，这些恒星的亮度低至V~22，包括V < 20的恒星，以补充盖亚使命的目标。将在红臂采用R = 5000的中分辨率模式，将能够测量银河系恒星的多种α元素丰度和更精确的速度，阐明银河系及其矮球状星系的每个主要恒星组成部分的详细化学动力学结构和演变。对于河外计划，我们的模拟表明，宽的波长范围将是强大的探测星系人口和它的集群在一个广泛的红移范围。我们建议对1<z<2的星系和16 deg^2到J~23.4的活动星系核进行颜色选择巡天，得到一个在z~2处恒星质量大于~10^{10}Ms的星系样本。对高红移LBG和LAE的两层调查将量化接近再电离时期的早期系统的性质。
The Subaru Prime Focus Spectrograph (PFS) is a massively-multiplexed fiber-fed optical and near-infrared 3-arm spectrograph (N_fiber=2400, 380<lambda<1260nm, 1.3 degree diameter FoV), offering unique opportunities in survey astronomy. Here we summarize the science case feasible for a survey of Subaru 300 nights. We describe plans to constrain the nature of dark energy via a survey of emission line galaxies spanning a comoving volume of 9.3 (Gpc/h)^3 in the redshift range 0.8<z<2.4. In each of 6 redshift bins, the cosmological distances will be measured to 3% precision via BAO, and redshift-space distortions will be used to constrain structure growth to 6% precision. In the GA program, radial velocities and chemical abundances of stars in the Milky Way and M31 will be used to infer the past assembly histories of spiral galaxies and the structure of their dark matter halos. Data will be secured for 10^6 stars in the Galactic thick-disk, halo and tidal streams as faint as V~22, including stars with V < 20 to complement the goals of the Gaia mission. A medium-resolution mode with R = 5000 to be implemented in the red arm will allow the measurement of multiple alpha-element abundances and more precise velocities for Galactic stars, elucidating the detailed chemo-dynamical structure and evolution of each of the main stellar components of the Milky Way Galaxy and of its dwarf spheroidal galaxies. For the extragalactic program, our simulations suggest the wide avelength range will be powerful in probing the galaxy population and its clustering over a wide redshift range. We propose to conduct a color-selected survey of 1<z<2 galaxies and AGN over 16 deg^2 to J~23.4, yielding a fair sample of galaxies with stellar masses above ~10^{10}Ms at z~2. A two-tiered survey of higher redshift LBGs and LAEs will quantify the properties of early systems close to the reionization epoch.