SDF和SXDF星系的光度H α和[O II ]光度函数：对未来重子振荡巡天的意义
Photometric H alpha and [O II] Luminosity Function of SDF and SXDF Galaxies: Implications for Future Baryon Oscillation Surveys
摘要：
在宽视场巡天中利用光度信息有效地选择z > 1的发射线星系是未来利用重子声学振荡（BAO）特征进行光谱巡天以限制暗能量的关键之一。在这里，我们估计的H α和[O II]线光度函数的星系在z = 0.5-1.7使用一种新的方法，多波长成像数据被用来共同估计光度红移和恒星形成率。这些高红移线光度的测光估算使用了斯巴鲁深场和斯巴鲁XMM-牛顿深场的大型数据集（覆盖\sim 1 deg^2），并使用当地斯隆数字巡天星系的光谱数据进行了校准。导出的光度函数（特别是H α）与过去基于光谱或窄带滤波器调查的估计值合理一致。这个数据集是有用的检查测光选择的目标星系的BAO调查，因为大的宇宙学体积覆盖和大量的星系详细的光度信息。我们使用的样品来获得的光度和物理性质的发射线星系，以协助规划未来的光谱BAO调查。我们还展示了一些光度选择程序，可以有效地选择这些发射线星系的例子。
英文摘要：
Efficient selection of emission line galaxies at z > 1 by photometric information in wide field surveys is one of the keys for future spectroscopic surveys to constrain dark energy using the baryon acoustic oscillation (BAO) signature. Here we estimate the H alpha and [O II] line luminosity functions of galaxies at z = 0.5-1.7 using a novel approach where multi-wavelength imaging data is used to jointly estimate both photometric redshifts and star-formation rates. These photometric estimates of line luminosities at high-redshift use the large data sets of the Subaru Deep Field and Subaru XMM-Newton Deep Field (covering \sim 1 deg^2) and are calibrated with the spectroscopic data of the local Sloan Digital Sky Survey galaxies. The derived luminosity functions (especially H alpha) are in reasonable agreement with the past estimates based on spectroscopic or narrow-band-filter surveys. This dataset is useful for examining the photometric selection of target galaxies for BAO surveys because of the large cosmological volume covered and the large number of galaxies with detailed photometric information. We use the sample to derive the photometric and physical properties of emission line galaxies to assist planning for future spectroscopic BAO surveys. We also show some examples of photometric selection procedures which can efficiently select these emission line galaxies.
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