Photometric H alpha and [O II] Luminosity Function of SDF and SXDF Galaxies: Implications for Future Baryon Oscillation Surveys
Photometric H alpha and [O II] Luminosity Function of SDF and SXDF Galaxies: Implications for Future Baryon Oscillation Surveys
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2009-02
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通讯作者：
Masanao Sumiyoshi;T. Totani;Shunsuke Oshige;K. Glazebrook;M. Akiyama;T. Morokuma;K. Motohara;K. Shimasaku;M. Hayashi;Makiko Yoshida;N. Kashikawa;T. Kodama
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作者：
Masanao Sumiyoshi;T. Totani;Shunsuke Oshige;K. Glazebrook;M. Akiyama;T. Morokuma;K. Motohara;K. Shimasaku;M. Hayashi;Makiko Yoshida;N. Kashikawa;T. Kodama
利用广域观测中的光度信息有效地选择z>；1处的发射线星系，是未来利用重子声振荡(BaO)信号限制暗能量的光谱探测的关键之一。在这里，我们使用一种新的方法来估计z=0.5-1.7的星系的Hα和[O II]线光度函数，其中多波长成像数据被用来联合估计光度红移和恒星形成速率。这些高红移线亮度的光度估计使用了斯巴鲁深场和斯巴鲁XMM-牛顿深场(覆盖1°2)的大型数据集，并用当地斯隆数字巡天星系的光谱数据进行了校准。得到的光度函数(尤其是Hα)与过去基于光谱或窄带滤光片测量的估计值符合得很好。由于覆盖的宇宙体积很大，而且有大量具有详细光度学信息的星系，这一数据集对于检验BAO调查的目标星系的光度学选择是有用的。我们使用这个样本来得出发射线星系的光度学和物理性质，以帮助规划未来的BAO光谱调查。我们还给出了一些光度选择程序的例子，这些程序可以有效地选择这些发射线星系。
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.