Designing Future Dark Energy Space Missions : I . Building Re alistic Galaxy SpectroPhotometric Catalogs and their first applic ations
Designing Future Dark Energy Space Missions : I . Building Re alistic Galaxy SpectroPhotometric Catalogs and their first applic ations
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设计未来的暗能量太空任务：I．
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发表时间：
2021
期刊：
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通讯作者：
N. Scoville
中科院分区：
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作者：
S. Jouvel;J. Kneib;O. Ilbert;G. Bernstein;S. Arnouts;T. Dahlén;A. Ealet;B. Milliard;H. Aussel;P.;Capak;A. Koekemoer;V. Brun;H. McCracken;M. Salvato;N. Scoville
上下文。未来的暗能量太空任务，如JDEM和EUCLID，正在设计用于调查星系人口，以追踪宇宙的几何形状和结构的增长，这两者都依赖于宇宙学模型。为了达到高精度宇宙学的目标，他们需要基于真实的模拟星系分布表来评估不同仪器设计的能力。目标。本文的目的是基于我们从目前的深度调查中获得的星系群知识，构建现实和灵活的星系表。我们探索了两类模拟数据日志：(i)基于我们拟合观测的光度函数（GOODS， UDF，COSMOS，VVDS） （ii）基于观测到的COSMOS星系分布。方法。COSMOS模拟星表得益于数据丰富的COSMOS巡天的所有特性，以及基于30波段光度法的高精度光度红移分布。然而，这个目录受到宇宙巡天深度的限制。因此，我们也使用Le Pharesoftware评估了由光度函数生成的模拟星系目录。对于这两个星表，我们制作了不同波段的模拟数字计数、颜色图和红移分布，以便与实际观测数据进行验证。结果。利用这些模拟星表，我们得出了一些基本的要求，以帮助设计未来的暗能量任务，根据弱透镜分析可获得的星系数量，以及PSF大小和调查深度的函数。我们还计算了未来光谱重移调查的光谱成功率(i)旨在测量广域光谱红移调查中的BAO，以及（ii）光度红移校准调查，这需要以很高的精度实现弱透镜层析成像。特别是，我们证明了对于光度红移校准，仅使用近红外（1-1.7μm）光谱，我们无法实现完整的光谱调查，直到光度调查的极限（I < 25.5）。将光谱调查的波长覆盖范围扩大到0.6-1.7μm，然后将非常安全的光谱红移的比例提高到近80%的星系，从而使非常精确的光度红移校准成为可能。结论。我们已经制作了两个真实的模拟星系目录，可以用来确定未来暗能量任务的最佳调查策略，在光度红移精度和光谱红移调查产量方面。这些目录可以在以下网址公开访问：// lamwww .oamp.fr /cosmowiki /RealisticSpectroPhotCat，也可以向本文的第一作者索取。
Context. Future dark energy space missions such as JDEM and EUCLID are being designed to survey the galaxy population to trace the geometry of the universe and the growth of structure, whi ch both depend on the cosmological model. To reach the goal of high precision cosmology they need to evaluate the capabilities of different instrument designs based on realistic mock catalogs o f the galaxy distribution. Aims. The aim of this paper is to construct realistic and flexible mo ck catalogs based on our knowledge of galaxy populations fro m current deep surveys. We explore two categories of mock cata logs : (i) based on luminosity functions that we fit to observa tions (GOODS, UDF,COSMOS,VVDS) (ii) based on the observed COSMOS galaxy distribution. Methods. The COSMOS mock catalog benefits from all the properties of th e data-rich COSMOS survey and the highly accurate photometric redshift distribution based on 30-band photom etry. Nevertheless this catalog is limited by the depth of th e COSMOS survey. Thus, we also evaluate a mock galaxy catalog generat ed from luminosity functions using the Le Pharesoftware. For these two catalogs, we have produced simulated number counts in sever al bands, color diagrams and redshift distributions for val idation against real observational data. Results. Using these mock catalogs we derive some basic requirements to help design future Dark Energy missions in terms of the number of galaxies available for the weak-lensing analysis a a function of the PSF size and depth of the survey. We also co mpute the spectroscopic success rate for future spectroscopic re dshift surveys(i) aiming at measuring BAO in the case of the wide field spectroscopic redshift survey, and (ii) for the photometric redshift calibration survey which is re quired to achieve weak lensing tomography with great accuracy. In particular, we demonstr ate that for the photometric redshift calibration, using on ly NIR (1-1.7μm) spectroscopy, we cannot achieve a complete spectroscopic s urvey down to the limit of the photometric survey ( I < 25.5). Extending the wavelength coverage of the spectroscopic survey to cove r 0.6-1.7μm will then improve the fraction of very secure spectroscopi redshifts to nearly 80% of the galaxies, making possible a ve ry accurate photometric redshift calibration. Conclusions. We have produced two realistic mock galaxy catalogs that can be used in determining the best survey strategy for future dark-energy missions in terms of photometric redshi ft accuracy and spectroscopic redshift surveys yield. These catalogues are publicly accessible at http: //lamwws.oamp.fr /cosmowiki /RealisticSpectroPhotCat, or by request to the first author o f this paper.