We examine the impact of fiber assignment on clustering measurements from fiber-fed spectroscopic galaxy surveys. We identify new effects which were absent in previous, relatively shallow galaxy surveys such as Baryon Oscillation Spectroscopic Survey . Specifically, we consider deep surveys covering a wide redshift range from z=0.6 to z=2.4, as in the Subaru Prime Focus Spectrograph survey. Such surveys will have more target galaxies than we can place fibers on. This leads to two effects. First, it eliminates fluctuations with wavelengths longer than the size of the field of view, as the number of observed galaxies per field is nearly fixed to the number of available fibers. We find that we can recover the long-wavelength fluctuation by weighting galaxies in each field by the number of target galaxies. Second, it makes the preferential selection of galaxies in under-dense regions. We mitigate this effect by weighting galaxies using the so-called individual inverse probability. Correcting these two effects, we recover the underlying correlation function at better than 1 percent accuracy on scales greater than 10 Mpc/h.

中文翻译：

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减轻纤维分配对深星系红移测量聚类测量的影响

我们研究了光纤分配对光纤馈送光谱星系调查的聚类测量的影响。我们发现了以前相对较浅的星系调查（例如重子振荡光谱调查）中不存在的新效应。具体来说，我们考虑涵盖从 z=0.6 到 z=2.4 的广泛红移范围的深度勘测，如斯巴鲁 Prime Focus 光谱仪勘测。这样的调查将拥有比我们可以放置光纤更多的目标星系。这会导致两个影响。首先，它消除了波长长于视场大小的波动，因为每个视场观察到的星系数量几乎固定为可用光纤的数量。我们发现我们可以通过用目标星系的数量对每个场中的星系进行加权来恢复长波长波动。第二，它优先选择低密度区域的星系。我们通过使用所谓的个体逆概率加权星系来减轻这种影响。纠正这两种影响后，我们在大于 10 Mpc/h 的尺度上以优于 1% 的准确度恢复了基础相关函数。