Measuring and modelling the redshift evolution of clustering: the Hubble Deep Field North
Measuring and modelling the redshift evolution of clustering: the Hubble Deep Field North
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DOI：
10.1046/j.1365-8711.1999.02978.x
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发表时间：
1999-02
影响因子：
4.8
通讯作者：
S. Arnouts;S. Cristiani;L. Moscardini;S. Matarrese;F. Lucchin;A. Fontana;E. Giallongo
中科院分区：
文献类型：
--
作者：
S. Arnouts;S. Cristiani;L. Moscardini;S. Matarrese;F. Lucchin;A. Fontana;E. Giallongo
ABSTRA C T从za 0 toz星系团的演化。利用角关联函数和光度红移分布分析了哈勃北深场中比IAB < 28：5亮的星系的角关联函数。在现有光谱红移的基础上讨论了测光红移估计的可靠性，比较了不同的代码，并调查了测光误差的影响。然后，考虑到光度红移的不确定性，优化的红移箱中的聚类特性进行测量。结果表明，随动关联长度r_0在0 & z & 1范围内有一个小的减小，然后在较高的z范围内又有一个增大。我们将这些结果与属于冷暗物质场景的一般类别的各种宇宙学模型的理论预测进行了比较，包括Einstein‐de Sitter模型，开放模型和具有非零宇宙学常数的平坦模型。与预期的质量成团演化的比较表明，观测到的高红移星系的暗物质与一个有效的偏置B强烈增加的红移偏置示踪剂。假设存在一个爱因斯坦-德西特宇宙，我们得到B。两点五分。2和B。5a tz。4.这些结果支持了偏置星系形成的理论方案，在高红移观测到的星系优先位于更大质量的晕。此外，他们认为，通常的参数化的集群演化为jOr; zUajOr; 0 UO 1 1 zU 2 O 31 eU是不是一个很好的描述任何值的e。我们在z测量的聚类幅度的比较。3与Adelberger等人和Giavalisco等人报告的结果一致，基于不同的选择，表明集群取决于物体的丰度：更丰富的物体较少集群，正如在分级星系形成的范例中所预期的那样。在z处测量的强聚类和高偏差。3是一致的，在这里考虑的各种宇宙学框架中预测的大质量晕的预期密度。在z。4，在哈勃深空中观察到的强集群需要在那个时代已经形成的大质量晕的很大一部分。如果未来的观测证实了这一特征，它可能成为宇宙学参数的判别检验。
ABSTRA C T The evolution of galaxy clustering from za 0t oz . 4:5 is analysed using the angular correlation function and the photometric redshift distribution of galaxies brighter than IAB < 28:5 in the Hubble Deep Field North. The reliability of the photometric redshift estimates is discussed on the basis of the available spectroscopic redshifts, comparing different codes and investigating the effects of photometric errors. The redshift bins in which the clustering properties are measured are then optimized to take into account the uncertainties of the photometric redshifts. The results show that the comoving correlation length r0 has a small decrease in the range 0 & z & 1 followed by an increase at higher z. We compare these results with the theoretical predictions of a variety of cosmological models belonging to the general class of Cold Dark Matter scenarios, including Einstein‐de Sitter models, an open model and a flat model with non-zero cosmological constant. Comparison with the expected mass clustering evolution indicates that the observed high-redshift galaxies are biased tracers of the dark matter with an effective bias b strongly increasing with redshift. Assuming an Einstein‐de Sitter universe, we obtain b . 2: 5a tz . 2 and b . 5a tz . 4. These results support theoretical scenarios of biased galaxy formation in which the galaxies observed at high redshift are preferentially located in more massive haloes. Moreover, they suggest that the usual parameterization of the clustering evolution as jOr; zUajOr; 0UO1 1 zU 2O31eU is not a good description for any value of e . Comparison of the clustering amplitudes that we measured at z . 3 with those reported by Adelberger et al. and Giavalisco et al., based on a different selection, suggests that the clustering depends on the abundance of the objects: more abundant objects are less clustered, as expected in the paradigm of hierarchical galaxy formation. The strong clustering and high bias measured at z . 3 are consistent with the expected density of massive haloes predicted in the frame of the various cosmologies considered here. At z . 4, the strong clustering observed in the Hubble Deep Field requires a significant fraction of massive haloes to be already formed by that epoch. This feature could be a discriminant test for the cosmological parameters if confirmed by future observations.