The ALHAMBRA survey: evolution of galaxy clustering since z ~ 1
The ALHAMBRA survey: evolution of galaxy clustering since z ~ 1
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ALHAMBRA 巡天：自 z ~ 1 以来星系团的演化
DOI：
10.1093/mnras/stu681
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发表时间：
2014
影响因子：
4.8
通讯作者：
Arnalte-Mur P
中科院分区：
文献类型：
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作者：
Arnalte-Mur P
我们研究了星系团在0.35<；z<；1.25范围内随光度和红移的变化。在这项工作中使用的阿尔罕布拉数据覆盖了七个独立领域的2.38°2，在应用了详细的角度选择掩模后，具有准确的光度红移，σz≲0.014(1+z)，向下到IAB<；24。考虑到调查的深度，我们从B波段的光度中选取样本，亮度降至Lth≃0.16L*atz=100.9。我们使用投影相关函数来测量真实空间的聚集性，考虑了光度学红移的不确定性。我们推断星系的偏向，并用光度来研究它的演化。我们研究了样本方差的影响，并证实了早期的结果，即宇宙演化调查(COSMOS)和欧洲大面积ISO调查北部1(ELAIS-N1)领域是由大结构的存在主导的。对于中等和明亮的样品，Lmed≳0.6L*，我们得到了偏置与光度的强烈依赖关系，这与以前在类似红移下的结果一致。我们能够将这项研究扩展到较暗的光度，在那里我们得到了一个几乎平坦的关系，类似于在低红移时观察到的关系。关于偏差随红移的演化，我们的结果表明，所研究的不同星系群驻留在质量范围为log10[Mh/(h−1M⊙)]≳11.5)对于Lmed≃0.3L*的样品到log10[Mh/(h−1M⊙)]≳13.0对于Lmed≃2L*的样品)]的晕中，典型的占据数在每个晕的∼1-3个星系的范围内。
We study the clustering of galaxies as function of luminosity and redshift in the range 0.35 <z< 1.25 using data from the Advanced Large Homogeneous Area Medium-Band Redshift Astronomical (ALHAMBRA) survey. The ALHAMBRA data used in this work cover 2.38 deg2in seven independent fields, after applying a detailed angular selection mask, with accurate photometric redshifts, σz≲ 0.014(1 +z), down toIAB< 24. Given the depth of the survey, we select samples inB-band luminosity down toLth≃ 0.16L* atz= 0.9. We measure the real-space clustering using the projected correlation function, accounting for photometric redshifts uncertainties. We infer the galaxy bias, and study its evolution with luminosity. We study the effect of sample variance, and confirm earlier results that the Cosmic Evolution Survey (COSMOS) and European Large Area ISO Survey North 1 (ELAIS-N1) fields are dominated by the presence of large structures. For the intermediate and bright samples,Lmed≳ 0.6L*, we obtain a strong dependence of bias on luminosity, in agreement with previous results at similar redshift. We are able to extend this study to fainter luminosities, where we obtain an almost flat relation, similar to that observed at low redshift. Regarding the evolution of bias with redshift, our results suggest that the different galaxy populations studied reside in haloes covering a range in mass between log10[Mh/(h−1M⊙)] ≳ 11.5 for samples withLmed≃ 0.3L* and log10[Mh/(h−1M⊙)] ≳ 13.0 for samples withLmed≃ 2L*, with typical occupation numbers in the range of ∼1–3 galaxies per halo.