The Canada-France deep fields survey-II: Lyman-break galaxies and galaxy clustering at z 3 ?
The Canada-France deep fields survey-II: Lyman-break galaxies and galaxy clustering at z 3 ?
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加拿大-法国深田调查-II：莱曼断裂星系和z 3 处的星系团？
DOI：
10.1051/0004-6361:20031181
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发表时间：
2003
影响因子：
6.5
通讯作者：
Y. Mellier
中科院分区：
文献类型：
--
作者：
S. Foucaud;H. McCracken;O. Fèvre;S. Arnouts;M. Brodwin;S. Lilly;D. Crampton;Y. Mellier
本文介绍了从加拿大-法国深场巡天（CFDF）中提取的z3 U带脱落星系的大样本。我们的星表涵盖了一个有效面积为1700弧分2的区域，分为三个大的，连续的领域，在天空中分开很远。IAB = 24.5，调查包含1294莱曼打破候选人，与以前的测量由其他作者，适当的不完整性校正后，已应用到我们的数据。基于与光谱观测和模拟的比较，我们估计我们的莱曼破裂星系样本被恒星和闯入者（低红移星系）污染不超过30%。我们找到了！（θ）很好地符合固定斜率的幂律，= 1.8，即使在小的角间距（θ < 10 "）。在我们的三个场中的两个，我们能够同时拟合斜率和振幅，并找到= 1.8 ± 0.2和r 0 =（5.3 + 6.8 −2.2）h −1 Mpc，以及= 1.8 ± 0.3和r 0 =（6.3 + 17.9 −2.8）h −1 Mpc（所有空间相关的量都引用了平坦宇宙学）。我们的数据勉强表明，在一个领域（在3-水平），莱曼break相关长度r 0取决于样本极限星等：明亮的莱曼break星系比昏暗的星系更聚集。对于整个CFDF样本，假设固定斜率= 1.8，我们发现r 0 =（5.9 ± 0.5）h −1 Mpc。使用这些集群测量和预测的暗物质密度场计算假设集群归一化线性理论，我们得出的线性偏差为B = 3.5±0.3。最后，我们表明，相关长度与莱曼break星系的表面密度的依赖关系是在一个简单的图片，其中更明亮的星系主办的更大质量的暗物质晕与一个简单的一对一的对应关系是很好的协议。
We present a large sample of z � 3 U band dropout galaxies extracted from the Canada-France deep fields survey (CFDF). Our catalogue covers an effective area of � 1700 arcmin 2 divided between three large, contiguous fields separated widely on the sky. To IAB = 24.5, the survey contains 1294 Lyman-break candidates, in agreement with previous measurements by other authors, after appropriate incompleteness corrections have been applied to our data. Based on comparisons with spectroscopic observations and simulations, we estimate that our sample of Lyman-break galaxies is contaminated by stars and interlopers (lower-redshift galaxies) at no more than � 30%. We find that !(�) is well fitted by a power-law of fixed slope, = 1.8, even at small (� < 10 '' ) angular separations. In two of our three fields, we are able to fit simultaneously for both the slope and amplitude and find = 1.8 ± 0.2 and r0 = (5.3 +6.8 −2.2)h −1 Mpc, and = 1.8 ± 0.3 and r 0 = (6.3 +17.9 −2.8 )h −1 Mpc (all spatially dependent quantities are quoted for a �-flat cosmology). Our data marginally indicates in one field (at a 3� level) that the Lyman-break correlation length r0 depends on sample limiting magnitude: brighter Lyman-break galaxies are more clustered than fainter ones. For the entire CFDF sample, assuming a fixed slope = 1.8 we find r0 = (5.9 ± 0.5)h −1 Mpc. Using these clustering measurements and prediction for the dark matter density field computed assuming cluster-normalised linear theory, we derive a linear bias of b = 3.5±0.3. Finally we show that the dependence of the correlation length with the surface density of Lyman-break galaxies is in good agreement with a simple picture where more luminous galaxies are hosted by more massive dark matter halos with a simple one-to-one correspondence.