CLUSTERING OF INFRARED-BRIGHT DUST-OBSCURED GALAXIES REVEALED BY THE HYPER SUPRIME-CAM AND WISE
CLUSTERING OF INFRARED-BRIGHT DUST-OBSCURED GALAXIES REVEALED BY THE HYPER SUPRIME-CAM AND WISE
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DOI：
10.3847/1538-4357/835/1/36
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发表时间：
2016-12
期刊：
影响因子：
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通讯作者：
Y. Toba;T. Nagao;M. Kajisawa;T. Oogi;M. Akiyama;H. Ikeda;J. Coupon;M. Strauss;Wei-hao Wang;Masayuki Tanaka;M. Niida;M. Imanishi;Chien-Hsiu Lee;H. Matsuhara;Y. Matsuoka;M. Onoue;Y. Terashima;Y. Ueda;Y. Harikane;Y. Komiyama;S. Miyazaki;Akatoki Noboriguchi;T. Usuda
中科院分区：
文献类型：
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作者：
Y. Toba;T. Nagao;M. Kajisawa;T. Oogi;M. Akiyama;H. Ikeda;J. Coupon;M. Strauss;Wei-hao Wang;Masayuki Tanaka;M. Niida;M. Imanishi;Chien-Hsiu Lee;H. Matsuhara;Y. Matsuoka;M. Onoue;Y. Terashima;Y. Ueda;Y. Harikane;Y. Komiyama;S. Miyazaki;Akatoki Noboriguchi;T. Usuda
我们提出了测量的红外（IR）明亮的尘埃遮蔽星系（DOG）的样本的聚类特性。结合125 deg 2的宽和深的光学图像获得的超Suprime-Cam的斯巴鲁望远镜和全天空中红外图像采取的宽视场红外巡天探测器，我们发现了4367红外明亮的DOG和通量密度在22毫焦耳年。我们计算了1411个DOG的均匀子样本的角度自相关函数（ACF），其中3.0 mJy <通量（22）< 5.0 mJy且< 24.0。我们的DOG子样本的ACF与单一幂律很好地拟合，=（0.010 ± 0.003），其中θ以度为单位。红外亮DOG的相关幅度大于红外暗DOG的相关幅度，这反映了DOG聚类的通量依赖性，正如Brodwin等人所建议的那样。我们假设我们的DOG样本的红移分布是高斯分布，并考虑两种情况：（1）红移分布与红外微弱DOG相同，通量为22 < 1.0 mJy，平均值和西格玛z = 1.99 ± 0.45，以及（2）z = 1.19 ± 0.30，这是从它们的光度红移推断出来的。红外亮DOG的关联长度分别为r 0 = 12.0 ± 2.0和10.3 ± 1.7 Mpc。在这两种情况下，红外明亮的DOG分别存在于质量为和的大质量暗物质晕中。
We present measurements of the clustering properties of a sample of infrared (IR) bright dust-obscured galaxies (DOGs). Combining 125 deg2 of wide and deep optical images obtained with the Hyper Suprime-Cam on the Subaru Telescope and all-sky mid-IR images taken with Wide-Field Infrared Survey Explorer, we have discovered 4367 IR-bright DOGs with and flux density at 22 mJy. We calculate the angular autocorrelation function (ACF) for a uniform subsample of 1411 DOGs with 3.0 mJy < flux (22 ) < 5.0 mJy and < 24.0. The ACF of our DOG subsample is well-fit with a single power law, = (0.010 ± 0.003) , where θ is in degrees. The correlation amplitude of IR-bright DOGs is larger than that of IR-faint DOGs, which reflects a flux dependence of the DOG clustering, as suggested by Brodwin et al. We assume that the redshift distribution for our DOG sample is Gaussian, and consider two cases: (1) the redshift distribution is the same as IR-faint DOGs with flux at 22 < 1.0 mJy, mean and sigma z = 1.99 ± 0.45, and (2) z = 1.19 ± 0.30, as inferred from their photometric redshifts. The inferred correlation length of IR-bright DOGs is r0 = 12.0 ± 2.0 and 10.3 ± 1.7 Mpc, respectively. IR-bright DOGs reside in massive dark matter halos with a mass of and in the two cases, respectively.