MOIRCS Deep Survey. II. Clustering Properties of K-band Selected Galaxies in GOODS-North Re.pdfVIP

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MOIRCS Deep Survey. II. Clustering Properties of K-band Selected Galaxies in GOODS-North Re.pdf

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MOIRCS Deep Survey. II. Clustering Properties of K-band Selected Galaxies in GOODS-North Re

a r X i v : a s t r o - p h / 0 7 0 1 8 2 0 v 1 2 9 J a n 2 0 0 7 PASJ: Publ. Astron. Soc. Japan , 1–??, c? 2008. Astronomical Society of Japan. MOIRCS Deep Survey. II. Clustering Properties of K-band Selected Galaxies in GOODS-North Region Takashi Ichikawa,1 Ryuji Suzuki,2 Chihiro Tokoku,2 Yuka Katsuno-Uchimoto,3 Masahiro Konishi,1,2 Tomohiro Yoshikawa,1,2 Masaru Kajisawa,5 Masami Ouchi,4 Takashi Hamana,5 Masayuki Akiyama,2 Tetsuo Nishimura,2 Koji Omata,2 Ichi Tanaka,2 and Toru Yamada2 1Astronomical Institute, Tohoku University, Aramaki, Aoba, Sendai 980-8578 ichikawa@astr.tohoku.ac.jp 2Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720, USA 3Institute of Astronomy, University of Tokyo, Mitaka, Tokyo 181-0015 4Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 5National Astronomical Observatory of Japan, Mitaka, Tokyo 181–8588 (Received ; accepted ) Abstract We present the first measurement of clustering properties of low mass galaxies with a stellar mass down to M? ～ 109M⊙ at 1z 4 in 24.4 arcmin2 of the GOODS-North region with a depth of KAB ～ 25, based on the near infrared observations performed with MOIRCS at the Subaru Telescope. The correlation amplitude strongly depends on the K-band flux, color, and stellar mass of the galaxies. We find that K-band luminous galaxies have a larger correlation length than K-band faint galaxies. For color selected samples at 2 z 4, distant red galaxies with J ?K 1.3 show a large bias of b ～ 7.2± 1.3 on scales up to θ～ 100′′ or 3.1 comoving Mpc, while blue galaxies with 0.5 J ?K 1.3, in which most Lyman break galaxies are populated, have a weak clustering signal on large scales, but a possible strong small scale excess at θ 10′′. For massive galaxies with M? ～ 1010M⊙, we estimate a correlation length and bias to be r0 ～ 4.5 h?1 Mpc and b= 1.9? 3.5, which are much larger than those of low mass (M? ～ 109–1010M⊙) galaxies. The comparison of