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Title:
Clustering of Star-forming Galaxies Near a Radio Galaxy at z=5.2
Authors:
Overzier, Roderik A.; Miley, G. K.; Bouwens, R. J.; Cross, N. J. G.; Zirm, A. W.; Benítez, N.; Blakeslee, J. P.; Clampin, M.; Demarco, R.; Ford, H. C.; Hartig, G. F.; Illingworth, G. D.; Martel, A. R.; Röttgering, H. J. A.; Venemans, B.; Ardila, D. R.; Bartko, F.; Bradley, L. D.; Broadhurst, T. J.; Coe, D.; Feldman, P. D.; Franx, M.; Golimowski, D. A.; Goto, T.; Gronwall, C.; Holden, B.; Homeier, N.; Infante, L.; Kimble, R. A.; Krist, J. E.; Mei, S.; Menanteau, F.; Meurer, G. R.; Motta, V.; Postman, M.; Rosati, P.; Sirianni, M.; Sparks, W. B.; Tran, H. D.; Tsvetanov, Z. I.; White, R. L.; Zheng, W.
Affiliation:
AA(Leiden Observatory, Postbus 9513, 2300 RA Leiden, Netherlands; .), AB(Leiden Observatory, Postbus 9513, 2300 RA Leiden, Netherlands; .), AC(UCO/Lick Observatory, University of California, Santa Cruz, CA 95064.), AD(Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK.), AE(Leiden Observatory, Postbus 9513, 2300 RA Leiden, Netherlands; .), AF(Instituto Astrofísica de Andalucía (CSIC), Camino Bajo de Huétor, 24, Granada 18008, Spain.), AG(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AH(NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771.), AI(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AJ(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AK(Science Space Telescope Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AL(UCO/Lick Observatory, University of California, Santa Cruz, CA 95064.), AM(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AN(Leiden Observatory, Postbus 9513, 2300 RA Leiden, Netherlands; .), AO(Leiden Observatory, Postbus 9513, 2300 RA Leiden, Netherlands; .), AP(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AQ(Bartko Science and Technology, 14520 Akron Street, Brighton, CO 80602.), AR(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AS(Racah Institute of Physics, Hebrew University, Jerusalem, Israel 91904.), AT(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AU(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AV(Leiden Observatory, Postbus 9513, 2300 RA Leiden, Netherlands; .), AW(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AX(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AY(Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802.), AZ(UCO/Lick Observatory, University of California, Santa Cruz, CA 95064.), BA(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BB(Departmento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile.), BC(NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771.), BD(Jet Propulsion Laboratory, Mail Stop 183-900, 4800 Oak Grove Drive, Pasadena, CA 91109.), BE(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BF(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BG(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BH(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.; Departmento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile.), BI(Science Space Telescope Institute, 3700 San Martin Drive, Baltimore, MD 21218.), BJ(European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany.), BK(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BL(Science Space Telescope Institute, 3700 San Martin Drive, Baltimore, MD 21218.), BM(W. M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, HI 96743.), BN(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BO(Science Space Telescope Institute, 3700 San Martin Drive, Baltimore, MD 21218.), BP(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.)
Publication:
The Astrophysical Journal, Volume 637, Issue 1, pp. 58-73. (ApJ Homepage)
Publication Date:
01/2006
Origin:
UCP
ApJ Keywords:
Cosmology: Observations, Cosmology: Early Universe, Galaxies: Clusters: General, Galaxies: High-Redshift, Galaxies: Individual: Alphanumeric: TN J0924-2201, Galaxies: Starburst, Cosmology: Large-Scale Structure of Universe
DOI:
10.1086/498234
Bibliographic Code:
2006ApJ...637...58O

Abstract

We present HST ACS observations of the most distant radio galaxy known, TN J0924-2201 at z=5.2. This radio galaxy has six spectroscopically confirmed Lyα-emitting companion galaxies and appears to lie within an overdense region. The radio galaxy is marginally resolved in i775 and z850, showing continuum emission aligned with the radio axis, similar to what is observed for lower redshift radio galaxies. Both the half-light radius and the UV star formation rate are comparable to the typical values found for Lyman break galaxies at z~4-5. The Lyα emitters are sub-L* galaxies, with deduced star formation rates of 1-10 Msolar yr-1. One of the Lyα emitters is only detected in Lyα. Based on the star formation rate of ~3 Msolar yr-1 calculated from Lyα, the lack of continuum emission could be explained if the galaxy is younger than ~2 Myr and is producing its first stars. Observations in V606i775z850 were used to identify additional Lyman break galaxies associated with this structure. In addition to the radio galaxy, there are 22 V606 break (z~5) galaxies with z850<26.5 (5 σ), two of which are also in the spectroscopic sample. We compare the surface density of ~2 arcmin-2 to that of similarly selected V606 dropouts extracted from GOODS and the UDF parallel fields. We find evidence for an overdensity to very high confidence (>99%), based on a counts-in-cells analysis applied to the control field. The excess suggests that the V606 break objects are associated with a forming cluster around the radio galaxy.

Based on observations made with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 9291.


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