HUBBLE SPACE TELESCOPE WEAK-LENSING STUDY OF THE GALAXY CLUSTER XMMU J2235.3 - 2557 AT z approx 1.4: A SURPRISINGLY MASSIVE GALAXY CLUSTER WHEN THE UNIVERSE IS ONE-THIRD OF ITS CURRENT AGE

Journal Article · Sat Oct 10 00:00:00 EDT 2009 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/704/1/672· OSTI ID:21367417

Jee, M J ^[1]; Rosati, P ^[2]; Ford, H C ^[3]; Dawson, K S ^[4]; Lidman, C ^[5]; Perlmutter, S ^[6]; Demarco, R ^[7]; Strazzullo, V ^[8]; Mullis, C ^[9]; Boehringer, H; Fassbender, R ^[10]

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1. Department of Physics, University of California, Davis, One Shields Avenue, Davis, CA 95616 (United States)
2. European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748, Garching (Germany)
3. Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States)
4. Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 (United States)
5. European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Santiago (Chile)
6. E. O. Lawrence Berkeley National Laboratory, Berkeley, CA 94720 (United States)
7. Department of Astronomy, Universidad de Concepcion. Casilla 160-C, Concepcion (Chile)
8. National Radio Astronomy Observatory, NM 87801 (United States)
9. Wachovia Corporation, NC6740, Winston-Salem, NC 27101 (United States)
10. Max-Planck-Institut fuer extraterrestrische Physik (MPE), Giessenbachstrasse 1, 85748 Garching (Germany)

We present a weak-lensing analysis of the z approx = 1.4 galaxy cluster XMMU J2235.3 - 2557, based on deep Advanced Camera for Surveys images. Despite the observational challenge set by the high redshift of the lens, we detect a substantial lensing signal at the approx>8sigma level. This clear detection is enabled in part by the high mass of the cluster, which is verified by our both parametric and non-parametric estimation of the cluster mass. Assuming that the cluster follows a Navarro-Frenk-White mass profile, we estimate that the projected mass of the cluster within r = 1 Mpc is (8.5 +- 1.7) x 10{sup 14} M {sub sun}, where the error bar includes the statistical uncertainty of the shear profile, the effect of possible interloping background structures, the scatter in concentration parameter, and the error in our estimation of the mean redshift of the background galaxies. The high X-ray temperature 8.6{sup +1.3} {sub -1.2} keV of the cluster recently measured with Chandra is consistent with this high lensing mass. When we adopt the 1sigma lower limit as a mass threshold and use the cosmological parameters favored by the Wilkinson Microwave Anisotropy Probe 5-year (WMAP5) result, the expected number of similarly massive clusters at z approx> 1.4 in the 11 square degree survey is N approx 5 x 10{sup -3}. Therefore, the discovery of the cluster within the survey volume is a rare event with a probability approx<1% and may open new scenarios in our current understanding of cluster formation within the standard cosmological model.

• OSTI ID: 21367417
• Journal Information: Astrophysical Journal, Vol. 704, Issue 1; Other Information: DOI: 10.1088/0004-637X/704/1/672; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ANISOTROPY
CAMERAS
COSMOLOGICAL MODELS
COSMOLOGY
GALAXY CLUSTERS
MASS
MICROWAVE RADIATION
NONLUMINOUS MATTER
PROBABILITY
RED SHIFT
SIGNALS
TELESCOPES
UNIVERSE
X-RAY GALAXIES
COSMIC RAY SOURCES
COSMIC X-RAY SOURCES
ELECTROMAGNETIC RADIATION
GALAXIES
MATHEMATICAL MODELS
MATTER
RADIATIONS