Weak Lensing Analysis of CL 1358+62 Using Hubble Space Telescope Observations

Details Weak Lensing Analysis of CL 1358+62 Using Hubble Space Telescope Observations Weak Lensing Analysis of CL 1358+62 Using Hubble Space Telescope Observations

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...504..636h&link_type=abstract

Astrophysical Journal v.504, p.636

Astronomy and Astrophysics

Astronomy

186

Galaxies: Clusters: Individual Alphanumeric: Cl 1358+62, Galaxies: Fundamental Parameters, Cosmology: Gravitational Lensing

Scientific paper

We report on the detection of weak gravitational lensing of faint, distant background objects by Cl 1358+62, a rich cluster of galaxies at a redshift of z = 0.33. The observations consist of a large, multicolor mosaic of Hubble Space Telescope WFPC2 images. The number density of approximately 50 background objects arcmin-2 allows us to do a detailed weak lensing analysis of this cluster. We detect a weak lensing signal out to~1.5 Mpc from the cluster center. The observed distortion is consistent with a singular isothermal sphere model with a velocity dispersion of 780 +/- 50 km s-1. The total projected mass within a radius of 1 Mpc corresponding to this model is (4.4 +/- 0.6) x 1014 M&sun;. The errors given here represent the random error due to the ellipticities of the background galaxies. The uncertainty in the redshift distribution introduces an additional systematic error of ~10% in the weak lensing mass. The weak lensing mass is slightly lower than dynamical estimates and agrees well with X-ray mass estimates. The mass distribution is elongated in a similar way as the light. The axis ratio of 0.30 +/- 0.15 and position angle of -21 deg +/- 7 deg were measured directly from the observations and agree very well with a previous strong lensing determination. A two-dimensional reconstruction of the cluster mass surface density shows that the peak of the mass distribution coincides with the peak of the light distribution. We find a value of (90 +/- 13)h50 M&sun; L^{-1}Vsolar for the mass-to-light ratio, consistent with being constant with radius. The point-spread function of HST is highly anisotropic at the edges of the individual chips. This systematically perturbs the shapes of objects, and we present a method for applying the appropriate correction.

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