Preprint typeset using L ATEX style emulateapj A JOINT SUNYAEV-ZEL’DOVICH EFFECT AND X-RAY ANALYSIS OF ABELL 3667

• Main Authors: C. M. Cantalupo, A. K. Romer, J. B. Peterson, P. Gomez, G. Griffin, M. Newcomb
• Other Authors: The Pennsylvania State University CiteSeerX Archives
• Format: Text
• Language: English
• Published: 2002
• Subjects: Antarctic; Hubble; South Pole; The Antarctic; Antarc*; South pole
• Online Access: http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.257.386; http://arxiv.org/pdf/astro-ph/0212394v2.pdf

We present a 40GHz (7.5 mm) raster scan image of a 3.6 ◦ × 2 ◦ region centered on the low redshift (z = 0.055) cluster of galaxies Abell 3667. The cluster was observed during the Antarctic winter of 1999 using the Corona instrument (15.7 ′ FWHM beam) on the Viper Telescope at the South Pole. The Corona image of A3667 is one of the first direct (i.e. rather than interferometer) thermal Sunyaev-Zel’dovich effect images of a low redshift cluster. The brightness temperature decrement at the X-ray centroid (20h12m28.9s, −56◦49 ′ 51 ′ ′ J2000) was measured to be ∆TCMB = −154µK. We have used the 40GHz map of A3667 in conjunction with a deep ROSAT PSPC (X-ray) image of the cluster, to make a measurement of the Hubble Constant. We find H0 = 64 +96 −30 km s−1 Mpc−1 (68 % confidence interval). Our H0 calculation assumes that the cluster can be described using an isothermal, tri-axial ellipsoidal, β-model and includes several new analysis techniques including an automated method to remove point sources from X-ray images with variable point spread functions, and an efficient method for determining the errors in multi-parameter maximum likelihood analyzes. The large errors on the H0 measurement are primarily due to the statistical noise in the Corona image. We plan to increase the precision of our measurement by including additional clusters in our analysis and by increasing the sensitivity of the Viper SZE maps. 1.