A Joint SunyaevZel'dovich Effect and X-ray Analysis of Abell 3667

• Main Authors: CM Cantalupo, Kathy Romer, JB Peterson, PL Gomez, G Griffin, M Newcomb, R.C. Nichol
• Format: Article in Journal/Newspaper
• Language: unknown
• Published: 2002
• Subjects: Uncategorised value; Antarctic; The Antarctic; South Pole; Hubble; Antarc*; South pole
• Online Access: https://figshare.com/articles/journal_contribution/A_Joint_SunyaevZel_dovich_Effect_and_X-ray_Analysis_of_Abell_3667/23330990

We present a 40GHz (7.5 mm) raster scan image of a 3.6x2 degree 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 (20h 12m 28.9s, -56 49 51 J2000) was measured to be $\\\\\\\\Delta T_{\\\\\\\\rm CMB}=-154\\\\\\\\mu K$. 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 $H_0 = 64^{+96}_{-30}$ km s$^{-1}$ Mpc$^{-1}$ (68% confidence interval). Our $H_0$ calculation assumes that the cluster can be described using an isothermal, tri-axial ellipsoidal, $\\\\\\\\beta$-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 $H_0$ 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.