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THE ATACAMA COSMOLOGY TELESCOPE (ACT): BEAM PROFILES AND FIRST SZ CLUSTER MAPS

2010; Institute of Physics; Volume: 191; Issue: 2 Linguagem: Inglês

10.1088/0067-0049/191/2/423

1538-4365

Adam D. Hincks, Viviana Acquaviva, P. A. R. Ade, Paula Aguirre, M. Amiri, John W. Appel, L. Felipe Barrientos, E. S. Battistelli, J. R. Bond, Ben Brown, B. Burger, J. A. Chervenak, S. Das, Mark J. Devlin, Simon Dicker, W. B. Doriese, Jo Dunkley, Rolando Dünner, Thomas Essinger-Hileman, R. P. Fisher, Joseph W. Fowler, A. R. Hajian, M. Halpern, Matthew Hasselfield, C. Hernández-Monteagudo, G. C. Hilton, Matt Hilton, Renée Hložek, K. M. Huffenberger, David H. Hughes, John P. Hughes, L. Infante, K. D. Irwin, Raúl Jiménez, J. B. Juin, Madhuri Kaul, Jeff Klein, Arthur Kosowsky, Judy M. Lau, M. Limon, Yen‐Ting Lin, Robert H. Lupton, Tobias A. Marriage, Danica Marsden, Krista Martocci, P. Mauskopf, F. Menanteau, Kavilan Moodley, H. Moseley, C. B. Netterfield, Michael D. Niemack, Michael R. Nolta, Lyman A. Page, Lucas Parker, Bruce Partridge, H. Quintana, Beth Reid, Neelima Sehgal, Jonathan Sievers, David N. Spergel, Suzanne T. Staggs, O. R. Stryzak, Daniel S. Swetz, Eric R. Switzer, Robert Thornton, Hy Trac, C. Tucker, Licia Verde, Ryan Warne, G. W. Wilson, Edward J. Wollack, Yue Zhao,

Scientific Research and Discoveries

The Atacama Cosmology Telescope (ACT) is currently observing the cosmic microwave background with arcminute resolution at 148 GHz, 218 GHz, and 277 GHz. In this paper, we present ACT's first results. Data have been analyzed using a maximum-likelihood map-making method which uses B-splines to model and remove the atmospheric signal. It has been used to make high-precision beam maps from which we determine the experiment's window functions. This beam information directly impacts all subsequent analyses of the data. We also used the method to map a sample of galaxy clusters via the Sunyaev–Zel'dovich (SZ) effect and show five clusters previously detected with X-ray or SZ observations. We provide integrated Compton-y measurements for each cluster. Of particular interest is our detection of the z = 0.44 component of A3128 and our current non-detection of the low-redshift part, providing strong evidence that the further cluster is more massive as suggested by X-ray measurements. This is a compelling example of the redshift-independent mass selection of the SZ effect.