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    Please use this identifier to cite or link to this item: http://tkuir.lib.tku.edu.tw:8080/dspace/handle/987654321/111980

    Title: AMiBA: Cluster Sunyaev-Zel'dovich Effect Observations with the Expanded 13-Element Array
    Authors: Lin, Kai-Yang;Nishioka, Hiroaki;Wang, Fu-Cheng;Huang, Chih-Wei Locutus;Liao, Yu-Wei;Wu, Jiun-Huei Proty;Koch, Patrick M.;Umetsu, Keiichi;Chen, Ming-Tang;Chan, Shun-Hsiang;Chang, Shu-Hao;Chang, Wen-Hsuan Lucky;Cheng, Tai-An;Duy, Hoang Ngoc;Fu, Szu-Yuan;Han, Chih-Chiang;Ho, Solomon;Ho, Ming-Feng;Ho, Paul T.P.;Huang, Yau-De;Jiang, Homin;Kubo, Derek Y.;Li, Chao-Te;Lin, Yu-Chiung;Liu, Guo-Chin;Pierre, Martin-Cocher;Molnar, Sandor M.;Nunez, Emmanuel;Oshiro, Peter;Pai, Shang-Ping;Raffin, Philippe;Ridenour, Anthony;Shih, Chia-You;Stoebner, Sara;Teo, Giap-Siong;Yeh, Jia-Long Johnny;Williams, Joshua;Birkinshaw, Mark
    Date: 20160801
    Issue Date: 2017-11-07 02:10:13 (UTC+8)
    Publisher: Institute of Physics Publishing, Inc.
    Abstract: The Yuan-Tseh Lee Array for Microwave Background Anisotropy (AMiBA) is a co-planar interferometer array operating at a wavelength of 3 mm to measure the Sunyaev–Zel'dovich effect (SZE) of galaxy clusters at arcminute scales. The first phase of operation—with a compact 7-element array with 0.6 m antennas (AMiBA-7)—observed six clusters at angular scales from $5^{\prime} $ to $23^{\prime} $. Here, we describe the expansion of AMiBA to a 13-element array with 1.2 m antennas (AMiBA-13), its subsequent commissioning, and cluster SZE observing program. The most noticeable changes compared to AMiBA-7 are (1) array re-configuration with baselines ranging from 1.4 m to 4.8 m, allowing us to sample structures between $2^{\prime} $ and $10^{\prime} $, (2) 13 new lightweight carbon-fiber-reinforced plastic (CFRP) 1.2 m reflectors, and (3) additional correlators and six new receivers. Since the reflectors are co-mounted on and distributed over the entire six-meter CFRP platform, a refined hexapod pointing error model and phase error correction scheme have been developed for AMiBA-13. These effects—entirely negligible for the earlier central close-packed AMiBA-7 configuration—can lead to additional geometrical delays during observations. Our correction scheme recovers at least 80 ± 5% of the point-source fluxes. We, therefore, apply an upward correcting factor of 1.25 to our visibilities to correct for phase decoherence, and a ±5% systematic uncertainty is added in quadrature with our statistical errors. We demonstrate the absence of further systematics with a noise level consistent with zero in stacked uv-visibilities. From the AMiBA-13 SZE observing program, we present here maps of a subset of 12 clusters with signal-to-noise ratios above five. We demonstrate combining AMiBA-7 with AMiBA-13 observations on Abell 1689, by jointly fitting their data to a generalized Navarro–Frenk–White model. Our cylindrically integrated Compton-y values for five radii are consistent with results from the Berkeley-Illinois-Maryland Array, the Owens Valley Radio Observatory, the Sunyaev–Zel'dovich Array, and the Planck Observatory. We also report the first targeted SZE detection toward the optically selected cluster RCS J1447+0828, and we demonstrate the ability of AMiBA SZE data to serve as a proxy for the total cluster mass. Finally, we show that our AMiBA-SZE derived cluster masses are consistent with recent lensing mass measurements in the literature.
    Relation: The Astrophysical Journal 830(2)
    DOI: 10.3847/0004-637X/830/2/91
    Appears in Collections:[物理學系暨研究所] 期刊論文

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