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Date and Time of the Query: 2019-07-22 T14:34:34 PDT
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For refcode 2016ApJ...830...91L:
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2016ApJ...830...91L AMiBA: Cluster Sunyaev-Zel'dovich Effect Observations with the Expanded 13-element Array Lin, Kai-Yang; Nishioka, Hiroaki; Wang, Fu-Cheng; Locutus Huang, Chih-Wei; Liao, Yu-Wei; Proty Wu, Jiun-Huei; Koch, Patrick M.; Umetsu, Keiichi; Chen, Ming-Tang; Chan, Shun-Hsiang; Chang, Shu-Hao; Lucky Chang, Wen-Hsuan; 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; Martin-Cocher, Pierre; 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 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' to 23' . 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' and 10', (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. Key words: cosmic background radiation, galaxies: clusters: general, instrumentation: interferometers
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