E-resources
-
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; 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
The Astrophysical journal, 10/2016, Volume: 830, Issue: 2Journal Article
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 to . 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 and , (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.
Author
![loading ... loading ...](themes/default/img/ajax-loading.gif)
Shelf entry
Permalink
- URL:
Impact factor
Access to the JCR database is permitted only to users from Slovenia. Your current IP address is not on the list of IP addresses with access permission, and authentication with the relevant AAI accout is required.
Year | Impact factor | Edition | Category | Classification | ||||
---|---|---|---|---|---|---|---|---|
JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
Select the library membership card:
If the library membership card is not in the list,
add a new one.
DRS, in which the journal is indexed
Database name | Field | Year |
---|
Links to authors' personal bibliographies | Links to information on researchers in the SICRIS system |
---|
Source: Personal bibliographies
and: SICRIS
The material is available in full text. If you wish to order the material anyway, click the Continue button.