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An upgrade of analog and digital infrastructure at the YTLA was necessary to enable IM. In particular, a digital correlator based on CASPER technology and the ASIAA-developed 5 GS/s sampler was developed. The digital correlator produces 2 x 2 GHz bandwidth in each of two polarizations for 7
586:
The YTLA uses the technique of intensity mapping (IM) to study molecular gas. Rather than attempting to detect individual, distant and faint galaxies directly, the YTLA measures the statistical properties of many galaxies over a very large volume. Although it is much smaller than powerful
391:) started in October 2006, and the detections of six clusters by the Sunyaev-Zel'dovich effect were announced in 2008. In 2009 the telescope was upgraded to 13 elements, and it is capable of further expansion to 19 elements. AMiBA is the result of a collaboration between the
516:
in clusters of galaxies, which has a maximum decrement around 100 GHz. In its initial configuration, it measures up to multipoles of 3,000 with a resolution of around 6 arcminutes. The telescope only observes at night during good weather, using planets for calibration.
570:
The YTLA has been repurposed with the goal of detection and characterization of molecular gas at high redshift through the technique of intensity mapping. Molecular gas, which is primarily in the form of the hydrogen molecule
575:, is the material from which stars form. Understanding the gas content and evolution throughout the history of the Universe informs astronomers about the processes of star formation and galaxy growth. Unfortunately, cold H
488:. The array was upgraded to have thirteen 1.2 m dishes in 2009 ("AMiBA13"). After extensive testing and calibration, scientific observations resumed in 2011. It is further expandable up to 19 elements.
1370:
937:
Bower, Geoffrey C.; Keating, Garrett K.; Marrone, Daniel P.; Y.T. Lee Array Team, SZA Team (1 January 2016). "Cosmic
Structure and Galaxy Evolution through Intensity Mapping of Molecular Gas".
365:
After completion of the SZE campaigns, the telescope has been repurposed to study the evolution of molecular gas throughout the history of the
Universe. It is now referred to as the
595:, the YTLA can provide critical and unique information on galaxy evolution. The intensity mapping technique is used over a wide range of wavelengths to study the distant Universe.
870:
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 (1 October 2016).
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476:. The mount arrived on site in 2004, and the platform was installed in 2005. The first 7 elements were then installed ("AMiBA7"), and the telescope's
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438:) to minimize foreground emission from other, non-thermal sources. The telescope has a retractable shelter, made from seven steel trusses and
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Umetsu, Keiichi; et al. (2009). "Mass and Hot
Baryons in Massive Galaxy Clusters from Subaru Weak Lensing and AMiBA SZE Observations".
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between 0.091 and 0.322. For the largest and brightest four of these—Abell 1689, 2261, 2142 and 2390—comparisons were made with X-ray and
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Wu, Jiun-Huei Proty; et al. (2008). "AMiBA Observations, Data
Analysis and Results for Sunyaev-Zel'dovich Effects".
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472:. A 2-element prototype was set up on Mauna Loa in 2002. Further funding for a second 4 years was provided by the
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Jiang, Homin; Liu, Howard; Guzzino, Kim; Kubo, Derek; Li, Chao-Te; Chang, Ray; Chen, Ming-Tang (1 August 2014).
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AMiBA started in 2000, with funding for 4 years from the
Cosmology and Particle Astrophysics Project of the
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data to study the cluster layout and radial properties, specifically of the mass profiles and
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Ho, Paul; et al. (2009). "The Yuan-Tseh Lee Array for
Microwave Background Anisotropy".
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872:"AMiBA: Cluster Sunyaev-Zel'dovich Effect Observations with the Expanded 13-element Array"
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hexapod mount. It is located on Mauna Loa, Hawaii, and observes at 3 mm (86–102
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Kovetz, Ely D; et al. (2017). "Line-Intensity
Mapping: 2017 Status Report".
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is not easily detectable. Carbon monoxide (CO) is commonly used as a tracer of H
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Ho, Paul T.P.; et al. (28 June 2008b). "The Yuan Tseh Lee AMiBA Project".
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to reduce their frequency, prior to correlation with an analog correlator. The
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The primary goal of AMiBA is to observe both the temperature and polarization
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atop a hexapod mount. Observations at a wavelength of 3 mm (86–102
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13-element results from the YTLA were published in this paper.
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between 800 and 8,000 (corresponding to between 2 and 20
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For the non-profit organization also known as AMIBA, see
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336:
Yuan-Tseh Lee Array for
Microwave Background Anisotropy
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Six clusters were imaged in 2007: the Abell clusters
380:, at 3,396 metres (11,142 ft) above sea level.
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607:AMiBA is the result of a collaboration between the
484:. The telescope was dedicated in October 2006 to
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641:Canadian Institute for Theoretical Astrophysics
457:of amplification. The signals are mixed with a
383:AMiBA was originally configured as a 7-element
512:on the sky), as well as observing the thermal
422:AMiBA was initially configured as a 7-element
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611:Institute of Astronomy and Astrophysics, the
395:Institute of Astronomy and Astrophysics, the
1095:Cosmic microwave background radiation (CMB)
621:Harvard-Smithsonian Center for Astrophysics
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16:Radio telescope on Mauna Loa, Hawaii
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657:List of astronomical observatories
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939:American Astronomical Society
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430:dishes mounted on a 6 m
418:The rear of the hexapod mount
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1301:Arcminute Microkelvin Imager
849:10.1088/0004-637X/694/2/1643
723:10.1088/0004-637X/694/2/1610
470:Taiwan Ministry of Education
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1376:Mobile Anisotropy Telescope
1336:Cosmic Anisotropy Telescope
1296:Atacama Cosmology Telescope
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637:Nottingham Trent University
502:cosmic microwave background
445:The receivers are based on
352:cosmic microwave background
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1106:Discovery of CMB radiation
907:10.3847/0004-637X/830/2/91
645:Carnegie-Mellon University
613:National Taiwan University
397:National Taiwan University
367:Yuan-Tseh Lee Array (YTLA)
173:radio interferometer
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876:The Astrophysical Journal
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1147:Sunyaev–Zeldovich effect
781:Modern Physics Letters A
474:National Science Council
449:(MMIC) technology, with
350:designed to observe the
316:Related media on Commons
120:3 mm (100 GHz)
81:19.536194°N 155.575278°W
419:
86:19.536194; -155.575278
633:University of Bristol
426:, using 0.576 m
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1421:South Pole Telescope
1165:image (2018) of the
787:(17/20): 1243–1251.
629:University of Hawaii
451:low-noise amplifiers
360:clusters of galaxies
338:, also known as the
162:Telescope style
150:September 2006
1321:BICEP (1,2,3,Array)
1028:2014PASP..126..761J
990:casper.berkeley.edu
951:2016AAS...22742604B
898:2016ApJ...830...91L
841:2009ApJ...694.1643U
793:2008MPLA...23.1243H
715:2009ApJ...694.1610H
587:telescopes such as
463:system temperatures
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1416:Simons Observatory
1152:Thomson scattering
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1515:Outer space
1503:Spaceflight
1177:Experiments
478:first light
84: /
72:155°34′31″W
60:Coordinates
46:Location(s)
1561:Categories
1371:LSPE/STRIP
1366:Keck Array
1361:GroundBIRD
1351:COSMOSOMAS
1245:LSPE/SWIPE
995:29 January
971:1709.09066
945:: 426.04.
889:1605.09261
663:References
599:antennas.
510:arcminutes
506:multipoles
428:Cassegrain
116:Wavelength
69:19°32′10″N
1567:Mauna Loa
1539:Education
1479:Astronomy
1411:Saskatoon
1386:POLARBEAR
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374:Mauna Loa
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132:2000–2006
128:2000–2006
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1230:Archeops
1209:RELIKT-1
1197:LiteBIRD
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534:2163
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