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Patrick M. Koch
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Cosmology and Nongalactic Astrophysics (19)
 
Astrophysics of Galaxies (17)
 
Instrumentation and Methods for Astrophysics (13)
 
Solar and Stellar Astrophysics (8)
 
Astrophysics (4)
 
Statistics - Machine Learning (1)
 
Earth and Planetary Astrophysics (1)
 
High Energy Astrophysical Phenomena (1)
 
Physics - Fluid Dynamics (1)

Publications Authored By Patrick M. Koch

2017Apr
Authors: Derek Ward-Thompson, Kate Pattle, Pierre Bastien, Ray S. Furuya, Woojin Kwon, Shih-Ping Lai, Keping Qiu, David Berry, Minho Choi, Simon Coudé, James Di Francesco, Thiem Hoang, Erica Franzmann, Per Friberg, Sarah F. Graves, Jane S. Greaves, Martin Houde, Doug Johnstone, Jason M. Kirk, Patrick M. Koch, Jungmi Kwon, Chang Won Lee, Di Li, Brenda C. Matthews, Joseph C. Mottram, Harriet Parsons, Andy Pon, Ramprasad Rao, Mark Rawlings, Hiroko Shinnaga, Sarah Sadavoy, Sven van Loo, Yusuke Aso, Do-Young Byun, Eswariah Chakali, Huei-Ru Chen, Mike C. -Y. Chen, Wen Ping Chen, Tao-Chung Ching, Jungyeon Cho, Antonio Chrysostomou, Eun Jung Chung, Yasuo Doi, Emily Drabek-Maunder, Stewart P. S. Eyres, Jason Fiege, Rachel K. Friesen, Gary Fuller, Tim Gledhill, Matt J. Griffin, Qilao Gu, Tetsuo Hasegawa, Jennifer Hatchell, Saeko S. Hayashi, Wayne Holland, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Ji-hyun Kang, Miju Kang, Sung-ju Kang, Koji S. Kawabata, Francisca Kemper, Gwanjeong Kim, Jongsoo Kim, Kee-Tae Kim, Kyoung Hee Kim, Mi-Ryang Kim, Shinyoung Kim, Kevin M. Lacaille, Jeong-Eun Lee, Sang-Sung Lee, Dalei Li, Hua-bai Li, Hong-Li Liu, Junhao Liu, Sheng-Yuan Liu, Tie Liu, A-Ran Lyo, Steve Mairs, Masafumi Matsumura, Gerald H. Moriarty-Schieven, Fumitaka Nakamura, Hiroyuki Nakanishi, Nagayoshi Ohashi, Takashi Onaka, Nicolas Peretto, Tae-Soo Pyo, Lei Qian, Brendan Retter, John Richer, Andrew Rigby, Jean-François Robitaille, Giorgio Savini, Anna M. M. Scaife, Archana Soam, Motohide Tamura, Ya-Wen Tang, Kohji Tomisaka, Hongchi Wang, Jia-Wei Wang, Anthony P. Whitworth, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Chuan-Peng Zhang, Guoyin Zhang, Jianjun Zhou, Lei Zhu, Philippe André, C. Darren Dowell, Sam Falle, Yusuke Tsukamoto

We present the first results from the B-fields In STar-forming Region Observations (BISTRO) survey, using the Sub-millimetre Common-User Bolometer Array 2 (SCUBA-2) camera, with its associated polarimeter (POL-2), on the James Clerk Maxwell Telescope (JCMT) in Hawaii. We discuss the survey's aims and objectives. We describe the rationale behind the survey, and the questions which the survey will aim to answer. Read More

We present a joint analysis of Chandra X-ray observations, Bolocam thermal Sunyaev-Zel'dovich (SZ) effect observations, Hubble Space Telescope (HST) strong lensing data, and HST and Subaru Suprime-Cam weak lensing data. The multiwavelength dataset is used to constrain parametric models for the distribution of dark and baryonic matter in a sample of six massive galaxy clusters selected from the Cluster Lensing And Supernova survey with Hubble (CLASH). For five of the six clusters, the multiwavelength dataset is well described by a relatively simple model that assumes spherical symmetry, hydrostatic equilibrium, and entirely thermal pressure support. Read More

2016Dec
Affiliations: 1ASIAA Hilo Office, 2Academia Sinica Institute of Astronomy & Astrophysics, 3Academia Sinica Institute of Astronomy & Astrophysics, 4Harvard-Smithsonian Center for Astrophysics, 5ASIAA Hilo Office, 6Harvard-Smithsonian Center for Astrophysics, 7Academia Sinica Institute of Astronomy & Astrophysics, 8Academia Sinica Institute of Astronomy & Astrophysics, 9Academia Sinica Institute of Astronomy & Astrophysics, 10Harvard-Smithsonian Center for Astrophysics, 11Academia Sinica Institute of Astronomy & Astrophysics, 12Academia Sinica Institute of Astronomy & Astrophysics, 13Academia Sinica Institute of Astronomy & Astrophysics, 14National Chung-Shan Institute of Science and Technology, 15Academia Sinica Institute of Astronomy & Astrophysics, 16Academia Sinica Institute of Astronomy & Astrophysics, 17ASIAA Hilo Office, 18Harvard-Smithsonian Center for Astrophysics, 19Academia Sinica Institute of Astronomy & Astrophysics, 20National Chung-Shan Institute of Science and Technology, 21Academia Sinica Institute of Astronomy & Astrophysics, 22Academia Sinica Institute of Astronomy & Astrophysics, 23Academia Sinica Institute of Astronomy & Astrophysics, 24Academia Sinica Institute of Astronomy & Astrophysics, 25Academia Sinica Institute of Astronomy & Astrophysics, 26Academia Sinica Institute of Astronomy & Astrophysics, 27Harvard-Smithsonian Center for Astrophysics, 28Academia Sinica Institute of Astronomy & Astrophysics, 29Harvard-Smithsonian Center for Astrophysics, 30Harvard-Smithsonian Center for Astrophysics, 31Academia Sinica Institute of Astronomy & Astrophysics, 32ASIAA Hilo Office, 33Harvard-Smithsonian Center for Astrophysics, 34ASIAA Hilo Office

Since the ALMA North America Prototype Antenna was awarded to the Smithsonian Astrophysical Observatory (SAO), SAO and the Academia Sinica Institute of Astronomy & Astrophysics (ASIAA) are working jointly to relocate the antenna to Greenland. This paper shows the status of the antenna retrofit and the work carried out after the recommissioning and subsequent disassembly of the antenna at the VLA has taken place. The next coming months will see the start of the antenna reassembly at Thule Air Base. Read More

The Atacama Large Millimeter/submillimeter Array(ALMA) Band 1 receiver covers the 35-50 GHz frequency band. Development of prototype receivers, including the key components and subsystems has been completed and two sets of prototype receivers were fully tested. We will provide an overview of the ALMA Band 1 science goals, and its requirements and design for use on the ALMA. Read More

We present ALMA 1.3 mm continuum, 12CO, C18O, and SO data for the Class 0 protostars, Lupus 3 MMS, IRAS 15398-3559, and IRAS 16253-2429 at resolutions of ~100 AU. By measuring a rotational profile in C18O, a 100 AU Keplerian disk around a 0. Read More

2016Nov
Affiliations: 1Academia Sinica Institute of Astronomy and Astrophysics, 2Academia Sinica Institute of Astronomy and Astrophysics, 3Academia Sinica Institute of Astronomy and Astrophysics, 4Academia Sinica Institute of Astronomy and Astrophysics, 5Academia Sinica Institute of Astronomy and Astrophysics, 6Academia Sinica Institute of Astronomy and Astrophysics, 7Academia Sinica Institute of Astronomy and Astrophysics, 8Harvard-Smithsonian Center for Astrophysics, 9National Oceanic and Atmospheric Administration

We present the 3.5-yr monitoring results of 225 GHz opacity at the summit of the Greenland ice sheet (Greenland Summit Camp) at an altitude of 3200 m using a tipping radiometer. We chose this site as our submillimeter telescope (Greenland Telescope; GLT) site, because its location offers favorable baselines to existing submillimeter telescopes for global-scale VLBI. Read More

We introduce a new stacking method in Keplerian disks that (1) enhances signal-to-noise ratios (S/N) of detected molecular lines and (2) that makes visible otherwise undetectable weak lines. Our technique takes advantage of the Keplerian rotational velocity pattern. It aligns spectra according to their different centroid velocities at their different positions in a disk and stacks them. Read More

We report a new 1-pc (30") resolution CS($J=2-1$) line map of the central 30 pc of the Galactic Center (GC), made with the Nobeyama 45m telescope. We revisit our previous study of the extraplanar feature called polar arc (PA), which is a molecular cloud located above SgrA* with a velocity gradient perpendicular to the Galactic plane. We find that the PA can be traced back to the Galactic disk. Read More

We conducted IRAM-30m C18O (2-1) and SMA 1.3mm continuum, 12CO (2-1), and C18O (2-1) observations toward the Class 0/I protostar L1455 IRS1 in Perseus. The IRAM results show L1455 IRS1 located in a dense core of 0. Read More

We highlight distinct and systematic observational features of magnetic field morphologies in polarized submm dust continuum. We illustrate this with specific examples and show statistical trends from a sample of 50 star-forming regions. Read More

We have conducted ALMA cycle 2 observations in the 1.3 mm continuum and in the C18O (2-1) and SO (5_6-4_5) lines at a resolution of ~0.3" toward the Class 0 protostar B335. Read More

We perform imaging and analyses of SMA 1.3 mm continuum, C18O (2-1) and 12CO (2-1) line data of 17 Class 0 and 0/I protostars to study their gas kinematics on a 1,000-AU scale. Continuum and C18O (2-1) emission are detected toward all the sample sources and show central primary components with sizes of ~600-1,500 AU associated with protostars. Read More

Submillimeter dust polarization measurements of a sample of 50 star-forming regions, observed with the SMA and the CSO covering pc-scale clouds to mpc-scale cores, are analyzed in order to quantify the magnetic field importance. The magnetic field misalignment $\delta$ -- the local angle between magnetic field and dust emission gradient -- is found to be a prime observable, revealing distinct distributions for sources where the magnetic field is preferentially aligned with or perpendicular to the source minor axis. Source-averaged misalignment angles $\langle|\delta|\rangle$ fall into systematically different ranges, reflecting the different source-magnetic field configurations. Read More

The ALMA North America Prototype Antenna was awarded to the Smithsonian Astrophysical Observatory (SAO) in 2011. SAO and the Academia Sinica Institute of Astronomy & Astrophysics (ASIAA), SAO's main partner for this project, are working jointly to relocate the antenna to Greenland to carry out millimeter and submillimeter VLBI observations. This paper presents the work carried out on upgrading the antenna to enable operation in the Arctic climate by the GLT Team to make this challenging project possible, with an emphasis on the unexpected telescope components that had to be either redesigned or changed. Read More

Massive stars ($M > 8$ \msun) typically form in parsec-scale molecular clumps that collapse and fragment, leading to the birth of a cluster of stellar objects. We investigate the role of magnetic fields in this process through dust polarization at 870 $\mu$m obtained with the Submillimeter Array (SMA). The SMA observations reveal polarization at scales of $\lsim$ 0. Read More

We report our analysis of MACS J0717.5+3745 using 140 and 268 GHz Bolocam data collected at the Caltech Submillimeter Observatory. We detect extended Sunyaev-Zel'dovich (SZ) effect signal at high significance in both Bolocam bands, and we employ Herschel-SPIRE observations to subtract the signal from dusty background galaxies in the 268 GHz data. Read More

Dust polarization observations from the Submillimeter Array (SMA) and the Caltech Submillimeter Observatory (CSO) are analyzed with the goal of providing a general tool to interpret the role of the magnetic field in molecular clouds. Magnetic field and dust emission gradient orientations are observed to show distinct patterns and features. The angle $\delta$ between these two orientations can be interpreted as a magnetic field alignment deviation, assuming the emission gradient orientation to coincide with the density gradient orientation in the magnetohydrodynamics (MHD) force equation. Read More

We report the past two years of collaboration between the different actors on the ALMA nutator. Building on previous developments, the nutator has seen changes in much of the design. A high-modulus carbon fiber structure has been added on the back of the mirror in order to transfer the voice coils forces with less deformation, thus reducing delay problems due to flexing. Read More

We present a new way to solve the platform deformation problem of co-planar interferometers. The platform of a co-planar interferometer can be deformed due to driving forces and gravity. A deformed platform will induce extra components into the geometric delay of each baseline, and change the phases of observed visibilities. Read More

We present the first high-angular resolution (up to 0.7", ~5000 AU) polarization and thermal dust continuum images toward the massive star-forming region W51 North. The observations were carried out with the Submillimeter Array (SMA) in both the subcompact (SMA-SubC) and extended (SMA-Ext) configurations at a wavelength of 870 micron. Read More

We describe Sunyaev-Zel'dovich (SZ) effect measurements and analysis of the intracluster medium (ICM) pressure profiles of a set of 45 massive galaxy clusters imaged using Bolocam at the Caltech Submillimeter Observatory. We have used masses determined from Chandra X-ray observations to scale each cluster's profile by the overdensity radius R500 and the mass-and-redshift-dependent normalization factor P500. We deproject the average pressure profile of our sample into 13 logarithmically spaced radial bins between 0. Read More

We describe in detail our characterization of the compact radio source population in 140 GHz Bolocam observations of a set of 45 massive galaxy clusters. We use a combination of 1.4 and 30 GHz data to select a total of 28 probable cluster-member radio galaxies and also to predict their 140 GHz flux densities. Read More

Recent high-angular-resolution (up to 0.7") dust polarization observations toward star forming regions are summarized. With the Sub-Millimeter Array, the emission from the dense structures is traced and resolved. Read More

Dust polarization orientations in molecular clouds often tend to be close to tangential to the Stokes $I$ dust continuum emission contours. The magnetic field and the emission gradient orientations, therefore, show some correlation. A method is proposed, which -- in the framework of ideal magneto-hydrodynamics (MHD) -- connects the measured angle between magnetic field and emission gradient orientations to the total field strength. Read More

Dust polarization observational results are analyzed for the high-mass star formation region W51 from the largest parent cloud ($\sim$ 2~pc, JCMT) to the large-scale envelope ($\sim$ 0.5~pc, BIMA) down to the collapsing core e2 ($\sim$ 60~mpc, SMA). Magnetic field and dust emission gradient orientations reveal a correlation which becomes increasingly more tight with higher resolution. Read More

We present Bolocam observations of two galaxy cluster candidates reported as unconfirmed in the Planck early Sunyaev-Zel'dovich (eSZ) sample, PLCKESZ G115.71+17.52 and PLCKESZ G189. Read More

Interferometric millimeter observations of the cosmic microwave background and clusters of galaxies with arcmin resolutions require antenna arrays with short spacings. Having all antennas co-mounted on a single steerable platform sets limits to the overall weight. A 25 kg lightweight novel carbon-fiber design for a 1. Read More

2010Sep
Affiliations: 1Institute of Astronomy and Astrophysics, 2Institute of Astronomy and Astrophysics, 3H. H. Wills Physics Laboratory, University of Bristol, 4Department of Astronomy, Columbia University, 5Department of Astronomy, Columbia University, 6ASC/Alliances Center for Astrophysical Thermonuclear Flashes, University of Chicago, 7Institute of Astronomy and Astrophysics, 8Department of Physics, Institute of Astrophysics, and Center for Theoretical Sciences, National Taiwan University, 9Institute of Astronomy and Astrophysics, 10Institute of Astronomy and Astrophysics, 11Institute of Astronomy and Astrophysics, 12Institute of Astronomy and Astrophysics, 13Institute of Astronomy and Astrophysics, 14Department of Physics, Institute of Astrophysics, and Center for Theoretical Sciences, National Taiwan University, 15Department of Physics, Institute of Astrophysics, and Center for Theoretical Sciences, National Taiwan University

Clusters of galaxies have been used extensively to determine cosmological parameters. A major difficulty in making best use of Sunyaev-Zel'dovich (SZ) and X-ray observations of clusters for cosmology is that using X-ray observations it is difficult to measure the temperature distribution and therefore determine the density distribution in individual clusters of galaxies out to the virial radius. Observations with the new generation of SZ instruments are a promising alternative approach. Read More

Polarization data from high mass star formation regions (W51 e2/e8, Orion BN/KL) are used to derive statistical properties of the plane of sky projected magnetic field. Structure function and auto-correlation function are calculated for observations with various resolutions from the BIMA and SMA interferometers, covering a range in physical scales from $\sim 70$~mpc to $\sim 2.1$~mpc. Read More

2010Jun
Affiliations: 1Academia Sinica, Institute of Astronomy and Astrophysics, 2Academia Sinica, Institute of Astronomy and Astrophysics, 3Academia Sinica, Institute of Astronomy and Astrophysics, 4Academia Sinica, Institute of Astronomy and Astrophysics

We present observational results of the thermal dust continuum emission and its linear polarization in one of the nearest massive star-forming sites Orion BN/KL in Orion Molecular Cloud-1. The observations were carried out with the Submillimeter Array. With an angular resolution of 1" (~2 mpc; 480 AU), we have detected and resolved the densest cores near the BN/KL region. Read More

2010Mar
Affiliations: 1ASIAA, 2ASIAA, 3ATNF, 4ASIAA, 5ASIAA, 6ASIAA, 7ASIAA, 8ASIAA, 9ASIAA, 10ASIAA, 11ASIAA, 12ASIAA, 13ASIAA, 14ASIAA, 15National Taiwan University, 16National Taiwan University, 17National Taiwan University, 18National Taiwan University, 19National Taiwan University, 20Carnegie-Mellon University, 21ASIAA, 22ASIAA, 23ASIAA, 24ATNF, 25ASIAA, 26ASIAA, 27ASIAA, 28ASIAA, 29ASIAA, 30National Taiwan University

A wideband analog correlator has been constructed for the Yuan-Tseh Lee Array for Microwave Background Anisotropy. Lag correlators using analog multipliers provide large bandwidth and moderate frequency resolution. Broadband IF distribution, backend signal processing and control are described. Read More

2010Mar
Affiliations: 1Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 2Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 3Institute of Astronomy and Astrophysics, Academia Sinica, 4Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 5Institute of Astronomy and Astrophysics, Academia Sinica, 6Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 7Institute of Astronomy and Astrophysics, Academia Sinica, 8Institute of Astronomy and Astrophysics, Academia Sinica, 9Institute of Astronomy and Astrophysics, Academia Sinica, 10Institute of Astronomy and Astrophysics, Academia Sinica, 11Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 12Institute of Astronomy and Astrophysics, Academia Sinica, 13Department of Physics, University of Bristol, 14Institute of Astronomy and Astrophysics, Academia Sinica, 15Institute of Astronomy and Astrophysics, Academia Sinica, 16Institute of Astronomy and Astrophysics, Academia Sinica, 17Institute of Astronomy and Astrophysics, Academia Sinica, 18Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 19Institute of Astronomy and Astrophysics, Academia Sinica, 20Institute of Astronomy and Astrophysics, Academia Sinica, 21Institute of Astronomy and Astrophysics, Academia Sinica, 22Institute of Astronomy and Astrophysics, Academia Sinica, 23Australia Telescope National Facility, 24Institute of Astronomy and Astrophysics, Academia Sinica, 25Institute of Astronomy and Astrophysics, Academia Sinica, 26Institute of Astronomy and Astrophysics, Academia Sinica, 27Institute of Astronomy and Astrophysics, Academia Sinica, 28Institute of Astronomy and Astrophysics, Academia Sinica, 29Institute of Astronomy and Astrophysics, Academia Sinica, 30Australia Telescope National Facility

The Sunyaev-Zel'dovich Effect (SZE) has been observed toward six massive galaxy clusters, at redshifts 0.091 \leq z \leq 0.322 in the 86-102 GHz band with the Y. Read More

Slow feature analysis (SFA) is a method for extracting slowly varying driving forces from quickly varying nonstationary time series. We show here that it is possible for SFA to detect a component which is even slower than the driving force itself (e.g. Read More

2009Nov
Affiliations: 1Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 2Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 3Institute of Astronomy and Astrophysics, Academia Sinica, 4Institute of Astronomy and Astrophysics, Academia Sinica, 5Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 6Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 7Institute of Astronomy and Astrophysics, Academia Sinica, 8Institute of Astronomy and Astrophysics, Academia Sinica, 9Institute of Astronomy and Astrophysics, Academia Sinica, 10LeCosPA Center, National Taiwan University, 11Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 12Institute of Astronomy and Astrophysics, Academia Sinica, 13Department of Physics, University of Bristol, 14Institute of Astronomy and Astrophysics, Academia Sinica, 15Institute of Astronomy and Astrophysics, Academia Sinica, 16Institute of Astronomy and Astrophysics, Academia Sinica, 17Institute of Astronomy and Astrophysics, Academia Sinica, 18Department of Physics, Institute of Astrophysics, & Center for Theoretical Sciences, National Taiwan University, 19Institute of Astronomy and Astrophysics, Academia Sinica, 20Institute of Astronomy and Astrophysics, Academia Sinica, 21Institute of Astronomy and Astrophysics, Academia Sinica, 22Institute of Astronomy and Astrophysics, Academia Sinica, 23Australia Telescope National Facility, 24Institute of Astronomy and Astrophysics, Academia Sinica, 25Institute of Astronomy and Astrophysics, Academia Sinica, 26Institute of Astronomy and Astrophysics, Academia Sinica, 27Institute of Astronomy and Astrophysics, Academia Sinica, 28Institute of Astronomy and Astrophysics, Academia Sinica, 29Institute of Astronomy and Astrophysics, Academia Sinica, 30Australia Telescope National Facility

We investigate the scaling relations between the X-ray and the thermal Sunyaev-Zel'dovich Effect (SZE) properties of clusters of galaxies, using data taken during 2007 by the Y.T. Lee Array for Microwave Background Anisotropy (AMiBA) at 94 GHz for the six clusters A1689, A1995, A2142, A2163, A2261, and A2390. Read More

We report our observational results of 870 $\mu$m continuum emission and its linear polarization in the massive star formation site W51 e2/e8. Inferred from the linear polarization maps, the magnetic field in the plane of sky (B$_{\bot}$) is traced with an angular resolution of 0$\farcs$7 with the Submillimeter Array (SMA). Whereas previous BIMA observations with an angular resolution of 3$\arcsec$ (0. Read More

2009Feb
Affiliations: 1ASIAA, Taiwan, 2ASIAA, Taiwan, 3ASIAA, Taiwan, 4ASIAA, Taiwan, 5ASIAA, Taiwan, 6ASIAA, Taiwan, 7ASIAA, Taiwan, 8ASIAA, Taiwan, 9NTU, Taiwan, 10NTU, Taiwan, 11ASIAA, Taiwan, 12ASIAA, Taiwan, 13ATNF, 14ASIAA, Taiwan, 15ASIAA, Taiwan, 16ASIAA, Taiwan, 17ASIAA, Taiwan, 18ASIAA, Taiwan, 19NTU, Taiwan, 20ATNF, 21ASIAA, Taiwan, 22NTU, Taiwan, 23ASIAA, Taiwan, 24NTU, Taiwan, 25ASIAA, Taiwan, 26ASIAA, Taiwan, 27ASIAA, Taiwan, 28ASIAA, Taiwan, 29ASIAA, Taiwan, 30NTU, Taiwan, 31NTU, Taiwan

The Y. T. Lee Array for Microwave Background (AMiBA) has reported the first science results on the detection of galaxy clusters via the Sunyaev Zel'dovich effect. Read More

2009Feb
Affiliations: 1Academia Sinica, Institute of Astronomy and Astrophysics, 2Australia Telescope National Facility, 3Academia Sinica, Institute of Astronomy and Astrophysics, 4Academia Sinica, Institute of Astronomy and Astrophysics, 5Academia Sinica, Institute of Astronomy and Astrophysics, 6Academia Sinica, Institute of Astronomy and Astrophysics, 7Academia Sinica, Institute of Astronomy and Astrophysics, 8Academia Sinica, Institute of Astronomy and Astrophysics, 9Academia Sinica, Institute of Astronomy and Astrophysics, 10Academia Sinica, Institute of Astronomy and Astrophysics, 11Academia Sinica, Institute of Astronomy and Astrophysics, 12Department of Physics, Institute of Astrophysics and Center for Theoretical Sciences, National Taiwan University, 13Academia Sinica, Institute of Astronomy and Astrophysics, 14Academia Sinica, Institute of Astronomy and Astrophysics, 15Vertex Antennentechnik GmbH, 16Vertex Antennentechnik GmbH, 17Academia Sinica, Institute of Astronomy and Astrophysics, 18Academia Sinica, Institute of Astronomy and Astrophysics, 19Academia Sinica, Institute of Astronomy and Astrophysics, 20Academia Sinica, Institute of Astronomy and Astrophysics, 21Academia Sinica, Institute of Astronomy and Astrophysics, 22Academia Sinica, Institute of Astronomy and Astrophysics, 23Academia Sinica, Institute of Astronomy and Astrophysics, 24Department of Physics, Institute of Astrophysics and Center for Theoretical Sciences, National Taiwan University, 25Academia Sinica, Institute of Astronomy and Astrophysics, 26Academia Sinica, Institute of Astronomy and Astrophysics, 27Academia Sinica, Institute of Astronomy and Astrophysics, 28Department of Physics, Institute of Astrophysics and Center for Theoretical Sciences, National Taiwan University, 29Academia Sinica, Institute of Astronomy and Astrophysics, 30Department of Physics, Institute of Astrophysics and Center for Theoretical Sciences, National Taiwan University, 31Department of Physics, University of Bristol, 32Department of Physics, Institute of Astrophysics and Center for Theoretical Sciences, National Taiwan University, 33Department of Physics, University of Bristol, 34National Radio Astronomy Observatory, 35CMA, 36Academia Sinica, Institute of Astronomy and Astrophysics, 37ESO Headquarters Garching, 38CMA

AMiBA is the largest hexapod astronomical telescope in current operation. We present a description of this novel hexapod mount with its main mechanical components -- the support cone, universal joints, jack screws, and platform -- and outline the control system with the pointing model and the operating modes that are supported. The AMiBA hexapod mount performance is verified based on optical pointing tests and platform photogrammetry measurements. Read More

We report high angular resolution (3") Submillimeter Array (SMA) observations of the molecular cloud associated with the Ultra-Compact HII region G5.89-0.39. Read More

2008Nov
Affiliations: 1ASIAA, 2NTU, 3NTU, 4ASIAA, 5NTU, 6ASIAA, 7NTU, 8ASIAA, 9ASIAA, 10ASIAA, 11ASIAA, 12Univ. of Bristol, 13ASIAA, 14ASIAA, 15ASIAA, 16ASIAA, 17ASIAA, 18ASIAA, 19ASIAA, 20ASIAA, 21ASIAA, 22ATNF, 23ASIAA, 24ASIAA, 25ASIAA, 26ASIAA, 27ASIAA, 28ASIAA, 29ATNF
Category: Astrophysics

We describe methods used to validate data from the Y.T. Lee Array for Microwave Background Anisotropy (AMiBA), an interferometric array designed to measure the Sunyaev-Zel'dovich effect and the anisotropy of the Cosmic Microwave Background (CMB). Read More

2008Oct
Affiliations: 1ASIAA, 2U. Bristol, 3ASIAA, 4, NTU, 5Tel Aviv U, 6Tel Aviv U, 7Tel Aviv U, 8Tel Aviv U, 9ASIAA, 10, NTU, 11ASIAA, 12, NTU, 13ASIAA, 14ASIAA, 15ASIAA, 16, NTU, 17ASIAA, 18ASIAA, 19ASIAA, 20ASIAA, 21ASIAA, 22ASIAA, 23ASIAA, 24ASIAA, 25ASIAA, 26ATNF, 27ASIAA, 28ASIAA, 29ASIAA, 30ASIAA, 31ASIAA, 32ASIAA, 33ATNF
Category: Astrophysics

We present a multiwavelength analysis of a sample of four hot (T_X>8keV) X-ray galaxy clusters (A1689, A2261, A2142, and A2390) using joint AMiBA Sunyaev-Zel'dovich effect (SZE) and Subaru weak lensing observations, combined with published X-ray temperatures, to examine the distribution of mass and the intracluster medium (ICM) in massive cluster environments. Our observations show that A2261 is very similar to A1689 in terms of lensing properties. Many tangential arcs are visible around A2261, with an effective Einstein radius \sim 40 arcsec (at z \sim 1. Read More