Next:
Introduction
ALMA Scientific Advisory Committee Active Observers
Introduction
ALMA Liaison Group Issues
Receivers
System
Configurations
Antennas and Total Power
Water-Vapor Radiometry
Future Issues
Summary
The ASAC Charter
ASAC Liaison to Working Groups
Polarization Observations With ALMA
INTRODUCTION
POLARIZATION SCIENCE
REQUIREMENTS
Sensitivity
Fourier sampling
Accuracy
MEETING THE SCIENCE REQUIREMENTS
Instrumental polarization issues
Calibration issues
RECOMMENDATIONS
Total Power Observing with the ALMA Antennas
Introduction
Candidate Schemes
OTF Mapping
Summary
183GHz Water Vapour Radiometers for ALMA
Introduction
Status of current 183 GHz phase correction experiments
Design Considerations for the ALMA water vapour monitors
Requirements
Basic technical approach
Mixer or HFET?
Cooled or uncooled?
SIS
Cooled Schottky
Form of switching
Form of backend
Local Oscillator
Beam Offsets
Conclusions
An Infrared Water Vapour Monitor for the Correction of Phase Errors in Submillimetre Astronomical Interferometry
Features of an infrared system (IWVM) for monitoring atmospheric water vapour content
Description of Infrared Water Vapour Monitor (IWVM)
Theoretical calculation of radiant power emitted by atmospheric water vapour in the 20
m band above Mauna Kea
Preliminary discussion of results from Dec 1999 run
Areas of improvement
Future plans
addendum: A comparison of the IWVM and 183 GHz WVR sensitivities (by C. Wilson)
Rationale for Band 1 (31.3-45 GHz) Receivers on ALMA
Cost
Sensitivity of the Band 1 - Incredible
Comparisons with other telescopes
Impact on sensitivity to other ALMA bands - None!
Test phase of ALMA and debugging
Science
Sunyaev-Zel'dovich Effect and secondary CMB anisotropy
Community support
About this document ...
Al Wootten
2000-04-04
m band above Mauna Kea