A Characterization of the ALMA Phasing System at 345 GHz

a study on construction of iranian life tables: the case study of modified brass logit system

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LAMA Memo 805 ALMA Calibration Source Counts at 250 GHz

Quasar source counts at millimeter and sub-millimeter wavelengths will be important for phase and delay calibration as well as focus and pointing observations. Some of these observations can be done at low frequencies, but some observations will need to be done at the target frequency. Having a good knowledge of the high frequency quasar source counts will help us with the ALMA calibration plan...

Issues for the 30-45.5 GHz band on ALMA

ALMA Memo 585 Loss of Gold Plated Waveguides at 210-280 GHz

The loss at 210-280 GHz of room temperature waveguides plated with BDT 200 bright gold and Pur-A-Gold 125 soft gold is within ~10% of the theoretical loss based on the DC conductivity of pure gold and the classical skin effect. This is not the case for some other types of gold plating meeting the same ASTM (or MIL) specs but in which a trace of nickel is used as a brightener. Introduction Follo...

The ALMA Telescope Control System

The Atacama Large Millimeter Array (ALMA) is a joint project between North America, Europe and Japan. ALMA is an aperture synthesis radio telescope consisting of 50 12-meter antennas located at an elevation of 5,000 meters in Llano de Chajnantor, Chile. These antennas will operate at frequencies ranging from 31.3 GHz to 950 GHz. The antennas can be moved and placed in different configurations, ...