At least 50 antennas of 12 m diameter located at an elevation of 5,000 m at Llano de Chajnantor Observatory, enhanced by a compact array of 4 x 12 m and 12 x 7 m antennas (consortium currently considering to build 50 or 64 After a Tough Year, ALMA's Star Begins to Rise at Last High and dry)
Imaging instrument in all atmospheric windows between 350 μm and 10 mm
Array configurations from approximately 150 m to 14 km
Spatial resolution of 10 milliarcseconds (10⁻⁷ radians), 10 times better than the Very Large Array (VLA) and 5 times better than the Hubble Space Telescope, but still considerably lower than the resolution achieved with optical and infrared interferometers.

The ability to image sources arcminutes to degrees across at one arcsecond resolution
Velocity resolution under 50 m/s
Faster and more flexible imaging instrument than the Very Large Array
Largest and most sensitive instrument in the world at millimeter and submillimeter wavelengths
Point source detection sensitivity 20 times better than the Very Large Array
Data reduction system will be CASA (Common Astronomy Software Applications) which is a new software package based on AIPS++
At least 50 antennas of 12 m diameter located at an elevation of 5,000 m at Llano de Chajnantor Observatory, enhanced by a compact array of 4 x 12 m and 12 x 7 m antennas (consortium currently considering to build 50 or 64 After a Tough Year, ALMA's Star Begins to Rise at Last High and dry)
Imaging instrument in all atmospheric windows between 350 μm and 10 mm
Array configurations from approximately 150 m to 14 km
Spatial resolution of 10 milliarcseconds (10⁻⁷ radians), 10 times better than the Very Large Array (VLA) and 5 times better than the Hubble Space Telescope, but still considerably lower than the resolution achieved with optical and infrared interferometers.
The ability to image sources arcminutes to degrees across at one arcsecond resolution
Velocity resolution under 50 m/s
Faster and more flexible imaging instrument than the Very Large Array
Largest and most sensitive instrument in the world at millimeter and submillimeter wavelengths
Point source detection sensitivity 20 times better than the Very Large Array
Data reduction system will be CASA (Common Astronomy Software Applications) which is a new software package based on AIPS++
Atacama Large Millimeter Array