General FAQs

The LMT has a 50 meter active primary surface.

Telescope gain is flat between 20 and 85 degrees of elevation. Atmospheric opacity is likely the main limiting factor at elevations below 30 degrees, especially in the 1mm window. The limit for physical obstruction of low-elevation sources is around 10 degrees.

The current suite of LMT instrumentation includes four heterodyne receivers: SEQUOIA, Redshift Search Receiver (RSR), B4R, and MSIP1mm, as well as the TolTEC continuum camera.

An additional instrument, the OMAyA 1mm spectroscopic imaging array, is in development.

Manuals and time calculators for each instrument can be found on the Hedwig Proposal System.

At the moment, the Sun avoidance angle of the LMT is 20 degrees.

Pointing models are constructed by observing radio sources over the entire sky and then using those measurements to determine a number of physical parameters about the antenna structure, such as tilt of the azimuth axis with respect to zenith, non-orthogonality of the azimuth and elevation axis, and collimation of the radio beam with the axis of symmetry of the parabolic dish. The goal is to remove antenna pointing errors caused by these structural misalignments.

No, the LMT cannot support a K-band receiver.

We do not yet have enough information to know if anomalous refraction effects are present.

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