MTR2 is made of a predispersor (“SP1” first one on the left part), forming a low resolution spectrum on the wavelength selector (so called the “mask plate”). From there, only the selected bandwiths travel to the high-resolution echelle spectrograph (right part), ending over the MTR cameras at the SP2 output (one bandwith per camera).

The optical layout along Y is fixed (no changes, never). The ruling of the gratings are along Y only and the dispersion of both spectra is along Z only. The entrance slit is fixed (but for its width), and such are the collimators and camera mirrors.

The moving parts are:

• The predisperser gratings selection table (EM35). There are 3 selectable predispersers, although only one (the central slot) is mainly used for MTR2 operation.
• PThe predisperser rotates about the Y axis to change its grating incidence angle (EM37). This allows shifting the lowres spectrum along Z over the masks stop plate.
• The mask plate translates in the Z direction (EM39)

  • The echelle grating rotates about the Y axis to change its grating incidence angle a (EM32). This allows shifting the highres spectrum along Z at the SP2 output.
• The legacy “DPSM engage” mirror (EM71, “out” in normal operation.
• Each of the 4 spectrograph mirrors has a mechanical shutter (EM50 to EM53)

In short:

1. The main optical layout (F2 to SP2) is static and does not require changes for daily operation.
2. Spectral configuration of the multi-line is obtained using:

   • both gratings rotation
   • masks plate tuning in translation
   • manual setup of the spectral cameras at the SP2 output

Data and formulae for the MTR2 can be found in the following document:
THEMIS spectrograph (auth: CLM)

These tools allow the observer to quick check the feasibility of a setup

• MTR spectrograph simulator (java web version / auth: CLM)
• MTR spectrograph simulator (Downloadable excel version / auth: CLM)
  Please enable macros to get a correct result.

Observers can also check the list of existing available mask plates to have an idea of readily available combination.

• Solar spectrum (3800 to 8700 Å with identified lines)
• Solar lines (2935 to 8770 Å, Moore & Minaert (M&M), NIST)
• Solar spectrum (BASS2000 interactive plot)
• Solar spectrum (Astrosurf: interactive 2d with M&M identification)