Principal investigators are encouraged to contact Sylvain Veilleux with any questions/concerns that they may have about the feasibility of their project before submitting their proposal.

• Large field of view (27' diameter, ~10' monochromatic)
• High emission-line sensitivity to point sources or filamentary structure (DIQ ~ 0.7'')
• Versatility in choice of emission lines, within the range of ~5000-9200Å
• Narrow bandpass, reducing sky noise
• Accurate continuum subtraction (off-band wavelength can be chosen to be arbitrarily close to on-band wavelength)

• Observations in bright moon conditions: Scattered light can make MMTF data very difficult to reduce; we recommend requesting at least grey time.
• Multiple (> 2) filter switches per night: Each filter used requires a careful wavelength calibration during the daytime (~1 hour each). Changing filters in the middle of the night adds an overhead of 15-30 minutes.
• Observation of structureless, extended emission/absorption-line sources: One of the key strengths of the MMTF is its location at Las Campanas, Chile. This site consistently produces seeing of 0.6-0.8'', providing excellent sensitivity to point source and filamentary emission.

• Are your exposure times long enough to achieve sufficient sensitivity for your targets? Consult the filter-dependent sensitivity measurements in order to determine an adequate exposure time.
• Have you accounted properly for overheads? Typically, you will need to check the parallelism every time you move the telescope by a sizeable amount (5-15 min) and the wavelength calibration every 30-60 mins (~5 min).
• Are all of the desired emission-line wavelengths observable? Be sure to also check the continuum wavelength (if desired)!
  (MMTF Transmission Calculator)
• Have you considered wavelength slicing? If your target covers a range in velocity or is larger than the monochromatic spot, you may have to plan for exposures at multiple wavelength in order to capture all line emission.