MAROON-X: A radial velocity spectrograph to identify habitable worlds

Status: (01/11/2019) The science grade detector systems, which were the final remaining components, have been delivered to U. Chicago and are being integrated with the spectrograph in the lab. The front-end unit was commissioned on the Gemini-N telescope in December 2018, and the environmental control chamber was installed in the telescope pier lab in July 2018. First stability tests using the core spectrograph, blue arm, and an engineering grade detector indicate that precisions <<1 m/s can be obtained with the simultaneous reference technique and our etalon calibrator. We are on schedule to ship the spectrograph to Hawaii in March with commissioning to follow soon afterwards.

See our SPIE 2016 and SPIE 2018 papers for more detailed discussion of the design and construction of MAROON-X.

Project description:
We aim to build a new instrument with the capability to detect Earth-size planets in the habitable zones of mid- to late-M dwarfs using the radial velocity method. The instrument will be a high-resolution, bench-mounted spectrograph capable of delivering 1 m/s radial velocity precision for M dwarfs down to and beyond V = 16. It will be installed on the Gemini North telescope located on Mauna Kea in Hawaii. The capability that this instrument will have is well beyond the reach of any existing instrument. The anticipated uses for the instrument are to (1) conduct a radial velocity only survey for potentially habitable planets around nearby mid- to late-M dwarfs and (2) to confirm and measure the masses of low-mass planet candidates identified in the habitable zones of M dwarfs by ground- and space-based transit surveys. These later objects will be the best objects for future atmospheric studies of potentially habitable planets.

The main constraint for the instrument is set by the desired wavelength coverage. The important wavelength range for the instrument is 700 -- 900 nm because this is the region containing the maximum radial velocity information for mid to late M dwarfs. There is no gas cell useful for this region, so the instrument must be intrinsically stable to deliver the desired radial velocity precision. This means that the optical setup must be fixed and that the entire instrument must be in a vacuum tank and in a temperature stabilized enclosure. The instrument must also be fiber-fed to maintain illumination stability. A resolving power of approximately 80,000 is necessary. A similar setup can not be realized by making straightforward modifications to existing instruments - a new instrument must be built to achieve the radial velocity precision goal for the target stars.

First light in the lab September 2016