KPF Modes and Instrument Properties

The Keck Planet Finder (KPF) is a fiber-fed, high-resolution, high-stability cross dispersed, spectrometer designed to characterize exoplanets via Doppler spectroscopy with a goal of a single measurement precision of 0.3 m/s or better. KPF covers a wavelength range of 440nm to 590nm in the green channel and 590nm to 870nm in the red channel.

KPF consists of 3 independant spectrographs:

The primary science spectrograph described above is designed to be highly stable and has both a green and a red arm. The spectrograph optical bench is made from low expansion Zerodur and is kept is a temperature stabilized environment. The detectors are 4kx4k with 15 um pixels. Resolving power is over 80,000.
A Calcium H&K spectrograph (official documentation to be written) which gets the light blueward of the main science spectrograph and is used to simultaneously measure stellar activity using the Ca H&K lines.
The exposure meter spectrograph (official documentation to be written) which gets a portion of the science light and is used to measure the flux level during long exposures of the primary science detectors. The exposure meter both measures the time weighted flux midpoint of each exposure, and can also be used to terminate an exposure at a specified flux level.

All three spectrographs are fed by optical fiber from the Fiber Injection Unit (FIU) which sits on the Keck I AO bench. The light entering the FIU is not AO corrected, but is fed off a fast tip tilt mirror which is used to maintain the target star's position on the science fiber within 50 mas rms of the fiber center.

More information can be on the KPF WMKO home page.

Please acknowledge the use of KOA by including this text in your publications:

This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration.

Please also acknowledge the PI(s) of datasets that have been obtained through KOA, and please contact the KOA Help Desk if you publish archival data.

If your research uses data reduced by the DEIMOS DRP or MOSFIRE DRP, please use the PypeIt Citation.

The Keck Observatory Archive (KOA) is a collaboration between the NASA Exoplanet Science Institute (NExScI) and the W. M. Keck Observatory (WMKO). NExScI is sponsored by NASA's Exoplanet Exploration Program, and operated by the California Institute of Technology in coordination with the Jet Propulsion Laboratory (JPL).

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+ Getting Started + KOA Search Form + KOA and Python + KI Search Form + Publicly Available Data + Contributed Datasets + KOA User Guide + Image API + Reducing Keck Data + KOA Helpdesk + KOA News + Related Archives + Login / Logout	KPF Modes and Instrument Properties The Keck Planet Finder (KPF) is a fiber-fed, high-resolution, high-stability cross dispersed, spectrometer designed to characterize exoplanets via Doppler spectroscopy with a goal of a single measurement precision of 0.3 m/s or better. KPF covers a wavelength range of 440nm to 590nm in the green channel and 590nm to 870nm in the red channel. KPF consists of 3 independant spectrographs: The primary science spectrograph described above is designed to be highly stable and has both a green and a red arm. The spectrograph optical bench is made from low expansion Zerodur and is kept is a temperature stabilized environment. The detectors are 4kx4k with 15 um pixels. Resolving power is over 80,000. A Calcium H&K spectrograph (official documentation to be written) which gets the light blueward of the main science spectrograph and is used to simultaneously measure stellar activity using the Ca H&K lines. The exposure meter spectrograph (official documentation to be written) which gets a portion of the science light and is used to measure the flux level during long exposures of the primary science detectors. The exposure meter both measures the time weighted flux midpoint of each exposure, and can also be used to terminate an exposure at a specified flux level. All three spectrographs are fed by optical fiber from the Fiber Injection Unit (FIU) which sits on the Keck I AO bench. The light entering the FIU is not AO corrected, but is fed off a fast tip tilt mirror which is used to maintain the target star's position on the science fiber within 50 mas rms of the fiber center. More information can be on the KPF WMKO home page.

Please acknowledge the use of KOA by including this text in your publications: This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. Please also acknowledge the PI(s) of datasets that have been obtained through KOA, and please contact the KOA Help Desk if you publish archival data. If your research uses data reduced by the DEIMOS DRP or MOSFIRE DRP, please use the PypeIt Citation. Privacy Policy Image Use Policy The Keck Observatory Archive (KOA) is a collaboration between the NASA Exoplanet Science Institute (NExScI) and the W. M. Keck Observatory (WMKO). NExScI is sponsored by NASA's Exoplanet Exploration Program, and operated by the California Institute of Technology in coordination with the Jet Propulsion Laboratory (JPL). KOA WMKO \#koashare.html\