Deputy Instrument Scientist:
|Follow this link for information about pre-observing activities: proposal preparation, mask design and submission, pre-run activities, etc.
|Follow this link for information about your observing run: instrument and telescope setups, scripts, software, procedures, etc.
|Follow this link for information about your post-observing activities: backups, comment forms, data reduction, etc.
|Trouble Shooting Confluence document.
|Portal to the technical pages: for the initiated only!
|A listing of the instrument pages.
KPF has been commissioned on sky, and is available for use. Many aspects of the instrument are still being optimized and the long term stability is still under evaluation. Short term stability looks excellent (exceeding the 50 cm/s target spec within a night) and we expect measures of the long term RV precision to become available as the DRP evolves.
See KPF Status Summary and Blog for the latest details on the instrument's operational status broken down by subsystem.
A detailed summary of the instrument status was presented at the September 2023 Keck Science Meeting. The slides from that presentation are viewable here.
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 445 nm to 870 nm over green and red channels.
KPF consists of 3 independant spectrographs:
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. Performance of the tip tilt loop is to be confirmed during commissioning.
During observations, the spectrograph can be fed with light from a simultaneous calibration fiber. This places calibration light alongside science and sky spectra in the pseudo-slit. The calibration light is fed from the calibration bench which contains several calibration sources.
In addition to the simultaneous calibration light, the calibration bench can be configured to feed light up to the FIU and through the science and sky fibers in order to bring cal light in to the science and sky portions of the pseudo-slit.