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| Habitable-zone Planet Finder | |
|---|---|
| Name | Habitable-zone Planet Finder |
| Acronym | HPF |
| Type | Astronomical spectrograph |
| Location | Hobby-Eberly Telescope at McDonald Observatory |
| Institution | Pennsylvania State University and collaborating institutions |
| Wavelength | Near-infrared (NIR) |
| Start | 2017 |
| Purpose | Precision radial velocity for M-dwarf exoplanets |
Habitable-zone Planet Finder is a near-infrared precision radial velocity spectrograph mounted on the Hobby-Eberly Telescope at McDonald Observatory. Designed and built by a consortium led by Pennsylvania State University, the instrument targets low-mass M-dwarf stars to detect planets in their habitable zone via Doppler shifts. HPF complements optical spectrographs used at facilities such as W. M. Keck Observatory and European Southern Observatory by operating in the Y and J bands to exploit the spectral energy distribution of cool stars.
The project was conceived within collaborative environments involving Pennsylvania State University, University of Texas at Austin, Texas A&M University, University of Chicago, University of California, Santa Cruz, and partners including Carnegie Institution for Science and NASA-affiliated groups. HPF addresses scientific priorities articulated by panels such as the Exoplanet Exploration Program Analysis Group and observational strategies similar to those advocated by teams at the California Institute of Technology and Massachusetts Institute of Technology. Deployment at McDonald Observatory leverages infrastructure associated with the Hobby-Eberly Telescope and programmatic coordination with observatories like Kitt Peak National Observatory.
HPF is a stabilized, cryogenic, fiber-fed echelle spectrograph operating primarily in the near-infrared Y and J bands. The optical train and mechanical design incorporate technologies developed at institutions like Jet Propulsion Laboratory, National Institute of Standards and Technology, and industrial partners such as Thorlabs. Key components include a high-resolution diffraction grating, a cryostat maintained by teams with expertise from Lawrence Livermore National Laboratory, and a finely controlled temperature environment inspired by systems used at Gemini Observatory and Subaru Telescope. The detector is a state-of-the-art infrared array similar in concept to devices used at Spitzer Space Telescope and James Webb Space Telescope instrumentation teams. HPF achieves velocity precision goals through vacuum enclosure and thermal control regimes comparable to those used in instruments at European Southern Observatory facilities.
HPF relies on simultaneous calibration strategies that draw on methods employed by teams at University of California, Berkeley, Harvard University, and Princeton University. Calibration sources include stabilized lamps and laser frequency comb concepts pioneered by researchers at National Institute of Standards and Technology and groups associated with Jet Propulsion Laboratory. Observing campaigns coordinate target selection using catalogs and surveys from Gaia missions and follow-up priorities from programs such as Kepler and Transiting Exoplanet Survey Satellite collaborations. Telescope operations integrate scheduling approaches used by NOIRLab and data acquisition pipelines that echo techniques at Palomar Observatory and Las Campanas Observatory.
HPF's principal goal is the detection and characterization of low-mass planets orbiting nearby M-dwarf stars, addressing questions framed by the Exoplanet Exploration Program and studies from European Space Agency science teams. Results contribute to planet occurrence rate estimates from analyses similar to work by the California Planet Survey and inform target lists for missions like James Webb Space Telescope and future missions proposed within NASA roadmaps. HPF has aided discoveries and confirmations in coordination with radial velocity follow-up efforts at W. M. Keck Observatory, transit detections from Transiting Exoplanet Survey Satellite, and validation frameworks developed by researchers at Northwestern University and University of Washington.
Data processing for HPF employs a reduction pipeline developed by consortium partners with algorithms influenced by software from Space Telescope Science Institute and the Astropy Project community. The pipeline performs extraction, wavelength calibration, and radial velocity determination using techniques developed at University of Pittsburgh, University of Texas at Austin, and collaborators at Carnegie Institution for Science. Validation and quality assurance draw on best practices from missions such as Kepler and observatories including Palomar Observatory and W. M. Keck Observatory. Processed datasets interface with archival systems and community tools popularized by NASA Exoplanet Archive and the Mikulski Archive for Space Telescopes.
HPF is the product of multi-institution collaboration involving universities, national laboratories, and observatories including Pennsylvania State University, University of Texas at Austin, University of Florida, NASA, Carnegie Institution for Science, and McDonald Observatory. Funding and program oversight have involved agencies and organizations such as National Science Foundation, NASA Science Mission Directorate, and support from foundation partners aligned with projects at Caltech and MIT. Scientific coordination has benefited from interactions with international groups at European Southern Observatory and survey teams linked to Gaia and TESS.
Limitations of HPF include wavelength coverage restricted to Y and J bands, instrument throughput constraints relative to near-infrared imagers at facilities like Subaru Telescope, and challenges in mitigating stellar activity signals noted by researchers at Harvard-Smithsonian Center for Astrophysics and University of California, Santa Cruz. Future paths mirror upgrade plans discussed by teams at Keck Observatory and European Southern Observatory and may involve expanded wavelength coverage, laser frequency comb integration refined by National Institute of Standards and Technology and cryogenic detector improvements inspired by James Webb Space Telescope engineering. Proposed collaborations could include wider survey synergies with TESS, JWST, and ground-based observatories such as Gemini Observatory and Large Binocular Telescope to enhance discovery yield and characterization capabilities.
Category:Astronomical spectrographs