Keck Planet Finder: design updates

Gibson, Steven R.; Howard, Andrew W.; Rider, Kodi; Roy, Arpita; Edelstein, Jerry; Kassis, Marc; Grillo, Jason; Halverson, Samuel; Sirk, Martin M.; Smith, Christopher L.; Allen, S. L.; Baker, Ashley; Beichman, Charles; Berriman, G. Bruce; Brown, Thomas M.; Casey, Kelleen; Chin, Jason C. Y.; Coutts, David W.; Cowley, David J.; Deich, William T. S.; Feger, Tobias; Fulton, B. J.; Gers, Luke; Gurevich, Yulia V.; Ishikawa, Yuzo; James, Ean; Jelinsky, Sharon R.; Kaye, Stephen B.; Lanclos, Kyle; Li, Adela; Lilley, Scott; McCarney, Ben; Miller, Tim; Milner, Steve; O'Hanlon, Timothy J.; Pember, Jacob; Raffanti, Mike; Rockosi, Constance M.; Rubenzahl, Ryan A.; Rumph, Dave; Sandford, Dale; Savage, Maureen L.; Schwab, Christian; Seifahrt, Andreas; Shaum, A.; Smith, Roger M.; Stuermer, Julian; Thorne, J. R.; Vandenberg, Adam; Boeckmann, Tod Von; Wang, Cindy; Wang, Qifan; Weisfeiler, Marie; Wilcox, Mavourneen K.; Wishnow, Edward H.; Wizinowich, Peter; Wold, T.; Wolfenberger, Anna

doi:10.1117/12.2561783

Cited by 10 publications

(2 citation statements)

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“…HISPEC and MODHIS offer unique advantages of extreme sensitivity for Precision Radial Velocity measurements (PRV) for cool stars, high spectral and angular resolution and, in some cases, coordinated operation with the visible-light PRV instruments, such as Keck Planet Finder (KPF) in the case of HISPEC. 51 The PRV precision resulting from combining all four wavelength bands will be roughly a factor of two better than that of an individual band, with the exact degree of improvement depending on stellar temperature. An aspect of combining the wavelengths not captured in these figures is the benefit of such a wide wavelength grasp in reducing the effects of stellar variability.…”

Section: Exoplanet Masses Orbits and Discovery With Nir Prvmentioning

confidence: 99%

The development of HISPEC for Keck and MODHIS for TMT: science cases and predicted sensitivities

Konopacky,

Baker,

Mawet

et al. 2023

Techniques and Instrumentation for Detection of Exoplanets XI

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HISPEC is a new, high-resolution near-infrared spectrograph being designed for the W.M. Keck II telescope. By offering single-shot, R 100,000 spectroscopy between 0.98 -2.5 µm, HISPEC will enable spectroscopy of transiting and non-transiting exoplanets in close orbits, direct high-contrast detection and spectroscopy of spatially separated substellar companions, and exoplanet dynamical mass and orbit measurements using precision radial velocity monitoring calibrated with a suite of state-of-the-art absolute and relative wavelength references. MODHIS is the counterpart to HISPEC for the Thirty Meter Telescope and is being developed in parallel with similar scientific goals. In this proceeding, we provide a brief overview of the current design of both instruments, and the requirements for the two spectrographs as guided by the scientific goals for each. We then outline the current science case for HISPEC and MODHIS, with focuses on the science enabled for exoplanet discovery and characterization. We also provide updated sensitivity curves for both instruments, in terms of both signal-to-noise ratio and predicted radial velocity precision.

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Section: Exoplanet Masses Orbits and Discovery With Nir Prvmentioning

confidence: 99%

The development of HISPEC for Keck and MODHIS for TMT: science cases and predicted sensitivities

Konopacky,

Baker,

Mawet

et al. 2023

Techniques and Instrumentation for Detection of Exoplanets XI

View full text Add to dashboard Cite

show abstract

“…Surveys of M dwarfs are being conducted with stabilized high-resolution infrared spectrographs, a relatively new technological development (see, e.g., Mahadevan et al 2012;Sabotta et al 2021). With a new generation of optical Doppler spectrographs, such as MAROON-X (Seifahrt et al 2016), ESPRESSO (Pepe et al 2021), EXPRES (Jurgenson et al 2016), KPF (Gibson et al 2020), and the planned HARPS3 (Thompson et al 2016) and G-CLEF (Szentgyorgyi et al 2018), it might be possible to detect Earth-mass planets with orbital periods approaching a year. In addition to finding potentially habitable planets, the results from these facilities will provide more overlap between Doppler-based occurrence measurements as a function of mass and transit-based occurrence measurements as a function of radius.…”

Section: Future Prospectsmentioning

confidence: 99%

Planet Occurrence: Doppler and Transit Surveys

Winn¹

2018

Handbook of Exoplanets

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Prior to the 1990s, speculations about the occurrence of planets around other stars were based only on planet formation theory, observations of circumstellar disks, and the knowledge that at least one seemingly ordinary star is the host of four terrestrial planets, two gas giants, and two ice giants. Since then, Doppler and transit surveys have been exploring the population of planets around other Sun-like stars, especially those with orbital periods shorter than a few years. Over the last decade, these surveys have risen to new heights with Doppler spectrographs with a precision better than 1 m s −1 precision, and space telescopes capable of detecting the transits of Earth-sized planets. This article is a brief introductory review of the knowledge of planet occurrence that has been gained from these surveys.

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Staring at the Sun with the Keck Planet Finder: An Autonomous Solar Calibrator for High Signal-to-noise Sun-as-a-star Spectra

Rubenzahl,

Halverson,

Walawender

et al. 2023

PASP

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Extreme precision radial velocity (EPRV) measurements contend with internal noise (instrumental systematics) and external noise (intrinsic stellar variability) on the road to 10 cm s−1 “exo-Earth” sensitivity. Both of these noise sources are well-probed using “Sun-as-a-star” RVs and cross-instrument comparisons. We built the Solar Calibrator (SoCal), an autonomous system that feeds stable, disk-integrated sunlight to the recently commissioned Keck Planet Finder (KPF) at the W. M. Keck Observatory. With SoCal, KPF acquires signal-to-noise ratio (S/N) ∼ 1200, R = 98,000 optical (445–870 nm) spectra of the Sun in 5 s exposures at unprecedented cadence for an EPRV facility using KPF’s fast readout mode (<16 s between exposures). Daily autonomous operation is achieved by defining an operations loop using state machine logic. Data affected by clouds are automatically flagged using a reliable quality control metric derived from simultaneous irradiance measurements. Comparing solar data across the growing global network of EPRV spectrographs with solar feeds will allow EPRV teams to disentangle internal and external noise sources and benchmark spectrograph performance. To facilitate this, all SoCal data products are immediately available to the public on the Keck Observatory Archive. We compared SoCal RVs to contemporaneous RVs from NEID, the only other immediately public EPRV solar data set. We find agreement at the 30–40 cm s−1 level on timescales of several hours, which is comparable to the combined photon-limited precision. Data from SoCal were also used to assess a detector problem and wavelength calibration inaccuracies associated with KPF during early operations. Long-term SoCal operations will collect upwards of 1000 solar spectra per six-hour day using KPF’s fast readout mode, enabling stellar activity studies at high S/N on our nearest solar-type star.

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Keck Planet Finder: design updates

Cited by 10 publications

References 0 publications

The development of HISPEC for Keck and MODHIS for TMT: science cases and predicted sensitivities

The development of HISPEC for Keck and MODHIS for TMT: science cases and predicted sensitivities

Planet Occurrence: Doppler and Transit Surveys

Staring at the Sun with the Keck Planet Finder: An Autonomous Solar Calibrator for High Signal-to-noise Sun-as-a-star Spectra

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