MOSES is a vacuum-stabilized white-pupil echelle spectrograph designed for >80,000 resolution over 380-680 nm and sub-2 m/s RV precision via dual-fiber simultaneous Fabry-Pérot calibration on the MONET telescope.
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5 Pith papers cite this work, alongside 26 external citations. Polarity classification is still indexing.
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One critical radial-velocity point bridging a multi-year instrument gap multiplies recovery of long-period super-Jupiters by up to 3.5× in injection-recovery tests.
Resolves six speculative companions into one giant planet, one eccentric brown dwarf, two low-mass stars, and two stars with no detectable companions.
N-body simulations demonstrate long-term dynamical stability of the HD 20794 system across a range of inclinations, with planet d identified as the lowest-mass high-eccentricity HZ-crossing planet.
Tentative evidence for a super-Jupiter at 15-100 AU or brown dwarf at 20-170 AU in 51 Pegasi from RV curvature, but the signal is likely driven by Lick/Hamilton instrument drift.
citing papers explorer
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MOSES -- The MONET Star and Exoplanet Spectrograph
MOSES is a vacuum-stabilized white-pupil echelle spectrograph designed for >80,000 resolution over 380-680 nm and sub-2 m/s RV precision via dual-fiber simultaneous Fabry-Pérot calibration on the MONET telescope.
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What's the (RV) Point? A $3.5\times$ Enhancement in Super-Jupiters with Saturn-like Periods from a Critical Observation
One critical radial-velocity point bridging a multi-year instrument gap multiplies recovery of long-period super-Jupiters by up to 3.5× in injection-recovery tests.
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The Pan-Pacific Planet Search -- IX. A menagerie of companions orbiting evolved stars
Resolves six speculative companions into one giant planet, one eccentric brown dwarf, two low-mass stars, and two stars with no detectable companions.
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Dynamical Stability and Habitability in the HD 20794 System
N-body simulations demonstrate long-term dynamical stability of the HD 20794 system across a range of inclinations, with planet d identified as the lowest-mass high-eccentricity HZ-crossing planet.
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An Outer Giant Planet or Brown Dwarf in the 51 Pegasi System?
Tentative evidence for a super-Jupiter at 15-100 AU or brown dwarf at 20-170 AU in 51 Pegasi from RV curvature, but the signal is likely driven by Lick/Hamilton instrument drift.