Joint Radial Velocity and Direct Imaging Planet Yield Calculations. I. Self-consistent Planet Populations

Dulz, Shannon; Plavchan, Peter; Crepp, Justin R.; Stark, Christopher C.; Morgan, Rhonda; Kane, Stephen R.; Newman, Patrick; Matzko, William; Mulders, Gijs D.

doi:10.3847/1538-4357/ab7b73

Cited by 26 publications

(31 citation statements)

References 68 publications

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“…(2019) at separations beyond 10 au. Dulz et al (2020) fit model distributions of planets to occurrence rates measured from Kepler and previous RV surveys. Although their constraints on Jovian-mass planets were relatively weak, they found that the occurrence of Neptune-mass and smaller planets must fall off beyond ∼5 au due to dynamical constraints.…”

Section: Comparison To Previous Rv Surveysmentioning

confidence: 99%

California Legacy Survey. II. Occurrence of Giant Planets beyond the Ice Line

Fulton

Rosenthal

Hirsch

et al. 2021

ApJS

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170

151

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We used high-precision radial velocity measurements of FGKM stars to determine the occurrence of giant planets as a function of orbital separation spanning 0.03-30 au. Giant planets are more prevalent at orbital distances of 1-10 au compared to orbits interior or exterior of this range. The increase in planet occurrence at ∼1 au by a factor of ∼4 is highly statistically significant. A fall-off in giant planet occurrence at larger orbital distances is favored over models with flat or increasing occurrence. We measure -+ 14.1 1.8 2.0 giant planets per 100 stars with semimajor axes of 2-8 au and -+ 8.9 2.4 3.0 giant planets per 100 stars in the range 8-32 au, a decrease in occurrence with increasing orbital separation that is significant at the ∼2σ level. We find that the occurrence rate of sub-Jovian planets (0.1-1 Jupiter masses) is also enhanced for 1-10 au orbits. This suggests that lower-mass planets may share the formation or migration mechanisms that drive the increased prevalence near the water-ice line for their Jovian counterparts. Our measurements of cold gas giant occurrence are consistent with the latest results from direct imaging surveys and gravitational lensing surveys despite different stellar samples. We corroborate previous findings that giant planet occurrence increases with stellar mass and metallicity. Unified Astronomy Thesaurus concepts: Exoplanets (498); Exoplanet astronomy (486); Exoplanet catalogs (488); Surveys (1671); Radial velocity (1332); Exoplanet detection methods (489); Extrasolar gaseous planets (2172); Extrasolar gaseous giant planets (509)

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Section: Comparison To Previous Rv Surveysmentioning

confidence: 99%

California Legacy Survey. II. Occurrence of Giant Planets beyond the Ice Line

Fulton

Rosenthal

Hirsch

et al. 2021

ApJS

Self Cite

170

151

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“…The exoplanet occurrence rates were based on the EXOPAG SAG-13 power law model of Kepler data, as modified by Dulz et al 38 for large mass and large semimajor axis planets.…”

Section: Astrophysical Inputsmentioning

confidence: 99%

Faster Exo-Earth yield for HabEx and LUVOIR via extreme precision radial velocity prior knowledge

Morgan

Savransky

Turmon

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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The HabEx and LUVOIR mission concepts reported science yields for mission scenarios in which the instruments must search for potentially habitable planets, determine their orbits, and, if worthwhile, invest the integration time for a spectral characterization. We evaluate the impact of prior knowledge of planet existence and orbital parameters on yield for four mission concept architectures: HabEx 4m telescope with hybrid starshade and coronagraph, HabEx 4m telescope with starshade only, HabEx 4m telescope with coronagraph only, and LUVOIR B 8m telescope with coronagraph only. We use perfect prior knowledge to establish an upper bound on yield and use partial prior knowledge from a potential future extreme precision radial velocity (EPRV) instrument with 3 cm∕s sensitivity. We detail a modeling framework that performs dynamically responsive observation scheduling with realistic mission constraints. We evaluate exo-Earth yields against three metrics of spectral characterization for the four mission architectures and three levels of prior knowledge (none, partial, and perfect). The EPRV provided prior knowledge increases yields by ∼30% and accelerates by a factor of 3 to 6 the time to achieve half of the yield of the mission. Prior knowledge makes all the mission architectures more nimble and powerful, and most especially starshade-based architectures. With prior knowledge, a small telescope with a starshade can achieve comparable yield to a larger telescope with a coronagraph.

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“…However, a further option to explore the possible planetary architecture of Beta CVn, particularly given the proximity of the star, is direct imaging (Kane et al 2018;Dulz et al 2020).…”

Section: Potential For Terrestrial Planetsmentioning

confidence: 99%

Dynamical Packing in the Habitable Zone: The Case of Beta CVn

Kane

Turnbull

Fulton

et al. 2020

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Uncovering the occurrence rate of terrestrial planets within the habitable zone (HZ) of their host stars has been a particular focus of exoplanetary science in recent years. The statistics of these occurrence rates have largely been derived from transiting planet discoveries, and have uncovered numerous HZ planets in compact systems around M-dwarf host stars. Here we explore the width of the HZ as a function of spectral type, and the dynamical constraints on the number of stable orbits within the HZ for a given star. We show that, although the Hill radius for a given planetary mass increases with larger semimajor axis, the width of the HZ for earlier-type stars allows for more terrestrial planets in the HZ than late-type stars. In general, dynamical constraints allow ∼6 HZ Earth-mass planets for stellar masses 0.7M e , depending on the presence of farther out giant planets. As an example, we consider the case of Beta CVn, a nearby bright solar-type star. We present 20 yr of radial velocities (RV) from the Keck/High Resolution Echelle Spectrometer (HIRES) and Automated Planet Finder (APF) instruments and conduct an injection-recovery analysis of planetary signatures in the data. Our analysis of these RV data rule out planets more massive than Saturn within 10 au of the star. These system properties are used to calculate the potential dynamical packing of terrestrial planets in the HZ and show that such nearby stellar targets could be particularly lucrative for HZ planet detection by direct imaging exoplanet missions.

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Joint Radial Velocity and Direct Imaging Planet Yield Calculations. I. Self-consistent Planet Populations

Cited by 26 publications

References 68 publications

California Legacy Survey. II. Occurrence of Giant Planets beyond the Ice Line

California Legacy Survey. II. Occurrence of Giant Planets beyond the Ice Line

Faster Exo-Earth yield for HabEx and LUVOIR via extreme precision radial velocity prior knowledge

Dynamical Packing in the Habitable Zone: The Case of Beta CVn

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