ESPRESSO: The next European exoplanet hunter

Pepe, F.; Molaro, P.; Cristiani, S.; Реболо, Р.; Santos, N. C.; Dekker, H.; Mégevand, D.; Zerbi, F. M.; Cabral, Alexandre; Marcantonio, P. Di; Abreu, Manuel; Affolter, Michael; Aliverti, Matteo; Prieto, C. Allende; Amate, M.; Ávila, G.; Baldini, V.; Bristow, Paul; Broeg, C.; Cirami, R.; Coelho, João M. P.; Conconi, P.; Coretti, I.; Cupani, G.; D’Odorico, V.; Caprio, Vincenzo De; Délabre, Bernard; Dorn, Reinhold J.; Figueira, P.; Fragoso, A.; Galeotta, S.; Genolet, L.; Gomes, Ricardo; Hernández, J. I. González; Hughes, I.; Iwert, Olaf; Kerber, F.; Landoni, Marco; Lizon, J. L.; Maire, C.; Mannetta, M.; Martins, C. J. A. P.; Monteiro, M. A.; Oliveira, Antônio César de; Poretti, E.; Rasilla, J. L.; Riva, M.; Tschudi, S. Santana; Santos, P.; Sоsnowska, Danuta; Sousa, S. G.; Spanó, P.; Tenegi, F.; Toso, Giorgio; Vanzella, E.; Viel, Matteo; Osorio, M. R. Zapatero

doi:10.48550/arxiv.1401.5918

Cited by 17 publications

(18 citation statements)

References 14 publications

(15 reference statements)

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“…This ensures we have sufficient precision to resolve the stellar RV signal. The typical measurement uncertainties range from 0.5 to 3 m s −1 , consistent with or larger than measurement uncertainties expected for current (Fischer et al 2016) and future generations of RV spectrographs (Pepe et al 2014).…”

Section: Impact Of Correlated Activity Noise On Planet Detectionsupporting

confidence: 73%

Radial velocity planet detection biases at the stellar rotational period

Vanderburg

Plavchan

Johnson

et al. 2016

Mon. Not. R. Astron. Soc.

102

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Future generations of precise radial velocity (RV) surveys aim to achieve sensitivity sufficient to detect Earth mass planets orbiting in their stars' habitable zones. A major obstacle to this goal is astrophysical radial velocity noise caused by active areas moving across the stellar limb as a star rotates. In this paper, we quantify how stellar activity impacts exoplanet detection with radial velocities as a function of orbital and stellar rotational periods. We perform data-driven simulations of how stellar rotation affects planet detectability and compile and present relations for the typical timescale and amplitude of stellar radial velocity noise as a function of stellar mass. We show that the characteristic timescales of quasi-periodic radial velocity jitter from stellar rotational modulations coincides with the orbital period of habitable zone exoplanets around early M-dwarfs. These coincident periods underscore the importance of monitoring the targets of RV habitable zone planet surveys through simultaneous photometric measurements for determining rotation periods and activity signals, and mitigating activity signals using spectroscopic indicators and/or RV measurements at different wavelengths.

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Section: Impact Of Correlated Activity Noise On Planet Detectionsupporting

confidence: 73%

Radial velocity planet detection biases at the stellar rotational period

Vanderburg

Plavchan

Johnson

et al. 2016

Mon. Not. R. Astron. Soc.

102

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show abstract

“…The next generation of spectrographs aim to detect such planets by achieving radial velocity resolutions of around 0.1 m s −1 (e.g. ESPRESSO, Pepe et al 2014) and 0.01 m s −1 (e.g. CODEX, Pasquini et al 2010).…”

Section: Exoplanet Populationmentioning

confidence: 99%

Stable habitable zones of single Jovian planet systems

Agnew

Maddison

Thilliez

et al. 2017

Monthly Notices of the Royal Astronomical Society

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With continued improvement in telescope sensitivity and observational techniques, the search for rocky planets in stellar habitable zones is entering an exciting era. With so many exoplanetary systems available for follow-up observations to find potentially habitable planets, one needs to prioritise the ever-growing list of candidates. We aim to determine which of the known planetary systems are dynamically capable of hosting rocky planets in their habitable zones, with the goal of helping to focus future planet search programs. We perform an extensive suite of numerical simulations to identify regions in the habitable zones of single Jovian planet systems where Earth mass planets could maintain stable orbits, specifically focusing on the systems in the Catalog of Earth-like Exoplanet Survey Targets (CELESTA). We find that small, Earth-mass planets can maintain stable orbits in cases where the habitable zone is largely, or partially, unperturbed by a nearby Jovian, and that mutual gravitational interactions and resonant mechanisms are capable of producing stable orbits even in habitable zones that are significantly or completely disrupted by a Jovian. Our results yield a list of 13 single Jovian planet systems in CELESTA that are not only capable of supporting an Earth-mass planet on stable orbits in their habitable zone, but for which we are also able to constrain the orbits of the Earth-mass planet such that the induced radial velocity signals would be detectable with next generation instruments.

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“…By finding similar frequencies having instead used more restrictive boundaries, we argue that this may be taken as a hint that the number of Earth-like planets in the Milky Way is higher than anticipated by the literature. This tantalizing possibility provides a high potential for any current or future planet-hunting experiments specifically designed to search for potentially habitable Earths orbiting solartype stars, such as the spectrograph ESPRESSO (Pepe et al (2014)), the space observatory PLATO (Rauer et al (2014)) and the proposed ESA astrometry satellite Theia (Theia Collaboration (2017)). In particular, Theia is expected to detect and characterize any super Earths with M p < 2.2 M ⊕ orbiting around 60 of the stars nearest to the Sun, showing again how astrometry promises to further push the boundaries of exoplanetology.…”

Section: Discussionmentioning

confidence: 99%

Revised estimates of the frequency of Earth-like planets in the Kepler field

Barbato,

Bonomo,

Sozzetti

et al. 2018

Preprint

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The search for Earth-like planets around Sun-like stars and the evaluation of their occurrence rate is a major topic of research for the exoplanetary community. Two key characteristics in defining a planet as 'Earth-like' are having a radius between 1 and 1.75 times the Earth's radius and orbiting inside the host star's habitable zone; the measurement of the planet's radius and related error is however possible only via transit observations and is highly dependent on the precision of the host star's radius. A major improvement in the determination of stellar radius is represented by the unprecedented precision on parallax measurements provided by the Gaia astrometry satellite. We present a new estimate of the frequency of Earth-sized planets orbiting inside the host stars's habitable zones, obtained using Gaia measurements of parallax for solar-type stars hosting validated planets in the Kepler field as input for reassessing the values of planetary radius and incident stellar flux. This updated occurrence rate can usefully inform future observational efforts searching for Earth-like system in the Sun backyard using a variety of techniques such as the spectrograph ESPRESSO, the space observatory PLATO and the proposed astrometric satellite Theia.

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ESPRESSO: The next European exoplanet hunter

Cited by 17 publications

References 14 publications

Radial velocity planet detection biases at the stellar rotational period

Radial velocity planet detection biases at the stellar rotational period

Stable habitable zones of single Jovian planet systems

Revised estimates of the frequency of Earth-like planets in the Kepler field

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