ESPRESSO: The next European exoplanet hunter

Pepe, F.; Molaro, P.; Cristiani, S.; Rebolo, R.; 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, M.; Lizon, Jean-Louis; Lovis, C.; 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:10.1002/asna.201312004

Cited by 179 publications

(75 citation statements)

References 22 publications

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“…Looking ahead, the ongoing UVES Large Program for Testing Fundamental Physics [8][9][10] is trying to confirm the earlier evidence for variations but is also playing a crucial role as preparatory work for the next generation of high-resolution ultrastable spectrographs, such as ESPRESSO [26] and ELT-HIRES [27] which have tests of the stability of fundamental couplings among their key science drivers. While the current sensitivity of individual measurements with UVES or similar spectrographs is at the 1-2 parts per million level, an improvement of about a factor of 3 is expected with ESPRESSO, and of at least an order of magnitude with ELT-HIRES.…”

Section: Discussionmentioning

confidence: 99%

Fine-structure constant constraints on Bekenstein-type models

2014

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Astrophysical tests of the stability of dimensionless fundamental couplings, such as the fine-structure constant $\alpha$, are an area of much increased recent activity, following some indications of possible spacetime variations at the few parts per million level. Here we obtain updated constraints on the Bekenstein-Sandvik-Barrow-Magueijo model, which is arguably the simplest model allowing for $\alpha$ variations. Recent accurate spectroscopic measurements allow us to improve previous constraints by about an order of magnitude. We briefly comment on the dependence of the results on the data sample, as well as on the improvements expected from future facilities.Comment: 5 pages, 2 figure

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Section: Discussionmentioning

confidence: 99%

Fine-structure constant constraints on Bekenstein-type models

2014

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“…We compute RV precision estimates for four example spectrograph designs; (1) an ultra-high resolution spectrograph at an 8-m telescope covering a very wide wavelength range like ESPRESSO (Pepe et al 2014), (2) Table 4 and visualized in Fig. 4.…”

Section: Spectrographsmentioning

confidence: 99%

“…Current instrumental limitations together with intrinsic stellar variability limits the RV technique to planets that cause stellar velocity amplitudes on the order of 1 m s −1 or larger . Instruments like ESPRESSO (Pepe et al 2014;Hojjatpanah et al 2019) aim for the 10 cm s −1 -limit, and a new generation of spectrographs at telescopes beyond the 10m-class are planned with similar perfomance goals (Marconi et al 2016;Szentgyorgyi et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Radial Velocity Photon Limits for the Dwarf Stars of Spectral Classes F–M

Reiners¹,

Zechmeister²

2020

ApJS

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The determination of extrasolar planet masses with the radial velocity (RV) technique requires spectroscopic Doppler information from the planet's host star, which varies with stellar brightness and temperature. We analyze Doppler information in spectra of F-M dwarfs utilizing empirical information from HARPS and CARMENES, and from model spectra. We come to the conclusions that an optical setup (BV R-bands) is more efficient that a near-infrared one (Y JHK) in dwarf stars hotter than 3200 K.We publish a catalogue of 46,480 well-studied F-M dwarfs in the solar neighborhood and compare their distribution to more than one million stars from Gaia DR2. For all stars, we estimate the RV photon noise achievable in typical observations assuming no activity jitter and slow rotation. We find that with an ESPRESSO-like instrument at an 8m-telescope, a photon noise limit of 10 cm s −1 or lower can be reached in more than 280 stars in a 5 min observation. At 4m-telescopes, a photon noise limit of 1 m s −1 can be reached in a 10 min exposure in approx. 10,000 predominantly sun-like stars with a HARPS-like (optical) instrument. The same applies to ∼3000 stars for a red-optical setup covering the RIz-bands, and to ∼700 stars for a near-infrared instrument. For the latter two, many of the targets are nearby M dwarfs. Finally, we identify targets in which Earth-mass planets within the liquid water habitable zone can cause RV amplitudes comparable to the RV photon noise. Assuming the same exposure times, we find that an ESPRESSO-like instrument can reach this limit for 1 M ⊕ planets in more than 1000 stars. The optical, red-optical, and near-infrared configurations reach the limit for 2 M ⊕ planets in approximately 500, 700, and 200 stars, respectively.

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“…The new ESPRESSO spectrograph (Pepe et al 2014;2019 in prep. ) started operations at the ESO Paranal observatory in September 2018.…”

Section: Espressomentioning

confidence: 99%

Decoding the radial velocity variations of HD 41248 with ESPRESSO

Faria

Adibekyan

Amazo-Gómez

et al. 2020

A&A

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Context. Twenty-four years after the discoveries of the first exoplanets, the radial-velocity (RV) method is still one of the most productive techniques to detect and confirm exoplanets. But stellar magnetic activity can induce RV variations large enough to make it difficult to disentangle planet signals from the stellar noise. In this context, HD 41248 is an interesting planet-host candidate, with RV observations plagued by activity-induced signals. Aims. We report on ESPRESSO observations of HD 41248 and analyse them together with previous observations from HARPS with the goal of evaluating the presence of orbiting planets. Methods. Using different noise models within a general Bayesian framework designed for planet detection in RV data, we test the significance of the various signals present in the HD 41248 dataset. We use Gaussian processes as well as a first-order moving average component to try to correct for activity-induced signals. At the same time, we analyse photometry from the TESS mission, searching for transits and rotational modulation in the light curve.Results. The number of significantly detected Keplerian signals depends on the noise model employed, which can range from 0 with the Gaussian process model to 3 with a white noise model. We find that the Gaussian process alone can explain the RV data while allowing for the stellar rotation period and active region evolution timescale to be constrained. The rotation period estimated from the RVs agrees with the value determined from the TESS light curve. Conclusions. Based on the data that is currently available, we conclude that the RV variations of HD 41248 can be explained by stellar activity (using the Gaussian process model) in line with the evidence from activity indicators and the TESS photometry.

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ESPRESSO: The next European exoplanet hunter

Cited by 179 publications

References 22 publications

Fine-structure constant constraints on Bekenstein-type models

Fine-structure constant constraints on Bekenstein-type models

Radial Velocity Photon Limits for the Dwarf Stars of Spectral Classes F–M

Decoding the radial velocity variations of HD 41248 with ESPRESSO

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