The exoplanet hunter HARPS: performance and first results

Rupprecht, G.; Pepe, F.; Mayor, M.; Queloz, D.; Bouchy, F.; Ávila, G.; Benz, W.; Bertaux, Jean-Loup; Bonfils, X.; Dall, Th.; Délabre, Bernard; Dekker, H.; Eckert, Wolfgang; Fleury, Michel; Gilliotte, A.; Gojak, D.; Guzman, Juan Carlos; Kohler, D.; Lizon, Jean-Louis; Curto, G. Lo; Longinotti, Antonio; Lovis, C.; Mégevand, D.; Pasquini, L.; Reyes, Javier Escalera; Sivan, J. P.; Sоsnowska, Danuta; Soto, R.; Udry, S.; Kesteren, A. van; Weber, L.; Weilenmann, U.

doi:10.1117/12.551267

Cited by 42 publications

(13 citation statements)

References 7 publications

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“…We predict that the radial velocity semi-amplitude of the Rossiter-McLaughlin effect for TOI-257 to be ∼ 8 m s −1 based on the stellar and planetary parameters we obtained for this system. The predicted signal, while small, should be detectable on very high-precision (∼ 1 m s −1 ) radial velocity 6 https://www.astro.keele.ac.uk/jkt/tepcat/ facilities in the south such as on HARPS (Rupprecht et al 2004), PFS (Crane et al 2006), and ESPRESSO (Pepe et al 2010). We predict, given the stellar rotational velocity (as determined from the rotational period and stellar radius) is consistent with the measured v sin i from spectroscopy (i.e., suggesting that the stellar obliquity is near 90 deg), that the projected spin-orbit angle λ when measured should be close to the true spin-orbit angle ψ.…”

Section: Discussionmentioning

confidence: 99%

TOI-257b (HD 19916b): a warm sub-saturn orbiting an evolved F-type star

Addison

Wright

Nicholson

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We report the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA’s Transiting Exoplanet Survey Satellite (TESS). The transit signal was detected by TESS and confirmed to be of planetary origin based on radial velocity observations. An analysis of the TESS photometry, the Minerva-Australis, FEROS, and HARPS radial velocities, and the asteroseismic data of the stellar oscillations reveals that TOI-257b has a mass of MP = 0.138 ± 0.023 $\rm {M_J}$ (43.9 ± 7.3 M⊕), a radius of RP = 0.639 ± 0.013 $\rm {R_J}$ (7.16 ± 0.15 R⊕), bulk density of $0.65^{+0.12}_{-0.11}$ (cgs), and period $18.38818^{+0.00085}_{-0.00084}$ $\rm {days}$. TOI-257b orbits a bright (V = 7.612 mag) somewhat evolved late F-type star with M* = 1.390 ± 0.046 $\rm {M_{sun}}$, R* = 1.888 ± 0.033 $\rm {R_{sun}}$, Teff = 6075 ± 90 $\rm {K}$, and vsin i = 11.3 ± 0.5 km s−1. Additionally, we find hints for a second non-transiting sub-Saturn mass planet on a ∼71 day orbit using the radial velocity data. This system joins the ranks of a small number of exoplanet host stars (∼100) that have been characterized with asteroseismology. Warm sub-Saturns are rare in the known sample of exoplanets, and thus the discovery of TOI-257b is important in the context of future work studying the formation and migration history of similar planetary systems.

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Section: Discussionmentioning

confidence: 99%

TOI-257b (HD 19916b): a warm sub-saturn orbiting an evolved F-type star

Addison

Wright

Nicholson

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Anglada-Escudé & Butler 2012;Zechmeister et al 2018;Dumusque 2018;Bedell et al 2019), the approach of cross-correlating observed spectra with a masked, weighted template (often called a delta function template when a binary mask is used) retains wide currency. For example, this approach is employed in the primary data reduction pipelines of HARPS (Rupprecht et al 2004) and HARPS-N (Cosentino et al 2012), as well as in the pipelines of newer instruments such as ESPRESSO (Di Marcantonio et al 2018) and EXPRESS (e.g. Blackman et al 2019).…”

Section: Introductionmentioning

confidence: 99%

A robust, template-free approach to precise radial velocity extraction

Rajpaul

Aigrain

Buchhave

2020

Monthly Notices of the Royal Astronomical Society

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Doppler spectroscopy is a powerful tool for discovering and characterizing exoplanets. For decades, the standard approach to extracting radial velocities (RVs) has been to cross-correlate observed spectra with a weighted template mask. While still widely used, this approach is known to suffer numerous drawbacks, and so in recent years increasing attention has been paid to developing new and improved ways of extracting RVs. In this proof-of-concept paper we present a simple yet powerful approach to RV extraction. We use Gaussian processes to model and align all pairs of spectra with each other; without constructing a template, we combine pairwise RV shifts to produce accurate differential stellar RVs. Doing this on a highly-localized basis enables a datadriven approach to identifying and mitigating spectral contamination, even without the input of any prior astrophysical knowledge. We show that a crude implementation of this method applied to an inactive standard star yields RVs with comparable precision to and significantly lower rms variation than RVs from industry-standard pipelines. Though amenable to numerous improvements, even in its basic form presented here our method could facilitate the study of smaller planets around a wider variety of stars than has previously been possible.

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“…In 2004 the HARPS precision velocity program began observing Proxima Cen. HARPS has been the state-of-theart precision velocity instrument since its inception (Rupprecht et al 2004), routinely approaching or exceeding a precision of 1 m s −1 (Pepe et al 2011). The HARPS spectrometer products, including the raw data, reduced spectra, and velocity measurements are available on the ESO archive after a typical embargo period of 1 year 1 .…”

Section: Introductionmentioning

confidence: 99%

A Reanalysis of the UVES M Dwarf Planet Search Program*

Butler

Jones

Feng

et al. 2019

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The UVES (Ultraviolet and Visible Spectrometer) M Dwarf Planet Search program surveyed 40 M dwarfs and 1 M giant from 2000 through 2007 March. Two of the M dwarfs were double-lined spectroscopic binaries. The 38 single-lined M dwarfs in this survey are among the nearest and brightest M dwarfs. Starting with the reduced 1D spectra provided by the UVES team, we reanalyzed the UVES velocities of Proxima Cen as part of the “Pale Red Dot” program. The velocity rms decreased from 3.6 to 2.3 m s−1. Motivated by this result, we have harvested all of the raw data from the UVES M Dwarf Planet Search from the European Southern Observatory (ESO) archives and have written custom packages to generate 1D spectra from the raw data, and velocities from the 1D spectra. The median improvement in the velocity rms from the new analysis is 1.8 m s−1. Six of the 38 M dwarfs from the original study had a velocity rms < 4 m s−1. In the reanalysis presented here, 22 of these stars have a velocity rms < 4 m s−1. We improve the upper limits on possible planets orbiting these stars by a factor of typically two to three. For many of these M dwarfs, these observations represent the first epoch of high-precision velocity measurements.

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The exoplanet hunter HARPS: performance and first results

Cited by 42 publications

References 7 publications

TOI-257b (HD 19916b): a warm sub-saturn orbiting an evolved F-type star

TOI-257b (HD 19916b): a warm sub-saturn orbiting an evolved F-type star

A robust, template-free approach to precise radial velocity extraction

A Reanalysis of the UVES M Dwarf Planet Search Program*

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