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Research at St Andrews

Separating planetary reflex Doppler shifts from stellar variability in the wavelength domain

Research output: Contribution to journalArticlepeer-review

Author(s)

A Collier Cameron, E B Ford, S Shahaf, S Aigrain, X Dumusque, R D Haywood, A Mortier, D F Phillips, L Buchhave, M Cecconi, H Cegla, R Cosentino, M Crétignier, A Ghedina, M González, D W Latham, M Lodi, M López-Morales, G Micela, E Molinari & 11 more F Pepe, G Piotto, E Poretti, D Queloz, J San Juan, D Ségransan, A Sozzetti, A Szentgyorgyi, S Thompson, S Udry, C Watson

School/Research organisations

Abstract

Stellar magnetic activity produces time-varying distortions in the photospheric line profiles of solar-type stars. These lead to systematic errors in high-precision radial-velocity measurements, which limit efforts to discover and measure the masses of low-mass exoplanets with orbital periods of more than a few tens of days. We present a new data-driven method for separating Doppler shifts of dynamical origin from apparent velocity variations arising from variability-induced changes in the stellar spectrum. We show that the autocorrelation function (ACF) of the cross-correlation function used to measure radial velocities is effectively invariant to translation. By projecting the radial velocities on to a subspace labelled by the observation identifiers and spanned by the amplitude coefficients of the ACF’s principal components, we can isolate and subtract velocity perturbations caused by stellar magnetic activity. We test the method on a 5-year time sequence of 853 daily 15-minute observations of the solar spectrum from the HARPS-N instrument and solar-telescope feed on the 3.58-m Telescopio Nazionale Galileo. After removal of the activity signals, the heliocentric solar velocity residuals are found to be Gaussian and nearly uncorrelated. We inject synthetic low-mass planet signals with amplitude K = 40 cm s−1 into the solar observations at a wide range of orbital periods. Projection into the orthogonal complement of the ACF subspace isolates these signals effectively from solar activity signals. Their semi-amplitudes are recovered with a precision of ∼ 6.6 cm s−1, opening the door to Doppler detection and characterization of terrestrial-mass planets around well-observed, bright main-sequence stars across a wide range of orbital periods.
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Original languageEnglish
Pages (from-to)1699–1717
JournalMonthly Notices of the Royal Astronomical Society
Volume505
Issue number2
Early online date12 May 2021
DOIs
Publication statusE-pub ahead of print - 12 May 2021

    Research areas

  • Methods: statistical, Planets and satellites: general, Sun: photosphere, Techniques: radial velocities, Techniques: spectroscopic

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