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Title:
A simple method to estimate radial velocity variations due to stellar activity using photometry
Authors:
Aigrain, S.; Pont, F.; Zucker, S.
Affiliation:
AA(Sub-department of Astrophysics, Department of Physics, University of Oxford, Oxford OX1 3RH), AB(Astrophysics Group, School of Physics, University of Exeter, Exeter EX4 4QL), AC(Department of Geophysics and Planetary Sciences, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, Israel)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 419, Issue 4, pp. 3147-3158. (MNRAS Homepage)
Publication Date:
02/2012
Origin:
WILEY
Astronomy Keywords:
methods: data analysis, techniques: photometric, techniques: radial velocities, Sun: activity, planetary systems, stars: individual: HD 189733
Abstract Copyright:
© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS
DOI:
10.1111/j.1365-2966.2011.19960.x
Bibliographic Code:
2012MNRAS.419.3147A

Abstract

We present a new, simple method to predict activity-induced radial velocity (RV) variations using high-precision time series photometry. It is based on insights from a simple spot model, has only two free parameters (one of which can be estimated from the light curve) and does not require knowledge of the stellar rotation period. We test the method on simulated data and illustrate its performance by applying it to MOST/SOPHIE observations of the planet host star HD 189733, where it gives almost identical results to much more sophisticated but highly degenerate models, and synthetic data for the Sun, where we demonstrate that it can reproduce variations well below the m s-1 level. We also apply it to quarter 1 data for Kepler transit candidate host stars, where it can be used to estimate RV variations down to the 2-3 m s-1 level, and show that RV amplitudes above that level may be expected for approximately two-thirds of the candidates we examined.

Throughout this paper, we use amplitude spectra computed by linear least-squares fitting of a sinusoid with free zero-point, amplitude and phase at each frequency. This is akin to the generalized periodogram of Zechmeister & Kürster (2009) but expressed in units of amplitude rather than χ2 reduction.

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