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Title:
Radial velocity data analysis with compressed sensing techniques
Authors:
Hara, Nathan C.; Boué, G.; Laskar, J.; Correia, A. C. M.
Affiliation:
AA(ASD/IMCCE, CNRS-UMR8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, F-75014 Paris, France ), AB(ASD/IMCCE, CNRS-UMR8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, F-75014 Paris, France), AC(ASD/IMCCE, CNRS-UMR8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, F-75014 Paris, France), AD(ASD/IMCCE, CNRS-UMR8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, F-75014 Paris, France; CIDMA, Departamento de Física, Universidade de Aveiro, Campus de Santiago, P-3810-193 Aveiro, Portugal)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 464, Issue 1, p.1220-1246 (MNRAS Homepage)
Publication Date:
01/2017
Origin:
OUP
Astronomy Keywords:
methods: data analysis, techniques: radial velocities, planets and satellites: detection
Abstract Copyright:
2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stw2261
Bibliographic Code:
2017MNRAS.464.1220H

Abstract

We present a novel approach for analysing radial velocity data that combines two features: all the planets are searched at once and the algorithm is fast. This is achieved by utilizing compressed sensing techniques, which are modified to be compatible with the Gaussian process framework. The resulting tool can be used like a Lomb-Scargle periodogram and has the same aspect but with much fewer peaks due to aliasing. The method is applied to five systems with published radial velocity data sets: HD 69830, HD 10180, 55 Cnc, GJ 876 and a simulated very active star. The results are fully compatible with previous analysis, though obtained more straightforwardly. We further show that 55 Cnc e and f could have been respectively detected and suspected in early measurements from the Lick Observatory and Hobby-Eberly Telescope available in 2004, and that frequencies due to dynamical interactions in GJ 876 can be seen.
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