Astronomy Thesis Collection
Published November 25, 2016 | Version v1
Thesis Open

Radial velocity fiber-fed spectrographs towards the discovery of compact planets and pulsations on M stars

Authors/Creators

  • 1. Instituto de Astrofísica de Andalucía-CSIC; Universidad de Granada

Contributors

  • 1. Instituto de Astrofísica de Andalucía - CSIC
  • 2. Queen Mary University of London

Description

This thesis is developed in the framework of the paradigm that seeks for the discovery of an Earth analog. Nowadays, low mass stars, and in particular M dwarf stars, are key targets towards achieving this goal. In this thesis, I focus on the study of the short-time domain of M dwarf stars with the aim of searching for short period planets, but also for the first detection of stellar pulsations on this spectral type. Both science goals are the primary objectives of the “Cool Tiny Beats” (CTB) survey, which has produced most of the data used in this thesis. CTB data consist in high resolution and high-cadence spectroscopic Doppler measurements taken either with HARPS or HARPS-N spectrographs.

First of all, a thorough understanding of the spectrographs response in the short time domain was performed to characterize the sources of noise in our range of study. Our first approach to the goals of this thesis consisted in the design of an observational experiment to delve into the HARPS-N sub-night performance. Results unveiled variability of the spectra continuum correlated with instabilities of the spectrograph illumination associated to the airmass. Such distortions, which are wavelength and time dependent, are also present in at least one of the data-products given by the HARPS-N reduction software: the width of the mean-line profiles (i.e. the so-called FWHM index), an index commonly used as a proxy of the stellar activity. As a consequence, we searched for an alternative approach to measure the width index. In particular, we calculated the mean-line profile of the spectrum with a least-squares-deconvolution technique and we obtained the profile indices as the moments of the profile distribution. As part of this study, we also corroborated that the radial velocities calculated with our template matching algorithm TERRA are not affected by the illumination stability. This work unveiled a possible failure of the HARPS-N atmospheric dispersion corrector (or ADC) and outlined two possible solutions: either the FWHM measurements need to be decorrelated with the changes of flux on the spectra as a function of wavelength, or the spectra need to be corrected very precisely before deriving proxies for the mean line profiles.

In the second part of this dissertation, and taking advantage of the above characterization of systematic effects in the sub-night domain, I present the first CTB results regarding the detection of stellar pulsations in M dwarfs. The detection of such pulsations would open a new field of study for these stars, namely the field of asteroseismology. The asteroseismology tools allow to calculate very precisely the star physical parameters, thus improving the calculation of the bulk properties of any orbiting planet. This part of the thesis is focused on GJ 588 and GJ 699 (Barnard’s star), two of the most long-term stable M dwarfs observed by HARPS and other high-precision surveys. Firstly in this section, I detail the procedures applied to correct the CTB data from known instrumental effects such as the charge transfer efficiency, the seeing effect, or the wavelength calibration 1−2 m/s night-to-night jumps produced by the wavelength calibration. Later, we used likelihood periodograms to unveil periodical signals embedded in the range of periods where stellar pulsations are predicted. Neither the radial velocities nor the time-series of the second order moment of the mean- line profile showed confident detections. In spite of that, our study with injected sinusoids indicates that signals above the \(\sim\)0.5 m/s threshold would be detected in 90% of the cases. In other words, this is an upper limit of sensibility showing that stellar pulsations in the predicted range of periods from 20 min to 3 h can be detected with four consecutive nights of observations provided that their amplitudes are larger than \(\sim\)0.5 m/s. This result combined with some tentative detection of some signals below this threshold motivates us to keep searching for M dwarf stellar pulsations.

The third part of this thesis presents our main results regarding the detection of extrasolar planets around nearby M dwarfs. The low temperatures of the M dwarfs atmospheres, as well as their intrinsic low masses compared with other spectral types, result in closer habitable zones (i.e. the range of orbital distances where a planet could maintain liquid water on its surface) and in Earth-mass rocky planets within this zone detectable with the current instrumentation. Moreover, the large abundance of M dwarfs in the solar vicinity (\(\sim\)70%) make the planetary systems around M dwarf stars to be rather unique for the interesting follow-up opportunities they offer. These characteristics motivate our search for planets around M dwarf stars. Firstly in this part, I describe the detection of two Earth-mass planet candidates hosted by Luyten’s star. The minimum masses of the planets are 1.11 and 2.13M\(_\oplus\) for Luyten b and c, respectively. Luyten b orbits very close to the star with a 4.7-day period, while, Luyten c, with a 18.6-day period orbit, lies within the optimistic estimation of the habitable zone. Later in this part, I detail our discovery of Kapteyn’s star b and c planets. They correspond to two super-Earth mass planets of which planet-b is considered as potentially habitable. Finally, I also describe our more recent discovery of an Earth-mass planet orbiting in the habitable zone of our closest neighbor Proxima Centauri: Proxima b. This study incorporated the experience acquired during this thesis regarding the characterization of the instrumental effects in the short-time domain of M dwarfs. In fact, we used for the first time in this study the moments of the least-square-deconvolution profiles as indices to monitor the shape of the mean-line profiles of Proxima.

Finally, the last part of this dissertation comprises the development of an astronomical instrumentation project, with the aim of improving the radial velocity precision limit attained by an spectrograph. In particular, we focus on correcting the distortions caused by illumination instabilities in fiber-fed spectrographs. I describe our first prototype, the Radiance Characterizer in two dimensions (RadiCa2D), which was specifically designed to correct the Doppler measurements of the CAFE spectrograph. The main underlying idea of RadiCa2D consists in simultaneously monitoring the illumination distortions inside the spectrograph, to correct, in real-time, the effects generated in the final radial velocity measurements. This project is still under development and the final performance of the corrector needs yet to be confirmed.

Notes

234 pages. Funding from FPI BES-2011-049647 of MINECO/Spain.

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References

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