Matias Diaz

The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey

This document is the Accepted Manuscript version of the following article: R. Paul Butler, et al, The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey, The Astronomical Journal, Vol 153 (5), 19 pp., published 13 April 2017. The Version of Record is available online at doi: https://doi.org/10.3847/1538-3881/aa66ca. Paper data available at: http://home.dtm.ciw.edu/ebps/data/.

New planetary systems from the Calan-Hertfordshire Extrasolar planet search

We report the discovery of eight new giant planets, and updated orbits for four known planets, orbiting dwarf and subgiant stars using the CORALIE, HARPS, and MIKE instruments as part of the Calan–Hertfordshire Extrasolar Planet Search. The planets have masses in the range 1.1–5.4 M J ’s, orbital periods from 40 to 2900 d, and eccentricities from 0.0 to 0.6. They include a double-planet system orbiting the most massive star in our sample (HD147873), two eccentric giant planets (HD128356 b and HD154672 b ), and a rare 14 Herculis analogue (HD224538 b ). We highlight some population correlations from the sample of radial velocity detected planets orbiting nearby stars, including the mass function exponential distribution, confirmation of the growing body of evidence that low-mass planets tend to be found orbiting more metal-poor stars than giant planets, and a possible period–metallicity correlation for planets with masses >0.1 M J , based on a metallicity difference of 0.16 dex between the population of planets with orbital periods less than 100 d and those with orbital periods greater than 100 d.

THE LICK-CARNEGIE EXOPLANET SURVEY: HD 32963—A NEW JUPITER ANALOG ORBITING A SUN-LIKE STAR

We present a set of 109 new, high-precision Keck/HIRES radial velocity (RV) observations for the solar-type star HD 32963. Our dataset reveals a candidate planetary signal with a period of 6.49

Fast Convergence Delayed Signal Cancellation Method for Sequence Component Separation

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NO EVIDENCE for ACTIVITY CORRELATIONS in the RADIAL VELOCITIES of KAPTEYN'S STAR

0.07 years and a corresponding minimum mass of 0.7

MagAO IMAGING of LONG-PERIOD OBJECTS (MILO). I. A BENCHMARK M DWARF COMPANION EXCITING A MASSIVE PLANET AROUND the SUN-LIKE STAR HD 7449

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Model Predictive Control of Modular Multilevel Matrix Converter

0.03 Jupiter masses. Given Jupiters crucial role in shaping the evolution of the early Solar System, we emphasize the importance of long-term radial velocity surveys. Finally, using our complete set of Keck radial velocities and correcting for the relative detectability of synthetic planetary candidates orbiting each of the 1,122 stars in our sample, we estimate the frequency of Jupiter analogs across our survey at approximately 3%.

A novel LVRT control strategy for Modular Multilevel Matrix Converter based high-power Wind Energy Conversion Systems

Delayed signal cancellation is one of the methods used to separate the negative- and positive-sequence components in unbalanced 3φ systems. In this letter, a DSC methodology with fast convergence time is proposed and it is shown that an improved separation of the positive and negative sequences is feasible. Experimental results are presented to demonstrate the performance of the proposed methodology.

Analysis of synchronous and stationary reference frame control strategies to fulfill LVRT requirements in Wind Energy Conversion Systems

This is an author-created, un-copyedited version of an article published in The Astrophysical Journal. IOP Publishing is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The version of record is available online at: https://doi.org/10.3847/0004-637X/830/2/74

Balancing energy and low frequency operation of the Modular Multilevel Converter in Back to Back configuration

We present high-contrast Magellan adaptive optics (MagAO) images of HD 7449, a Sun-like star with one planet and a long-term radial velocity (RV) trend. We unambiguously detect the source of the long-term trend from 0.6-2.15 \microns ~at a separation of \about 0\fasec 54. We use the objects colors and spectral energy distribution to show that it is most likely an M4-M5 dwarf (mass \about 0.1-0.2 \msun) at the same distance as the primary and is therefore likely bound. We also present new RVs measured with the Magellan/MIKE and PFS spectrometers and compile these with archival data from CORALIE and HARPS. We use a new Markov chain Monte Carlo procedure to constrain both the mass (