The<tt>rvfit</tt>Code: A Detailed Adaptive Simulated Annealing Code for Fitting Binaries and Exoplanets Radial Velocities

Iglesias-Marzoa, R.; López‐Morales, Mercedes; Morales, Maria

doi:10.1086/682056

Cited by 89 publications

(36 citation statements)

References 40 publications

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“…2 The best-fitting period for HD 92607 is 3.6993 ± 0.0001 d. Figure 3 shows the progression of He i λ5876 over this period. After our initial orbital fit converged on an eccentricity of zero, we fixed e = 0 for further fitting, allowing rvfit to treat ω and T p (which are ill-defined at very low eccentricities) in a consistent manner (see Iglesias-Marzoa et al 2015). The final best-fitting orbital solution is shown in Figure 4, and the orbital parameters are listed in Table 4.…”

Section: Hd 92607mentioning

confidence: 99%

“…Orbital and physical parameters of new and updated binary solutions. -amplitude RV variations and N obs ≥ 7 using the IDL package rvfit(Iglesias-Marzoa et al 2015). Spectroscopic binary orbits are defined by the following parameters: P (orbital period), e (eccentricity), γ (systemic velocity), ω (argument of periastron), T p (epoch of periastron), K 1 (primary semi-amplitude), and, where applicable, K 2 (secondary semi-amplitude).…”

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confidence: 99%

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A radial velocity survey of the Carina Nebula's O-type stars

Kiminki

Smith

2018

Monthly Notices of the Royal Astronomical Society

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We have obtained multi-epoch observations of 31 O-type stars in the Carina Nebula using the CHIRON spectrograph on the CTIO/SMARTS 1.5-m telescope. We measure their radial velocities to 1-2 km s −1 precision and present new or updated orbital solutions for the binary systems HD 92607, HD 93576, HDE 303312, and HDE 305536. We also compile radial velocities from the literature for 32 additional O-type and evolved massive stars in the region. The combined data set shows a mean heliocentric radial velocity of 0.6 km s −1 . We calculate a velocity dispersion of ≤ 9.1 km s −1 , consistent with an unbound, substructured OB association. The Tr 14 cluster shows a marginally significant 5 km s −1 radial velocity offset from its neighbor Tr 16, but there are otherwise no correlations between stellar position and velocity. The O-type stars in Cr 228 and the South Pillars region have a lower velocity dispersion than the region as a whole, supporting a model of distributed massive-star formation rather than migration from the central clusters. We compare our stellar velocities to the Carina Nebula's molecular gas and find that Tr 14 shows a close kinematic association with the Northern Cloud. In contrast, Tr 16 has accelerated the Southern Cloud by 10-15 km s −1 , possibly triggering further massive-star formation. The expansion of the surrounding H ii region is not symmetric about the O-type stars in radial velocity space, indicating that the ionized gas is constrained by denser material on the far side.

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Section: Hd 92607mentioning

confidence: 99%

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confidence: 99%

A radial velocity survey of the Carina Nebula's O-type stars

Kiminki

Smith

2018

Monthly Notices of the Royal Astronomical Society

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“…Pollacco et al 2006;Nutzman & Charbonneau 2008;Wheatley et al 2013;Burdanov et al 2017;Pepper et al 2018;Bakos 2018) surveys, along with ambitious space-based transit searches (Borucki et al 2010;Ricker et al 2015), has transformed and nurtured the known field today of extrasolar planets. These efforts have not only increased the number of known planets 2012; Parviainen 2015), radial-velocities (see, e.g., Meschiari et al 2009;Wright & Howard 2009;Baluev 2013;Iglesias-Marzoa et al 2015;Malavolta et al 2016;Fulton et al 2018;Faria et al 2018) or both (see, e.g., Bakos et al 2010;Hartman et al 2012;Espinoza et al 2016;Baluev 2018;Barragán et al 2019;Günther & Daylan 2019;Foreman-Mackey et al 2019), some of which even include the modelling of the stellar properties jointly with the modelling of the photometry and radial-velocities (Eastman et al 2013;Eastman 2017;Eastman et al 2019;Hartman et al 2018).…”

Section: Introductionmentioning

confidence: 99%

juliet: a versatile modelling tool for transiting and non-transiting exoplanetary systems

Espinoza

Kossakowski

Brahm

2019

Monthly Notices of the Royal Astronomical Society

264

253

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Here we present juliet, a versatile tool for the analysis of transits, radial-velocities, or both. juliet is built over many available tools for the modelling of transits, radialvelocities and stochastic processes (here modelled as Gaussian Processes; GPs) in order to deliver a tool/wrapper which can be used for the analysis of transit photometry and radial-velocity measurements from multiple instruments at the same time, using nested sampling algorithms which allows it to not only perform a thorough sampling of the parameter space, but also to perform model comparison via bayesian evidences. In addition, juliet allows to fit transiting and non-transiting multi-planetary systems, and to fit GPs which might share hyperparameters between the photometry and radial-velocities simultaneously (e.g., stellar rotation periods), which might be useful for disentangling stellar activity in radial-velocity measurements. Nested Sampling, Importance Nested Sampling and Dynamic Nested Sampling is performed with publicly available codes which in turn give juliet multi-threading options, allowing it to scale the computing time of complicated multi-dimensional problems. We make juliet publicly available via GitHub.

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“…Even if exoplanet archives do not have an unambigous convention about the ω value to adopt when e = 0, however we call out that the most popular standard that is adopted in the literature is ω = 90 • (see e.g. Eastman et al 2013;Iglesias-Marzoa et al 2015;Kreidberg 2015).…”

Section: Comments On Jump Parametersmentioning

confidence: 99%

MCMCI: A code to fully characterise an exoplanetary system

Bonfanti

Gillon

2020

A&A

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Context. Useful information can be retrieved by analysing the transit light curve of a planet-hosting star or induced radial velocity oscillations. However, inferring the physical parameters of the planet, such as mass, size, and semi-major axis, requires preliminary knowledge of some parameters of the host star, especially its mass or radius, which are generally inferred through theoretical evolutionary models. Aims. We seek to present and test a whole algorithm devoted to the complete characterisation of an exoplanetary system thanks to the global analysis of photometric or radial velocity time series combined with observational stellar parameters derived either from spectroscopy or photometry. Methods. We developed an integrated tool called MCMCI. This tool combines the Markov chain Monte Carlo (MCMC) approach of analysing photometric or radial velocity time series with a proper interpolation within stellar evolutionary isochrones and tracks, known as isochrone placement, to be performed at each chain step, to retrieve stellar theoretical parameters such as age, mass, and radius.Results. We tested the MCMCI on the HD 219134 multi-planetary system hosting two transiting rocky super Earths and on WASP-4, which hosts a bloated hot Jupiter. Even considering different input approaches, a final convergence was reached within the code, we found good agreement with the results already stated in the literature and we obtained more precise output parameters, especially concerning planetary masses. Conclusions. The MCMCI tool offers the opportunity to perform an integrated analysis of an exoplanetary system without splitting it into the preliminary stellar characterisation through theoretical models. Rather this approach favours a close interaction between light curve analysis and isochrones, so that the parameters recovered at each step of the MCMC enter as inputs for purposes of isochrone placement.A&A proofs: manuscript no. mcmcIsoc sits are expected to be available as a result of already active and forthcoming missions.Our unified approach of simultaneously modelling the star and its planets is remarkable even if it is not unique, since it has already been followed, for example by Hartman et al. (2019), who carry out an isochrone-based joint analysis using a differential evolution MCMC procedure (Ter Braak 2006) and PARSEC stellar evolutionary models (Marigo et al. 2017). Also Siverd et al. (2012) simultaneously model the stellar host and its companion, but to break the M -R degeneracy they simply consider the mass-radius relation by Torres et al. (2010), as they use the first version of the Idl fitting package EXOFAST (Eastman et al. 2013). We notice that our version of MCMC without the support of stellar evolutionary models also allows us to select a modified version of the Torres et al. (2010) M -R law from wellconstrained detached binary systems (Gillon et al. 2011); thus we can use this tool during the LC or RV fitting. Recently, a new version of the EXOFAST package called EXOFASTv2 has been released (Eastman et...

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The`rvfit`Code: A Detailed Adaptive Simulated Annealing Code for Fitting Binaries and Exoplanets Radial Velocities

Cited by 89 publications

References 40 publications

A radial velocity survey of the Carina Nebula's O-type stars

A radial velocity survey of the Carina Nebula's O-type stars

juliet: a versatile modelling tool for transiting and non-transiting exoplanetary systems

MCMCI: A code to fully characterise an exoplanetary system

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ThervfitCode: A Detailed Adaptive Simulated Annealing Code for Fitting Binaries and Exoplanets Radial Velocities

Cited by 89 publications

References 40 publications

A radial velocity survey of the Carina Nebula's O-type stars

A radial velocity survey of the Carina Nebula's O-type stars

juliet: a versatile modelling tool for transiting and non-transiting exoplanetary systems

MCMCI: A code to fully characterise an exoplanetary system

Contact Info

Product

Resources

About

The`rvfit`Code: A Detailed Adaptive Simulated Annealing Code for Fitting Binaries and Exoplanets Radial Velocities