The Exoplanet Orbit Database

By Jason T. Wright, Onsi Fakhouri, G. Marcy, E. Han, Ying Feng, J. Johnson, Andrew W. Howard, Debra A. Fischer, J. Valenti, Jay Anderson and 1 more. 2010

428 citations recorded by the source corpus.

We present a database of well-determined orbital parameters of exoplanets, and their host stars’ properties. This database comprises spectroscopic orbital elements measured for 427 planets orbiting 363 stars from radial velocity and transit measurements as reported in the literature. We have also compiled fundamental transit parameters, stellar parameters, and the method used for the planets discovery. This Exoplanet Orbit Database includes all planets with robust, well measured orbital parameters reported in peer-reviewed articles. The database is available in a searchable, filterable, and sortable form online through the Exoplanets Data Explorer table, and the data can be plotted and explored through the Exoplanet Data Explorer plotter. We use the Data Explorer to generate publication-ready plots, giving three examples of the signatures of exoplanet migration and dynamical evolution: We illustrate the character of the apparent correlation between mass and period in exoplanet orbits, the different selection biases between radial velocity and transit surveys, and that the multiplanet systems show a distinct semimajor-axis distribution from apparently singleton systems.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a68f8e1f7b9f4144049537c766be3faec5b54786

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Citations in the corpus

Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, methodology): “The observational data was taken from exoplanets.org (Wright et al. 2011) on 23.3.2012.”
Parametrizing the exoplanet eccentricity distribution with the beta distribution. (2013, methodology): “As an example, we downloaded the eccentricites for all planets (413) discovered via RV from www.exoplanets.org (Wright et al. 2011) on April 4th 2013.”
THE MASS OF KOI-94d AND A RELATION FOR PLANET RADIUS, MASS, AND INCIDENT FLUX (2013, methodology): “This population of planets was compiled from exoplanets.org (Wright et al. 2011), which was queried on September 27, 2012.”
CHARACTERIZING K2 PLANET DISCOVERIES: A SUPER-EARTH TRANSITING THE BRIGHT K DWARF HIP 116454 (2014, methodology): “We used the Exoplanet Orbit Database34 (Wright et al. 2011; Han et al. 2014) to compare HIP 116454b to other transiting sub-Neptune sized planets orbiting bright stars.”
Optimized transit detection algorithm to search for periodic transits of small planets (2019, methodology): “…limit of Rp/Rs < 0.05 ∼ 5.4 R⊕/R on the planet-to-star radius ratio and retrieve the orbital inclination (i), semimajor axis in units of stellar radii (a/Rs), Rp/Rs, and the orbital period (P) for all transiting Kepler planets from the Exoplanet Orbit Database (exoplanets.org; Wright et al. 2011).”
MOST 1.6 EARTH-RADIUS PLANETS ARE NOT ROCKY (2014, background): “To date, more than 200 transiting planets have measured masses (e.g., exoplanets.org, Wright et al. 2011).”
Defining and cataloging exoplanets: the exoplanet.eu database (2011, methodology): “This new version has been followed by two other professional online databases: the NStED Database at http:// nsted.ipac.caltech.eduand the Exoplanet Data Explorer at http://exoplanets.org (Wright et al. 2011), the later providing some online tools.”
The Occurrence and Architecture of Exoplanetary Systems (2014, background): “The debris disk has an inclination of 26±3◦ (Matthews et al. 2014), whereas the star has an inclination >∼ 40◦ according to the asteroseismic analysis of Wright et al. (2011a).”
Kepler Planet Masses and Eccentricities from TTV Analysis (2016, methodology): “The radial velocity (RV) method has provided the majority of exoplanet mass and eccentricity measurements to date (e.g., exoplanets.org; Wright et al. 2011).”
An Open Catalog for Supernova Data (2016, background): “For relatively young sub-fields in astronomy, such as the exoplanet community, many have advocated for open data access (Wright et al. 2011; Rein 2012), and the result has been an abundance of rapid scientific progress enabled not just by the data collectors, but also the broader community with…”
The NASA Exoplanet Archive: Data and Tools for Exoplanet Research (2013, background): “For example, the Extrasolar Planet Encyclopedia (Schneider et al. 2011, http://exoplanet.eu/) has been operating since 1995 and includes a comprehensive list of confirmed and retracted exoplanets, and the Exoplanet Orbit Database (Wright et al. 2011, http://exoplanets.org) maintains a database of pl”
ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES (2012, methodology): “…the λi are the observed angles, σ λ i the observational errors, and N(x;µ, σ) is the Gaussian PDF with 6 The spin–orbit observations reported at http://exoplanets.org (Wright et al. 2011), include data from Simpson et al. (2011); Narita et al. (2010); Triaud et al. (2010); Queloz et al. (2010);…”
REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, background): “Since thousands of exoplanets and exoplanet candidates have been discovered (Schneider et al. 2011; Wright et al. 2011), we are now in a position to study the statistical attributes of the ensemble of known exoplanets.”
UNDERSTANDING THE MASS–RADIUS RELATION FOR SUB-NEPTUNES: RADIUS AS A PROXY FOR COMPOSITION (2013, methodology): “We used masses and radii from exoplanets.org (Wright et al. 2011), except for where there are more recent values in the literature.”
THE IMPACT OF STELLAR MULTIPLICITY ON PLANETARY SYSTEMS. I. THE RUINOUS INFLUENCE OF CLOSE BINARY COMPANIONS (2016, background): “Radial velocity surveys and ground-based transit searches have discovered nearly 1000 confirmed planets around other stars (Wright et al. 2011) and thousands of additional candidates (Borucki et al. 2010; Batalha et al. 2013; Burke et al. 2014), revolutionizing the demography of planetary systems…”
THE STATISTICS OF MULTI-PLANET SYSTEMS (2011, methodology): “We determine the observable multiplicity function for RV planets using all planets with FGK dwarf host stars in the exoplanets.org database (Wright et al. 2011) as of 2010 (A color version of this figure is available in the online journal.)”