Five New Extrasolar Planets

By G. Marcy, R. P. Butler, S. Vogt, Debra A. Fischer, G. Henry, Gregory Laughlin, Jason T. Wright, John A. Johnson. 2005

151 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d048b52bcde4374e55f97eb1841ceea0b8deacdb

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In Astronomy and Astrophysics

Citations in the corpus

Improving the Efficiency of Markov Chain Monte Carlo for Analyzing the Orbits of Extrasolar Planets (2005, methodology): “As noted by Marcy et al. (2005) the observations provide only modest constraints on the orbital parameters, since the orbital period is comparable to the duration of observations.”
Radial Velocity Jitter in Stars from the California and Carnegie Planet Search at Keck Observatory (2005, background): “Only after many planetary orbits with good phase coverage can one use the periodic nature of the signals and Keplerian fits to distinguish these signals from jitter (Marcy et al. 2005).”
State of the Field: Extreme Precision Radial Velocities (2016, methodology): “As noted by Marcy et al. (2005), the FAP test specifies the probability that incoherent noise could have yielded a superior Keplerian fit by chance.”
THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS (2010, methodology): “The Keplerian parameter uncertainties for each planet were derived using a Monte Carlo method (Marcy et al. 2005) and do not account for correlations between parameter errors.”
Prospects for the Characterization and Confirmation of Transiting Exoplanets via the Rossiter-McLaughlin Effect (2006, background): “It has been envisioned that the confirmation process will require measuring the orbital velocity of the parent star, and there is hope that this can be achieved, given the recent excellent progress in improving the accuracy of Doppler measurements (Mayor et al. 2003; Marcy et al. 2005).”
A Jovian-Mass Planet in Microlensing Event OGLE-2005-BLG-071 (2005, background): “…Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS, UK. czan & Frail 1992), radial velocities (Mayor et al. 2004; Marcy et al. 2005; references therein), and transits (Udalski et al. 2002; Konacki et al. 2003; Bouchy et al. 2004; Alonso et al. 2004), which rely…”
Limits on Planetary Companions from Doppler Surveys of Nearby Stars (2016, background): “…al. 2009, 2011a, 2011b, 2014), demonstration of the planet–metallicity correlation (Fischer et al. 2005), statistical studies of planet occurrence (Marcy et al. 2005a; Cumming et al. 2008; Howard et al. 2010b), and recently measurements of transiting planets discovered by NASAʼs Kepler Mission…”
Can Planets Survive Stellar Evolution? (2007, methodology): “Planet migration (e.g., Trilling et al. 1998; Armitage et al. 2002) is then used in order to explain the close distances at which such planets are observed around Sun-like stars (e.g., Mayor & Queloz 1995; Vidal-Madjar et al. 2004; Marcy et al. 2005).”
Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, background): “The four single-planet systems in the region τ > 9Gyr in and e > 0.6 in Figure 19, HD20782 (e = 0.92, Jones et al. 2006), HD45350 (e = 0.78, Marcy et al. 2005b), HD222582 (e = 0.76, Vogt et al. 2000) and HD3651 (e = 0.63, Fischer et al. 2003) are also good candidates where secular eccentricity…”
PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER (2011, background): “Not included here is an analysis of the orbital eccentricities that span the range e = 0–0.93 (e.g., Marcy et al. 2005b; Udry & Santos 2007; Moorhead et al. 2011), and the close-in “hot Jupiters” show a wide distribution of inclinations relative to the equatorial plane of the host star (Winn et al.…”
Five New Multicomponent Planetary Systems (2005, methodology): “The selection criteria for the target stars were described in Marcy et al. (2005).”
Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems (2006, background): “Through these discoveries, we are now poised to gain a better understanding of the environments of exoplanet systems and compare them to our Solar System.”
The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets (2008, methodology): “We systematically searched for planets by calculating the false alarm probability associated with Keplerian orbit fits to the data for each star (C04; Marcy et al. 2005b; O’Toole et al. 2007).”
Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs (2005, methodology): “Sample Description We performed a serendipitous analysis of stars observed at least once by the Keck, Lick, and AAT planet search programs (Cummings et al. 1999; Fischer et al. 1999; Butler et al. 2003; Marcy et al. 2004, 2005), so our sample is defined by the selection criteria of these programs.”
Circumstellar Dust Disks in Taurus-Auriga: The Submillimeter Perspective (2005, background): “Radial velocity surveys suggest that roughly 10% of stars harbor a gas giant planet within a few AU (e.g., Marcy et al. 2005), with the prospect that better sensitivity to long-period planets could significantly increase that fraction (e.g., Fischer et al. 2001).”
On the evolution of multiple protoplanets embedded in a protostellar disc (2006, background): “…and COROT will extend the discovery-space of extrasolar planets further, covering the sub-Neptune mass range where current observations typically cannot detect planets (e.g. Bonfils et al. 2005; Marcy et al. 2005; Rivera et al. 2005; Vogt et al. 2005; Santos et al. 2004; Butler et al. 2003, 2004).”
Catalog of Nearby Exoplanets (2006, methodology): “Butler et al. (2005) and Marcy et al. (2005a) analyze the properties and distribution of planets detected around 1330 FGKM dwarfs monitored at Lick, Keck, and the AAT, and discuss the biases in and uniformity of that sample.”