CATALOG OF NEARBY EXOPLANETS1R. P. Butler,2J. T. Wright,3G. W. Marcy,3,4D. A. Fischer,3,4S. S. Vogt,5C. G. Tinney,6H. R. A. Jones,7B. D. Carter,8J. A. Johnson,3C. McCarthy,2,4and A. J. Penny9,10Received 2005 November 5; accepted 2006 March 10ABSTRACTWe present a catalog of nearby exoplanets. It contains the 172 known low-mass companions with orbits establishedthrough radial velocity and transit measurements around stars within 200 pc. We include five previously unpublishedexoplanets orbiting the stars HD 11964, HD 66428, HD 99109, HD 107148, and HD 164922. We update orbit s for 83additional exoplanets, including many whose orbits have not been revised since their announcement, and includeradial velocity time series from the Lick, Keck, and Anglo-Australian Observatory planet searches. Both these newand previously published velocities are more precise here due to improvements in our data reduction pipeline, whichwe applied to archival spectra. We present a brief summary of the global properties of the known exoplanets,including their distributions of orbital semimajor axis, minimum mass, and orbital eccentricity.Subject headinggs: planetary systems — stars: a ctivity — stars: chromospheresOnline material: machine-readable tables1. INTRODUCTIONIt has now been more than 10 yr since the discovery of the firstobjects that were identified as planets orbiting normal stars. Theepochal announcement in 1995 October of 51 Peg b (Mayor &Queloz 1995) was confirmed within a week (Marcy et al. 1997)and followed within 2 months by two other planets, 47 UMa band 70 Vir b (Butler & Marcy 1996; Marcy & Butler 1996). Theunexpected diversity and mass distribution of exoplanets wasrepresented well by those first three planets, as the first one orbitsclose in, the second orbits beyond 2 AU, and the last resides in avery eccentric orbit. The paucity of companions having largermasses, with M sin i between 10MJand 80MJ, suggested a massdistribution separated from that of stars, rising with decreasingmass and peaking below 1MJ(Marcy & Butler 2000; Halbwachset al. 2000; Udry et al. 2003a).During the past 10 yr, over 160 exoplanet candidates havebeen identified orbiting stars within 200 pc, and most have beendetected by Doppler search programs based at the Keck, Lick,and Anglo-Australian Observatories (the California & Carnegieand Anglo-Australian planet searches; e.g., Butler et al. 1996;Tinney et al. 2001) and teams based at l’Observatoire de HauteProvence and La Silla Observatory (the Geneva ExtrasolarPlanet Search; e.g., Mayor & Santos 2003). Other Dopplerprograms have contributed important discoveries of nearbyplanets (Cochran et al. 1997; Endl et al. 2003; Noyes et al. 1999;Ku¨rster et al. 2003; Charbonneau et al. 2000; Sato et al. 2005).One nearby planet, TrES-1, has been discovered by its transitacross the star (Alonso et al. 2004).Here we present a catalog of all known exoplanets that residewithin 200 pc, containing the vast majority of well-studied exo-planets. This distance thresho ld serves several purposes. First,nearby planets and their host stars are amenable to confirmationand follow-up by a variety of techniques, including high-resolution imaging and stellar spectroscopy with high signal-to-noise ratios, as well as astrometric follow-up (e.g., Benedict et al.2001; McArthur et al. 2004). In addition, milliarcsecond as-trometry for planet host stars within 200 pc can provide precisedistance estimates, and most planet search target stars within100 pc already have parallaxes from Hipparcos ( Perryman et al.1997). Third, nearby planet host stars are bright enough to permitprecise photometric and chromospheric monitoring by telescopesof modest size, permitting careful assessment of velocity jitter,starspots, and possible transits (e.g., Henry 1999; Henry et al.2000; Queloz et al. 2001; Eaton et al. 2003).This paper updates the last published list of exoplanets (Butleret al. 2002). The growth of the field is reflected by the disco veryof over 100 planet s in the 3 yr since the publication of that list of57 exoplanets.About a dozen exoplanet candidates have been discoveredthat reside beyond 200 pc, including a ha lf-dozen in the Galacticbulge found in the OGLE survey and a few other planets foundby microlensing (e.g., Torres et al. 2003; Konacki et al. 2003;Bouchy et al. 2005a). Perhaps most notable are the first planetsever found outside our solar system, orbiting a pulsar (Wolszczan& Frail 1992). Such distant planets reside beyond the scope ofthis catalog.We include known companions with minimum masses (M sin i)up to 24MJ. This is well above the usual 13MJdeuterium-burninglimit for planets adopted by the IAU. We do this for two reasons.First, uncertainties in stellar mass and orbital inclination com-plicate the measurement of sufficiently precise masses to apply arobust 13MJcutoff. Second, there is little or no evidence indi-cating that such a cutoff has any relevance to the formationA1Based on observations obtained at the W. M. Keck Observatory, which isoperated jointly by the University of California and the California Institute ofTechnology. The Keck Observatory was made possible by the generous financialsupport of the W. M. Keck Foundation.2Department of Terrestrial Magnetism, Carnegie Institute of Washington,5241 Broad Branch Road NW, Washington, DC 20015-1305.3Department of Astronomy, University of California, 601 Campbell Hall,Berkeley, CA 94720-3411.4Department of Physics and Astronomy, San Francisco State University,1600 Holloway Avenue, San Francisco, CA 94132.5University of California Observatories/ Lick Observatory, University ofCalifornia, 373 Interdisciplinary Sciences, Santa Cruz, CA 95064.6Anglo-Australian Observatory, P.O. Box 296, Epping NSW 1710,Australia.7Centre for Astrophysics Research, University of Hertfordshire, Hatfield,AL 10 9AB, UK.8Faculty of Sciences, University of Southern Queensland, Toowoomba4350, Australia.9Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX, UK.10SETI Institute, 515 North Whisman Road, Mountain View, CA 94043.505The Astrophysical Journal, 646:505–522, 2006 July 20# 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A.mechanisms of these objects. We therefore use a generous min-imum mass criterion for inclusion in this catalog and decline tochoose a precise definition of an ‘‘exoplanet.’’Two other planet candidates were detected by direct imaging,2M 1207b (Chauvin et al. 2004) and GQ Lup b (
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