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THE CALIFORNIA PLANET SURVEY I. FOUR NEW GIANT EXOPLANETS1 Andrew W

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THE CALIFORNIA PLANET SURVEY I. FOUR NEW GIANT EXOPLANETS1 Andrew W Submitted to ApJ A Preprint typeset using LTEXstyleemulateapjv.08/13/06 THE CALIFORNIA PLANET SURVEY I. FOUR NEW GIANT EXOPLANETS1 Andrew W. Howard2,3,JohnAsherJohnson4, Geoffrey W. Marcy2, Debra A. Fischer5, Jason T. Wright6, David Bernat6, Gregory W. Henry7,KathrynM.G.Peek2, Howard Isaacson5,KevinApps8,MichaelEndl9, William D. Cochran9,JeffA.Valenti10, Jay Anderson10,andNikolaiE.Piskunov11 Submitted to ApJ ABSTRACT We present precise Doppler measurements of four stars obtained during the past decade at Keck Observatory by the California Planet Survey (CPS). These stars, namely, HD 34445, HD 126614, HD13931, and Gl179, all show evidence for a single planet in Keplerian motion. We also present Doppler measurements from the Hobby-Eberly Telescope (HET)fortwoofthestars,HD34445and Gl 179, that confirm the Keck detections and significantly refine the orbital parameters. These planets add to the statistical properties of giant planets orbiting near or beyond the ice line, and merit follow- up by astrometry, imaging, and space-borne spectroscopy. Their orbital parameters span wide ranges of planetary minimum mass (M sin i =0.38–1.9MJup), orbital period (P =2.87–11.5yr), semi-major axis (a =2.1–5.2AU),andeccentricity(e =0.02–0.41). HD34445b (P =2.87yr, M sin i =0.79MJup, e =0.27)isamassiveplanetorbitinganold,G-typestar.Weannounce a planet, HD 126614 Ab, and an Mdwarf,HD126614B,orbitingthemetal-richstarHD126614(which we now refer to as HD 126614 A). The planet, HD 126614 Ab, has minimum mass M sin i =0.38MJup and orbits the stellar primary with period P =3.41yrandorbitalseparationa=2.3AU.ThefaintM dwarfcompanion, HD 126614 B, is separated from the stellar primary by 489 mas (33 AU) and was discovered with direct observations using adaptive optics and the PHARO camera at Palomar Observatory. The stellar primary in this new system, HD 126614 A, has the highest measured metallicity([Fe/H] = +0.56) of any known planet- bearing star. HD 13931b (P =11.5yr,M sin i =1.88MJup, e =0.02)isaJupiteranalogorbitinganear solar twin. Gl 179 b (P =6.3yr, M sin i =0.82MJup, e =0.21)isa massiveplanetorbitinga faintM dwarf. The high metallicity of Gl 179 is consistent with the planet-metallicity correlation among M dwarfs, as documented recently by Johnson & Apps. Subject headings: planetary systems — stars: individual (HD 34445, HD 126614, HD 13931, Gl 179) —binaries:visual—techniques:radialvelocity—techniques: photometric — techniques: high angular resolution 1. INTRODUCTION yond the “snow line” and migrate inward on a time scale The distributions of the masses and orbits of jovian- that competes with the lifetime of the protoplanetary mass exoplanets offer key tests of planet formation the- disk (Thommes et al. 2008; Ida & Lin 2008; Rice & Ar- ory. Most theories predict that giant planets form be- mitage 2005; Alibert et al. 2005; Trilling et al. 2002). Among various theories for formation, core accretion has 1 Based on observations obtained at the W. M. Keck Observa- been shown efficient at producing, within ∼3Myr,plan- tory, which is operated jointly by the University of California and ets of Neptune to Jupiter mass, orbiting within 5 AU the California Institute of Technology. Keck time has been granted (Benz et al. 2008; Dodson-Robinson et al. 2008). by both NASA and the University of California. Two of the planets announced here are also based on observations obtained with the These models of giant planet formation and orbital Hobby-Eberly Telescope, which is a joint project of the University evolution may be directly tested against observations of Texas at Austin, the Pennsylvania State University, Stanford of giant planets found by the Doppler method. The University, Ludwig-Maximilians-Universit¨at M¨unchen, and Georg- models predict a clearing of gaps in the protoplanetary August-Universit¨at G¨ottingen. 2 Department of Astronomy, University of California, Berkeley, disks, establishing the distribution of planet masses, al- CA 94720-3411 USA lowing a direct comparison with Doppler observed min- 3 Townes Fellow, Space Sciences Laboratory, University of Cali- imum masses (M sin i). According to the models, the fornia, Berkeley, CA 94720-7450 USA; [email protected] disk dissipates after the planets have undergone some 4 Department of Astrophysics, California Institute of Technol- ogy, MC 249-17, Pasadena, CA 91125, USA inward migration, leaving them at their current orbital 5 Department of Astronomy, Yale University, New Haven, CT distances. The resulting predicted distribution of semi- 06511, USA 6 major axes can be compared with the observed orbits The Pennsylvania State University, University Park, PA 16802 of giant planets. There remains potential value in both 7 Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville,TN enhancing the sophistication of planet formation theory 37209 USA and in observing a large enough statistical sample of gi- 8 75B Cheyne Walk, Horley, Surrey RH6 7LR, UK ant planets to permit robust and informative tests of the 9 McDonald Observatory, University of Texas at Austin, Austin, TX 78712, USA theory. Moreover, planet-planet interactions among gi- 10 Space Telescope Science Institute, 3700 San Martin Dr., Bal- ant planets must be predicted and compared with the timore, MD 21218, USA distributions of orbital elements (especially eccentricity) 11 Department of Astronomy and Space Physics, Uppsala Uni- for systems containing multiple giant planets, e.g. Wright versity, Box 515, 751 20 Uppsala, Sweden et al. (2009); Ford & Chiang (2007); Ford & Rasio (2008); 2 Howard et al. Juri´c& Tremaine (2008). Giant planets also gravitation- ∼1yr,constitutinganastrophysical“noise”,compromis- ally interact with the dust in their planetary system to ing the detection of the terrestrial planets. Thus, future shape, on timescales of only years, the dust evolution of astrometric missions will benefit greatly from ∼15 yr of the planetary system (Lisse et al. 2007; Beichman et al. radial velocity (RV) data. The characterization of both 2007; Payne et al. 2009). giant and rocky planets will be important for future mis- As of May 2009, 350 exoplanets have been discov- sions that image and take spectra of planets, such as ered, with remarkable properties including close-in or- the Terrestrial Planet Finder and Darwin (Kaltenegger bits, large orbital eccentricities, multi-planet systems, et al. 2006; Lawson et al. 2008). As a result we con- and orbital resonances (Mayor & Udry 2008; Marcy et al. tinue to survey nearby stars that are likely targets for 2008). The hot jupiters have received the most attention, such surveys (Kaltenegger et al. 2010). Here we describe observationally and theoretically, yielding extraordinary Doppler measurements from Keck Observatory and from information about their chemical composition, internal the Hobby-Eberly Telescope (HET) for four stars that structure, atmospheric behavior. However most known shows signs of harboring a planet beyond 1 AU. gas giant planets orbit beyond 1 AU, realizing the pop- 2. ulation that formed beyond the ice line as predicted by STELLAR SAMPLE AND PROPERTIES theory, and as seen in our Solar System. Among the 1800 FGKM stars we monitor at the Keck In 1997, we began a Doppler search for giant planets telescope for giant planets, 1330 of them have been mon- in Jovian orbits at Keck Observatory. We monitor over itored from 1997 to the present with a precision of 1– 1800 stars within 50 pc, with special attention given to 3ms−1.Thesamplecontainsanearlyvolume-limited those within 20pc. We have acquired a Doppler time sample of stars within five bins of B − V color, between baseline of well over 8 yr for nearly all of them. The 0.60 and 1.5. It is nearly devoid of both binary stars sep- detected long-period exoplanets reveal the distribution arated by less than 2"" due to mutual contamination at of their masses, semimajor axes, and orbital eccentrici- the slit of the spectrometer and magnetically active stars ties for the general population of planetary systems. Re- younger than 1Gyr due to their excessive velocity “jit- markably, the exoplanets exhibit a sharp rise in occur- ter” (Wright 2005). The complete list of target stars is rence beyond 1 AU (Johnson et al. 2007b; Cumming et al. given in Wright et al. (2004) including the stars that do 2008), indicating a great population of giant planets re- not have detected planets, permitting statistical analyses sides there. Many of these planets remain undiscovered of the frequency of planets, e.g. Johnson et al. (2007a); even after 10 yr of Doppler monitoring, as the amplitudes Cumming et al. (2008); Butler et al. (2006). of a few meters per second require high Doppler preci- Only 7% of our stars surveyed for a decade reveal clear sion and a clear indication of Keplerian motion, which is Keplerian Doppler variations at a 3-σ limit of 10 m s−1. challenging for orbital periods comparable to the dura- However Cumming et al. (2008) accounted for incom- tion of observations. Nonetheless, the analysis of Doppler pleteness in our Doppler survey and predicted that ∼18% completeness shows that 15–18% of all nearby stars have of FGK stars harbor a gas giant of saturn mass or above giant planets between 3–20 AU (Cumming et al. 2008). within 20 AU. This prediction suggests that another 11% Surely, these giant planets offer strong statistical infor- of our target stars harbor giant planets yet to be revealed, mation on the formation and subsequent dynamical evo- with continued monitoring. The four stars presented here lution of gas giants in general. presumably harbor some of these giant planets by pre- Unfortunately, with only a decade of data orbits be- dicted Cumming et al. (2008). yond 4AU are just coming into our Doppler field of We measure atmospheric parameters of the target stars view. The recently announced Jupiter-analog orbiting by LTE spectroscopic analysis of our Keck/HIRES spec- HD 154345 with a =5.0AU(anda circularorbit)exhib- tra using the “SME” (Spectroscopy Made Easy) code ited nearly one full orbital period only after 10 full years (Valenti & Piskunov 1996) as implemented by Valenti & of Doppler data were collected (Wright et al.
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