THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS

Journal Article · Fri Oct 01 00:00:00 EDT 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/721/2/1467· OSTI ID:21464761

Howard, Andrew W; Marcy, Geoffrey W; Peek, Kathryn M. G. ^[1]; Johnson, John Asher ^[2]; Fischer, Debra A; Isaacson, Howard ^[3]; Wright, Jason T; Bernat, David ^[4]; Henry, Gregory W ^[5]; Apps, Kevin ^[6]; Endl, Michael; Cochran, William D ^[7]; Valenti, Jeff A; Anderson, Jay ^[8]

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1. Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States)
2. Department of Astrophysics, California Institute of Technology, MC 249-17, Pasadena, CA 91125 (United States)
3. Department of Astronomy, Yale University, New Haven, CT 06511 (United States)
4. Pennsylvania State University, University Park, PA 16802 (United States)
5. Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209 (United States)
6. 75B Cheyne Walk, Horley, Surrey RH6 7LR (United Kingdom)
7. McDonald Observatory, University of Texas at Austin, Austin, TX 78712 (United States)
8. Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218 (United States)

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, HD 13931, and Gl 179, all show evidence for a single planet in Keplerian motion. We also present Doppler measurements from the Hobby-Eberly Telescope (HET) for two of the stars, HD 34445 and 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 = 0.38-1.9 M{sub Jup}), orbital period (P = 2.87-11.5 yr), semimajor axis (a = 2.1-5.2 AU), and eccentricity (e = 0.02-0.41). HD 34445 b (P = 2.87 yr, M sin i = 0.79 M{sub Jup}, e = 0.27) is a massive planet orbiting an old, G-type star. We announce a planet, HD 126614 Ab, and an M dwarf, HD 126614 B, orbiting the metal-rich star HD 126614 (which we now refer to as HD 126614 A). The planet, HD 126614 Ab, has minimum mass M sin i = 0.38 M{sub Jup} and orbits the stellar primary with period P = 3.41 yr and orbital separation a = 2.3 AU. The faint M dwarf companion, 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 13931 b (P = 11.5 yr, M sin i = 1.88 M{sub Jup}, e = 0.02) is a Jupiter analog orbiting a near solar twin. Gl 179 b (P = 6.3 yr, M sin i = 0.82 M{sub Jup}, e = 0.21) is a massive planet orbiting a faint M dwarf. The high metallicity of Gl 179 is consistent with the planet-metallicity correlation among M dwarfs, as documented recently by Johnson and Apps.

• OSTI ID: 21464761
• Journal Information: Astrophysical Journal, Vol. 721, Issue 2; Other Information: DOI: 10.1088/0004-637X/721/2/1467; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ASTRONOMY
ICE
JUPITER PLANET
MASS
METALS
RADIAL VELOCITY
SPECTROSCOPY
STARS
TELESCOPES
ELEMENTS
PLANETS
VELOCITY