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|Title:||The N2K consortium. III. short-period planets orbiting HD 149143 and HD 109749|
|Citation:||Astrophysical Journal, 2006; 637(2):1094-1101|
|Publisher:||Univ Chicago Press|
|Debra A. Fischer, Gregory Laughlin, Geoffrey W. Marcy, R. Paul Butler, Steven S. Vogt, John A. Johnson, Gregory W. Henry, Chris McCarthy, Mark Ammons, Sarah Robinson, Jay Strader, Jeff A. Valenti, P. R. McCullough, David Charbonneau, Joshua Haislip, Heather A. Knutson, Daniel E. Reichart, Padric McGee, Berto Monard, Jason T. Wright, Shigeru Ida, Bun'ei Sato, and Dante Minniti|
|Abstract:||We report the detection of two short-period planets discovered at Keck Observatory. HD 149143 is a metal-rich G0 IV star with a planet of M sin i = 1.33MJ and an orbital radius of 0.053 AU. The best-fit Keplerian model has an orbital period, P = 4.072 days, semivelocity amplitude, K = 149.6 m s-1, and eccentricity, e = 0.016 ± 0.01. The host star is chromospherically inactive and metal-rich, with [Fe/H] = 0.26. Based on the Teff and stellar luminosity, we derive a stellar radius of 1.49 R☉. Photometric observations of HD 149143 were carried out using the automated photometric telescopes at Fairborn Observatory. HD 149143 is photometrically constant over the radial velocity period to 0.0003 ± 0.0002 mag, supporting the existence of the planetary companion. No transits were detected down to a photometric limit of approximately 0.02%, eliminating transiting planets with a variety of compositions and constraining the orbital inclination to less than 83°. A short-period planet was also detected around HD 109749, a G3 IV star. HD 109749 is chromospherically inactive, with [Fe/H] = 0.25 and a stellar radius of 1.24. The radial velocities for HD 109749 are modeled by a Keplerian with P = 5.24 days and K = 28.7 m s-1. The inferred planet mass is M sin i = 0.28MJ and the semimajor axis of this orbit is 0.0635 AU. Photometry of HD 109749 was obtained with the SMARTS consortium telescope, the PROMPT telescope, and by transitsearch.org observers in Adelaide and Pretoria. These observations did not detect a decrement in the brightness of the host star at the predicted ephemeris time, and they constrain the orbital inclination to less than 85° for gas giant planets with radii down to 0.7RJ.|
|Keywords:||planetary systems; stars: individual (HD 149143, HD 109749)|
|Rights:||© 2006. The American Astronomical Society|
|Appears in Collections:||Physics publications|
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