Hartman, J. D. and Bakos, G. Á. and Torres, G. and Latham, D. W. and Kovács, Géza and Béky, B. and Quinn, S. N. and Mazeh, T. and Shporer, A. and Marcy, G. W. and Howard, A. W. and Fischer, D. A. and Johnson, J. A. and Esquerdo, G. A. and Noyes, R. W. and Sasselov, D. D. and Stefanik, R. P. and Fernandez, J. M. and Szklenár, T. and Lázár, J. and Papp, I. and Sári, P. (2011) HAT-P-32b and HAT-P-33b: Two Highly Inflated Hot Jupiters Transiting High-jitter Stars. Astrophysical Journal, 742 (1). Art. No. 59. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:20111206-133628759
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We report the discovery of two exoplanets transiting high-jitter stars. HAT-P-32b orbits the bright V = 11.289 late-F-early-G dwarf star GSC 3281-00800, with a period P = 2.150008 ± 0.000001 d. The stellar and planetary masses and radii depend on the eccentricity of the system, which is poorly constrained due to the high-velocity jitter (~80 m s^(–1)). Assuming a circular orbit, the star has a mass of 1.16 ± 0.04 M_☉ and radius of 1.22 ± 0.02 R_☉, while the planet has a mass of 0.860 ± 0.164 M_J and a radius of 1.789 ± 0.025 R_J. The second planet, HAT-P-33b, orbits the bright V = 11.188 late-F dwarf star GSC 2461-00988, with a period P = 3.474474 ± 0.000001 d. As for HAT-P-32, the stellar and planetary masses and radii of HAT-P-33 depend on the eccentricity, which is poorly constrained due to the high jitter (~50 m s^(–1)). In this case, spectral line bisector spans (BSs) are significantly anti-correlated with the radial velocity residuals, and we are able to use this correlation to reduce the residual rms to ~35 m s^(–1). We find that the star has a mass of 1.38 ± 0.04 M_☉ and a radius of 1.64 ± 0.03 R_☉ while the planet has a mass of 0.762 ± 0.101 M_J and a radius of 1.686 ± 0.045 R_J for an assumed circular orbit. Due to the large BS variations exhibited by both stars we rely on detailed modeling of the photometric light curves to rule out blend scenarios. Both planets are among the largest radii transiting planets discovered to date.
|Additional Information:||© 2011 The American Astronomical Society. Received 2011 June 6; accepted 2011 September 28; published 2011 November 3. Based in part on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology. Keck time has been granted by NOAO (A285Hr, A146Hr, A201Hr, A289Hr), NASA (N128Hr, N145Hr, N049Hr, N018Hr, N167Hr, N029Hr), and the NOAO Gemini/Keck time-exchange program (G329Hr). HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G and SAO IR&D grants. Works of G. Á. B. and J. J. were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). G.T. acknowledges partial support from NASA grant NNX09AF59G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (PI:D.W.L.). G.K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. This research has made use of Keck telescope time granted through NOAO (A285Hr, A146Hr, A201Hr, A289Hr), NASA (N128Hr, N145Hr, N049Hr, N018Hr, N167Hr, N029Hr), and the NOAO Gemini/Keck time-exchange program (G329Hr). We gratefully acknowledge F. Bouchy, F. Pont, and the SOPHIE team for their efforts in gathering OHP/SOPHIE observations of HAT-P-33.|
|Subject Keywords:||planetary systems; stars: individual (HAT-P-32, GSC 3281-00800, HAT-P-33, GSC 2461-00988); techniques: photometric; techniques: spectroscopic|
|Official Citation:||HAT-P-32b and HAT-P-33b: Two Highly Inflated Hot Jupiters Transiting High-jitter Stars J. D. Hartman et al. 2011 ApJ 742 59|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||06 Dec 2011 22:58|
|Last Modified:||26 Dec 2012 14:34|
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