The Transiting Extrasolar Giant Planet around the Star OGLE-TR-113

By Maciej Konacki, G. Torres, D. Sasselov, G. Pietrzyński, A. Udalski, S. Jha, M. Ruiz, W. Gieren, D. Minniti. 2004

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We report the independent discovery of a new extrasolar transiting planet around OGLE-TR-113, a candidate star from the Optical Gravitational Lensing Experiment. Small radial velocity variations have been detected based on observations conducted with the MIKE spectrograph on the Magellan I (Baade) telescope at the Las Campanas Observatory (Chile) during 2003. We have also carried out a light-curve analysis incorporating new photometry and realistic physical parameters for the star. OGLE-TR-113b has an orbital period of only 1.43 days, a mass of (1.08 ± 0.28)MJup, and a radius of (1.09 ± 0.10)RJup. Similar parameters have been obtained very recently in an independent study by Bouchy et al., from observations taken a year later. The orbital period of OGLE-TR-113b and the previously announced planet OGLE-TR-56b (Porb = 1.21 days)—the first two found photometrically—are much shorter than the apparent cutoff of close-in giant planets at 3-4 day periods found in high-precision radial velocity surveys. Along with a third case reported by Bouchy et al. (OGLE-TR-132b, Porb = 1.69 days), these objects appear to form a new class of "very hot Jupiters" that pose very interesting questions for theoretical study.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/aef34deda32e0147a7be9032b1318add3ca3945f

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Citations in the corpus

Prospects for the Characterization and Confirmation of Transiting Exoplanets via the Rossiter-McLaughlin Effect (2006, background): “…all of which were originally identified as candidates by the OGLE collaboration (Udalski et al. 2002a, 2002b, 2002c, 2003), and subsequently confirmed with radial velocity follow-up (Konacki et al. 2003a, 2003b, 2004, 2005; Bouchy et al. 2004, 2005b; Pont et al. 2004, 2005; Moutou et al. 2004).”
CHARACTERISTICS OF KEPLER PLANETARY CANDIDATES BASED ON THE FIRST DATA SET (2010, methodology): “when a transit occurs. Medium-precision radial velocity (RV) measurements are made to rule out stellar or brown dwarf mass companions and to better characterize the host star. A stellar –blend model (Torres et al. 2004) is used to check that the photometry is consistent with a planet orbiting a star”
Using Stellar Limb-Darkening to Refine the Properties of HD 209458b (2006, background): “…the radii of other transiting planets are within the predicted range of values for irradiated hot Jupiters (Torres et al. 2004; Moutou et al. 2004; Pont et al. 2004; Konacki et al. 2004; Laughlin et al. 2005b; Sato et al. 2005; Charbonneau et al. 2006b; Bouchy et al. 2005; Bakos et al. 2006).”
Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, methodology): “It was independently confirmed as a TEP by Konacki et al. (2004), also from the OGLE light curve and high-precision RVs, and an abundance analysis of the parent star has been presented by Santos et al. (2006).”
A giant planet candidate near a young brown dwarf - Direct VLT/NACO observations using IR wavefront sensing (2004, background): “In recent years, the field of extrasolar planet detection and characterization has been exclusively reserved to the domain of indirect detection measurements, radial velocity surveys (Fisher et al. 2003; Mayor et al. 2004) or transit detections (Charbonneau et al. 2000; Konacki et al. 2004).”
Efficient identification of exoplanetary transit candidates from SuperWASP light curves (2007, background): “Deeper surveys based on light curves from the Optical Gravitational Lensing Experiment (OGLE) project have produced a further five such planets (Konacki et al. 2003; Bouchy et al. 2004, Konacki et al. 2004; Pont et al. 2004; Konacki et al. 2005).”