The missing link: A 4-day period transiting exoplanet around OGLE-TR-111

By F. Pont, F. Bouchy, D. Queloz, Nuno C. Santos, C. Melo, M. Mayor, S. Udry. 2004

133 citations recorded by the source corpus.

We report the discovery of a transiting hot Jupiter around OGLE-TR-111, from our radial velocity follow-up of OGLE transiting candidates in Carina. The planet has a mass of $0.53 \pm 0.11$  M J and a radius of $1.0^{+0.13}_{-0.06}$  R J . Three transiting exoplanets have already been found among OGLE candidates, all with periods near 1.5 days. The planet presented here, with $P=4.0$ days, is the first exoplanet detected by transits with the characteristics of a “normal” hot Jupiter, as found in abundance by radial velocity surveys. The radius of OGLE-TR-111b and the scarcity of hot Jupiters detected among OGLE transit candidates tend to indicate that the case of HD 209458b, with a radius of 1.4  R J , is exceptional, with most hot Jupiters being smaller.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/208c6c45d334524f07235c407b527df3a4827581

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Jon Fortney
2. J. Southworth
3. D. Charbonneau
4. J. Winn
5. N. Madhusudhan
6. A. Showman
7. M. Marley
8. H. Knutson

In Instrumentation

1. J. Southworth
2. Jon Fortney
3. J. Winn
4. D. Charbonneau
5. M. Marley
6. H. Knutson
7. A. Showman
8. Sara Seager

Citations in the corpus

• The Rossiter-McLaughlin Effect and Analytic Radial Velocity Curves for Transiting Extrasolar Planetary Systems (2004, methodology): “…et al. 2004) and OGLE-TR 10, 56, 111, 113, 132 by the Optically Gravitational Lens Event survey (e.g., Udalski et al. 2002c, 2002b, 2002a, 2003; Konacki et al. 2003; Bouchy et al. 2004; Pont et al. 2004), TrES-1 has similar orbital period and mass to those of HD 209458b, but its radius is smaller.”
• 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).”
• A correlation between the heavy element content of transiting extrasolar planets and the metallicity of their parent stars (2006, unknown): “…et al. (2002); [4] Bouchy et al. (2005a); [5] Santos et al. (2006); [6] Bouchy et al. (2004); [7] Moutou et al. (2004); [8] Pont et al. (2006); [9] Pont et al. (2004); [10] Konacki et al. (2005); [11] Holman et al. (2005); [12] Sozzetti et al. (2004); [13] Sato et al. (2005); [14] Charbonneau et…”
• ELODIE metallicity-biased search for transiting Hot Jupiters. II. A very hot Jupiter transiting the bright K star HD 189733 (2005, methodology): “Within the past two years, 6 exoplanets have been discovered first by the photometric observation of a transit in front of the stellar disk and then confirmed by spectroscopic followup: OGLE-TR-56b (Konacki et al. 2003), OGLE-TR-113b and 132b (Bouchy et al. 2004), TrES-1 (Alonso et al. 2004), OGLE- ”
• 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).”
• Spectroscopic metallicities for planet-host stars: Extending the samples (2005, background): “To these we add the transiting planets detected by the OGLE survey (Konacki et al. 2003; Bouchy et al. 2004; Pont et al. 2004), three currently with poor estimates giventh low quality of the now available spectra, as well as TrEs-1 (Alonso et al. 2004).”
• Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2 (2007, background): “An alternative measure of intrinsic brightness (or evolution) that has been used in the past is the spectroscopically determined value of log g (see, e.g., Konacki et al. 2003, 2004, 2005; Pont et al. 2004; Bouchy et al. 2005; Santos et al. 2006).”
• Atmosphere, Interior, and Evolution of the Metal-rich Transiting Planet HD 149026b (2005, background): “The transiting planet most similar in mass to HD 149026b, OGLE-Tr111b, has a mass of 0.53 MJ and a radius of ∼1 RJ (Pont et al. 2004).”
• 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).”
• DHP Framework: Digital Health Passports Using Blockchain - Use case on international tourism during the COVID-19 pandemic (2004, background): “…transit searches are being carried out which are starting to yield an handful of giant planets (Charbonneau et al. 2000; Konacki et al. 2003; Pont et al. 2004; Konacki et al. 2004; Bouchy et al. 2004; Alonso et al. 2004), and many more planned searches should reap a large harvest of…”
• Dynamics and Disequilibrium Carbon Chemistry in Hot Jupiter Atmospheres, with Application to HD 209458b (2006, unknown): “…of transiting planets OGLETR-56b (Konacki et al. 2003), OGLE-TR-113b and 132b (Bouchy et al. 2004), TrES-1 (Alonso et al. 2004), OGLETR-111b (Pont et al. 2004), OGLE TR-10b (Bouchy et al. 2005a; Konacki et al. 2005), HD 149026b (Sato et al. 2005), and HD 189733b (Bouchy et al. 2005b)…”
• Homogeneous studies of transiting extrasolar planets – I. Light-curve analyses (2008, background): “This work Pont et al. (2004) Winn et al. (2007b) Minniti et al. (2007) rA + rb 0.0952± 0.0044 0.0943 0.09288 k 0.1316± 0.0023 0.1209 0.132± 0.002 0.1245+0.0050 −0.0030 i (◦) 88.11± 0.66 86.5 to 90.0 88.1± 0.3 87.0 to 90.0 rA 0.0842± 0.0038 0.0841 0.0926 +0.006 −0.011 rb 0.01107± 0.00067 0.01017…”
• The effect of red noise on planetary transit detection (2006, background): “2The OGLE survey has been up to now the most successful survey for transiting planets in terms of detections, five confirmed planets (Konacki et al. 2003; Bouchy et al. 2004; Pont et al. 2004; Bouchy et al. 2005; Konacki et al. 2005) and 177 published transit candidates.”
• A trend filtering algorithm for wide-field variability surveys (2004, unknown): “…yet for bright Galactic field stars, based on the OGLE survey of faint Galactic Bulge stars and the very low number of positive cases obtained by spectroscopic follow-ups (Alonso et al. 2004; Pont et al. 2004, and references therein), the predicted low incidence rate could be close to reality.”