Frequency of Hot Jupiters and Very Hot Jupiters from the OGLE-III Transit Surveys toward the Galactic Bulge and Carina

Gould, A.; Dorscher, S.; Gaudi, B. S.; Udalski, A.

Artykuł - szczegóły

Tytuł artykułu

Frequency of Hot Jupiters and Very Hot Jupiters from the OGLE-III Transit Surveys toward the Galactic Bulge and Carina

Autorzy

Gould A. , Dorscher S. , Gaudi B. S. , Udalski A.

Wybrane pełne teksty z tego czasopisma

http://acta.astrouw.edu.pl/

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Języki publikacji

Abstrakty

We derive the frequencies of hot Jupiters (HJs) with 3-5 day periods and very hot Jupiters (VHJs) with 1-3 day periods by comparing the planets actually detected in the OGLE-III survey with those predicted by our models. The models are constructed following Gould and Morgan (2003) by populating the line of sight with stars drawn from the Hipparcos Catalogue. Using these, we demonstrate that the number of stars with sensitivity to HJs and VHJs is only 5-16% of those in the OGLE-III fields satisfying the spectroscopic-follow-up limit of V_max17.5 mag. Hence, the frequencies we derive are much higher than a naive estimate would indicate. We find that at 90% confidence the fraction of stars with planets in the two period ranges is (1/320)(1±[+1.37][-0.59]) for HJs and (1/710)(1±[+1.10][-0.54]) for VHJs. The HJ rate is statistically indistinguishable from that found in radial velocity (RV) studies. However, we note that magnitude-limited RV samples are heavily biased toward metal-rich (hence, planet-bearing) stars, while transit surveys are not, and therefore we expect that more sensitive transit surveys should find a deficit of HJs as compared to RV surveys. The detection of three transiting VHJs, all with periods less than 2 days, is marginally consistent with the complete absence of such detections in RV surveys. The planets detected are consistent with being uniformly distributed between 1.00 and 1.25 Jovian radii, but there are too few in the sample to map this distribution in detail.

Słowa kluczowe

planetary systems binaries: eclipsing Stars: fundamental parameters

Wydawca

Copernicus Foundation for Polish Astronomy

Czasopismo

Acta Astronomica

Rocznik

2006

Tom

Vol. 56, No. 1

Strony

1--50

Opis fizyczny

Bibliogr. 53 poz., tab., wykr.

Twórcy

autor

Gould A.

gould@astronomy.ohio-state.edu

Department of Astronomy, Ohio State University, 140W. 18th Ave., Columbus, OH43210, USA

autor

Dorscher S.

dorsher@astronomy.ohio-state.edu

Department of Astronomy, Ohio State University, 140W. 18th Ave., Columbus, OH43210, USA

autor

Gaudi B. S.

sgaudi@cfa.harvard.edu

Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA

autor

Udalski A.

udalski@astrouw.edu.pl

Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland

Bibliografia

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