OGLE-TR-132

OGLE-TR-132 is a distant magnitude 15.72 star in the star fields of the constellation Carina. Because of its great distance, about 4,900 light-years, and location in the crowded field it was not notable in any way. The spectral type of the star is type F. A yellow-white, very metal-rich dwarf star, it is slightly hotter and more luminous than the Sun.

OGLE-TR-132
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Carina[1]
Right ascension  10h 50m 34.72s[1]
Declination –61° 57′ 25.9″[1]
Apparent magnitude (V) 15.72[1]
Distance4,892 ly
(1,500[2] pc)
Spectral typeF[3]
Database references
SIMBADdata
Extrasolar Planets
Encyclopaedia		data

Planetary system

In 2003 the Optical Gravitational Lensing Experiment (OGLE) detected periodic dimming in the star's light curve indicating a transiting, planetary-sized object.[1] Since low-mass red dwarfs and brown dwarfs may mimic a planet radial velocity measurements were necessary to calculate the mass of the body. In 2004 the object was proved to be a new transiting extrasolar planet, OGLE-TR-132b.[3]

The OGLE-TR-132 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.14 ± 0.12 MJ 0.0306 ± 0.0008 1.689868 ± 0.000003 0 — —
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See also

References
  1. Udalski, A.; et al. (2003). "The Optical Gravitational Lensing Experiment. Additional Planetary and Low-Luminosity Object Transits from the OGLE 2001 and 2002 Observational Campaigns". Acta Astronomica. 53: 133. arXiv:astro-ph/0306444. Bibcode:2003AcA....53..133U.
  2. Santos, N. C.; et al. (2006). "Chemical abundances for the transiting planet host stars OGLE-TR-10, 56, 111, 113, 132, and TrES-1". Astronomy and Astrophysics. 458 (3): 997–1005. arXiv:astro-ph/0606758. Bibcode:2006A&A...458..997S. doi:10.1051/0004-6361:20065683.
  3. Bouchy, F.; et al. (2004). "Two new "very hot Jupiters" among the OGLE transiting candidates". Astronomy and Astrophysics. 421: L13–L16. arXiv:astro-ph/0404264. Bibcode:2004A&A...421L..13B. doi:10.1051/0004-6361:20040170.


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