Volume 558, October 2013
|Number of page(s)||10|
|Section||Planets and planetary systems|
|Published online||09 October 2013|
HAT-P-42b and HAT-P-43b
Centro de Astrofísica, Universidade do Porto,
Rua das Estrelas, 4150-762
2 Princeton University, Department of Astrophysical Sciences, Princeton, NJ, USA
3 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
4 Konkoly Observatory, Budapest, Hungary
5 Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark
6 Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, 1350 Copenhagen, Denmark
7 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
8 LCOGT, 6740 Cortona Drive, Santa Barbara, CA, USA
9 Department of Physics, Broida Hall, University of California, Santa Barbara, CA 93106, USA
10 Institute for Astronomy, University of Hawaii, Honolulu, HI, USA
11 Hungarian Astronomical Association, Budapest, Hungary
12 Department of Physics and Astrophysics, University of North Dakota, Grand Forks, ND, USA
Accepted: 14 April 2013
Aims. We announce the discovery of two new transiting planets, and provide their accurate initial characterization.
Methods. First identified from the HATNet wide-field photometric survey, these candidate transiting planets were then followed-up with a variety of photometric observations. Determining the planetary nature of the objects and characterizing the parameters of the systems were mainly done with the SOPHIE spectrograph at the 1.93 m telescope at OHP and the TRES spectrograph at the 1.5 m telescope at FLWO.
Results. HAT-P-42b and HAT-P-43b are typical hot Jupiters on circular orbits around early-G/late-F main sequence host stars, with periods of 4.641878 ± 0.000032 and 3.332687 ± 0.000015 days, masses of 1.044 ± 0.083 and 0.662 ± 0.060 MJ, and radii of 1.280 ± 0.153 and 1.28+0.062-0.033RJ, respectively. These discoveries increase the sample of planets with measured mean densities, which are needed to constrain theories of planetary interiors and atmospheres. Moreover, their hosts are relatively bright (V < 13.5), which facilitates further follow-up studies.
Key words: planetary systems / techniques: radial velocities / techniques: photometric / stars: individual: HAT-P-42 / stars: individual: HAT-P-43
Full Table 2 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/558/A86
The photometric/spectroscopic data presented in this paper are based in part on observations carried out by the Hungarian-made Automated Telescope Network, using telescopes operated at the Fred Lawrence Whipple Observatory (FLWO) of the Smithsonian Astrophysical Observatory (SAO), and at the Submillimeter Array (SMA) of SAO, by the Tillinghast Reflector 1.5 m telescope and the 1.2 m telescope, both operated by SAO at FLWO, by the SOPHIE spectrograph mounted on the 1.93 m telescope at Observatoire de Haute Provence, France (runs DDT-Dec. 2011), by the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, and by the facilities of the Las Cumbres Observatory Global Telescope.
© ESO, 2013
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