CaltechAUTHORS
Published January 20, 2012 | Version Published
Journal Article Open

Hat-P-25b: A Hot-Jupiter Transiting a Moderately Faint G Star

Creators

  • 1. ROR icon Harvard-Smithsonian Center for Astrophysics
  • 2. ROR icon Konkoly Observatory
  • 3. ROR icon Yale University
  • 4. ROR icon California Institute of Technology
  • 5. ROR icon University of California, Berkeley
  • 6. ROR icon University of Copenhagen
  • 7. ROR icon University of South Dakota
  • 8. ROR icon Hungarian Astronomical Association

Abstract

We report the discovery of HAT-P-25b, a transiting extrasolar planet orbiting the V = 13.19 G5 dwarf star GSC 1788-01237, with a period P = 3.652836 ± 0.000019 days, transit epoch T_c = 2455176.85173 ± 0.00047 (BJD—barycentric Julian dates throughout the paper are calculated from Coordinated Universal Time, UTC), and transit duration 0.1174 ± 0.0017 days. The host star has a mass of 1.01 ± 0.03 M_☉, radius of 0.96^(+0.05)_(– 0.04) R_☉, effective temperature 5500 ± 80 K, and metallicity [Fe/H] = +0.31 ± 0.08. The planetary companion has a mass of 0.567 ± 0.022 M_J and radius of 1.190^(+0.081)_(–0.056) R_J yielding a mean density of 0.42 ± 0.07 g cm^(–3).

Additional Information

© 2012 American Astronomical Society. Received 2010 August 20; accepted 2011 November 4; published 2011 December 29. Based in part on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology. Keck time has been granted by NOAO (A201Hr), NASA (N018Hr and N167Hr), and the NASA Gemini-Keck time-exchange program (G329Hr). Based in part on observations made with 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. HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR&D grants. Work of G.Á.B. and J. Johnson were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). G.T. acknowledges partial support from NASA grant NNX09AF59G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (PI: D.W. Latham). G.K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. This research has made use of Keck telescope time granted through NOAO (A201Hr), NASA (N018Hr and N167Hr), and the NASA Gemini-Keck time-exchange program (G329Hr). This research has also made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.

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Additional details

Identifiers

Eprint ID
29968
Resolver ID
CaltechAUTHORS:20120404-072516851

Funding

NASA
NNG04GN74G
NASA
NNX08AF23G
Smithsonian Astrophysical Observatory
NSF Astronomy and Astrophysics Fellowship
AST-0702843
NSF Astronomy and Astrophysics Fellowship
AST-0702821
NASA
NNX09AF59G
NASA
NCC2-1390
Hungarian Scientific Research Foundation (OTKA)
K-81373
National Optical Astronomy Observatory (NOAO)
A201Hr
NASA
N018Hr
NASA
N167Hr
NASA
G329Hr
NASA/JPL/Caltech

Dates

Created
2012-04-04
Created from EPrint's datestamp field
Updated
2021-11-09
Created from EPrint's last_modified field