Constraints on a second planet in the WASP-3 system

Journal Article · Sun Dec 01 00:00:00 EST 2013 · Astronomical Journal (New York, N.Y. Online)

DOI:https://doi.org/10.1088/0004-6256/146/6/147· OSTI ID:22340077

Maciejewski, G.; Niedzielski, A.; Nowak, G.; Deka, B.; Adamów, M.; Górecka, M. ^[1]; Wolszczan, A. ^[2]; Neuhäuser, R.; Errmann, R.; Seeliger, M. ^[3]; Winn, J. N.; McKnight, L. ^[4]; Fernández, M.; Aceituno, F. J. ^[5]; Ohlert, J. ^[6]; Dimitrov, D. ^[7]; Latham, D. W.; Esquerdo, G. A.; Holman, M. J. ^[8]; Jensen, E. L. N. ^[9] ; others, and

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1. Centre for Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Torun (Poland)
2. Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 (United States)
3. Astrophysikalisches Institut und Universitäts-Sternwarte, Schillergässchen 2-3, D-07745 Jena (Germany)
4. Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139 (United States)
5. Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía 3, E-18008 Granada (Spain)
6. Michael Adrian Observatorium, Astronomie Stiftung Trebur, D-65468 Trebur (Germany)
7. Institute of Astronomy, Bulgarian Academy of Sciences, 72 Tsarigradsko Chausse Blvd., 1784 Sofia (Bulgaria)
8. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
9. Department of Physics and Astronomy, Swarthmore College, Swarthmore, PA 19081 (United States)

There have been previous hints that the transiting planet WASP-3b is accompanied by a second planet in a nearby orbit, based on small deviations from strict periodicity of the observed transits. Here we present 17 precise radial velocity (RV) measurements and 32 transit light curves that were acquired between 2009 and 2011. These data were used to refine the parameters of the host star and transiting planet. This has resulted in reduced uncertainties for the radii and masses of the star and planet. The RV data and the transit times show no evidence for an additional planet in the system. Therefore, we have determined the upper limit on the mass of any hypothetical second planet, as a function of its orbital period.

• OSTI ID: 22340077
• Journal Information: Astronomical Journal (New York, N.Y. Online), Vol. 146, Issue 6; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-3881
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
DIAGRAMS
LIMITING VALUES
MASS
PERIODICITY
PLANETS
RADIAL VELOCITY
SATELLITES
STARS
VISIBLE RADIATION
WASPS