CaltechAUTHORS
  A Caltech Library Service

TrES-3: A Nearby, Massive, Transiting Hot Jupiter in a 31 Hour Orbit

O'Donovan, Francis T. and Charbonneau, David and Bakos, Gáspár Á. and Mandushev, Georgi and Dunham, Edward W. and Brown, Timothy M. and Latham, David W. and Torres, Guillermo and Sozzetti, Alessandro and Kovács, Géza and Everett, Mark E. and Baliber, Nairn and Hidas, Márton G. and Esquerdo, Gilbert A. and Rabus, Markus and Deeg, Hans J. and Belmonte, Juan A. and Hillenbrand, Lynne A. and Stefanik, Robert P. (2007) TrES-3: A Nearby, Massive, Transiting Hot Jupiter in a 31 Hour Orbit. Astrophysical Journal Letters, 663 (1). L37-L40. ISSN 2041-8205. https://resolver.caltech.edu/CaltechAUTHORS:20100419-103543556

[img]
Preview
PDF - Published Version
See Usage Policy.

75Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20100419-103543556

Abstract

We describe the discovery of a massive transiting hot Jupiter with a very short orbital period (1.30619 days), which we name TrES-3. From spectroscopy of the host star GSC 03089-00929, we measure T_(eff) = 5720 ± 150 K, log g = 4.6 ± 0.3, and v sin i < 2 km s^(-1) and derive a stellar mass of 0.90 ± 0.15 M_☉. We estimate a planetary mass of 1.92 ± 0.23 M_(Jup), based on the sinusoidal variation of our high-precision radial velocity measurements. This variation has a period and phase consistent with our transit photometry. Our spectra show no evidence of line bisector variations that would indicate a blended eclipsing binary star. From detailed modeling of our B and z photometry of the 2.5% deep transits, we determine a stellar radius 0.802 ± 0.046 R_☉ and a planetary radius 1.295 ± 0.081 R_(Jup). TrES-3 has one of the shortest orbital periods of the known transiting exoplanets, facilitating studies of orbital decay and mass loss due to evaporation, and making it an excellent target for future studies of infrared emission and reflected starlight.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/519793DOIArticle
http://iopscience.iop.org/1538-4357/663/1/L37PublisherArticle
ORCID:
AuthorORCID
Latham, David W.0000-0001-9911-7388
Torres, Guillermo0000-0002-5286-0251
Additional Information:© 2007 American Astronomical Society. Received 2007 April 27; accepted 2007 May 14; published 2007 June 14. We thank B. S. Gaudi for a useful discussion. We thank the referee for helpful comments that improved the Letter. This material is based on work supported by NASA under grants NNG04GN74G, NNG04LG89G, NNG05GI57G, NNG05GJ29G, and NNH05AB88I issued through the Origins of Solar Systems Program. We acknowledge support from the NASA Kepler mission under cooperative agreement NCC2-1390. Work by G.A. B. was supported by NASA through Hubble Fellowship Grant HSTHF- 01170.01-A. G. K. acknowledges the support of OTKA K-60750.
Funders:
Funding AgencyGrant Number
NASANNG04GN74G
NASANNG04LG89G
NASANNG05GI57G
NASANNG05GJ29G
NASANNH05AB88I
NASANCC2-1390
NASAHST-HF-01170.01-A
OTKAK-60750
Subject Keywords:planetary systems; stars: individual (GSC 03089–00929, GSC 03089–00929); techniques: photometric; techniques: radial velocities
Issue or Number:1
Record Number:CaltechAUTHORS:20100419-103543556
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20100419-103543556
Official Citation:Francis T. O'Donovan et al 2007 ApJ 663 L37 doi: 10.1086/519793
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:18015
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:19 Apr 2010 20:45
Last Modified:03 Oct 2019 01:36

Repository Staff Only: item control page