TY - JOUR
T1 - A new spectroscopic and photometric analysis of the transiting planet systems TrES-3 and TrES-4
AU - Sozzetti, Alessandro
AU - Torres, Guillermo
AU - Charbonneau, David
AU - Winn, Joshua N.
AU - Korzennik, Sylvain G.
AU - Holman, Matthew J.
AU - Latham, David W.
AU - Laird, John B.
AU - Fernandez, José
AU - O'Donovan, Francis T.
AU - Mandushev, Georgi
AU - Dunham, Edward
AU - Everett, Mark E.
AU - Esquerdo, Gilbert A.
AU - Rabus, Markus
AU - Belmonte, Juan A.
AU - Deeg, Hans J.
AU - Brown, Timothy N.
AU - Hidas, Márton G.
AU - Baliber, Nairn
PY - 2009/2/1
Y1 - 2009/2/1
N2 - We report new spectroscopic and photometric observations of the parent stars of the recently discovered transiting planets TrES-3 and TrES-4. A detailed abundance analysis based on high-resolution spectra yields [Fe/H] = -0.19 ± 0.08, T eff = 5650 ± 75 K, and log g = 4.4 ± 0.1 for TrES-3, and [Fe/H] = +0.14 ± 0.09, T eff = 6200 ± 75 K, and log g = 4.0 ± 0.1 for TrES-4. The accuracy of the effective temperatures is supported by a number of independent consistency checks. The spectroscopic orbital solution for TrES-3 is improved with our new radial velocity measurements of that system, as are the light-curve parameters for both systems based on newly acquired photometry for TrES-3 and a reanalysis of existing photometry for TrES-4. We have redetermined the stellar parameters taking advantage of the strong constraint provided by the light curves in the form of the normalized separation a/R * (related to the stellar density) in conjunction with our new temperatures and metallicities. The masses and radii we derive are M * = 0.928+0.028 -0.048 M , R * = 0.829 +0.015 -0.022 R , and M * = 1.404+0.066 -0.134 M , R * = 1.846+0.096 -0.087 R for TrES-3 and TrES-4, respectively. With these revised stellar parameters, we obtain improved values for the planetary masses and radii. We find Mp = 1.910+0.075 -0.080 M Jup, Rp = 1.336+0.031 -0.036 R Jup for TrES-3, and Mp = 0.925 ± 0.082 M Jup, Rp = 1.783+0.093 -0.086 R Jup for TrES-4. We confirm TrES-4 as the planet with the largest radius among the currently known transiting hot Jupiters.
AB - We report new spectroscopic and photometric observations of the parent stars of the recently discovered transiting planets TrES-3 and TrES-4. A detailed abundance analysis based on high-resolution spectra yields [Fe/H] = -0.19 ± 0.08, T eff = 5650 ± 75 K, and log g = 4.4 ± 0.1 for TrES-3, and [Fe/H] = +0.14 ± 0.09, T eff = 6200 ± 75 K, and log g = 4.0 ± 0.1 for TrES-4. The accuracy of the effective temperatures is supported by a number of independent consistency checks. The spectroscopic orbital solution for TrES-3 is improved with our new radial velocity measurements of that system, as are the light-curve parameters for both systems based on newly acquired photometry for TrES-3 and a reanalysis of existing photometry for TrES-4. We have redetermined the stellar parameters taking advantage of the strong constraint provided by the light curves in the form of the normalized separation a/R * (related to the stellar density) in conjunction with our new temperatures and metallicities. The masses and radii we derive are M * = 0.928+0.028 -0.048 M , R * = 0.829 +0.015 -0.022 R , and M * = 1.404+0.066 -0.134 M , R * = 1.846+0.096 -0.087 R for TrES-3 and TrES-4, respectively. With these revised stellar parameters, we obtain improved values for the planetary masses and radii. We find Mp = 1.910+0.075 -0.080 M Jup, Rp = 1.336+0.031 -0.036 R Jup for TrES-3, and Mp = 0.925 ± 0.082 M Jup, Rp = 1.783+0.093 -0.086 R Jup for TrES-4. We confirm TrES-4 as the planet with the largest radius among the currently known transiting hot Jupiters.
KW - planetary systems
KW - stars: abundances
KW - stars: fundamental parameters
KW - stars: individual (TrES-3, TrES-4)
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UR - http://www.scopus.com/inward/citedby.url?scp=66649108998&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/691/2/1145
DO - 10.1088/0004-637X/691/2/1145
M3 - Article
AN - SCOPUS:66649108998
SN - 0004-637X
VL - 691
SP - 1145
EP - 1158
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -