Measurement of the Rossiter–McLaughlin Effect in the Transiting Exoplanetary System TrES-1 | Zendy

Norio Narita | Zendy; Keigo Enya | Zendy; Bun’ei Sato | Zendy; Yasuhiro Ohta | Zendy; Joshua N. Winn | Zendy; Yasushi Suto | Zendy; Atsushi Taruya | Zendy; Edwin L. Turner | Zendy; Wako Aoki | Zendy; Yoichi Tamura | Zendy; Tōru Yamada | Zendy; Yuzuru Yoshii | Zendy

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Measurement of the Rossiter–McLaughlin Effect in the Transiting Exoplanetary System TrES-1

Author(s) -

Norio Narita,

Keigo Enya,

Bun’ei Sato,

Yasuhiro Ohta,

Joshua N. Winn,

Yasushi Suto,

Atsushi Taruya,

Edwin L. Turner,

Wako Aoki,

Yoichi Tamura,

Tōru Yamada,

Yuzuru Yoshii

Publication year - 2007

Publication title -

publications of the astronomical society of japan

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 1.99

H-Index - 110

eISSN - 2053-051X

pISSN - 0004-6264

DOI - 10.1093/pasj/59.4.763

Subject(s) - physics , transit (satellite) , exoplanet , lambda , planetary system , astrophysics , radial velocity , trojan , eccentricity (behavior) , subaru telescope , astronomy , orbital eccentricity , stars , orbit (dynamics) , sky , spectral line , optics , public transport , engineering , political science , spectrograph , law , aerospace engineering

We report a measurement of the Rossiter--McLaughlin effect in the transitingextrasolar planetary system TrES-1, via simultaneous spectroscopic andphotometric observations with the Subaru and MAGNUM telescopes. By modeling theradial velocity anomaly that was observed during a transit, we determine thesky-projected angle between the stellar spin axis and the planetary orbitalaxis to be $\lambda = 30 \pm 21$ [deg]. This is the third case for which$\lambda$ has been measured in a transiting exoplanetary system, and the firstdemonstration that such measurements are possible for relatively faint hoststars ($V \sim 12$, as compared to $V \sim 8$ for the other systems). We alsoderive a time of mid-transit, constraints on the eccentricity of the TrES-1borbit ($e = 0.048 \pm 0.025$), and upper limits on the mass of the Trojancompanions ($\lesssim$14 $M_{\oplus}$) at the 3$\sigma$ level.Comment: 8 pages, 5 figures, 2 tables. Published in PASJ. Corrected typo

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