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30 results on '"Noyes, Robert W."'

2. DISCOVERY OF A TRANSITING PLANET AND EIGHT ECLIPSING BINARIES IN HATNet FIELD G205

Author

Latham, David W., primary, Bakos, Gáspár Á., additional, Torres, Guillermo, additional, Stefanik, Robert P., additional, Noyes, Robert W., additional, Kovács, Géza, additional, Pál, András, additional, Marcy, Geoffrey W., additional, Fischer, Debra A., additional, Butler, R. Paul, additional, Sipőcz, Brigitta, additional, Sasselov, Dimitar D., additional, Esquerdo, Gilbert A., additional, Vogt, Steven S., additional, Hartman, Joel D., additional, Kovács, Gábor, additional, Lázár, József, additional, Papp, István, additional, and Sári, Pál, additional

Published
2009
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3. HAT-P-9b: A LOW-DENSITY PLANET TRANSITING A MODERATELY FAINT F STAR

Author

Shporer, Avi, primary, Bakos, GÁspÁr Á., additional, Bouchy, Francois, additional, Pont, Frederic, additional, Kovács, Géza, additional, Latham, Dave W., additional, Sipöcz, Brigitta, additional, Torres, Guillermo, additional, Mazeh, Tsevi, additional, Esquerdo, Gilbert A., additional, Pál, András, additional, Noyes, Robert W., additional, Sasselov, Dimitar D., additional, Lázár, József, additional, Papp, István, additional, Sári, Pál, additional, and Kovács, Gábor, additional

Published
2008
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7. Transit Photometry of the Core‐dominated Planet HD 149026b

Author

Charbonneau, David, primary, Winn, Joshua N., additional, Latham, David W., additional, Bakos, Gaspar, additional, Falco, Emilio E., additional, Holman, Matthew J., additional, Noyes, Robert W., additional, Csak, Balazs, additional, Esquerdo, Gilbert A., additional, Everett, Mark E., additional, and O’Donovan, Francis T., additional

Published
2006
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8. Measurement of Spin‐Orbit Alignment in an Extrasolar Planetary System

Author

Winn, Joshua N., primary, Noyes, Robert W., additional, Holman, Matthew J., additional, Charbonneau, David, additional, Ohta, Yasuhiro, additional, Taruya, Atsushi, additional, Suto, Yasushi, additional, Narita, Norio, additional, Turner, Edwin L., additional, Johnson, John A., additional, Marcy, Geoffrey W., additional, Butler, R. Paul, additional, and Vogt, Steven S., additional

Published
2005
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12. Evidence for Multiple Companions to υ Andromedae

Author

Butler, R. Paul, primary, Marcy, Geoffrey W., additional, Fischer, Debra A., additional, Brown, Timothy M., additional, Contos, Adam R., additional, Korzennik, Sylvain G., additional, Nisenson, Peter, additional, and Noyes, Robert W., additional

Published
1999
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16. A Planet Orbiting the Star ρ Coronae Borealis

Author

Noyes, Robert W., primary, Jha, Saurabh, additional, Korzennik, Sylvain G., additional, Krockenberger, Martin, additional, Nisenson, Peter, additional, Brown, Timothy M., additional, Kennelly, Edward J., additional, and Horner, Scott D., additional

Published
1997
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21. HAT-P-9b: A LOW-DENSITY PLANET TRANSITING A MODERATELY FAINT F STAR

Author

Shporer, Avi, Bakos, GAspAr A., Bouchy, Francois, Pont, Frederic, Kovacs, Geza, Latham, Dave W., Sipocz, Brigitta, Torres, Guillermo, Mazeh, Tsevi, Esquerdo, Gilbert A., Pal, Andras, Noyes, Robert W., Sasselov, Dimitar D., Lazar, Jozsef, Papp, Istvan, Sari, Pal, and Kovacs, Gabor

Abstract

We report the discovery of a planet transiting a moderately faint (V = 12.3 mag) late F star, with an orbital period of 3.92289 +- 0.00004 days. From the transit light curve and radial velocity measurements, we determine that the radius of the planet is Rp = 1.40 +- 0.06 R Jup and that the mass is Mp = 0.78 +- 0.09 M Jup. The density of the new planet, r p = 0.35 +- 0.06 g cm-3, fits to the low-density tail of the currently known transiting planets. We find that the center of transit is at T c = 2454417.9077 +- 0.0003 (HJD), and the total transit duration is 0.143 +- 0.004 days. The host star has M [?] = 1.28 +- 0.13 M and R [?] = 1.32 +- 0.07 R .

Published
2009

22. Hubble Space Telescope Time-Series Photometry of the Transiting Planet of HD 209458

Author

Brown, Timothy M., Charbonneau, David, Gilliland, Ronald L., Noyes, Robert W., and Burrows, Adam

Abstract

We have observed four transits of the planet of HD 209458 using the STIS spectrograph on the Hubble Space Telescope (HST). Summing the recorded counts over wavelength between 582 and 638 nm yields a photometric time series with 80 s time sampling and relative precision of about 1.1 x 10-4 per sample. The folded light curve can be fitted within observational errors using a model consisting of an opaque circular planet transiting a limb-darkened stellar disk. In this way we estimate the planetary radius Rp = 1.347 +- 0.060 RJup, the orbital inclination i = 86.deg6 +- 0.deg14, the stellar radius R* = 1.146 +- 0.050 R, and one parameter describing the stellar limb darkening. Our estimated radius is smaller than those from earlier studies but is consistent within measurement errors and also with theoretical estimates of the radii of irradiated Jupiter-like planets. Satellites or rings orbiting the planet would, if large enough, be apparent from distortions of the light curve or from irregularities in the transit timings. We find no evidence for either satellites or rings, with upper limits on satellite radius and mass of 1.2 R[?] and 3 M[?], respectively. Opaque rings, if present, must be smaller than 1.8 planetary radii in radial extent. The high level of photometric precision attained in this experiment confirms the feasibility of photometric detection of Earth-sized planets circling Sun-like stars.

Published
2001

23. Evidence for Multiple Companions to Andromedae

Author

Butler, Paul, Marcy, Geoffrey W., Fischer, Debra A., Brown, Timothy M., Contos, Adam R., Korzennik, Sylvain G., Nisenson, Peter, and Noyes, Robert W.

Abstract

The bright F8 V star u Andromedae was previously reported to have a 4.6 day Doppler velocity periodicity, consistent with having a Jupiter-mass companion orbiting at 0.059 AU. Follow-up observations by both the Lick and Advanced Fiber-Optic Echelle spectrometer (AFOE) planet survey programs confirm this periodicity and reveal additional periodicities at 241 and 1267 days. These periodicities are consistent with Keplerian orbital motion and imply two additional companions orbiting at 0.83 and 2.5 AU, with minimum (M sin i) masses of 2.0 and 4.6 MJUP, respectively. Non-Keplerian explanations for the observed Doppler velocity variations, including radial and nonradial pulsations, rotational modulation of surface features, and stellar magnetic cycles, are examined. These explanations seem unlikely based on the observed photometric and chromospheric stability of the star. This putative three-planet system is found to be dynamically stable by both analytic techniques and numerical simulations. The outer two companions both reside in eccentric orbits, as do all nine known extrasolar planet candidates in distant orbits. If real, this multiple-planet system is the first around a main-sequence star, and its study should offer insights into planet formation, planet-planet interactions, and the observed eccentricities of planetary orbits.

Published
1999

24. A Radial Velocity Search for p-Mode Pulsations in ? Bootis

Author

Brown, Timothy M., Kennelly, Edward J., Korzennik, Sylvain G., Nisenson, Peter, Noyes, Robert W., and Horner, Scott D.

Abstract

The subgiant ? Boo (G5 IV) has been reported to show p-mode pulsations, as evidenced by variations in the equivalent width of its hydrogen Balmer lines (reported by Kjeldsen et al.). In an attempt to confirm this report, we observed ? Boo's radial velocity with the AFOE spectrograph for a total of 22 hours spread over seven successive nights in 1995 March. We find no evidence for the presence of excess power at the frequencies reported by Kjeldsen et al.; our upper limit corresponds to typical mode amplitudes of 0.5 m s-1, about 3 times smaller than the velocity amplitudes they inferred. Signals with amplitudes larger than 0.5 m s-1may be present at other frequencies within the 0-1000 ?Hz range, but evidence for such signals is scanty, and typical mode amplitudes greater than 1.5 m s-1are clearly inconsistent with our observations.

Published
1997
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