T ~N Gautier

Publications (7)6.02 Total impact

• Article: KEPLER-21b: A 1.6 R-Earth PLANET TRANSITING THE BRIGHT OSCILLATING F SUBGIANT STAR HD 179070

  S B Howell, J F Rowe, S T Bryson, S N Quinn, G W Marcy, H Isaacson, D R Ciardi, W J Chaplin, T S Metcalfe, Mjpfg Monteiro, [......], J L Christiansen, C K Middour, M R Haas, J R Hall, J M Jenkins, S McCaulif, M N Fanelli, C Kulesa, D McCarthy, C E Henze
  [show abstract] [hide abstract]
  ABSTRACT: We present Kepler observations of the bright (V = 8.3), oscillating star HD 179070. The observations show transit-like events which reveal that the star is orbited every 2.8 days by a small, 1.6 R-Earth object. Seismic studies of HD 179070 using short cadence Kepler observations show that HD 179070 has a frequency-power spectrum consistent with solar-like oscillations that are acoustic p-modes. Asteroseismic analysis provides robust values for the mass and radius of HD 179070, 1.34 +/- 0.06 M-circle dot and 1.86 +/- 0.04 R-circle dot, respectively, as well as yielding an age of 2.84 +/- 0.34 Gyr for this F5 subgiant. Together with ground-based follow-up observations, analysis of the Kepler light curves and image data, and blend scenario models, we conservatively show at the >99.7% confidence level (3 sigma) that the transit event is caused by a 1.64 +/- 0.04 R-Earth exoplanet in a 2.785755 +/- 0.000032 day orbit. The exoplanet is only 0.04 AU away from the star and our spectroscopic observations provide an upper limit to its mass of similar to 10 M-Earth (2 sigma). HD 179070 is the brightest exoplanet host star yet discovered by Kepler.
  The Astrophysical Journal 02/2012; 746:123 (18pp). · 6.02 Impact Factor
• Source

  Available from: articles.adsabs.harvard.edu

  Article: Optimization of the Kepler Field of View

  Natalie M. Batalha, W. Borucki, D. A. Caldwell, H. Chandrasekaran, T. N. Gautier, J. Jenkins, D. G. Koch
  [show abstract] [hide abstract]
  ABSTRACT: The Kepler field was chosen by maximizing the numbers of stars, satisfying constraints on the ecliptic latitude, and ensuring sufficient ground-based resources for follow-up. The question is revisited in an effort to optimize the probability of detecting Earth-size planets in the habitable zone of late-type stars. The number density of stars as a function of galactic coordinates, apparent magnitude, spectral type, and luminosity class is simulated using the Besancon galactic model. Models generate synthetic star samples for specific coordinates and photometer constraints. From synthetic fields, we cull out the primary targets: stars bright and/or small enough to allow for detection of a 1 R⊕ planet within the habitable zone. We look to maximize the number of primary targets in the field. Using the number density of fainter background stars, we quantify the expected number of false-positives due to background eclipsing binaries. For each target, background stars are placed randomly in the photometric aperture. Half are selected as binaries using orbital period and eccentricity distributions as per Duquennoy and Mayor (1991). False positives are identified when a background binary injects a detectable photometric signal for which none of the following are observed: unequal secondary/primary eclipse depths, durations or epoch timings, or photocenter motion. Star counts (l=70) peak near b=+3 degrees and drop by 80% at b=+13. The number of primary targets, however, drops by only 10% in the same interval. The number of expected false positives drops dramatically with increasing galactic latitude. At b=+13, we expect no false positives mimicking habitable, Earth-size planets. A shift of 5-10 degrees in galactic latitude eliminates a significant source of false positives while preserving 90-95% of the primary targets. The Kepler field has, consequently, been moved to a higher galactic latitude centered at l=76.53, b=+13.29. Support for this work came from NASA's Discovery Program.
  11/2006; 38:1188.
• Source

  Available from: cips.berkeley.edu

  Conference Proceeding: KEPLER: Search for Earth-Size Planets in the Habitable Zone

  W Borucki, D Koch, N Batalha, D Caldwell, J Christensen-Dalsgaard, W ~D Cochran, E Dunham, T ~N Gautier, J Geary, R Gilliland, J Jenkins, H Kjeldsen, J ~J Lissauer, J Rowe
  IAU Symposium;
• Conference Proceeding: Finding Earth-size planets in the habitable zone: the Kepler Mission

  W Borucki, D Koch, G Basri, N Batalha, T Brown, D Caldwell, J Christensen-Dalsgaard, W Cochran, E Dunham, T ~N Gautier, J Geary, R Gilliland, J Jenkins, Y Kondo, D Latham, J ~J Lissauer, D Monet
  IAU Symposium;
• Article: The Kepler Mission: Astrophysics and Eclipsing Binaries

  D Koch, W Borucki, G Basri, T Brown, D Caldwell, J Christensen-Dalsgaard, W Cochran, E Dunham, T ~N Gautier, J Geary, R Gilliland, J Jenkins, Y Kondo, D Latham, J Lissauer, D Monet
  apss.
• Article: Kepler Planet-Detection Mission: Introduction and First Results

  W ~J Borucki, D Koch, G Basri, N Batalha, T Brown, D Caldwell, J Caldwell, J Christensen-Dalsgaard, W ~D Cochran, E DeVore, [......], E ~V Quintana, B ~D Clarke, C Allen, J Li, H Wu, P Tenenbaum, E Verner, F Bruhweiler, J Barnes, A Prsa
  Science. 327:977-.
• Article: Kepler's First Rocky Planet: Kepler-10b

  N ~M Batalha, W ~J Borucki, S ~T Bryson, L ~A Buchhave, D ~A Caldwell, J Christensen-Dalsgaard, D Ciardi, E ~W Dunham, F Fressin, T ~N Gautier, [......], R ~C Morehead, D Ragozzine, P Tenenbaum, J Twicken, S Quinn, J VanCleve, L ~M Walkowicz, W ~F Welsh, E Devore, A Gould
  apj. 729:27-+.