Publication: The first extrasolar planet discovered with a new-generation high-throughput Doppler instrument
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2006-09-01
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We report the detection of the first extrasolar planet, ET-1 (HD 102195b), using the Exoplanet Tracker (ET), a new-generation Doppler instrument. The planet orbits HD 102195, a young star with solar metallicity that may be part of the local association. The planet imparts radial velocity variability to the star with a semiamplitude of 63.4 ± 2.0 m s^-1 and a period of 4.11 days. The planetary minimum mass (m sin i) is 0.488MJ ± 0.015M_J. The planet was initially detected in the spring of 2005 with the Kitt Peak National Observatory (KPNO) 0.9 m coudé feed telescope. The detection was confirmed by radial velocity observations with the ET at the KPNO 2.1 m telescope and also at the 9 m Hobby-Eberly Telescope (HET) with its High Resolution Spectrograph. This planetary discovery with a 0.9 m telescope around a V = 8.05 magnitude star was made possible by the high throughput of the instrument: 49% measured from the fiber output to the detector. The ET's interferometer-based approach is an effective method for planet detection. In addition, the ET concept is adaptable to multiple-object Doppler observations or very high precision observations with a cross-dispersed echelle spectrograph to separate stellar fringes over a broad wavelength band. In addition to spectroscopic observations of HD 102195, we obtained brightness measurements with one of the automated photometric telescopes at Fairborn Observatory. Those observations reveal that HD 102195 is a spotted variable star with an amplitude of ~0.015 mag and a 12.3 ± 0.3 day period. This is consistent with spectroscopically observed Ca II H and K emission levels and line-broadening measurements but inconsistent with rotational modulation of surface activity as the cause of the radial velocity variability. Our photometric observations rule out transits of the planetary companion.
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© 2006. The American Astronomical Society.
Artículo firmado por 20 autores.
We are grateful to Stuart Shaklan, Michael Shao, Chas Beichman, Richard Green, Skip Andree, Daryl Wilmarth, and the KPNO staff for their generous support and advice and to Larry Molnar for his help in the early photometric data acquisition. The HET observations, whose timings were critical, were made possible by the dedicated efforts of the HET staff. We are indebted to Sara Seager and Eric Agol for a number of stimulating discussions. We thank Aldo Martínez Fiorenzano for helping the line bisector analysis of HD 102195. We appreciate many valuable comments made by the referee, which helped to improve the paper quality. This work is supported by the National Science Foundation grant AST 02-43090, JPL, Pennsylvania State University, and the University of Florida. S. M. and J. v. E. acknowledge the JPL Michelson Fellowship funded by NASA. G. W. H. is grateful for the efforts of Lou Boyd at Fairborn Observatory and acknowledges support from NASA grant NCC5-511 and NSF grant HRD 97-06268. E. B. F. acknowledges the support of the Miller Institute for Basic Research. W. D. C., M. E., and R. A. W. were supported by NASA grants NNG04G141G and NNG05G107G to the University of Texas at Austin. The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, Pennsylvania State University, Stanford University, Ludwig-MaximilliansUniversität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors,William P. Hobby and Robert E. Eberly. D. M. was supported by the Universidad Complutense de Madrid and the Spanish Ministerio de Educación y Ciencia (MEC), Programa Nacional de Astronomía y Astrofísica under grant AYA2005-02750. D. M. is grateful to Raquel M. Martínez, Jesús Maldonado, and Benjamín Montesinos for their help during the observations. FOCES high-resolution optical spectra were based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). This research has made use of the SIMBAAD database, operated at ADC, Strasbourg, France.
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