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The ESO Precise RV Survey for Extra-solar Planets: Results from the First Five Years

Published online by Cambridge University Press:  12 April 2016

M. Kürster ,
A. P. Hatzes ,
W. D. Cochran ,
K. Dennerl ,
S. Döbereiner  and
M. Endl
M. Kürster
Affiliation:
European Southern Observatory, Casilla 19001, Santiago, Chile
A. P. Hatzes
Affiliation:
Astronomy Dept., University of Texas, Austin, TX 78712-1083, USA
W. D. Cochran
Affiliation:
Astronomy Dept., University of Texas, Austin, TX 78712-1083, USA
K. Dennerl
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, D-85740 Garching, Germany
S. Döbereiner
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, D-85740 Garching, Germany
M. Endl*
Affiliation:
European Southern Observatory, Casilla 19001, Santiago, Chile
*
1Also at: Institut für Astronomie, Univ. Wien, Türkenschanzstr. 17, A-1180 Wien, Austria

Abstract

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Results are presented from the first five years of the high precision RV survey carried out with the 1.4m CAT+CES spectrograph at ESO La Silla. This RV survey of 37 solar-type stars was begun in Nov. 1992. Using an iodine gas absorption cell for self-calibration we currently achieve a long-term precision of 20 m/s in a 30-min exposure of a 5.5 mag star. This value is the typical ‘working’ precision in survey work, i.e. an average over all observing conditions.

We present the RV data for our most variable star, ι Hor (G0V), with a possible periodicity of 600 d that could imply a companion of minimum mass m sin i = 2.0 MJup. However, these data are severely complicated by stellar activity to which a large part of the variability must be attributed. Our RV data for ϕ2 Pav (F8V) contain a possible period of 43 d which would imply a planet with m sin i = 0.69 MJup. It must be stressed that for both stars the significance of the periods is still insufficient to conclude that planets are indeed orbiting them. We also show our data for a Hipparcos astrometric brown dwarf candidate, GJ 570A, that do not confirm expectations for a correspondingly high RV signal. Longer monitoring of the star is required in order to confirm a possible low amplitude variation.

Type
Part 3. Extrasolar Planets
Information
International Astronomical Union Colloquium , Volume 170: Precise Stellar Radial Velocities , 1999 , pp. 154 - 161
Copyright
Copyright © Astronomical Society of the Pacific 1999

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