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The planet search program at the ESO Coudé Echelle spectrometer. III. The complete Long Camera survey results
We present the complete results of the planet search program carried outat the ESO Coudé Echelle Spectrometer (CES) on La Silla, usingthe Long Camera from Nov. 1992 to April 1998. The CES survey hasmonitored 37 late-type (F8V - M5V) stars in the southern hemisphere forvariations in their differential radial velocities (RV) in order todetect Doppler reflex motions caused by planetary companions. This ledto the discovery of the first extrasolar planet in an Earth-like orbitaround the young (ZAMS) and active G0V star iota Horologii (Kürsteret al. \cite{martin00}). Here we present the RV results for all surveystars and perform a statistical examination of the whole data-set. Eachstar is tested for RV variability, RV trends (linear and non-linear) andsignificant periodic signals. beta Hyi and epsilon Ind are identified aslong-term, low-amplitude RV variables. Furthermore, for 30 CES surveystars we determine quantitative upper mass-limits for giant planetsbased on our long-term RV results. We find that the CES Long Camerasurvey would have detected short-period (``51 Peg-type'') planets aroundall 30 stars but no planets with msin i < 1 {M}_Jup at orbitalseparations larger than 2 AU. Finally, we demonstrate that the CESplanet search can be continued without applying velocity corrections tothe RV results coming from the currently installed Very Long Camera atthe CES. Based on observations collected at the European SouthernObservatory, La Silla. Appendices A and B are only available inelectronic form at http://www.edpsciences.org
| Ca II H and K Filter Photometry on the UVBY System. II. The Catalog of Observations
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....109.2828T&db_key=AST
| A narrow-band search for extraterrestrial intelligence (SETI) using the interstellar contact channel hypothesis
A search is reported for narrow spectral line emission from 176 targets(including 166 stars and seven globular clusers) at the hypothesized'interstellar communications channel' frequency of 4.462336275 GHz (= pitimes the neutral hydrogen line at 1.42 GHz) using the Parkes Radiotelescope. The frequency was Doppler corrected for the solar barycenter,target barycenter, and cosmic microwave background (CMB) referenceframes. If a 'Galactic club' of extraterrestrial civilizations exists,then the null results, down to a 3 sigma limit of 2 Jy (6 Jy in CMBframe), set an upper limit of 10 exp 8 yr on the lifetime of suchcivilizations.
| Large and kinematically unbiased samples of G- and K-type stars. II - Observations of evolved stars in the Bright Star sample. III - Evolved young disk stars in the Bright Star sample
Four color and RI observations were obtained for a large sample ofG-type and K-type stars in the Bright Star Catalogue. Data are firstpresented for 110 evolved stars. Photometry of evolved young diskpopulation stars have then been calibrated for luminosity, reddening,and metallicity on the basis of results for members of the Hyades andSirius superclusters. New DDO results are given for 120 stars.
| Radial velocities of southern stars obtained with the photoelectric scanner CORAVEL. III - 790 late-type bright stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1985A&AS...59...15A&db_key=AST
| Variability of A and F main sequence stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971A&A....12..223J&db_key=AST
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| Takýmyýldýz: | Yelken |
| Sað Açýklýk: | 09h14m57.20s |
| Yükselim: | -37°36'09.0" |
| Görünürdeki Parlaklýk: | 5.86 |
| Uzaklýk: | 192.308 parsek |
| özdevim Sað Açýklýk: | 4.2 |
| özdevim Yükselim: | -12.2 |
| B-T magnitude: | 6.878 |
| V-T magnitude: | 5.942 |
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