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The CORALIE Survey for Southern Extra-Solar Planets

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The CORALIE Survey for Southern Extra-Solar Planets A&A 415, 391–402 (2004) Astronomy DOI: 10.1051/0004-6361:20034250 & c ESO 2004 Astrophysics The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE?;?? M. Mayor1,S.Udry1, D. Naef1,F.Pepe1,D.Queloz1,N.C.Santos1;2,andM.Burnet1 1 Observatoire de Gen`eve, 51 ch. des Maillettes, 1290 Sauverny, Switzerland 2 Centro de Astronomia e Astrof´ısica da Universidade de Lisboa, Observat´orio Astron´omico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal Received 2 September 2003 / Accepted 25 September 2003 Abstract. This paper summarizes the information gathered for 16 still unpublished exoplanet candidates discovered with the CORALIE echelle spectrograph mounted on the Euler Swiss telescope at La Silla Observatory. Amongst these new can- didates, 10 are typical extrasolar Jupiter-like planets on intermediate- or long-period (100 < P 1350 d) and fairly eccen- tric (0.2 e 0.5) orbits (HD 19994, HD 65216, HD 92788, HD 111232, HD 114386, HD 142415,≤ HD 147513, HD 196050, HD 216437,≤ ≤ HD 216770). Two of these stars are in binary systems. The next 3 candidates are shorter-period planets (HD 6434, HD 121504) with lower eccentricities among which we find a hot Jupiter (HD 83443). More interesting cases are given by the multiple-planet systems HD 82943 and HD 169830. The former is a resonant P2=P1 = 2/1 system in which planet-planet interactions are influencing the system evolution. The latter is more hierarchically structured. Key words. techniques: radial velocities – techniques: spectroscopic – stars: activity – stars: planetary systems 1. Introduction The majority of our CORALIE exoplanet candidates have been published in a series of dedicated papers1, the latest For more than 5 years the CORALIE planet-search programme among them reporting the detection of the shortest-period Hot in the southern hemisphere (Udry et al. 2000a) has been on- Jupiter discovered by radial-velocity surveys around HD 73256 going at the 1.2-m Euler Swiss telescope – designed, built and (Udry et al. 2003c) and the very interesting case of HD 10647 operated by the Geneva Observatory – at La Silla Observatory (Udry et al. 2003a), a star with a high IR excess indicative (ESO/Chile). During these 5 years, CORALIE has allowed the of the presence of a debris disk. The present paper of this se- detection (or has contributed to the detection) of 38 extra-solar ries describes the CORALIE exoplanets that have not been pub- planet candidates. This substantial contribution together with lished yet. This subsample includes candidates announced sev- discoveries from various other programmes have provided a eral months ago, rapidly after their detection to allow follow-up sample of more than 115 exoplanets that now permits us to observations. It also includes some candidates with very long point out interesting statistical constraints for the planet forma- periods or that are members of multi-planet systems requiring tion and evolution scenarios (see e.g. Mayor 2003; Udry et al. a delay in their final analysis. Also, some of the new candidates 2003d; Santos et al. 2003b, for reviews on different aspects of correspond to very recent detections. the orbital-element distributions or primary star properties). The paper is organized as follows. In the next section Send offprint requests to: M. Mayor, we summarize the primary star properties. The radial-velocity e-mail: [email protected] measurements and inferred orbital solutions will be presented ? Based on observations collected with the CORALIE echelle spec- in Sect. 3. In the last section we summarize the results and pro- trograph on the 1.2-m Euler Swiss telescope at La Silla Observatory, vide some concluding remarks. ESO Chile. ?? The precise radial velocities presented in this paper are available in electronic form at the CDS via anonymous ftp to 1 Another dedicated series has also been started for close binaries cdsarc.u-strasbg.fr (130.79.128.5) or via requiring a 2-dimensional correlation analysis for radial-velocity es- http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/415/391, timates. The method has already revealed a 2.5-MJup planet orbiting except for the multi-planet systems that will appear in a future paper the primary (Zucker et al. 2003b) and a 19-MJup brown dwarf orbit- describing their dynamical evolutions, taking planet-planet interaction ing the secondary (Zucker et al. 2003a) of the HD 41004 close visual into account. binary system. Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20034250 392 M. Mayor et al.: The CORALIE survey for southern extra-solar planets. XII. Table 1. Observed and inferred stellar parameters for the stars hosting planets presented in this paper. Definitions and sources of the quoted values are given in the text. The age and rotational period estimates are based on calibrations of the RHK0 activity indicator (Donahue 1993; Noyes et al. 1984), whose reference source is also indicated: (S) for this paper following Santos et al. (2000), (H) for Henry et al. (1996) and (B) for Butler et al. (2002). The applied analyses and uncertainty estimates can be found in the quoted references. HD Sp VBV π MV LTeff log g [Fe/H] M? v sin i log(RHK0 )ageProt − 1 [mas] [L ][K][cgs] [M ][kms− ] [Gy] [day] 6434 G3IV 7.72 0.613 24.80 4.69 1.12 5835 4.60 0:52 0.79 2.3 4:89 (H) 3.8 18.6 19994 F8V 5.07 0.575 44.69 3.32 3.81 6217 4.29− 0.25 1.34 8.1 −4:77 (S) 2.4 12.2 65216 G5V 7.97 0.672 28.10 5.21 0.71 5666 4.53 0:12 0.92 <1–− –– − 82943 G0 6.54 0.623 36.42 4.35 1.50 6005 4.45 0.32 1.15 1.7 4:82 (S) 2.9 18.0 83443 K0V 8.23 0.811 22.97 5.04 0.88 5454 4.33 0.35 0.90 1.4 −4:85 (B) 3.2 35.3 92788 G5 7.31 0.694 30.94 4.76 1.05 5821 4.45 0.32 1.10 1.8 −4:73 (S) 2.1 21.3 − 111232 G5V 7.59 0.701 34.63 5.29 0.69 5494 4.50 0:36 0.78 1.2 4:98 (H) 5.2 30.7 114386 K3V 8.73 0.982 35.66 6.49 0.29 4804 4.36 −0:08 0.68 1.0− – – – 121504 G2V 7.54 0.593 22.54 4.30 1.55 6075 4.64− 0.16 1.18 2.6 4:57 (S) 1.2 8.6 − 142415 G1V 7.33 0.621 28.93 4.64 1.14 6045 4.53 0.21 1.03 3.3 4:55 (S) 1.1 9.6 147513 G3/5V 5.37 0.625 77.69 4.82 0.98 5883 4.51 0.06 1.11 1.5 −4:38 (S) 0.3 4.7 169830 F8V 5.90 0.517 27.53 3.10 4.59 6299 4.10 0.21 1.40 3.3 −4:82 (S) 2.8 8.3 − 196050 G3V 7.50 0.667 21.31 4.14 1.83 5918 4.34 0.22 1.10 3.1 4:65 (S) 1.6 16.0 216437 G4IV/V 6.04 0.660 37.71 3.92 2.25 5887 4.30 0.25 1.06 2.5 −5:01 (H) 5.8 26.7 216770 K0V 8.11 0.821 26.39 5.22 0.79 – – 0.23 0.90 1.4 −4:84 (H) 3.1 35.6 − 2. Parent star characteristics Such an indicator is then used to derive calibrated estimates of the stellar rotational periods and ages (Noyes et al. 1984; The CORALIE planet-search targets have been selected from Donahue 1993). Table 1 gathers the photometric, astrometric, the Hipparcos catalogue (ESA 1997). Our planet-star subsam- spectroscopic information and inferred quantities available for ple benefits thus from the photometric and astrometric infor- our sample of stars hosting exoplanet candidates. mation gathered by the satellite. A high-resolution spectroscopic abundance study was per- The activity indicator is, however, not always available in formed for most of these stars by N.C. Santos in his study the literature or cannot be estimated from our spectra because demonstrating the metallicity enrichment of stars with planets of the star faintness (HD 65216, HD 114386). Calcium reemis- with regard to comparison “single” stars analysed in a homoge- sion can then be visually checked on the co-addition of the neous way (Santos et al. 2001, 2003b, and references therein). CORALIE best-S/N spectra. For our subsample, this is shown This study provides precise values of the effective tempera- in Fig. 1 for the λ 3968.5 Å Ca ii H absorption line region. A tures, metallicities and gravity estimates, using a standard lo- prominent reemission feature is clearly visible for HD 114386 cal thermodynamical equilibrium (LTE) analysis. These val- and HD 147513, the latter presenting, moreover, a strong activ- ues have also been updated by using better recent oscillator ity indicator. However, these stars are only slowly rotating and strengths (log g f ) in the procedure (Santos et al. 2003a). From no large influence on the radial-velocity measurements is then calibrations of the width and surface of the CORALIE cross- expected (Santos et al. 2000; Saar et al. 1998). Hints of reemis- correlation functions (CCF; described in Santos et al.
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