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The HARPS Search for Southern Extra-Solar Planets. III. Three Saturn

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The HARPS Search for Southern Extra-Solar Planets. III. Three Saturn Astronomy & Astrophysics manuscript no. 2864 November 14, 2018 (DOI: will be inserted by hand later) The HARPS search for southern extra-solar planets⋆ III. Three Saturn-mass planets around HD 93083, HD 101930 and HD 102117 C. Lovis1, M. Mayor1, F. Bouchy2, F. Pepe1, D. Queloz1, N.C. Santos3,1, S. Udry1, W. Benz4, J.-L. Bertaux5, C. Mordasini4, and J.-P. Sivan2 1 Observatoire de Gen`eve, 51 ch. des Maillettes, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Laboratoire d’Astrophysique de Marseille, Traverse du Siphon, 13013 Marseille, France 3 Centro de Astronomia e Astrof´isica da Universidade de Lisboa, Observat´orio Astron´omico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal 4 Physikalisches Institut Universit¨at Bern, Sidlerstrasse 5, 3012 Bern, Switzerland 5 Service d’A´eronomie du CNRS, BP 3, 91371 Verri`eres-le-Buisson, France Received 11 February 2005 / Accepted 16 March 2005 Abstract. We report on the detection of three Saturn-mass planets discovered with the HARPS instrument. HD 93083 shows radial-velocity (RV) variations best explained by the presence of a companion of 0.37 MJup orbiting in 143.6 days. HD 101930 b has an orbital period of 70.5 days and a minimum mass of 0.30 MJup. For HD 102117, we present the independent detection of a companion with m2 sin i = 0.14 MJup and orbital period P = 20.7 days. This planet was recently detected by Tinney et al. (2004). Activity and bisector indicators exclude any significant RV perturbations of stellar origin, reinforcing the planetary interpreta- tion of the RV variations. The radial-velocity residuals around the Keplerian fits are 2.0, 1.8 and 0.9 m s−1 respectively, showing the unprecedented RV accuracy achieved with HARPS. A sample of stable stars observed with HARPS is also presented to illustrate the long-term precision of the instrument. All three stars are metal-rich, confirming the now well-established relation between planet occurrence and metallicity. The new planets are all in the Saturn-mass range, orbiting at moderate distance from their parent star, thereby occupying an area of the parameter space which seems difficult to populate according to planet formation theories. A systematic exploration of these regions will provide new constraints on formation scenarios in the near future. Key words. stars: individual: HD 93083, HD 101930, HD 102117 – stars: planetary systems – techniques: radial velocities – techniques: spectroscopic arXiv:astro-ph/0503660v1 30 Mar 2005 1. Introduction Moreover, the combination of CORALIE (Queloz et al. 2000) and HARPS data, extending over several years, will allow the The HARPS instrument is the new ESO high-resolution (R characterization of long-period planets and complex planetary = 115,000) fiber-fed echelle spectrograph, mainly dedicated systems. The low-mass and long-period regions of the exo- to planet search programmes and asteroseismology. It has al- planet parameter space will therefore be under close scrutiny in ready proved to be the most precise spectro-velocimeter to the coming monthsand years. This will improveour knowledge ∼ −1 date, reaching an instrumental RV accuracy of 1 m s of the planet distribution in the mass-period diagram and will (Mayor et al. 2003; Pepe et al. 2004; Santos et al. 2004a), and allow comparisons with theoretical predictions (see for exam- even better on a short-term basis. This opens a new field in the ple Armitage et al. 2002; Ida & Lin 2004; Alibert et al. 2005). search for extrasolar planets, allowing the detection of com- panions of a few Earth masses around solar-type stars. Indeed, the increase of the planet frequency towards very low masses is In this paper we present the discovery of three plane- confirmed by the recent discovery of Neptune-mass exoplanets tary companions to the stars HD 93083, HD 101930 and (McArthur et al. 2004; Santos et al. 2004a; Butler et al. 2004). HD 102117. Interesting characteristics of these planets include a mass in the Saturn-mass regime and below, and an orbital dis- Send offprint requests to: C. Lovis tance to the star of 0.1-0.5 AU. According to recent planet for- ⋆ Based on observations made with the HARPS instrument on the mation scenarios (Ida & Lin 2004), they are situated in a region ESO 3.6 m telescope at La Silla Observatory under programme ID of the mass-period diagram that seems difficult to populate. 072.C-0488(E). The systematic exploration of this mass and distance regime is 2 C. Lovis et al.: The HARPS search for southern extra-solar planets therefore an important test for the core-accretion and migration theories of planet formation. This paper is structured as follows. Section 2 describes the observations, the data reduction process and discusses the long-term precision of the HARPS measurements. The physi- cal properties of the parent stars are presented in Sect. 3, fol- lowed by the RV measurements and orbital solutions in Sect. 4. We discuss in the last section the characteristics of these new planets in the context of the already-known properties of exo- planets and highlight some theoretical questions that might be answered by radial-velocity surveys in the near future. 2. Observations and measurement precision HD 93083, HD 101930 and HD 102117 are all members of the HARPS high-precision RV sample. The aim of this sur- vey is to obtain RV measurements with photon errors below Fig. 1. Radial velocities for a sample of 12 stable stars from 1 m s−1 to detect very low-mass extrasolar planets. The stars the HARPS high-precision programme, observed over about in this sample have been selected from the CORALIE planet 700 days. For each star, the mean RV has been subtracted. search database for being non-evolved, having low projected −1 −1 The overall RMS of 1.81 m s is made of different contri- rotational velocity (v sin i < 3kms ) and exhibiting low activ- −1 ′ butions, among which photon noise (∼0.8 m s ), calibration ity levels (log R < -4.7). These criteria should eliminate most − − HK noise (∼0.8 m s 1), guiding errors (0.2-0.6 m s 1) and stellar stars showing large intrinsic RV variations and select only very − acoustic modes (0.5-2.0 m s 1). Seasonal averages have been quiet, chromospherically inactive stars, so that stellar RV jit- −1 computed (bottom part). The absence of long-term drifts and ter does not hide possible planetary signals down to 1-2 m s . − the dispersion of only 0.64 m s 1 illustrate the long-term sta- Obviously, the photon noise error on the radial velocity must bility of ThAr reference lamps. also remain below 1 m s−1. For each HARPS spectrum we compute the photon-limited, ultimate RV precision using the formulae given by Connes (1985) and Bouchy et al. (2001). In spite of that, the global RV dispersion of the measurements − HARPS typically delivers 0.5-1 m s 1 photon-limited accuracy amountsto 1.81 m s−1 (see Fig.1). This includes many different − ataS/N ratio of ∼100per pixel(0.8km s 1) at 550nmonsolar- effects, which can be estimated as follows. type stars. The exact number mainly depends on the depth of absorption lines and the projected rotational velocity. – The mean photon error, computed according to The radial velocities for HD 93083, HD 101930 and Bouchy et al. (2001), is 0.8 m s−1. HD 102117 have been obtained with the standard HARPS re- – The zero-point wavelength calibration, given by nightly duction pipeline, based on the cross-correlation with a stellar ThAr reference spectra, is presently determined with an ac- template, the precise nightly wavelength calibration with ThAr curacy of ∼0.8 m s−1. spectra and the tracking of instrumental drifts with the simulta- – Guiding errors are responsible for 0.2-0.6 m s−1 of extra neous ThAr technique (Baranne et al. 1996). Of particular in- dispersion, due to the non-optimal tuning of the guiding terest is the fact that the nightly instrumental drifts always re- software. This issue has now been solved and the guiding main below 1 m s−1 for HARPS due to the high instrumental noise should remain below 0.3 m s−1 in the future. stability. – The largest contribution to the global RV dispersion comes To assess the long-term precision of the instrument, we from the star itself, mainly due to acoustic modes (p- selected a sample of 12 stable stars, which have been fol- modes). For our 12 stars we estimate this contribution to lowed regularly over the past two years. These stars include be 0.5-2.0 m s−1, depending on spectral type and evolu- HD 55 (K5V, V=8.49), HD 1581 (F9V, V=4.23), HD 6673 tionary status (see Mayor et al. 2003; Bouchy et al. 2005). (K1V, V=8.84), HD 20794 (G8V, V=4.26), HD 28471 The observational strategy has been recently optimized to (G5V, V=7.89), HD 30278 (G8V, V=7.61), HD 44594 (G4V, minimize these stellar oscillations, essentially by integrat- V=6.61), HD 82342 (K3/K4V, V=8.31), HD 114853 (G2V, ing over long enough periods to cover more than 1-2 oscil- V=6.93), HD 162396 (F8V, V=6.19), HD 196761 (G8/K0V, lations (3-15 minutes, depending on spectral type). V=6.36) and HD 215152 (K0V, V=8.11). For each of these stars, several measurements have been gathered, spanning at Adding all these effects quadratically, we obtain a total dis- least 300 days, and the mean RV was subtracted to enable a persion that is very close to the measured value of 1.81 m s−1 comparison between different stars.
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