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• Top
• Abstract
• 1. Introduction
• 2. Characteristics of the host stars
• 3. HARPS radial-velocity data and orbital solutions
• 4. Conclusions
• Acknowledgments
• References
• List of tables
• List of figures

© ESO, 2010

1. Introduction

In this paper, we present new detections from the HARPS planet search programme. It has been ongoing since 2003. Its detections are based on radial velocities obtained with theHigh Accuracy Radial velocity Planet Searcher(HARPS,Mayor et al. 2003). HARPS is a high-resolution echelle spectrograph mounted on the ESO–3.6-m telescope in La Silla (Chile). The instrument is installed in a vacuum vessel, and it is thermally controlled. These characteristics result in a very high stability of the intrumental radial-velocity zero point (measured drifts smaller than 1 m s^-1 over one night). HARPS possesses two optical fibres. The first one collects the target light, whereas the second one can be used for recording a reference Thorium-Argon spectrum. The second spectrum has been used for measuring the residual drift of the instrument since the time of the latest wavelength calibration, allowing us to apply a correction to the velocities (Baranne et al. 1996). The second fibre can also be used for measuring the spectrum of the sky background. With more than 70 detections obtained so far, including the lightest planet (Gl 581 e,Mayor et al. 2009), the HARPS contribution to the exoplanet research field is a major one.

Since its beginning, the HARPS planet search programme has been divided into several sub-programmes related to specific scientific questions. One of these sub-programmes is theHARPSvolume-limited programmeto which about 20% of the HARPS Guaranteed Time Observation (GTO) programme allocated time was dedicated. The sample of the HARPS volume-limited programme is an extension up to 57.5 pc of the CORALIE planet search sample (volume-limited sample up to 50 pc, seeUdry et al. 2000). It contains about 850 F8–M0 dwarfs. As in the case of the CORALIE sample, the maximum distance decreases with theB−V colour index for targets with late spectral types (later than K0). Our target list will be published in another paper (Lo Curto et al., in prep.).

Targets in this sample are observed at lower signal-to-noise ratios (typically 40 − 50) than the ones in the high-precision programme and without using the simultaneous calibration. The typical photon-noise error obtained in this case is about 1 − 2 m s^-1 depending on the target spectral type and projected rotational velocity. This strategy, optimized for the follow-up of a large stellar sample, is a good compromise between precision and observing efficiency.

Rather short exposure times (less than 5 min) are usually enough for reaching the targetted signal-to-noise ratio. An exposure time of 5 min is too short for correctly averaging out intrinsic stellar signals due for example to pulsation or granulation. Our velocities can thus be affected by those effects that in some cases can reach a peak-to-peak amplitude of several m s^-1 (see e.g. the case ofμ Arae,Santos et al. 2004a;Bouchy et al. 2005). The amplitudes of these signals depend on the target spectral types and on the averaging strategy. Expected radial-velocity errors due to intrinsic signals are greater for earlier spectral types and for evolved targets.

With such an observing strategy, our programme is mostly sensitive to Saturn or Jupiter-like planets but is also sensitive to lower-mass planets around stars with a low intrinsic radial-velocity variability. Also, we generally avoid taking exposures shorter than 1 min in order to reduce the impact of observing overheads. As a consequence, the brightest targets in our sample frequently have photon-noise errors significantly lower than the targetted one. For illustrating these facts, we mention the recent detections of a 5.5 M_⊕ planet aroundHD 215497 (Lo Curto et al. 2010), of the 12.6 M_⊕ planetHD 125595 b (Ségransan et al. 2010) and of the 14.4 M_⊕ planet aroundBD  − 08 2823 b (Hébrard et al. 2010).

The main aim of this observational effort is a better characterization of orbital elements distributions of gaseous planets. With the increasing size of the sample of known planets, a quantitative comparison between the observed sample and the predictions of planet formation models becomes possible and reliable (see for exampleMordasini et al. 2009). With the eight planetary companions presented in this paper, the total number of planets detected in the volume-limited sample now reaches 39 (seePepe et al. 2004a;Moutou et al. 2005,2009b;Lo Curto et al. 2006,2010;Naef et al. 2007;Mordasini et al. 2010;Ségransan et al. 2010).

In this paper, we present our HARPS radial-velocity data for 8 solar-type stars hosting low-mass companions:HD 6718,HD 8535,HD 28254, HD 290327,HD 43197,HD 44219,HD 148156, andHD 156411. This paper is organized as follows. We present the main characteristics of the 8 host stars in Sect. 2. Section 3 contains the description of the radial-velocity sets and orbital solutions obtained for these targets. Finally, we provide concluding remarks in Sect. 4.

2. Characteristics of the host stars

We list the main characteristics of the nine host stars in Table 1. ApparentV-band magnitudesm_V and colour indexesB − V are from the HIPPARCOS Catalogue (ESA 1997). Distancesd are based on the improved HIPPARCOS astrometric parallaxesπ derived byvan Leeuwen (2007). Absolute magnitudesM_V were computed usingm_V andd.

For each star, we derived the atmospheric parametersT_eff, log g, and  [ Fe/H ]  by performing a detailed local thermodynamical equilibrium spectroscopic analysis. A high signal-to-noise co-added HARPS spectrum was built for each target. The set of Fe i/Fe iiequivalent widths used for the analysis were measured on the co-added spectra with the ARES code (Sousa et al. 2007). The list of spectral lines for the analysis, as well as more details on the method can be found inSantos et al. (2004b).

Stellar luminositiesL were computed using HIPPARCOS apparent magnitudes and parallaxes and the bolometric correction obtained via theT_eff-based calibration inFlower (1996). Stellar massesM_∗, and radiiR_∗ were derived fromT_eff,  [ Fe/H ] , andM_V by interpolating theGirardi et al. (2000) theoretical isochrones. FollowingFernandes & Santos (2004), a relative uncertainty of  ≃ 10% can be assumed forM_∗. We also computed surface gravities, log g, usingM_∗ andR_∗. These values are in fair agreement with the spectroscopic ones: a mean difference (spectroscopy − isochrones) of 0.06 dex and an rms of the differences equal to 0.11 dex. Spectral types listed in Table1 are based on the stellar parameters we determined in this paper.Jenkins et al. (2008) have published iron abundances forHD 43197 andHD 148156. Their values,  [ Fe/H ]  = 0.37 ± 0.09 and 0.22  ±  0.15, respectively, are in good agreement with ours. The atmospheric parameters forHD 44219 have also been determined byRobinson et al. (2007). They foundT_eff = 5723 ± 82, log g = 4.37 ± 0.13 and  [ Fe/H ]  =  − 0.05 ± 0.07. These values agree with ours within uncertainties.

Activity indexes were extracted from individual HARPS spectra using a method similar to the one described inSantos et al. (2000). Values indicated in Table 1 are average activity indexes obtained for each target. All the targets exhibit a very low level of activity. Our values forHD 43197 andHD 148156 are in good agreement with those published inJenkins et al. (2008):  − 5.12 and  − 5.08, respectively. We did not try to estimate chromospheric ages for our targets because these two quantities are no longer correlated for weakly active stars (Pace & Pasquini 2004). However, we can infer for most of these stars (if not all) a safe age constraint based on their low activity indexes and rather high luminosities: age > 3 Gyr. The projected rotational velocitiesvsini were derived from the widths of the HARPS cross-correlation functions (CCF) following the method presented inSantos et al. (2002).

Finally,HD 28254 is the bright component of a visual binary. According to the Catalogue of Components of Double and Multiple stars (Dommanget & Nys 2002), the visual companion,CCDM J04248-5037 B, is located at a separation of 4.3″ and at a position angle of 254 degrees. With an apparent magnitude ofm_V = 13.8, this object is 6.11 mag fainter (i.e. a flux ratio less than 0.4%). It was thus clearly outside the detection capabilities of HIPPARCOS. Assuming the two stars form a bound system and using the distance ofHD 28254 (54.7 pc), we computed the projected separation between them: 235 AU. We also computed the absolute magnitude of the B component:M_V = 10.11 corresponding to an M0V-M2V star. With this absolute magnitiude and the mass-luminosity relations inDelfosse et al. (2000), we computed a mass of 0.48 M_⊙ for this object. Its minimum period is about 1000 yr. Assuming that this companion is on a circular edge-on orbit, the maximal radial-velocity amplitude it would induce on the primary star is of the order of 1.1 km s^-1.

3. HARPS radial-velocity data and orbital solutions

As explained before, stars belonging to the HARPS volume-limited sample are generally observed without simultaneous thorium-argon reference. Possible instrumental drifts therefore remain uncorrected. This has only a limited impact on our results because: 1) the instrument is very stable: on average, the radial-velocity drifts of HARPS remain below 0.5 m s^-1 over one night and 2) the targetted photon-noise error for this programme is 1 − 2 m s^-1. We stress again the fact that our observing strategy is not optimally designed for averaging out stellar intrinsic signals. We list in Table 2 the median exposure times for all the targets. This median is below 3 min in all cases. We thus expect our velocities to be affected at some level by stellar intrinsic jitter in particular the velocities of our early type and/or slightly evolved targets, namelyHD 8535 (G0V),HD 28254 (G1IV/V),HD 148156 (F8V), andHD 156411 (F8IV/V).

Our radial velocities can be obtained from the extracted spectra by cross-correlating them with a numerical template. Numerical templates are chosen to minimize the mismatch with the target spectral type. Our radial-velocity uncertainties include two well-quantified contributions: photon noise and calibration error. An additional error of 0.5 m s^-1 is added quadratically to account for the absence of simultanous calibration and thus the possibility of a small uncorrected radial-velocity drift of the HARPS zero point.

All the orbital solutions presented in the following sections were obtained with software that includes a genetic algorithm. In general, the only a priori information used by this algorithm is the type of model we want to use (i.e., 1-Keplerian, 2-Keplerian, 1-Keplerian plus a linear/quadratic drift, etc.). Once the global parameter space minimum is identified, we use it as the starting point for a standard Levenberg-Marquardt minimization out of which the final solution is obtained. In all the cases, we have verified the absence of correlation between the post-fit residuals and the measured cross-correlation function bisectors. Finally, uncertainities on the fitted parameters are determined using Monte-Carlo simulations.

Fig. 1 HARPS radial-velocity data for the eight stars presented in this paper. Temporal velocities (filled dots) and fitted orbital solutions (solid lines) are displayed inthe upper panels. Residuals to the fitted orbits are displayed inthe bottom panels. ForHD 28254 andHD 44219, the dashed lines in the upper panels show additional quadratic radial-velocity drifts that were included to the orbital fits. For all the other targets, theupper panelsdashed lines represent the systemic velocityγ.

3.1. HD 6718

The 22 HARPS radial-velocity measurements were gathered forHD 6718 (HIP 5301) between BJD = 2 452 991 (December 18, 2003) and BJD = 2 455 019 (July 6, 2009). These velocities have a mean uncertainty of 1.59 m s^-1. We have fitted a long-period Keplerian orbit to these data. The orbital parameters resulting from this fit are listed in Table 2. With these parameters and assuming a mass of 0.96 M_⊙ for the host star, we computed a minimum mass of 1.56 M_Jup for the companion and a semi-major axis of 3.56 AU. Residuals to the fitted orbit have a very low dispersion (σ_O − C = 1.79 m s^-1), and a 1-planet model is thus sufficient for explaining the detected signal. We display our data and the fitted orbit in panelaof Fig. 1.

Fig. 2 HARPS phase-folded velocities and fitted orbits for the 6 targets observed for at least two orbital periods. The radial-velocities ofHD 28254 andHD 44219 have been corrected for the fitted quadratic drift.

3.2. HD 8535

A set of 45 HARPS radial velocities was obtained forHD 8535 (HIP 6511) between BJD = 2 452 850 (July 29, 2003) and BJD = 2 455 070 (August 26, 2009). The mean radial-velocity uncertainty of these measurements is 1.57 m s^-1. The presence of a long-period signal is obvious (see panel bof Fig. 1). The results of the Keplerian fit to our data are presented in Table 2. The dispersion of the residuals to the fitted orbit are somewhat larger than expected ( = 2.48). We have tried to fit orbits including additional signals (linear or quadratic trend; 2-Keplerian model) but we were unable to significantly improve the quality of the solution. We have also verified the absence of any correlation between the residuals and the CCF bisectors.

Assuming a primary mass of 1.13 M_⊙, we computed the minimum mass of the companion and the semi-major axis of its orbit:m₂sini = 0.68M_Jup anda = 2.45 AU. The fitted orbit and the fit residuals are displayed in panel bof Fig. 1. The phase-folded orbit and velocities are displayed in panelaof Fig. 2.

3.3. HD 28254

We collected 32 HARPS radial velocities forHD 28254 (HIP 20606) between BJD = 2 452 941 (October 28, 2003) and BJD = 2 454 931 (April 9, 2009). The average velocity uncertainty of these measurements is 1.34 m s^-1. As indicated in Sect. 2,HD 28254 is the main component of a visual binary system. The presence of a nearby visual companion can induce radial-velocity errors via the seeing-dependent contamination of the spectrum of the main component.Pepe et al. (2004b) have simulated this effect for HARPS and using the La Silla seeing statisitics. We have performed the same simulations using the characteristics of theHD 28254 system (ρ = 4.3″, Δm_V = 6.11). The expected effect is negligible in this case ( ≪ 0.1 m s^-1).

A long-period signal is visible on the data (see panelcof Fig. 1). From the visual inspection of these data, it is also obvious that the Keplerian signal is highly eccentric. We first attempted to fit a single orbit to our velocities. Withe > 0.99, the obtained orbit was not physical so we rejected it. After this initial unsuccessful attempt, we tried to fit orbits with additional signals. The following two models did not give satisfactory results: the 1-Keplerian plus linear drift model and the 2-Keplerian one. The best fit we obtained and finally adopted is based on a 1-Keplerian plus quadratic drift model. Despite the poor coverage of the second radial-velocity maximum, hence the poorly constrained velocity semi-amplitude, the planetary nature of HD 23254 b is well established. The orbital period is very well constrained. Solutions with significantly larger amplitudes are possible, but they also have much larger eccentricities. The effect of the increasing amplitude on the minimum mass of the companion is largely compensated for by the increasing eccentricity as the mass function scales with.

More data are necessary for better constraining the shape of the orbit ofHD 28254 b. In particular, a better coverage of the periastron passage will allow us to constrain the radial-velocity semi-amplitude and orbital eccentricity. These future observations will also help us characterizing the secondary signal better. The orbital solution we present here is thus a preliminary one. The observed additional quadratic signal remains compatible with the signal that the visual companion described in Sect. 2 could induce.

Using our fitted parameters, we computed the minimum mass of the planetary companion and its orbital semi-major axis:m₂sini = 1.16M_Jup anda = 2.15 AU. Our radial-velocity data and the fitted orbit are displayed in panelcof Fig. 1. The phase-folded orbit and velocities are displayed in panelbof Fig. 2.

3.4. HD 290327

Between BJD = 2 452 945 (November 1, 2003) and BJD = 2 454 931 (April 9, 2009), we have observed HD 290327 (HIP 25191) 18 times with HARPS. The obtained radial velocities have a mean uncertainty of 1.73 m s^-1. A long-period signal is well visible on the data. We list in Table 2 the parameters resulting from a Keplerian fit to the data. With these parameters and using the primary mass of Table 1 (0.90 M_⊙), we computed the minimum mass of the companion that induces the detected radial-velocity signal and the semi-major axis of its orbit:m₂sini = 2.54 M_Jup anda = 3.43 AU. The dispersion of the residuals to the fitted orbit is very low: 1.6 m s^-1. Our velocity data and the fitted orbit are displayed in paneldof Fig. 1.

3.5. HD 43197

We have gathered a set of 33 radial velocities forHD 43197 (HIP 29550). These data were obtained between BJD = 2 452 989 (December 15, 2003) and BJD = 2 454 932 (April 10, 2009), and they have a mean velocity uncertainty of 1.42 m s^-1. A visual inspection of the data displayed in panel eof Fig. 1 shows a periodic highly eccentric signal. The parameters resulting from a Keplerian fit to the data are listed in Table 2. The fitted eccentricity is indeed very high and very well constrained in spite of our poor coverage of the radial-velocity minimum. The rms of the residuals to the fitted orbit is very low: 1.42 m s^-1. This 1-planet fit is thus satisfactory. With a primary mass of 0.96 M_⊙, the computed minimum mass of the companion is 0.6 M_Jup. The orbital semi-major axis is 0.92 AU. Our data, the fitted orbit, and the residuals are displayed in paneleof Fig. 1. Panelcof Fig. 2 shows the phase-folded orbit.

3.6. HD 44219

The HARPS data set we have in hand forHD 44219 (HIP 30114) consists of 46 radial velocities measured between BJD = 2 452 944 (October 31, 2003) and BJD = 2 454 932 (April 10, 2009). These velocities have an average uncertainty of 1.55 m s^-1. We first fitted a 1-Keplerian model to these data. The residuals to this fitted orbit were a bit large (σ_O − C = 2.95 m s^-1). We then tried to include an additional signal in the fitted model. Adding a linear drift improved the quality of the fit in a marginally significant way ( decreasing from 3.79 to 3.30; f-test probability = 71%). The improvement resulting from including a quadratic trend in the fitted model was more significant: = 2.62 and f-test probability equals 90%. We also tried to fit a 2-planet model but we were unable to find any convincing solution. We finally decided to adopt the Keplerian + quadratic drift model. The parameters resulting from this fit are listed in Table 2. The orbital parameters obtained with our initial 1-planet fit did not differ much from the ones in the adopted solution (P = 447 d;e = 0.57;K₁ = 17 m s^-1 andm₂sini = 0.52 M_Jup).

The dispersion of the residuals to the finally selected solution is still a bit large (σ_O − C = 2.39 m s^-1), but this is probably due to the still not very well constrained additional signal. With this solution and assumingM_∗ = 1 M_⊙, the computed minimum mass forHD 44219 b is 0.58 M_Jup and its orbital semi-major axis is 1.19 AU. We display the fitted model and the temporal residuals in panel fof Fig. 1. The phase-folded orbit and velocities are displayed in paneldof Fig. 2.

3.7. HD 148156

We have collected 42 radial velocities with HARPS forHD 148156 (HIP 80680) between BJD = 2 452 852 (July 31, 2003) and BJD = 2 455 020 (July 7, 2009). The mean radial-velocity uncertainty of this data set is 2.24 m s^-1. A long-period signal is visible in the data displayed in panel gof Fig. 1. The results of the Keplerian fit performed on our velocity set are presented in Table 2. The rms of the residuals is a bit large (σ_O − C = 3.69 m s^-1; = 2.89). We were unable to significantly improve the fit by adding extra signals. No obvious correlation between CCF bisectors and residuals could be detected. The origin of these abnormal residuals remains unknown, but they may be due to intrinsic stellar jitter.

The minimum mass ofHD 148156 b is 0.85 M_Jup and the semi-major axis of its orbit is 2.45 AU (assumingM_∗ = 1.22 M_⊙). The fitted orbit and the fit residuals are displayed in panel gof Fig. 1. The phase-folded orbit and velocities are displayed in paneleof Fig. 2.

3.8. HD 156411

We obtained 50 HARPS radial-velocity measurements ofHD 156411 (HIP 84787). These measurements were taken between BJD = 2 452 850 (July 29, 2003) and BJD = 2 455 081 (September 6, 2009) and they have a mean velocity uncertainty of 1.26 m s^-1. A long-period signal is visible on the data displayed in panel hof Fig. 1. We fitted a Keplerian orbit to these data. The resulting parameters are listed in Table 2. The dispersion of the residuals to the fitted orbit is too large (σ_O − C = 2.94 m s^-1), and the fit quality quite poor ( = 5.21).

We tried to fit models including additional signals. First, we tried to add linear and quadratic drifts. In both cases, the fit quality improved a bit ( and 4.70, respectively) but the corresponding f-test probabilities indicated that the achieved improvements were only marginally significant (at the 1σ level). A 2-planet fit was also tried, but we were unable to find any convincing solution. We also verified the absence of correlation between CCF bisectors and residuals.HD 156411 is slightly evolved so we speculate that intrinsic stellar signals are responsible for the abnormal residuals.

For this paper, we finally decided to adopt our initial 1-planet orbital solution. With this solution and assuming a mass of 1.25 M_⊙ for the host star, we computed a minimum mass of 0.74 M_Jup and an orbital semi-major axis of 1.88 AU forHD 156411 b. The fitted orbit and the temporal residuals are displayed in panel hof Fig. 1. The phase-folded orbit and velocities are displayed in panelfof Fig. 2.

4. Conclusions

In this paper, we have presented our HARPS radial-velocity data for 8 low-activity solar-type stars orbited by at least one long-period planetary companion.HD 6718 has a 1.56 M_Jup companion on a 2496-d low-eccentricity orbit (e = 0.1). The companion orbitingHD 8535 is a 0.68 M_Jup planet with a period of 1313 days and an eccentricity of 0.15.HD 28254 b is a 1.16 M_Jup planet on a 1116-d highly eccentric orbit (e = 0.81). The companion to HD 290327 has a minimum mass of 2.54 M_Jup. Its 2442-d orbit is nearly circular (e = 0.08). As forHD 28254 b, the 0.6 M_Jup companion toHD 43197 is on a highly eccentric orbit:e = 0.83. Its orbital period is 327 d.HD 44219 is orbited by a 0.58 M_Jup planet on a 472-d 0.61 eccentricity orbit.HD 148156 b is a 0.85 M_Jup planet orbiting its parent star on a 1027-d eccentric orbit (e = 0.52) and the companion toHD 156411 is a 0.74 Jupiter-mass planet with a mildly eccentric (e = 0.22) 842-d orbit.

We find some evidence of additional longer-period companions aroundHD 28254 andHD 44219. In both cases, we are unable to fit full double-Keplerian orbits because of our short observing time span. Future observations of these two systems will probably allow us to better characterize the companions responsible for these signals.

Finally, with the addition ofHD 28254 b andHD 43197 b, the population of exoplanets with extremely high eccentricities now amounts to 6. The other planets withe ≥ 0.8 areHD 4113 (e = 0.903,Tamuz et al. 2008), 156846 (e = 0.8472,Tamuz et al. 2008),HD 20782 b (e = 0.92,Jones et al. 2006), andHD 80606 b (e = 0.934,Moutou et al. 2009a). Five of these stars hosting highly eccentric planets are members of wide visual binaries (seeTamuz et al. 2008 forHD 4113 andHD 156846,Desidera & Barbieri 2007 forHD 20792, andNaef et al. 2001 forHD 80606). OnlyHD 43197 is not known to be in a multiple stellar system. This large number of eccentric-planet hosts in binaries tend to favour scenarios in which the extreme orbital eccentricity results from the influence of a third body via Kozai oscillations (Kozai 1962) or Kozai migration (Wu & Murray 2003).

Acknowledgments

We thank the Swiss National Science Foundation (SNSF) and Geneva University for their continuous support of our planet search programmes. N.C.S. would like to acknowledge the support from the European Research Council/European Community under the FP7 through a Starting Grant, as well from Fundação para a Ciência e a Tecnologia (FCT), Portugal, through programme Ciência 2007, and in the form of grants PTDC/CTE-AST/098528/2008 and PTDC/CTE-AST/098604/2008. This research has made use of the Simbad database, operated at the CDS in Strasbourg, France.

References

All Tables

All Figures

Fig. 1 HARPS radial-velocity data for the eight stars presented in this paper. Temporal velocities (filled dots) and fitted orbital solutions (solid lines) are displayed inthe upper panels. Residuals to the fitted orbits are displayed inthe bottom panels. ForHD 28254 andHD 44219, the dashed lines in the upper panels show additional quadratic radial-velocity drifts that were included to the orbital fits. For all the other targets, theupper panelsdashed lines represent the systemic velocityγ.

In the text

	Fig. 2 HARPS phase-folded velocities and fitted orbits for the 6 targets observed for at least two orbital periods. The radial-velocities ofHD 28254 andHD 44219 have been corrected for the fitted quadratic drift.
In the text

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