The SOPHIE northern extrasolar planets. I. A companion close to the planet/brown-dwarf transition around HD16760
aa r X i v : . [ a s t r o - ph . E P ] J u l Astronomy&Astrophysicsmanuscript no. hd16760˙arxiv c (cid:13)
ESO 2018November 8, 2018
The
SO PH I E northern extrasolar planets ⋆ I. A companion close to the planet/brown-dwarf transition around HD 16760
Bouchy, F. , , H´ebrard, G. , Udry, S. , Delfosse, X. , Boisse, I. , Desort, M. , Bonfils, X. , Eggenberger, A. ,Ehrenreich, D. , Forveille, T. , Le Coroller, H. , Lagrange, A.M., , Lovis, C. , Moutou, C. , Pepe, F. , Perrier, C. ,Pont, F. , Queloz, D. , Santos, N.C. , S´egransan, D. , and Vidal-Madjar, A. Institut d’Astrophysique de Paris, UMR7095 CNRS, Universit´e Pierre & Marie Curie, 98bis Bd Arago, 75014 Paris, France Observatoire de Haute-Provence, CNRS / OAMP, 04870 St Michel l’Observatoire, France Observatoire de Gen`eve, Universit´e de Gen`eve, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland Laboratoire d’Astrophysique, Observatoire de Grenoble, Universit´e J. Fourier, CNRS, BP 53, 38041 Grenoble cedex 9, France Laboratoire d’Astrophysique de Marseille, 38 rue Fr´ed´eric Joliot-Curie, 13388 Marseille cedex 13, France School of Physics, University of Exeter, Exeter, EX4 4QL, UK Centro de Astrof´ısica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, PortugalReceived ; accepted
ABSTRACT
We report on the discovery of a substellar companion or a massive Jupiter orbiting the G5V star HD 16760 with the spectrograph
SOPHIE installed on the OHP 1.93-m telescope. Characteristics and performances of the spectrograph are presented, as well as the
SOPHIE exoplanet consortium program. With a minimum mass of 14.3 M
Jup , an orbital period of 465 days and an eccentricity of0.067, HD 16760b seems to be located just at the end of the mass distribution of giant planets, close to planet / brown-dwarf transition.Its quite circular orbit supports a formation in a gaseous protoplanetary disk. Key words. planetary systems – Techniques: radial velocities – stars: individual: HD 16760
1. Introduction
The vast majority of 350 known exoplanets have been foundthanks to radial velocity measurements. Far to be an old-fashioned technique, Doppler measurements illustrated theselast years their capabilities to extend the exoplanet search arounda large variety of stars. The sensitivity of this technique contin-uously increases, opening the possibility to explore the domainof low-mass planets down to few Earth masses, to discover andcharacterize multiple planetary systems, to perform long termsurveys to find true Jupiter-like planets, to establish the plane-tary nature and to characterize the transiting candidates of pho-tometric surveys. Doppler surveys for exoplanet search requirehigh-precision spectrographs and a significant amount of tele-scope time over a long duration.The
S OPHIE spectrograph (Bouchy et al. 2006, Perruchotet al. 2008) is in operation since October 2006 at the 1.93-m tele-scope of Observatoire de Haute-Provence. Benefiting from ex-perience acquired on HARPS (Pepe et al. 2002) and taking intoaccount the limitations of the ELODIE spectrograph (Baranneet al. 1996),
S OPHIE was designed to obtain precise radial ve-locities with much higher throughput than its predecessor andto be operated as a northern counterpart of HARPS. This instru-ment is briefly described in section 2. The
S OPHIE consortiumstarted in October 2006 a large and comprehensive program ofsearch and characterization of exoplanets described in section 3.We report in section 4 the detection of a substellar companion or ⋆ Based on observations made with
S OPHIE spectrograph on the1.93-m telescope at Observatoire de Haute-Provence (CNRS / OAMP),France (program 07A.PNP.CONS). a massive Jupiter around HD 16760 and we discuss in section 5the properties and nature of this object located at the upper limitof the mass distribution of giant planets.
2. The
SOPHIE spectrograph
S OPHIE architecture mainly benefits from ELODIE andHARPS experiences. A detailed technical description of this in-strument is given by Perruchot et al. (2008). In this section webriefly describe the main properties of the spectrograph and itsdi ff erent observing modes. S OPHIE is a cross-dispersed, envi-ronmentally stabilized echelle spectrograph dedicated to high-precision radial velocity measurements. The detector (EEV-4482) is a thinned, back-illuminated, anti-reflection coated 4kx 2k 15- µ m-pixel CCD cooled at -100 o C, with slow- and fast-readout modes. It records 39 spectral orders covering the wave-length domain from 3872 to 6943 Å. The spectrograph is fedthrough a pair of 3”-wide optical fibers for the high-resolutionmode (R = ffi ciency mode (R = thosimult mode), or on the skyto estimate background pollution, especially in case of strongmoonlight ( objAB mode). Both aperture can also be simultane-ously put on Thorium-Argon or tungsten lamps for wavelengthor flat-field calibrations, respectively. Apart from thermal pre- F. Bouchy et al.: A massive Jupiter around HD 16760 cautions, the key-point for stability is the encapsulation of thedispersive components in a constant pressure tank. This solutionstabilizes the air refractive index sensitive to atmospheric pres-sure variations. With such a concept typical intrinsic drift of thespectrograph is less than 3 m s − per hour. The ELODIE front-end adaptor (Baranne et al. 1996), is still used for S OPHIE . Itholds the calibration lamps, the atmospheric dispersion correc-tor and the guiding system. Compared to ELODIE,
S OPHIE leads to 1) gain on photon e ffi ciency by a factor of 10 in high-e ffi ciency mode, 2) increase the spectrograph radial velocity sta-bility by a factor of 3, and 3) increase spectral resolution from42000 to 75000 for the high-resolution mode.The spectra are extracted from the detector images and theradial velocities are measured online with the S OPHIE pipelinederived and adapted from the HARPS one . The spectra extrac-tion includes localization of the 39 spectral orders on the 2D-images, optimal order extraction, cosmic-ray rejection, wave-length calibration and spectral flat-field correction yielding a twodimension spectra (E2DS). The orders are then merged and re-binned after correction of the blaze function, yielding a one di-mension spectra (S1D). The E2DS spectra are cross-correlatedwith numerical masks corresponding to di ff erent spectral types(F0, G2, K0, K5, M4); the resulting cross-correlation func-tions (CCFs) are fitted by Gaussians to get the radial velocities(Baranne et al. 1996, Pepe et al. 2002).Following the approach of Santos et al. (2002), we calibratedthe CCF to determine the projected rotational velocity v sin i andthe metallicity index [Fe / H]. We also calibrated the CCF to com-pute the RV photon-noise uncertainty σ VR . Following the ap-proach of Santos et al. (2000), we computed and calibrated thechromospheric-activity index R ′ HK based on our SOPHIE spec-tra. The
S OPHIE radial velocity measurements were initiallya ff ected by a systematic e ff ect at low signal-to-noise ratio, dueto CCD charge transfer ine ffi ciency, which increases at lowflux level. This e ff ect was calibrated and is now correctedby the pipeline, which reallocates the charge lost during thereadout process on each extracted pixel (Bouchy et al. 2009).Uncertainties on the radial velocity measurements include pho-ton noise, uncertainties in the wavelength calibration, and sys-tematic instrumental errors. The photon noise RV uncertaintydepends on the signal-to-noise of the spectra, as well as on thespectral type and the rotation velocity v sin i of the observedstar. It can be approximated by the semi-empirical estimator σ RV = A × √ FWHM / (S / N × C ), where FWHM is the full widthat half maximum of the CCF (in same unit as σ RV ), C is its con-trast (in percent of the continuum), S / N is the signal-to-noiseratio per pixel at 550 nm, and the scaling factor A = . ffi ciency mode, respectively. For a non-rotating K-dwarf star, a S / N per pixel of 150 provides a photon-noise RV uncertainty of 1 m s − . Such a S / N is obtained on 5-mnon a 6.5 magnitude star. The uncertainty of the wavelength cali-bration was estimated to 1 m s − . Telescope guiding and center-ing errors in averaged weather conditions are typically of 0.3 - 1arcsec. In high-resolution mode, these errors imply a RV jitter of3-4 m s − due to the insu ffi cient scrambling gain of the fiber.This corresponds to the dispersion obtained on the S OPHIE measurements around the orbit of HD 189733b, after correctionof the stellar jitter (Boisse et al. 2009). Uncertainties due to guid-ing errors are more than twice this level in high-e ffi ciency modedue to the absence of scrambler in this instrumental setup. http: // / sci / facilities / lasilla / instruments / harps / doc / index.html The present radial velocity precision obtained on stable starsis about 4-5 m s − over several semesters. This limitation ismainly due to guiding and centering e ff ects on the fiber entranceat the telescope focal plan and the insu ffi cient scrambling pro-vided by the fiber and the double scrambler. An upgrade of theCassegrain fiber adapter is presently on-going, including newhigh-precision guiding camera and new double scrambler, withthe goal to reach the precision level of 1-2 m / s.
3. The
SOPHIE exoplanet program
The
S OPHIE consortium program is devoted exclusively tothe study and characterization of exoplanets, in continuation ofa planet-search program initiated 15 years ago with ELODIEspectrograph (Queloz et al. 1998) and in complement to theHARPS program performed in the southern hemisphere (Mayoret al. 2003). We started on October 2006 a key program withthe aims to cover a large part of the exoplanetary science and tobring constraints on the formation and evolution processes ofplanetary systems. Our observing strategies and target samplesare optimized to achieve a variety of science goals and to solveseveral important issues: 1) mass function of planets below themass of Saturn, 2) planetary statistical properties to constrainthe formation and evolution models, 3) relationships betweenplanets and the physical and chemical properties of theirstars, 4) detection of exoplanets around nearby stars, allowingspace and ground-based follow-up, 5) deep characterizationof known transiting exoplanets including long term follow-upand spectroscopic transit analysis. All these aspects are treatedthrough 5 complementary sub-programs discussed below andusing an amount of 60 to 90 nights per semester allocated on
S OPHIE at the 1.93-m telescope. - High precision search for super-Earth
Only a few percents of the 350 detected planets have massesless than 0.1 M
Jup , and due to the present precision of radialvelocity surveys, the distribution of planetary masses is heavilybiased against low-mass planets. Recent HARPS discoveriesindicate that these low-mass exoplanets are not rare and suggestthat 30% of non-active G and K dwarfs solar-type harborNeptune or rocky planets with periods shorter than 50 days(Lovis et al. 2009, Mayor et al. 2009). From the ELODIE surveyand from our volume-limited sub-program, we pre-selected asample of about 200 non-active bright solar-type stars to explorethis domain of low-mass planets. - Giant planets survey on a volume-limited sample
For a large volume-limited sample of 2000 stars, we performa first screening to identify new Hot Jupiters and other Jovian-type planets orbiting near and bright stars. Increasing the list ofHot Jupiters o ff ers a chance to find a transiting one orbiting abright star appropriate for additional study of planetary atmo-sphere. This survey will also provide better statistics to searchfor new properties of the distribution of exoplanet parameters.We include on this sub-program the long term follow-up andthe spin-orbit analysis – from the Rossiter-McLaughlin e ff ect– of known transiting giant exoplanets to respectively detectadditional companions and determine the spin-orbit angle of thesystem. - Search for exoplanets around M-dwarfs A systematic search for planets is made for a volume-limitedsample of 180 M-dwarfs closer than 12 parsecs. Such a surveyof low mass stars will give us a chance to derive the frequency . Bouchy et al.: A massive Jupiter around HD 16760 3 of planets as function of the stellar mass. The objectives are1) to detect exoplanets of few Earth masses in the habitablezone, 2) to determine the statistics of planetary systems orbitingM-dwarfs in combining these 180-M dwarfs sample with 100-Mdwarfs monitored with HARPS, 3) to identify new potentialtransiting Hot Neptunes. - Search for exoplanets around early-type main sequence stars
A systematic search for planets around a sample of 300early-type main sequence stars (A and F stars) is performedto study the impact of the host star mass on the exoplanetformation processes. Such stars were previously not includedin the exoplanet surveys due to their lack of spectral lines andhigh rotation broadening. A specific pipe-line was developedto compute radial velocity on these specific targets (Galland etal. 2005a) with an accuracy allowing the detection of planetsfrom massive hot Jupiters for fast rotating A stars, and down toNeptune-mass planets for the slowest F stars. - Long term follow-up of ELODIE long period candidates
The ELODIE program for exoplanet search which started on1994 was performed on a sample of 320 G and K stars. About40 of these stars present evidence of long term trends whichmay be due to giant planets with Jupiter or Saturn like orbit. Along term follow-up of these candidates is performed to explorethe domain of long period ( ≥
10 years) planets.As part of the
S OPHIE consortium programs, the detectionof four exoplanets have been published up to now: HD 43691band HD 132406b (Da Silva et al. 2008), HD 45652b (Santos etal. 2008), and θ Cygni b (Desort et al. 2009). These planets haverespectively minimum masses of 2.5, 5.6, 0.5 and 2.3 M
Jup witha 37, 975, 44 and 154 day periods. There were first found fromthe ELODIE or CORALIE survey then monitored by
S OPHIE .Spectroscopic transits of the massive planets HD 147506b andXO-3b were also observed (Loeillet et al. 2008 and H´ebrard et al.2008, respectively), allowing a refinement of the parameters ofthe systems, and the detection of a first case of misaligned spin-orbit for XO-3 (recently confirmed by Winn et al. 2009). A studyof the stellar activity of the transiting planet host star HD 189733is also presented by Boisse et al. (2009). Recently the transitof the 111-day period exoplanet HD 80606b was established byMoutou et al. (2009).Outside of the consortium programs,
S OPHIE plays an ef-ficient role in the Doppler follow-up of photometric surveys forplanetary transits search. It allowed the planetary nature to beestablished for transiting candidates found by SuperWASP (e.g.Collier Cameron et al. 2007, Pollacco et al. 2008, Hebb et al.2008), by HAT (Bakos et al. 2007) and by CoRoT space mis-sion (e.g. Barge et al. 2008, Bouchy et al. 2008, Moutou et al.2008, Deleuil et al. 2008, Rauer et al. 2009), as well as the pa-rameters of these new planets to be characterized, including themeasurement of the masses.In the next section we present the detection of the substel-lar companion orbiting HD 16760 as part of our sub-program 2“
Giant planets survey on a volume-limited sample ”.
4. The substellar companion of HD 16760
HD 16760 (HIP 12638, BD +
37 604) is a G5V star located 50 pcaway according the Hipparcos parallax. Table 1 summarizes thestellar parameters. From spectral analysis of the
SOPHIE data using the method presented in Santos et al. (2004), we derived T e ff = ±
20 K, log g = . ± .
10, [Fe / H] = − . ± . M ∗ = . ± .
06 M ⊙ , which agrees with values from lit-erature. For the temperature and the mass, the values we adoptin Table 1 are compromise values between ours and those ob-tained by Nordstr¨om et al. (2004) ( T e ff = M ∗ = . + . − . M ⊙ ). We derive v sin i = . ± . − from theparameters of the CCF using a calibration similar to those pre-sented by Santos et al. (2002), in agreement with the value v sin i = − from Nordstr¨om et al. (2004). The CCF alsoallows the value [Fe / H] = . ± .
05 to be measured, in agree-ment but less accurate than the metallicity obtained above fromspectral analysis. This target has a quiet chromosphere with noemissions in the Ca ii lines (log R ′ HK = − . ± . Table 1.
Adopted stellar parameters for HD 16760.
Parameters Values References m v .
744 Nordstr¨om et al. (2004)Spectral type G5V Hipparcos catalog B − V . ± .
02 Hipparcos catalogDistance [pc] 50 ± / yr] 82 . ± . / yr] − . ± . v sin i [ km s − ] 2 . ± . R ′ HK − . ± . / H] − . ± .
03 this work T e ff [K] 5620 ±
30 Nordstr¨om et al. (2004) & this worklog g [cgi] 4 . ± . ⊙ ] 0 . ± .
08 Nordstr¨om et al. (2004) & this work
HD 16760 has a stellar companion, HIP 12635 (Apt 1988,Sinachopoulos 2007), located 14 . ± .
008 arcsec in theNorth and 1 . ± .
002 mag fainter. From Hipparcos cata-log (Perryman et al., 1997), HIP 12635 has similar distance(45 ± = ± = ±
12) with HD 16760, making them a likely phys-ical system, with a separation >
700 AU and an orbital period >
10 000 years. This would induce tiny radial velocity variationson the stars, below 0 . − yr − . We acquired with
SOPHIE
20 spectra of HD 16760 within objAB mode between December 2006 and October 2008 under goodweather conditions. Two of these 20 spectra were polluted bysignificant Moon contamination. The velocity of the CCF due tothe Moon was far enough from those of the target to avoid anysignificant e ff ect on the radial velocity measurement. We did notuse these two spectra however for the spectral analysis presentedin § − , which is the quadratic sum of three sources ofnoise: photon noise (3 m s − ), guiding (4 m s − ), and spectro-graph drift (3 m s − ).The radial velocities, shown in Fig. 1, present clear varia-tions of the order of hundreds m s − , without significant vari-ations ( σ <
10 m s − ) of the CCF bisector (Fig. 2), thus inagreement with the reflex motion due to a companion. We fit-ted the data with a Keplerian model. The solution is a 465-day F. Bouchy et al.: A massive Jupiter around HD 16760
Fig. 1.
Top:
Radial velocity
SOPHIE measurements ofHD 16760 as a function of time, and Keplerian fit to the data.The orbital parameters corresponding to this fit are reported inTable 3.
Bottom:
Residuals of the fit with 1- σ error bars. Table 2.
Radial velocities of HD 16760 measured with
SOPHIE . BJD RV ± σ exp. time S / N p. pix.-2 400 000 (km s − ) (km s − ) (sec) (at 550 nm)54099.3679 -3.6736 0.0055 300 62.554126.3439 -3.7916 0.0058 300 52.154127.2914 -3.8085 0.0068 480 36.254133.2541 -3.8478 0.0055 224 61.454138.3414 -3.8366 0.0054 673 67.154148.3393 -3.8898 0.0071 224 35.154151.3375 -3.9150 0.0092 225 30.054155.2737 -3.9168 0.0063 180 43.554339.6353 -3.3666 0.0053 512 78.754352.6607 -3.2786 0.0058 380 52.054367.6375 -3.2481 0.0055 300 61.254407.4733 -3.1806 0.0053 500 79.554434.4441 -3.1703 0.0055 620 64.254502.2489 -3.3798 0.0057 443 54.554513.2880 -3.4358 0.0059 464 53.454546.2900 -3.5725 0.0061 1304 47.354683.6329 -3.9680 0.0058 393 51.454705.6646 -3.9045 0.0058 379 51.254739.5899 -3.7242 0.0059 350 50.154755.5295 -3.6488 0.0058 270 51.2 period oscillation with a semi-amplitude K =
408 m s − , cor-responding to a substellar companion, with a minimum mass m p sin i = . Jup . The derived orbital parameters are reportedin Table 3, together with error bars, which were computed from χ variations and Monte Carlo experiments.The standard deviation of the residuals to the fit is σ ( O − C ) = . − . This is higher than the 6- m s − estimated uncertaintyon the individual measurements. Although about 23% of gaseousgiant planets are in a multiple planetary system, we do not iden-tify yet an indication for a second body orbiting HD 16760. Witha maximum semi-amplitude of 20 m s − , the residuals of the fitdo not exhibit structures, denying a possible inner planet with a m p sin i ≥ Jup . A longer period planet may induce a driftlower than 20 m s − yr − during our observational period. Fig. 2.
Bisector span as a function of the radial velocity.
Table 3.
Fitted orbit and planetary parameters for HD 16760b.
Parameters Values and 1- σ error bars Unit V r − . ± .
004 km s − P . ± . e . ± . ω − ± ◦ K ± − T (periastron) 2 454 723 ±
12 BJD σ ( O − C ) 10.1 m s − reduced χ N obs m p sin i . ± . † M Jup a . ± . † AU † : using M ⋆ = . ± .
08 M ⊙
5. Discussion and Conclusion
Our RV measurements indicates that a substellar companionwith a projected mass m p sin i = . Jup is orbiting HD 16760.With the degeneracy of inclination angle i , it is di ffi cult to con-clude about the exact nature of this companion. It may corre-spond to a massive planet, formed in a gaseous protoplanetarydisk, or a brown dwarf, issued from collapse in a giant molecu-lar cloud.Figure 3 shows the mass distribution of massive planets( m p sin i ≥ Jup ) and light brown dwarfs ( M c sin i ≤
30 M
Jup )found by radial velocity surveys. From the Extrasolar PlanetsEncyclopaedia list , we completed with HD 137510b (Endl etal. 2004), HD 180777b (Galland et al. 2005b), and HD 16760b(this paper), totalizing 89 objects including 10 with mass in-between 15 and 30 M Jup . The dashed curve corresponds to therelation M − (dN / dM = M − ). The black shaded histogram corre-sponds to the transiting planets with true masses (excluding non-confirming objects SWEEPS-11 and SWEEPS-04). It is worth-while to notice that, although based on a small number of object,the mass distribution of transiting planets is following the sametrend than non-transiting planets. Indeed, the ratio of transitingplanets over non-transiting planets is about the same : 9.2, 9.5and 10 for the bins 3-6, 6-9 and 9-12 M Jup respectively. In thishistogram, HD 16760b seems to be located just at the end of themass distribution of giant planets. Although based on small num- http: // exoplanet.eu. Bouchy et al.: A massive Jupiter around HD 16760 5 bers, sub-stellar companions with minimum mass greater than17 M Jup do not seem to follow the M − relation.Figure 4 shows the eccentricity - period diagram of mas-sive exoplanets and light brown dwarfs. The size of circle isfunction of the mass (3-5, 5-10, 10-15 M Jup ). Hexagonal pointscorresponds to objets with mass greater than 15 M
Jup . Blackfilled symbols correspond to transiting companions. HD 16760bconfirms the observed trend that more massive companions arefound for longer period planets (Udry & Santos 2007). We alsonotice that all companions with mass greater than 15 M
Jup havean eccentricity greater than 0.2 except CoRoT-exo-3b (Deleuil etal. 2008) and HD 41004Bb (Zucker et al. 2004) in very close-inorbit (with periods of respectively 4.2 et 1.3 days) tidally cir-cularized. The properties of HD 16760b make it an interrestingsub-stellar companion. With a mass greater than the Deuteriumburning limit (13 M
Jup ), it may be defined as a brow-dwarf.However its quite circular orbit supports a formation in a gaseousprotoplanetary disk. On another way, Halbwachs et al. (2005)studied the eccentricity distribution for exoplanets and binarystars with a mass ratio smaller than 0.8 (non twin binaries). Theyfound that exoplanets have orbits with eccentricities significantlysmaller than those of the non-twin binaries, reinforcing the hy-pothesis that planetary systems and stellar binaries are not theproducts of the same physical process.HD 16760b is in a visual and physical binary system.However, in the mass-period and eccentricity-period diagrams,HD 16760 b is located in a region not much populated by plan-ets in binary systems. The discovery of this long-period low-eccentricity planet thus adds to the growing evidence that con-trary to short-period planets, long-period ( &
100 days) planetsresiding in binaries possess the same statistical properties astheir counterparts orbiting single stars (Eggenberger et al. 2004,Mugrauer et al. 2005, Desidera et al. 2007).HD 16760b would induce a motion of its host star of at least ± .
35 milli-arcsec. The future Gaia ESA space mission sched-uled for launch in late-2011, should be able to detect this sys-tem from astrometry, and thus would allow the inclination ofthe system to be measured and the true mass to be determined.Detailed caracterization of this sub-stellar companion close toplanet / brow-dwarf transition will help to distinguish the di ff er-ences of formation processes between these two populations. Acknowledgements.
The authors thanks all the sta ff of Haute-ProvenceObservatory for their contribution to the success of the SOPHIE project and theirsupport at the 1.93-m telescope. We wish to thank the “Programme National dePlan´etologie” (PNP) of CNRS / INSU, the Swiss National Science Foundation,and the French National Research Agency (ANR-08-JCJC-0102-01 and ANR-NT05-4-44463) for their continuous support to our planet-search programs. F.B.acknowledges S.F.Y.B.L.S for continuous support and advices.
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