Long-Period Objects in the Extrasolar Planetary Systems 47 UMa and 14 Her
a r X i v :a s t r o -p h /0609117v 1 5 S e p 2006
Accepted for publication in ApJ
Preprint typeset using L A T E X style emulateapj v.6/22/04
LONG-PERIOD OBJECTS IN THE EXTRASOLAR PLANETARY SYSTEMS 47UMA AND 14HER 1
Robert A.Wittenmyer,Michael Endl,William D.Cochran
McDonald Observatory,University of Texas at Austin,Austin,TX 78712
Accepted for publication in ApJ
ABSTRACT
The possible existence of additional long-period planetary-mass objects in the extrasolar planetary systems 47UMa and 14Her is investigated.We combine all available radial-velocity data on these stars,spanning up to 18years.For the 47UMa system,we show that while a second planet improves the ?t to all available data,there is still substantial ambiguity as to the orbital parameters of the proposed planetary companion 47UMa c.We also present new observations which clearly support a long-period companion in the 14Her system.With a period of 6906±70days,14Her c may be in a 4:1resonance with the inner planet.We also present revised orbital solutions for 7previously known planets incorporating recent additional data obtained with the 2.7m Harlan J.Smith Telescope at McDonald Observatory.
Subject headings:stars:individual,47UMa,14Her –stars:planetary systems –extrasolar planets –
techniques:radial velocities
1.INTRODUCTION
The longest-running radial-velocity surveys are now approaching time baselines of 16-18years (Butler et al.1996;Cochran et al.1997).These surveys now achieve internal measurement precisions such that the signals from long-period giant planets (P >～10yr)are now enter-ing the realm of detectability (Wittenmyer et al.2006).For example,the High Resolution Spectrograph (HRS)on the Hobby-Eberly Telescope (HET)now has a ve-locity precision of 3-4m s ?1(Cochran et al.2004),the Keck HIRES is achieving 1-2m s ?1since its 2004CCD upgrade (Butler et al.2006),and the HARPS instrument has demonstrated precision better than 1m s ?1(Lovis et al.2006).Of particular interest are pu-tative multi-planet systems,wherein the residuals of a known-planet’s orbit show Keplerian periodicity indica-tive of a distant giant planet companion in the system.Finding systems which contain long-period giant planets as well as planets in closer orbits will address important questions about the uniqueness of our own Solar System’s architecture.
Long-period planet candidates have been reported for 47UMa (P =7.1yr,Fischer et al.2002),55Cancri (P =12.4yr,McArthur et al.2004),HD 217107(P >7yr,Vogt et al.2005),and HD 72659(P =9.9yr,Butler et al.2006).Of particular interest are systems which contain both short-period and long-period jovian planets.Such systems could provide clues to address the question of how the processes of planet formation and migration can result in both “hot”and “cold”Jupiters in the same planetary system.
In this paper,we present improved ?ts to the known planets in nine systems using all available data,and we investigate the possibility of additional long-period ob-jects.In §2,we brie?y describe the data acquisition and
Electronic address:robw@https://www.wendangku.net/doc/0a15067056.html,
1Based on observations obtained with the Hobby-Eberly Tele-scope,which is a joint project of the University of Texas at Austin,the Pennsylvania State University,Stanford University,Ludwig-Maximilians-Universit¨a t M¨u nchen,and Georg-August-Universit¨a t G¨o ttingen.
?tting procedure.The results are given in §3,including
our solutions for seven additional planetary systems in the McDonald Observatory planet search program.All of our radial-velocity measurements for these objects are presented in Tables 5-14.In this paper,we use the terms “McDonald”to refer to data taken with the McDonald Observatory 2.7m Harlan J.Smith (HJS)Telescope,and “HET”to refer to data taken with the 9.2m Hobby-Eberly Telescope.
2.OBSERVATIONS AND DATA ANALYSIS
Data obtained from the McDonald Observatory planet search program (Endl et al.2005)are discussed fully in Wittenmyer et al.(2006).Available published data were combined with the McDonald data to ?t Keplerian or-bits using GaussFit (Je?erys et al.1987).GaussFit has the ability to allow the o?sets between data sets to be a free parameter.Parameters of the primary stars con-sidered are given in Table 1;masses,[Fe/H],and T eff are from Santos et al.(2004),and the chromospheric ac-tivity index log R ′
HK is derived from Ca II measure-ments from the McDonald Observatory spectra.For each object,we searched for periodic signals in the residu-als to the known planet’s orbit using the periodogram method (Lomb 1976;Scargle 1982).To assess the statis-tical signi?cance of those periods,the false alarm prob-abilities (FAP)were calculated using the bootstrap ran-domization method detailed by K¨u rster et al.(1997)and Endl et al.(2002).
3.RESULTS AND DISCUSSION
The Keplerian orbital ?ts are shown in Figures 1-4,and the orbital parameters implied by those ?ts are given in Table 2.In computing the planetary minimum mass M sin i and semimajor axis a ,the stellar masses derived by Santos et al.(2004)listed in Table 1were used,with adopted uncertainties of 0.05M ⊙.
3.1.47UMa (=HD 95128):Ambiguities concerning the
second planet
Butler &Marcy (1996)?rst reported the 1090-day companion to 47UMa using data from Lick Observa-
2Wittenmyer,Endl,Cochran
tory.With additional velocity measurements over13 years,Fischer et al.(2002)announced a long-period sec-ond planet,47UMa c,with a period of2594±90days and a mass of0.76M Jup.Naef et al.(2004)presented ELODIE observations of47UMa,and noted that the second planet was not evident in their data,which were ?t well with a single Keplerian model.
We now?t four data sets for47UMa:Lick(Fischer et al2002,N=91),ELODIE(Naef et al.2004,N=44),2.7m HJS telescope(N=35),and the Hobby-Eberly Telescope (HET,N=201).The HET data,which consist of multi-ple exposures per visit,were binned using the weighted mean value of the velocities in each visit.The quadra-ture sum of the rms about the mean and the mean in-ternal error bar was adopted as the error bar of each binned point(N=63).The o?set between the overlap-ping HJS and HET datasets was used to merge them into one,which was used in all?ts.The one-planet?t (Model1)and the residuals to that?t are shown in Fig-ure1.We emphasize that this?t includes all available published data,over a time span of more than18years, and includes195high-precision measurements obtained with the HET High-Resolution Spectrograph at61inde-pendent epochs,which are given in Table6.The total rms about the combined one-planet?t is10.4m s?1. The rms scatter about the one-planet?t for each of the four datasets is:Lick–10.7m s?1,ELODIE–13.0m s?1, HJS–13.5m s?1,HET–4.9m s?1.A periodogram of the residuals of all of the data to the1-planet?t is shown in Figure2.No clear peak rises above the noise level at any period between2and10000days;the total duration of the available data is now about6900days(18.3years). While a peak is present at about2212days,close to the period reported for47UMa c by Fischer et al.(2002), its false-alarm probability(FAP)is27.2%.
To further explore the possible presence of47UMa c, we?t all of the datasets with a two-planet model?xed at the parameters of Fischer et al.(2002)(Model2), and then repeated the?t allowing all parameters to be free except for e andωof the second planet(Model3), which were?xed at0.005and127o,respectively,after Fischer et al.(2002).No models achieved convergence with those two parameters free.The?t obtained by Model3is shown in the right panel of Figure2.Model 2had a reduced chi-square(χ2ν)of5.81and an rms of 12.7m s?1about the?t,whereas Model3had aχ2νof 2.11and an rms of8.4m s?1.For comparison,the one-planet?t(Model1)had aχ2νof3.23and an rms of 10.4m s?1.Noting that the poor?t of Model2was largely due to errors in the period of the inner planet, we re-did the?ts allowing the parameters for the inner planet to be free while?xing those of the outer planet at the values reported by Fischer et al.(2002)(Model4). Theχ2νof this?t was2.68,with an rms of10.2m s?1. These tests are summarized in Table3.The free two-planet(Model3)?t was the best of the four,in terms of both the goodness-of-?t criterion(χ2ν)and the total rms scatter about the?ts.The rms about the individ-ual datasets for this?t is the following:Lick–8.0m s?1, ELODIE–11.1m s?1,HJS–10.1m s?1,HET–5.3m s?1. The parameters for the47UMa planetary system given in Table2are those obtained by Model3.Although the best-?t set of parameters obtained a period of7586days for the outer planet,there is no corresponding peak on the periodogram shown in Figure2.However,the pe-riodogram method is not as reliable when the periodic signal approaches or exceeds the total duration of obser-vations,as is the case here,where the total time baseline is6942days.We note that we have been able to repro-duce the result of Fischer et al.(2002)by this method;
i.e.a periodogram analysis of the Lick data alone after removing47UMa b revealed a strong peak at2083days, but still with a FAP of0.15%.We are also able to re-cover the Fischer et al.(2002)parameters of47UMa c from the Lick data alone.Since the total time coverage of the Lick data presented in Fischer et al.(2002)is5114 days(14yr),an analysis of those data alone is not ad-equate to fully constrain the7586-day period obtained by our best-?t model which adds four years to the total duration of observations.It is possible that the shorter period for47UMa c reported by Fischer et al.(2002)is an alias of the true period;at present,our?ts indicate that period to be about three times longer,but with sub-stantial uncertainty.
To further test the methods by which we conclude that the parameters of47UMa c reported by Fischer et al. (2002)are dubious,we performed some Monte Carlo sim-ulations.From each of the three data sets considered in the?ts described above,we generated1000simulated sets of velocities consisting of a Keplerian signal plus 7m s?1of Gaussian noise for each of the two planets. The parameters for the inner planet were those listed in Table2,and those of the outer planet were those of Fischer et al.(2002).These simulated datasets re-tained the times of observation and the error bars of the originals.The simulated data were then?t with a one-planet model exactly as described above,then the residuals of the one-planet?t were examined by the pe-riodogram method,to determine whether the signal of the second planet was recovered.The criteria for re-covery were that the period of the second planet had to be detected correctly and with a FAP of less than 0.1%.This FAP was computed using the analytic FAP formula of Horne&Baliunas(1986).Of the1000trials, only6did not result in a successful recovery of the signal of the second planet.The correct period was recovered 999times,and the FAP exceeded0.1%only5times;the worst FAP was0.24%.For comparison,the analytic FAP of the2212-day peak in the residuals of the1-planet?t is1.7%,a factor of7higher.These results indicate that our method should have been able to detect the signal of47UMa c,had it been present with the parameters given by Fischer et al.(2002)and Butler et al.(2006). We conclude that while an additional long-period object may be present,the data currently available do not pro-vide su?cient evidence for an orbital solution.
3.2.14Her(=HD145675):Evidence for an outer
companion
Thirty-?ve radial-velocity measurements of14Her (=HD145675)obtained at McDonald Observatory were combined with published data from Keck HIRES (Butler et al.2006)and ELODIE(Naef et al.2004).The ?t to the combination of these three data sets is shown in Figure3,and the system parameters implied by that ?t are given in Table2.It is evident from Figure3that the single Keplerian?t is inadequate(rms=13.0m s?1); indeed,the residuals to the?t show a clear curvature.
Long-Period Companions3
Naef et al.(2004)noted an upward linear velocity trend of3.6±0.3m s?1yr?1in their observations which covered the time interval1994to2003,but the Keck data of Butler et al.(2003)indicated no such trend.When the complete12yr duration of observations is examined,we see that those Keck data were serendipitously obtained during a period of relatively constant residual velocity, and the more recent McDonald data are now indicating a downward trend.Fitting a double-Keplerian model(Fig-ure4)with T0for the outer body?xed at2449100.0yields an eccentricity consistent with zero:e=0.02±0.06.Fix-ing the eccentricity of14Her c at0.0gives a minimal orbit solution with period P=6906±70days,and a velocity semi-amplitude K=24.5±1.4m s?1.These orbital elements imply a minimum mass M sin i=2.1 M Jup at a semimajor axis of6.9AU.This represents the lowest possible mass and the shortest period for the outer companion.The rms scatter about the three data sets is as follows:ELODIE–10.4m s?1,Keck–2.9 m s?1,McDonald–5.8m s?1.The total rms about this two-planet?t is8.4m s?1,with aχ2νof1.67.The minimal orbit proposed above for14Her c has a perias-tron distance of6.2AU,and14Her b has an apastron distance of3.76AU.The orbit of14Her c,at a large semimajor axis with a small eccentricity,is similar to that of HD72659b(Butler et al.2003)and HD50499b (Vogt et al.2005).We emphasize that such?ts are pre-liminary,and are only given in order to place a lower limit on the period and mass of this object.Go′z dziewski et al. (2006)performed dynamical simulations of the14Her system,and proposed the existence of14Her c based on?ts to data from Butler et al.(2003)and Naef et al. (2004).The two most-favored models had14Her c near the3:1or6:1mean-motion resonance(MMR),which co-incided with highly stable orbital con?gurations as de-termined by their dynamical simulations.The prelimi-nary?t obtained in this work suggests a4:1resonance for14Her c.We attempted to?t a double-Keplerian model with14Her c?xed at the3:1MMR parameters indicated in Go′z dziewski et al.(2006),but obtained a substantially worse?t(χ2ν=2.2).
An upper limit on the mass of14Her c can be es-timated from the results of adaptive-optics(AO)imag-ing by Luhman&Jayawardhana(2002),who used the Keck II AO system to search for companions to25 extrasolar planet-host stars.No candidate compan-ions were found around14Her,and the detection lim-its derived from their study exclude stellar-mass ob-jects objects at orbital separations>～9AU(see Luh-man&Jayawardhana2002,their Fig.10).A simi-lar study by Patience et al.(2002)using the Lick AO system also excluded stellar-mass objects beyond about 12.7AU.We can therefore use the upper limit pro-vided by Luhman&Jayawardhana(2002)and our lower bound to constrain the mass of the outer companion be-tween about2.1and80M Jup.A more de?nitive state-ment on its nature,of course,requires many more years of observations,until a second velocity turnaround is con-?rmed.The large separation implied by these data make 14Her an attractive target for future direct imaging at-tempts and for astrometric follow-up.The astrometric perturbation due to14Her c would beα=0.9mas,us-ing the minimal orbit solution given above.For sin i=0.5,this signal would beα=1.8mas,equivalent to that of ?Eri b(Benedict et al.2006).Since the astrometric per-turbation increases with semimajor axis and planet mass, the signal could be much larger(Sozzetti2005).
3.3.Revised orbital parameters for7additional systems The addition of new data from the HJS Telescope pre-sented in this paper,and the use of multiple independent data sets in?tting Keplerian orbits,have generally im-proved the precision of the derived planetary parameters by25-50%.In particular,the precision of the orbital pe-riods have been improved by the addition of new data, due to the increased number of orbits now observed.In this section,we brie?y describe the results of our com-bined?ts for seven additional systems for which the re-vised orbital solutions are in agreement with previously published results.Our parameters are within2σof pre-vious values except for T0andωofυAnd c,and P and ωofυAnd d,which di?er from Butler et al.(2006)by between2.7and3.8sigma.
The inner planet of HD217107,with a period of7.1 days,was?rst reported in Fischer et al.(1999),and ad-ditional CORALIE data supporting this discovery were published by Naef et al.(2001).A shallow parabolic trend in the residuals was noted by Fischer et al.(2001). Vogt et al.(2005)used more recent Keck data to postu-late an outer companion with P>7years.However,this object has not completed a full orbit,and hence there is a wide range of possible solutions.Wright et al.(2005)re-vised the period of HD217107c to20,140days(55years), and Vogt et al.(2005)give a period of3150days;our?ts with the short period improvedχ2νby only0.07over the long period.We?t four datasets for HD217107:Lick (Fischer et al.1999),CORALIE(Naef et al.2001),Keck (Vogt et al.2005),and20observations from McDonald. We?t a double-Keplerian model using the parameters for planet c from Vogt et al.(2005)as a starting point for the least-squares?tting procedure.The rms of this double-Keplerian?t is9.0m s?1,and the results are given in Table2.The resulting parameters are in agreement with Vogt et al.(2005)to within2σ.Vogt et al.(2005)per-formed separate?ts to the Lick and Keck data and com-mented on the high degree of uncertainty in the parame-ters of HD217107c.The combined?ts given in this work support the～3150-day period reported by Vogt et al. (2005),but the uncertainties remain large.At present, no de?nitive statements can be made until this object completes a signi?cant fraction of an orbit,or until such time as it can be detected via direct imaging or astrome-try,techniques which are well-suited to very long-period objects.
The three planets aroundυAnd(=HD9826)were ?t with a triple-Keplerian model,combining the Lick data of Butler et al.(2006)and the Advanced Fiber Op-tic Echelle(AFOE)data of Butler et al.(1999)with41 observations from McDonald.Lick data preceding the Hamilton spectrometer upgrade(1995February)were excluded following Butler et al.(1997).The total rms about the?t is14.6m s?1.As shown in Table4,analy-sis of the residuals to a triple-Keplerian?t resulted in only a marginally signi?cant periodicity at2000days (FAP=0.4%).
Marcy et al.(1999)?rst detected the inner compan-ion to HD168443using the HIRES spectrograph on
4Wittenmyer,Endl,Cochran
Keck I.The outer4.8-yr planet was then reported in Marcy et al.(2001)and con?rmed by Udry et al.(2002).
A two-planet?t to the McDonald data combined with that of Butler et al.(2006)and Udry et al.(2002)yields an rms of9.5m s?1.The parameters given in Table2 are in agreement with those of Butler et al.(2006)within 2σ.Periodogram analysis of the residuals to the double-Keplerian?t revealed a63-day periodicity with a FAP of0.12%(Table4).Performing the same analysis on the three datasets separately,however,showed no enhanced power at that period.Additionally,the period of the in-ner planet is58days,preventing any object in a63-day orbit.
The following?ve planets showed no residual period-icities of interest.The hot Jupiter orbiting HD179949 was found by the Anglo-Australian Planet Search pro-gram using the3.9m Anglo-Australian Telescope(AAT) (Tinney et al.2001).The rms about the combined ?t is11.5m s?1,and the?tted parameters agree with those of Butler et al.(2006)to within1σ.For 16Cyg B(=HD186427),data from the discovery paper (Cochran et al.1997)and Lick data from Butler et al. (2006)were combined with37additional measurements from McDonald Observatory.The rms about the com-bined?t is10.6m s?1,and the orbital elements are within2σof those given in Butler et al.(2006).For HD195019b,Lick data from Butler et al.(2006)were combined with19McDonald observations.The rms about the combined?t is15.8m s?1,and the param-eters agree with those of Butler et al.(2006)within2σ. For HD210277b,data from Butler et al.(2006)and Naef et al.(2001)were combined with21measurements from McDonald.The rms about the combined?t is6.8m s?1,and the planetary parameters agree with those of Butler et al.(2006)to within2σ.
4.SUMMARY
We have combined new radial-velocity observations from McDonald Observatory with previously published data to improve the precision of the orbital parameters for9planetary systems.The largest data set yet as-sembled on47UMa indicates no statistically signi?cant signal attributable to a second planet in the system.We have examined the residuals to our Keplerian?ts,and for the case of14Her,we?nd clear evidence for a distant outer companion,which appears to be in a4:1resonance with the inner planet.
This research was supported by NASA grants NNG04G141G and NNG05G107G.R.W.acknowledges support from the Sigma Xi Grant-in-Aid of Research and the Texas Space Grant Consortium.We are grate-ful to Barbara McArthur for her assistance with Gauss-Fit software,and to G.F.Benedict for helpful discus-sions on astrometry.This research has made use of NASA’s Astrophysics Data System(ADS),and the SIM-BAD database,operated at CDS,Strasbourg,France. The Hobby-Eberly Telescope(HET)is a joint project of the University of Texas at Austin,the Pennsyl-vania State University,Stanford University,Ludwig-Maximilians-Universit¨a t M¨u nchen,and Georg-August-Universit¨a t G¨o ttingen The HET is named in honor of its principal benefactors,William P.Hobby and Robert E.Eberly.
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6Wittenmyer,Endl,Cochran
TABLE1
Stellar Parameters
Star Spec.Type Mass(M⊙)[Fe/H]T ef f(K)log R′HK
υAnd F8V 1.300.13±0.086212±64-5.01
47UMa G1V 1.070.06±0.035954±25-5.04
14Her K0V0.900.43±0.085311±87-5.06
HD168443G50.960.06±0.055617±35-5.14
HD179949F8V 1.280.22±0.056260±43-4.75
16Cyg B G3V0.990.08±0.045772±25-5.03
HD195019G3IV-V 1.060.08±0.045842±13-4.89
HD210277G0V0.920.19±0.045532±14-5.11
HD217107G8IV 1.020.37±0.055646±26-5.13
TABLE2
Keplerian Orbital Solutions
Planet Period T0eωK M sin i a
(days)(JD-2400000)(degrees)(m s?1)(M Jup)(AU)υAnd b 4.61708±0.0000650001.8±0.40.029±0.01346±2971.1±1.00.69±0.030.059±0.001
υAnd c241.52±0.2150149.7±3.30.254±0.016232.4±4.956.1±1.2 1.98±0.090.83±0.01
υAnd d1274.6±5.050074±160.242±0.017258.5±5.464.1±1.1 3.95±0.16 2.51±0.04
47UMa b1083.2±1.850173±650.049±0.014111±2249.3±1.0 2.60±0.13 2.11±0.04
47UMa c a7586±72752134±1460.005(?xed)127(?xed)13.3±1.4 1.34±0.227.73±0.58
14Her b1773.4±2.551372.7±3.60.369±0.00522.6±0.990.0±0.5 4.64±0.19 2.77±0.05
HD168443b58.1112±0.000950047.45±0.040.530±0.001172.7±0.2476.0±1.07.48±0.270.290±0.005
HD168443c1765.8±2.250255±40.222±0.00364.6±0.8299.2±1.016.87±0.64 2.84±0.05
HD179949b 3.09250±0.0000351793.98±0.290.022±0.014183±34112.8±1.60.95±0.040.045±0.001
16Cyg B b799.5±0.650539.3±1.60.689±0.01183.4±2.151.2±1.1 1.68±0.07 1.68±0.03
HD195019b18.2008±0.000350033.1±0.80.014±0.004239±16272.8±1.0 3.67±0.130.138±0.002
HD210277b442.1±0.450988.2±1.60.472±0.011118.2±1.939.5±0.5 1.23±0.05 1.10±0.02
HD217107b7.12689±0.0000549998.50±0.040.132±0.00522.7±2.0140.6±0.7 1.33±0.050.073±0.001
HD217107c3352±15750921±840.537±0.026164(?xed)39.8±6.4 2.50±0.48 4.41±0.21 a Results for47UMa from Model3in Table3.
TABLE3
47UMa Orbital Solutions
Parameter Model1Model2a Model3b Model4c
P b(days)1078.31089.01083.21073.1
T b(JD-2400000)52391503565017350148
e b0.0880.0610.0490.028
ωb(degrees)127171.8111100
K b(m s?1)46.749.349.350.2
P c(days) (259475862594)
T c(JD-2400000)···51363.55213451363.5
e c···0.0050.0050.005
ωc(degrees) (127127127)
K c(m s?1)···11.113.311.1
rms(m s?1)10.412.78.410.2
χ2ν 3.23 5.81 2.11 2.68
a All parameters?xed at those of Fischer et al.(2002)
b All parameters free except for e
c andωc
c Only parameters for planet c?xe
d at thos
e o
f Fischer et al.(2002)
Long-Period Companions7
TABLE4
Periodogram Analysis
Star Period(days)F AP a
υAnd2000.00.004
47UMa22120.272
14Her b 2.370.118
HD16844363.370.001
HD17994932.050.023
16Cyg B 2.320.895
HD19501941.600.045
HD21027715.500.392
HD217107b485.440.332
a10000bootstraps.
b Residuals obtained from2-planet?t.
TABLE5
HJS Telescope Radial Velocities forυAnd
(=HD9826)
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
51452.86152-13.89.2
51452.86540-3.013.4
51504.692480.88.1
51530.78235-22.29.4
51532.65475-16.010.8
51557.6458926.87.7
51750.96883113.110.6
51775.91401-54.78.1
51778.9325163.89.8
51809.77554-62.08.6
51859.76793-50.3 6.8
51861.8529796.77.1
51861.8589396.17.7
51862.7911191.511.9
51862.7973568.810.1
51918.75978 5.08.7
51918.7643423.19.5
51920.6730946.5 6.9
51946.6890323.814.3
51987.57597 6.39.1
52142.8769055.59.3
52218.75362-63.59.6
52249.68686-6.38.5
52329.57235-125.98.7
52495.93509-151.814.9
52539.84157-104.79.3
52539.84425-113.39.4
52577.85533 5.08.5
52619.7586244.48.5
52933.79237102.310.4
52933.7950392.79.8
52958.68304-5.69.1
53015.6706428.98.2
53035.57199-20.07.0
53394.6338977.310.2
53394.6495085.310.0
53394.6554576.510.8
53632.91257-106.39.2
53690.78040-29.410.0
53691.77259-130.313.4
53746.71222-150.98.3
8Wittenmyer,Endl,Cochran
TABLE6
HJS Telescope Radial Velocities for47UMa
(=HD95128)
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
51010.6289851.6 6.4
51212.97474-10.8 5.5
51240.81250-7.3 6.2
51274.78993-11.2 5.4
51326.70558-22.4 6.2
51504.95996-42.2 6.0
51530.01978-29.4 6.9
51555.94972-25.5 5.8
51655.74023 5.8 5.8
51686.75156-6.7 6.5
51750.60418 2.0 6.6
51861.0189553.7 6.9
51917.9308647.57.1
51987.8552747.88.5
52004.8323559.7 6.0
52039.7793654.87.5
52116.6055439.47.6
52249.000109.57.6
52303.89238-9.6 5.5
52305.84757-11.8 6.1
52327.8628512.316.6
52353.85949-12.97.7
52661.95399-24.9 5.4
53017.9369561.57.5
53069.7668660.7 6.4
53692.03243-49.78.1
53748.89147-47.9 6.0
53787.91198-35.2 6.3
53805.88756-29.3 5.6
53809.80777-30.8 6.1
53805.88756-29.3 5.6
53809.80777-30.8 6.1
53787.91198-35.2 6.3
53861.74397-17.1 6.1
53909.6197713.87.0
Long-Period Companions9
TABLE7
HET Radial Velocities for47UMa(=HD95128)
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
53313.9922561.3 1.5
53313.9941764.1 1.6
53313.9960852.5 1.7
53314.9901256.2 1.3
53314.9920359.9 1.3
53317.9889148.4 1.6
53317.9908248.4 1.4
53317.9927347.5 1.4
53334.9487348.2 1.4
53334.9529650.9 1.4
53334.9559154.0 1.4
53335.9441352.8 1.4
53335.9470854.5 1.4
53335.9500354.5 1.3
53338.9256957.9 2.0
53338.9275653.0 3.1
53338.9294746.4 2.1
53338.9380045.0 1.9
53338.9399148.6 1.9
53338.9418157.3 1.8
53338.9442652.2 1.9
53338.9461746.5 1.8
53338.9480847.7 1.9
53340.9153358.2 1.4
53340.9172453.0 1.5
53340.9191558.0 1.4
53346.9201550.0 1.5
53346.9220750.6 1.4
53346.9239851.7 1.3
53348.9074951.3 1.6
53348.9093956.8 1.6
53348.9113152.4 1.5
53350.9169951.9 1.4
53357.8781839.1 1.8
53357.8800950.8 1.8
53357.8820040.8 1.6
53359.8735146.6 2.2
53359.8754243.8 2.1
53359.8773348.4 2.1
53365.8630239.9 1.9
53365.8648948.7 2.1
53365.8667847.2 2.0
53367.8619849.4 1.8
53367.8638941.8 1.7
53367.8658043.7 1.8
53371.8554232.8 1.8
53371.8573341.6 2.5
53371.8592541.8 1.7
53373.8575940.9 2.1
53373.8595032.0 4.0
53389.7957042.8 2.0
53389.7976237.9 2.0
53389.7995335.2 1.9
53391.7909435.3 2.0
53391.7928536.6 2.1
53391.7947734.5 1.8
53395.7762942.2 1.8
53395.7781932.7 1.8
53395.7801042.7 1.9
53400.9927933.2 1.7
53400.9947028.6 1.7
53400.9966126.1 1.7
53408.7677637.1 1.9
53408.7696830.5 2.1
53408.7715829.1 2.2
53414.7264328.5 2.1
53414.7283234.6 2.0
53414.7302333.9 1.9
53416.7084929.2 2.2
53416.7103831.4 2.1
53416.7123133.6 2.1
53421.9392423.3 1.3
53421.9411525.9 1.4
53421.9430624.6 1.4
53423.7029029.4 1.3
53423.7048126.5 1.4
53423.7067223.0 1.4
53432.9061221.4 1.3
53432.9080218.9 1.3
10Wittenmyer,Endl,Cochran
TABLE8
HJS Telescope Radial Velocities for14Her
(=HD145675)
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
51329.82953154.37.4
51358.76587148.8 6.5
51417.72632127.87.5
51449.62644106.7 6.9
51656.8988611.77.3
51689.69367-0.57.2
51750.74058-0.88.0
51777.71797-20.2 6.7
51809.60771-21.1 6.8
52037.88607-31.47.0
52115.73144-35.17.1
52145.70159-23.47.7
52181.62915-23.77.1
52354.98989-25.012.7
52451.80971-2.17.4
52454.80637-3.2 6.7
52471.72725-12.3 6.4
52495.71816-13.97.4
52541.58879-0.77.0
52806.7425453.6 6.9
52841.8213555.67.5
52933.5558890.87.2
53215.7368390.98.0
53505.84769-31.710.0
53505.87913-42.98.2
53563.74131-39.8 6.6
53586.66183-31.38.0
53633.61295-47.07.2
53636.60040-56.8 6.6
53805.95471-71.07.2
53809.96897-66.37.2
53840.90354-62.08.2
53863.84247-62.09.3
53909.73446-57.67.3
53927.75413-58.5 6.8
TABLE9
HJS Telescope Radial Velocities for HD168443
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
51329.88720-523.3 6.2
51360.83723161.3 5.9
51417.74908208.1 6.2
51451.63634-54.8 6.2
51689.83601267.1 5.9
51752.70677369.2 5.8
51776.68347364.6 6.7
51810.65202369.8 5.8
51861.53311252.07.5
52040.91217136.4 5.7
52116.7844697.1 6.5
52453.83556-197.4 6.1
52473.72399-233.8 6.4
52492.69696-766.57.6
52540.69172-552.2 6.3
52577.57953-156.6 5.8
52840.83905-684.67.1
52932.59046 2.3 5.7
53504.89012392.3 6.5
53565.82109442.8 6.8
53863.9255278.8 6.8
53911.8930127.4 6.6
Long-Period Companions11
TABLE10
HJS Telescope Radial Velocities for HD179949
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
51067.67648-72.47.7
51121.53727109.310.2
51328.9037294.18.3
51360.81419-106.49.0
51451.6044755.68.2
51689.8841472.19.0
51750.78249-121.09.2
51775.71719-81.58.6
51812.66687-89.611.2
52040.93486-62.98.6
52116.80005104.09.2
52492.71373-77.88.7
52577.5434598.78.4
52840.82950100.412.2
52933.58832122.38.0
53565.85370-104.110.6
53911.90672-41.010.4
TABLE11
HJS Telescope Radial Velocities for16Cyg B
(=HD186427)
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
51008.86449-7.0 6.7
51011.86885-1.97.0
51065.737040.57.7
51121.6952815.67.9
51154.5710014.77.3
51328.9439529.1 6.7
51361.87182-43.27.5
51414.67124-48.47.3
51449.78342-41.3 6.8
51502.60158-42.57.8
51529.57703-36.68.0
51689.90882-19.1 6.9
51753.742287.57.6
51777.79311-3.6 6.9
51861.6667624.47.1
52039.9428535.7 6.4
52115.8491048.7 6.9
52144.77541-16.57.0
52181.72467-51.17.3
52451.88739-16.3 6.2
52471.85446-15.1 6.4
52495.78667 2.49.2
52538.66450-7.3 6.8
52577.67137-9.17.4
52600.58553 1.57.4
52620.563410.27.4
52807.8858023.2 6.8
52840.9669434.97.7
52930.6822036.57.5
52932.6627321.3 6.7
52960.59294-27.47.3
53163.86157-7.07.0
53321.64999-9.614.7
53585.8477727.67.0
53654.6851545.47.0
53689.5998057.87.4
53907.87292-24.17.7
12Wittenmyer,Endl,Cochran
TABLE12
HJS Telescope Radial Velocities for HD195019
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
51451.76016-165.6 5.6
51503.63673-199.1 6.2
51776.76858-221.6 4.8
51778.74737-191.2 4.5
51860.61320298.7 5.3
51862.64533152.9 6.3
52114.90052317.7 5.9
52221.65789290.27.1
52472.85791-14.4 6.9
52492.82837136.87.5
52538.72733-74.6 6.4
52807.86835268.4 6.9
53321.56421-95.512.3
53505.93331-185.122.4
53563.87408-103.1 5.6
53584.81430159.57.8
53633.65906-217.57.7
53636.72312-86.5 6.7
53691.64472-69.9 6.8
TABLE13
HJS Telescope Radial Velocities for HD210277
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
51531.59673-30.4 5.4
51557.5362613.1 6.1
51558.54314-1.3 6.3
51689.9388312.3 6.3
51750.8807824.3 5.9
51776.8167227.7 5.3
51860.63668 1.911.7
51917.54532-58.37.4
52116.8891710.37.7
52221.6789530.4 6.2
52473.83462-9.8 5.6
52492.85694-2.78.2
52540.77428 6.2 6.4
52621.618309.1 5.3
52840.95838-28.5 6.0
52931.71553 3.2 6.1
53563.9443835.3 5.5
53633.72641-26.7 5.7
53635.81499-11.6 5.9
53689.64535-46.1 5.8
53927.9088941.68.1
Long-Period Companions13
TABLE14
HJS Telescope Radial Velocities for HD217107
JD-2400000Velocity(m s?1)Uncertainty(m s?1)
51449.84000-44.9 4.8
51556.57950-52.7 5.1
51750.89391154.4 5.2
51776.82866-79.6 4.9
51777.837050.8 5.7
51778.8095497.5 4.6
51778.82275101.5 5.3
51809.8038138.2 5.0
51860.65078-28.016.0
51862.66594-75.8 6.8
51918.58936-102.3 4.7
52116.89988-15.77.3
52219.68045 1.5 6.5
52473.84637-83.3 5.0
52492.88220157.88.7
52540.7898546.9 5.3
52895.85865-72.5 5.0
52931.80527-49.1 4.9
53017.56950-29.9 6.0
53563.89812-51.8 4.8
53630.81136-9.2 6.8
53635.82600-81.0 6.5
53689.65961177.3 5.9
14Wittenmyer,Endl,Cochran
Fig.1.—Left panel:One-planet orbital?t for47UMa b(Model1).Open triangles are from Lick(Fischer et al.2002),open circles are from ELODIE(Naef et al.2004),and?lled circles are from McDonald(2.7m and HET).Right panel:Residuals to the1-planet?t.
Fig.2.—Left panel:Lomb-Scargle periodogram for47UMa,after removal of47UMa b.Right panel:Best-?t double Keplerian model for47UMa.The symbols have the same meaning as in Fig.1.
Long-Period Companions15
Fig. 3.—Same as Fig.1,but for a one-planet?t for14Her b.Open circles are from Naef et al.(2004),open triangles are from Butler et al.(2006),and?lled circles are from McDonald.
Fig.4.—Left panel:Double-Keplerian?t for14Her.Right panel:Residuals of the2-planet?t.Open circles are from Naef et al.(2004), open triangles are from Butler et al.(2006),and?lled circles are from McDonald.