( 2001. The American Astronomical Society. All rights reserved. Printed in U.S.A. FIRST RES

T HE A STROPHYSICAL J OURNAL ,551:507è511,2001April 10

FIRST RESULTS FROM THE ANGLO-AUSTRALIAN PLANET SEARCH:A BROWN DWARF CANDIDATE AND A 51PEG èLIKE PLANET 1

C.G.T INNEY ,2R.P AUL B UTLER ,3,2G EOFFREY W.M ARCY ,4,5H UGH R.A.J ONES ,6A LAN J.P ENNY ,7

S TEVEN S.V OGT ,8K EVIN A PPS ,9AND G REGORY W.H ENRY 10

Received 2000October 11;accepted 2000December 3

ABSTRACT

We report results from the Anglo-Australian Planet Search,a survey for planets around 200solar-type stars in the southern hemisphere that is being carried out on the 3.9m Anglo-Australian Telescope.Lim-iting Doppler precisions of 3m s ~1have been demonstrated from the Drst 2.5years of operation,making this the highest-precision planet search in the southern hemisphere.From these data we report results for two new substellar detections.The Drst is a 51Peg èlike planet around the star HD 179949with M sin i \0.84Photometric study reveals this is not a transiting system.The second is a

M JUP .brown dwarf or very low

mass star companion to HD 164427in an eccentric orbit with M sin i \46

Hipparcos data indicate this latter object is unlikely to have a mass greater than 0.18M JUP .M _.Subject headings:planetary systems èstars:individual (HD 164427,HD 179949)è

stars:low-mass,brown dwarfs

INTRODUCTION Since the discovery of the Drst extra solar planet by Doppler velocity techniques in 1994by Mayor &Queloz (1995),planetary detections have been dominated by north-ern hemisphere search programsèmost proliDcally by the precision velocity programs at Lick (e.g.,Butler et al.1996)and Keck (e.g.,Vogt et al.2000),but also complemented by lower precision programs at the Observatoire de Haute-Provence (Baranne et al.1996),McDonald Observatory (Cochran et al.1997),at Whipple Observatory with the Advanced Fiber Optic Echelle spectrograph (Noyes et al.

1997),and programs at La Silla et al.2000;Queloz (Ku

rster et al.2000).Of these,only the programs at La Silla have access to the sky south of approximately [20?,and these achieve precisions of D 10m s ~1.In 1998,therefore,the Anglo-Australian Planet Search was begun to complete the all-sky coverage of the brightest stars at precisions reaching 3m s ~1.In this paper we present some Drst results from this program.A companion paper (Butler et al.2001,hereafter Paper II)presents results for a further two new planets,along with a detailed description of our observational program.

1Based on observations obtained at the Anglo-Australian Telescope,Siding Spring,Australia,and the W.M.Keck Observatory,which is oper-ated jointly by the University of California and the California Institute of Technology.

2Anglo-Australian Observatory,P.O.Box 296,Epping 1710,Australia;cgt =https://www.wendangku.net/doc/ec508673.html,.au.

3Carnegie Institution of Washington,Department of Terrestrial Mag-netism,5241Branch Road NW,Washington,DC 20015-1305.

4Department of Astronomy,University of California,Berkeley,CA 94720.

5Department of Physics and Astronomy,San Francisco State Uni-versity,San Francisco,CA 94132.

6Astrophysics Research Institute,Liverpool John Moores University,Twelve Quays House,Egerton Wharf,Birkenhead CH411LD,England,UK.

7Rutherford Appleton Laboratory,Chilton,Didcot,Oxon OX110QX,England,U.K.

8UCO/Lick Observatory,University of California,Santa Cruz,CA 95064.

9Physics and Astronomy,University of Sussex,Falmer BN19QJ,England,U.K.

10Center of Excellence in Information Systems,Tennessee State Uni-versity,Nashville,TN 37203-3401.

2.THE ANGLO -AUSTRALIAN PLANET SEARCH

The Anglo-Australian Planet Search is being carried out on the 3.92m Anglo-Australian Telescope (AAT),using the University College of London Echelle Spectrograph (UCLES)and an absorption cell.UCLES is operated in

I 2

its 31line mm ~1mode with an MIT/Lincoln Laboratory 2048]409615k m pixel CCD.This lumogen-coated CCD (denoted MITLL2)underwent a serious failure at the end of 1999,which required its readout to be switched to the second of its working ampliDers in 2000January (following which it was denoted MITLL2a).No change in the oper-ation of the detector (apart from a ?ipped readout format)has been detected by our program.

Our target sample of B 200stars with d \[20?includes F,G,and K V èIV stars with V \7.5and M V stars with V \11.5.Where age/activity information is available from S or indices (see,e.g.,Henry et al.1996),target stars are

R hk required

to have ages greater than 3Gyr.Our Drst observ-ing run was in 1998January,and the last run for which observations are reported here was in 2000November.The observing and data processing procedure follows that described in Butler et al.(1996)and is described in detail in Paper II.In particular,Paper II presents velocities for a number of stable stars illustrating that we reach a velocity-precision ?oor of 3m s ~1for the bright stars included in our program.One of the stars presented here (HD 179949)has also had conDrmatory observations acquired at three epochs in 2000September 5è8,as part of the Keck planet search (Vogt et al.2000).

CHARACTERISTICS OF HD 179949AND HD 164427

HD 179949(HR 7291,HIP 94645,GJ 749)is an F8V (Houck &Smith-Moore 1998)star that shows moderate rotation with a measured v sin i \6.3^0.9km s ~1(Groot,Piters,&van Paradijs 1996).Its Hipparcos parallax puts it at 27.0^0.5pc,with M V \4.09^0.04

(ESA 1997).There is no published evidence

to indicate

that HD 179949is a binary.The photometry of Eggen (1998)indicates HD 179949has roughly solar metallicity with [Fe/H]\]0.02^0.1.The ubvy calibration of Vogt et al.(2000)and published photometry would indicate a more metal-rich [Fe/H]\]0.22^0.07.The latter is 507

508TINNEY ET AL.Vol.551

supported by Twarog &Anthony-Twarog (1995),Figure 8,which indicates HD 179949is as metal-rich,if not more so,than the majority of disk main-sequence stars.HD 179949has a moderate X-ray luminosity as determined by ROSAT ?s Position Sensitive Proportional CounterèSchmitt,&Voges (1998)determine a Hu

nsch,L X

\41.0]10ergs s ~1,while in an independent analysis Piters et al.(1998)determine Both are

L X /L bol \(9.7^3.3)]10~6.some 10times higher

than the equivalent quantity in the quiet Sun.The spectra acquired at Keck have been used to derive a index of [4.72for this star,using the

R hk @same procedure

as Vogt et al.(2000).Figure 1compares the

Ca II H line with that seen in the Sun.The mass of HD 179949is estimated to be 1.24^0.1based on inter-M _,polation between evolutionary tracks of Fuhrmann,Pfeif-fer,&Bernkopf (1997)and Fuhrmann,Pfei?er,&Bernkopf (1998).

HD 164427(HIP 88531,Gl 700A)is an inactive G0V (Houk &Cowley 1975)star,with a index of [4.95

R hk @(Henry et al.1996).Its Hipparcos parallax

puts it at a dis-tance of 39.1^1.4pc and (ESA 1997),

M V

\3.91^0.8making it somewhat overluminous for its spectral type.Indeed,Evans et al.(1964)classiDed it as a subgiant,with luminosity class IV.The uvby calibration of Vogt et al.(2000)suggests a metallicity of [Fe/H]\]0.11^0.07.HD 164427was cataloged as a very wide binary (Gl 700AB)by Gliese (1969)(although both have since dropped out of the nearby star sample (Gliese &Jahreiss 1991)because better parallaxes have placed them outside the 25pc limit).The binary identiDcation is actually due to Luyten (1957),who cataloged this pair as LTT 7172and LTT 7173,respec-tively,with common proper motion and a 28A separation at a position angle of 336?.There is no subsequent astrometry of this pair in the literature.Examination of Digital Sky Survey scans of a United Kingdom Schmidt Telescope plate from 1992.6shows no evidence for an object with the mag-nitude di?erence indicated by Luyten (*m \7.2)at this separation relative to HD 164427,leading us to conclude it may not be a common proper-motion pair.Even if the system were a binary,it would be a very wide system (1090AU)èso wide as to be irrelevant for the purposes of high-precision Doppler velocities.The mass of HD 164427is estimated to be 1.05^0.1M _

F I

G .1.èComparison of the Ca II

H line core in the Sun (solid line )and HD 179949(dotted line ).With and v sin i \6.3km s ~1,HD

R hk @\[4.72179949is slightly more active than

the Sun and rotates somewhat faster.The estimated Doppler velocity ““jitter ??in an F8V star due to this B 10m s ~1(see °4).

Both stars were seen to be photometrically stable over the life of the Hipparcos mission at a 95%conDdence level of \0.015mag (ESA 1997).

RADIAL VELOCITY OBSERVATIONS AND

ORBITAL SOLUTIONS

Twenty-three observations of HD 179949are listed in Table 1,where the column labelled ““Uncertainty ??is the velocity uncertainty produced by the least-squares Dtting process,which simultaneously determines the Doppler shift and the spectrograph point-spread function,given an iodine absorption spectrum,an ““iodine-free ??template spectrum of the object,and an ““iodine ??spectrum of the object (Butler et al.1996).This uncertainty includes the e?ects of photon-counting uncertainties,residual errors in the spectrograph point-spread function model,and variation in the underlying spectrum between the template and ““iodine ??epochs.Only observations for which the uncer-tainty is less than twice the median uncertainty are listed.These data are shown in Figure 2phased with a period of 3.093days.The Dgure shows the best-Dt Keplerian model for the data,with the resulting orbital parameters listed in Table 2.The best-Dt period from Keplerian Dtting is the same as the period found from the peak of the Scargle periodogram,with a false alarm probability less than 0.001.Both AAT (Dlled circles )and Keck (squares )data are shown,with the Keck data completely conDrming the orbital Dts derived from the AAT data alone.Like the pre-viously observed giant planets in 3to 5day orbits,HD 179949appears to be in a circular orbit.Table 2includes the best-Dt orbital solutions both for the case of a circular orbit and ?oating eccentricity.The resulting minimum com-panion mass is 0.84with an orbital semimajor axis of

M JUP

,0.045AU.

TABLE 1

V ELOCITIES FOR HD 179949

Radial Velocity

Uncertainty JD ([2,440,000)(m s ~1)

(m s ~1)

11120.910.......118.1 5.811383.024.......[43.38.911410.943.......[47.7 5.311413.052.......[15.0 4.711413.924.......[42.1 6.111472.917.......[3.6 5.711683.133.......[40.68.011684.180.......113.7 6.111706.151.......91.19.811718.161.......127.1 6.811742.960.......115.9 5.911743.992.......[42.9 5.911745.101.......0.0 5.811766.970.......40.8 6.211768.000.......109.68.511770.107.......44.6 6.111792.751a ......122.2 2.611793.798a ......[80.7 2.511795.803a ......115.6 2.511827.956.......[74.3 6.111828.911.......61.5 6.711829.915.......117.18.211855.942.......

[74.4

10.3

a Observations from Keck.All other observations are from the AAT.

1998.51999.0

1999.52000.02000.52001.0

Time (Years)

2000

4000 V e l o c i t y (m s ?1)

No.1,2001ANGLO-AUSTRALIAN PLANET SEARCH RESULTS

509

TABLE 2O RBITAL P ARAMETERS HD 179949HD 179949Parameter

(e \0.0)(e Dtted)HD 164427Orbital period P (days)............. 3.093^0.001 3.093^0.001108.55^0.04Velocity amplitude K (m s ~1)......101.3^3.0102.2^3.02229^77.0Eccentricity e ........................0.0a 0.05^0.030.55^0.02u (deg)................................0.0

226^25356.9^0.5

a 1

sin i (km)..........................4307.3^15.04338.7^15.0(2.776^0.049)]106Periastron time (JD-244000).......11718.19^0.1

11723.24^0.1

11724.6^0.2

M sin i (M JUP

)........................

0.84^0.050.84^0.0546.4^3.4a (AU)................................0.045^0.0040.045^0.0040.46^0.05

rms about Dt (m s ~1)...............10.8

10.3

7.7

a Fixed.

The residuals about the Dt are at the level of ““jitter ??expected in an F8V star with HD 179949?s level of rotation (6.3km s ~1)and activity ““Jitter ??here is

(R hk @\[4.72).used to refer to the scatter in the

observed velocity about a

F I

G .2.èAAT (Dlled circles )and Keck (squares )Doppler velocities for HD 179949phased with a period of 3.093days.The rms of the velocities about the Dt is 10.3m s ~1.The solid line is a best-Dt Keplerian with the parameters shown in Table 2.Assuming 1.24M for the primary,the

_minimum (M sin i )mass of the companion is 0.84^0.05and the

M JUP ,semimajor axis is 0.045^0.004AU.

F I

G .3.èAAT Doppler velocities for HD 179949from 1998January to 2000September.The solid line is a best-Dt Keplerian with the parameters shown in Table 2.The rms of the velocities about the Dt is 7.7m s ~1.Assuming a 1.05for the primary,the minimum (M sin i )mass of the

M _companion is and the semimajor axis is 0.46^0.05AU.

46.4^

3.4M JUP

,mean value in systems observed over the long term to have no Keplerian Doppler shifts.It is thought to be the com-bined e?ect of surface inhomogeneities,stellar activity,and stellar rotation.Saar,Butler,&Marcy (1998)have studied the correlations between jitter and stellar rotation and activity in the Lick precision velocity program.They indi-cate we would expect HD 179949to show B 10m s ~1of jitter due to activity,spots,etc.We measure a scatter of 10m s ~1about our Keplerian Dt,which is consistent with this expectation.

The 27observations of HD 166427are listed in Table 3,and they are shown in Figure 3along with a Keplerian Dt to the data with the orbital parameters listed in Table 2.The rms scatter about this Dt is 7.7m s ~1,slightly larger than the median uncertainty from the Dtting process of 5.6m s ~1.

TABLE 3

V ELOCITIES FOR HD 164427

Radial Velocity

Uncertainty JD ([2,440,000)(m s ~1)(m s ~1)

10917.287

.......[1071.27.511002.091.......[897.710.211118.891.......[1026.59.811119.905.......[1025.78.311236.281.......[1065.7 6.411274.300.......[3.9 5.311385.868.......347.2 6.811386.879.......513.8 4.911410.911.......703.9 4.211413.034.......378.0 3.611413.904.......286.7 5.611472.893.......[914.8 4.611630.300.......391.3 4.911683.096.......[1014.7 5.611684.147.......[1006.3 6.411706.112.......[217.9 4.911717.923.......1718.7 5.311718.123.......1775.8 4.911742.913.......[44.6 5.511743.933.......[126.67.011745.067.......[218.7 4.611766.942.......[968.3 5.211767.992.......[985.48.411827.914.......2169.0 5.511828.890.......2480.8 6.311829.894.......2791.57.011855.921

.......

[371.0

8.0

510TINNEY ET AL.Vol.551

This is larger than the systematic precision limit of the Anglo-Australian Planet Search,as the earliest obser-vations of this object were performed in very poor condi-tions.As soon as it became apparent that HD 164427was a velocity variable with large amplitude,it was ““prorated ??within the program to only short exposures (and thus lower precision than the rest of the program),although still more than sufficient to precisely determine the companion?s orbit.The resulting minimum companion mass is 46or

M JUP

,0.043and the orbital semimajor axis is 0.46AU.

M _

,5.

DISCUSSION

5.1.HD 179949

Ten other 51Peg èlike planets are currently known with periods under 10days and eccentricities less than 0.1.11The minimum masses of these planets span the range 0.24è3.87with orbital semimajor axes in the range 0.038è0.059M JUP ,AU.

In all respects,HD 179949falls squarely into this class of objects.Even its above-solar metallicity is similar to that seen in the other 51Peg èlike planets (e.g.,Queloz et al.2000;Gonzalez 2001).

5.2.Transit Search in HD 179949

As with all the other 51Peg èlike planets,HD 179949is an excellent candidate for a transit search.The Hipparcos magnitude,color index,and parallax of the star imply a radius of about 1.24which,combined with the orbital

R _

,radius of 0.045AU,places the probability of observable transits at 12.8%.Successful transit observations (already carried out for HD 209458by Charbonneau et al.2000and Henry et al.2000b)not only tightly constrain orbital incli-nation,but provide planetary radii as well.

To search for transits in HD 179949,we obtained photo-metric observations between 2000September 21and October 1with the T80.80m Automatic Photoelectric Telescope (APT)at Fairborn Observatory in southern Arizona.12The instrumentation and techniques used for this transit search are described in Henry (1999)and Henry et al.(2000a).The observations were made di?erentially with respect to the comparison star HD 178075(V \6.30,B [V \0.01,B9.5V).The precision of an individual obser-vation is approximately 0.004mag,somewhat worse than the typical precision of 0.001mag obtainable with the APT due to observations being at air masses between 2and 3.No transit events were detected at the times predicted by the orbital parameters of Table 2.For an assumed planetary radius of 1.4(the measured radius of the

R JUP

planetary companion of HD 209458;Henry et al.2000b;Jha et al.2000),the predicted transit depth is 0.014mag.The mean of our 16photometric observations of HD 179949taken within the predicted transit window is 0.1058^0.0010mag;the mean of the 38observations outside the transit window is 0.1044^0.0007mag.Thus,the two means agree within their respective errors and tran-sits deeper than about 0.001mag are ruled out.This nonde-

11In the absence of a formal classiDcation scheme,we consider HD 83443,HD 168746,HD 46375,HD 75289,BD 103166,HD 187123,HD 209458,t And b,and q Boo to be 51Peg èlike,as well as 51Peg itself.

12These observations are available at https://www.wendangku.net/doc/ec508673.html,/t8/hd179949/hd179949.html.

tection of transits limits the orbital inclination i to less than 83?,and sin i to less than 0.992.Furthermore,the photo-metric observations place a limit of about 0.001mag on any photometric variability of HD 179949on the radial velocity period.This conDrms that neither starspots nor stellar pul-sations can be the cause of the radial velocity variations (see Henry et al.2000a),and thus strongly supports the existence of the planet even in the absence of transits.

5.3.HD 164427

Recent work on the mass function of brown dwarfs in star clusters (Luhman et al.2000;Lucas &Roche 2000;Zapatero Osorio et al.2000)has failed to show that star formation processes cannot form objects below the 13M JUP deuterium-burning limit.(Although the same results can be interpretedèless straightforwardlyèas implying the exis-tence of free-?oating sub-13objects formed by

M JUP

dynamical evolution ejecting objects formed by planetary processes.)Certainly they provide no evidence that the deuterium-burning limit is a useful demarcation boundary between star and planet formation processes.Difficult as it may be,only an understanding of formation mechanisms (and possible subsequent dynamical evolution)can allow us to determine whether objects in the 5è20range are

M JUP

planets or brown dwarfs.Nonetheless,the minimum mass of the companion to HD 164427clearly lies in a range unlikely to be due to planetary formation processesèthat is,it is a brown dwarf or a star,not a planet.

Hipparcos astrometry,however,allows us to place some limits on the orbital inclination and mass for HD 164427?s companion.The astrometric solution for HD 164427shows a good Dt for the parallax and proper motion of a single star,with 1p residuals of B 3mas.The uncertainty on the derived parallax is 0.9mas.Based on this,we can assume an upper limit to the astrometric perturbation of HD

(a 0

)164427due to an unseen companion of B 2mas.Then,from the relationship between the spectroscopic and astrometric orbital elements (e.g.,Halbwachs et al.2000,eq.[1]),we conclude that sin i [0.24,or equivalently that the compan-ion mass is less than 190or 0.18making it either

M JUP M _,a brown dwarf or a very low

mass star.With an orbital

semimajor axis of 0.46AU at 39pc,such a companion will have a maximum apparent separation of 11.8mas.Table 4compares the absolute K magnitudes of HD 164427with predicted magnitudes of the companion in the range of allowed masses.Only at the very massive end of this range is the companion likely to be detectable by either ground-based adaptive optics or space-based imaging.

TABLE 4

P REDICTED K M AGNITUDES FOR HD 164427

C OMPANION M K \5.4

Companion Mass Age (Gyr)

M K

0.18M _

a .........

...7.7 2.30.10M _a .........

...9.2 3.8111.2 5.975M JUP

b ..........

511.7 6.3113.78.342M JUP

b ..........

[16[10.6

a Empirical values due to Henry &McCarthy

M K (1993).

b Model values due to Chabrier et al.(2000).

M K

No.1,2001ANGLO-AUSTRALIAN PLANET SEARCH RESULTS511

Nonetheless,such a challenging observation must be pursued.Of the small number of brown dwarf candidates identiDed by precision Doppler surveys to date(around11), many have been shown to actually be stars(Halbwachs et al.2000),making bonaDde brown dwarf companions rare and well worth unambiguously identifying.

6.CONCLUSIONS

We presentDrst results from the Anglo-Australian Planet Search,which is now the highest-precision Doppler planet search in the southern hemisphere.These include a new member of the51Pegèlike class of planets around the F8 dwarf HD179949and a new brown dwarf candidate com-panion to the G0dwarf HD164427.This program has now been running on the AAT for over2years and has demon-strated velocity precisions reaching3m s~1.We conDdently expect many more discoveries in the years to comeèparticularly as it extends its sensitivity toward the Jupiter-like planet regime.

The Anglo-Australian Planet Search team would like to gratefully acknowledge the support of the Director of the AAO,Dr.Brian Boyle,and the superb technical support provided throughout the program by AAT sta?èin partic-ular E.Penny,R.Patterson,D.Sta?ord,F.Freeman,S.Lee, J.Pogson,and G.Schafer.We further acknowledge support by the partners of the Anglo-Australian Telescope Agree-ment(C.G.T.,H.R.A.J.,A.J.P.);NASA grant NAG 5-8299and NSF grant AST95-20443(G.W.M.);NASA grant NAG5-4445and NSF grant AST96-19418(S.S.V.); NSF grant AST99-88087(R.P. B.);NASA grants NCC5-96and NCC5-228,NSF grant HRD97-06268,and the Richard Lounsbery Foundation(G.W.H.);and Sun Microsystems.

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河南统计年鉴2010

河南统计年鉴2010 河南统计年鉴2010 《河南统计年鉴2010》是一部全面反映河南省经济和社会发展情况的资料性年刊。本书收录了全省和各市(县)2009年以及重要历史年份的经济和社会各方面大量的统计数据，并收录了全国及各省市区2009年的主要统计数据。全书内容分为30个部分，即，1、行政区划和自然资源;2、综合;3、国民经济核算;4、人口;5、从业人员和职工工资;6、固定资产投资;7、对外贸易;8、能源;9、财政;10、物价;11、人民生活;12、城市概况;13、农业;14、工业;15、建筑业;16、交通运输、仓储、邮政业;17、信息传输、计算机服务和软件业;18、批发和零售业、住宿和餐饮业;19、金融业;20、房地产业;21、租赁和商务服务业;22、科学研究、技术服务和地质勘查业;23、水利、环境和公共设施管理业;24、居民服务业和其他服务业;25、教育;26、卫生、社会保障和社会福利业;27、文化、体育和娱乐业;28、公共管理和社会组织;29、各县(市、区)主要统计指标;30、全国及各省市区主要统计指标。各篇前有简要说明，篇末附有《主要统计指标解释》。本年鉴与上年相比，有重大调整的内容如下:1、从三大需求考虑，将“对外贸易”篇前移至“固定资产

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