Kinematic analysis and membership status of TWA22ABR
R. Teixeira, C. Ducourant, G. Chauvin, A. Krone-Martins, M. Bonnefoy, I. Song
AAstronomy & Astrophysics manuscript no. Teixeira˙arXiv c (cid:13)
ESO 2018November 21, 2018
Kinematic analysis and membership status of TWA22 AB (cid:63),(cid:63)(cid:63)
R. Teixeira , , C. Ducourant , G. Chauvin , A. Krone-Martins , , M. Bonnefoy , and I. Song Instituto de Astronomia, Geof´ısica e Ciˆencias Atmosf´ericas, Universidade de S˜ao Paulo, Rua do Mat˜ao, 1226 - Cidade Universit´aria,05508-900 S˜ao Paulo - SP, Brazil. Observatoire Aquitaine des Sciences de l’Univers, CNRS-UMR 5804, BP 89, 33270 Floirac, France. Laboratoire d’Astrophysique, Observatoire de Grenoble, 414, Rue de la piscine, 38400 Saint-Martin d’H`eres, France. Department of Physics & Astronomy, the University of Georgia, Athens, GA 30605 USA.Received / Accepted
ABSTRACT
Context.
TWA22 was initially regarded as a member of the TW Hydrae association (TWA). In addition to being one of the youngest( ≈ ≈
20 pc) stars to Earth, TWA22 has proven to be very interesting after being resolved as a tight, very low-mass binary. This binary can serve as a very useful dynamical calibrator for pre-main sequence evolutionary models. However, itsmembership in the TWA has been recently questioned despite due to the lack of accurate kinematic measurements.
Aims.
Based on proper motion, radial velocity, and trigonometric parallax measurements, we aim here to re-analyze the membershipof TWA22 to young, nearby associations.
Methods.
Using the ESO NTT / SUSI2 telescope, we observed TWA22 AB during 5 di ff erent observing runs over 1.2 years to measureits trigonometric parallax and proper motion. This is a part of a larger project measuring trigonometric parallaxes and proper motionsof most known TWA members at a sub-milliarcsec level. HARPS at the ESO 3.6m telescope was also used to measure the system’sradial velocity over 2 years. Results.
We report an absolute trigonometric parallax of TWA22 AB, π = . ± . . ± . µ α cos ( δ ) = − . ± . / yr and µ δ = − . ± . / yr. Finally, fromHARPS measurements, we obtain a radial velocity V rad = . ± . / s. Conclusions.
A kinematic analysis of TWA22 AB space motion and position implies that a membership of TWA22 AB to knownyoung, nearby associations can be excluded except for the β Pictoris and TW Hydrae associations. Membership probabilities basedon the system’s Galactic space motion and / or the trace-back technique support a higher chance of being a member to the β Pictorisassociation. Membership of TWA22 in the TWA cannot be fully excluded because of large uncertainties in parallax measurementsand radial velocities and to the uncertain internal velocity dispersion of its members.
Key words.
Astrometry: trigonometric parallaxes – Techniques: radial velocities – Stars: binaries, distances, fundamental parameters– Galaxy: open cluster and association
1. Introduction
Over the past decade, various coeval moving groups of starshave been discovered in the solar neighborhood, includ-ing three well-known associations, TW Hydrae (hereafterTWA, Kastner et al. 1997), β Pictoris (hereafter β Pic,Barrado y Navascu´es et al. 1999), and Tucana / Horologium(hereafter Tuc-Hor, Zuckerman & Webb 2000,Torres et al. 2000). These groups occupy an important as-trophysical niche thanks to their proximity ( ≤
100 pc) and youth( ≤
100 Myr). They o ff er the best targets for various studies, suchas imaging searches for young brown dwarf and planetary masscompanions, proto-planetary or debris disk-related programs,etc. Any young (sub)stellar binary members in tight orbitsin these moving groups can serve as valuable calibrators forevolutionary models.Song et al. (2003) identified the TWA22 system as a newmember of TWA based essentially on the presence of a strongLi λ Send o ff print requests to : [email protected] (cid:63) Based on observations performed at the European SouthernObservatory, Chile (76.C-0543, 077.C-0112, 078.C-0158, 079.C-0229). (cid:63)(cid:63)
Table 4 is only available in the electronic edition of the journal. to conclude that TWA22 could indeed be the nearest TWAmember to Earth. However, more recently, Mamajek (2005)has performed a convergent point analysis using several TWAmembers. He found that TWA22 has a low probability ofmembership in the TWA. This conclusion was refuted bySong et al. (2006) arguing a lack of reliable distance determi-nations for most TWA members to firmly reject TWA22’s mem-bership. Song et al. (2006) argued instead that the strong lithiumline seen at TWA22, rarely seen among other stars with similarspectral types, implies a probable membership to TWA or β Pic.During a VLT / NACO deep-imaging survey for close com-panions to stars in young associations, TWA22 was resolved asa tight ( ≈
100 mas) binary with a projected physical separationof 1 . ± .
10 AU (see Bonnefoy et al. 2009).Regardless of TWA22’s membership in TWA or β Pic,TWA22 AB is a precious dynamical mass calibrator because ofits young age ( ≈
10 Myr) and the low masses of its components.A well-known age and a distance are crucial to the validity ofcalibrating evolutionary model calculations. Therefore, there isneed for accurate observational data, such as the trigonometricparallax, proper motions, and radial velocity.As a part of a larger project for the trigonometric parallax de-termination of all TWA members, we performed astrometric andphotometric observations of TWA22 AB at ESO NTT / SUSI2 a r X i v : . [ a s t r o - ph . S R ] J un R. Teixeira et al.: TWA22 AB kinematics (La Silla - Chile). Radial velocity measurements were also ob-tained to complete the kinematic analysis of TWA22 AB. Usingthese new data, we performed a kinematic analysis to test themembership of TWA22 AB in TWA, β Pic, and Tuc-Hor. Ouranalysis uses only moving- group members with Hipparcos mea-sured distances. In addition to Hipparcos moving-group mem-bers, we used 2M1207A whose accurate trigonometric distancewas obtained from gound-based measurement (Ducourant et al.2008). The possibility of TWA22 AB being a member of othernearby groups was investigated and discarded by more evidentincompatibilities.We present observation and data reduction in Sect. 2, and inSect. 3, we discuss the membership of TWA22 in TWA, β Pic,and Tuc-Hor. The conclusion is provided in Sect. 4.
2. Observations and data treatment
We used ESO NTT-SUSI2 which provides a good compromisebetween a large field of view (5 . (cid:48) × . (cid:48) ) for a su ffi cient sam-pling of background stars and a small pixel size (80 . ≤ ff erentialcolor refraction e ff ects (DCR). Residual DCR e ff ects were re-moved from single observations following the method describedin Ducourant et al. (2007). Multiple images were obtained ateach epoch to reduce astrometric errors. The image of highestquality is selected as a master frame that will be used for cross-identification, alignement and scaling. The alignment of CCDaxes and the plate scale were estimated using 2MASS catalogsources (Cutri et al. 2003).A stellar point-spread function for each frame was fittedusing the DAOPHOT II package (Stetson 1987). Then, we cre-ated catalogs of measured positions ( x , y ), internal magnitudes,and associated errors for all stars on each frame. Observationaldata were processed through a global treatment, as described inDucourant et al. (2007, 2008), and a solution was derived forTWA22 AB relative to background stars (14.5 ≤ I ≤ ff ect of binarity in Sect.2.2. Then, a statistical conversion from relative to absolute par-allax and proper motions, based on the Besanc¸on Galaxy model(Robin et al. 2003, 2004), was derived ( ∆ π = . ± .
01 mas, ∆ µ α cos ( δ ) = − . ± .
02 mas / yr, ∆ µ δ = + . ± .
02 mas / yr).Both the final estimated TWA22 AB ( α = h m . s , δ = − ◦ (cid:48) . (cid:48)(cid:48) , epoch = Table 1.
Absolute astrometric parameters for TWA22 AB andradial velocity derived in this work. π d µ α cos ( δ ) µ δ V rad mas pc mas / yr mas / yr km / s57.0 ± ± ± ± ± Fig. 1.
Apparent astrometric displacement of TWA22 AB to-gether with the best parallax and proper motion fit of the data.Blue dots correspond to weighted mean positions at each obser-vational epoch.
Table 2.
Apparent and absolute magnitudes of TWA22 AB: V,R, I Bessell filter data from this work and J, H, and K s data from2MASS. m M(mag)V 13.99 ± ± ± ± ± ± ± ± ± ± ± ± With ESO NTT / SUSI2, it is not possible to resolve two com-ponents of TWA22 AB. Therefore, with our astrometric obser-vations we are measuring the photocenter of the system. Thisphotocenter may not coincide with the center of mass becausethese two di ff erent positions depend on the ratio of mass and lu-minosity of the components. A photocenter of a binary should bea ff ected by an elliptic, periodic movement with the same periodas the binary orbit. The amplitude of this variation depends onthe orbital parameters, mass, and luminosity ratios.Following Van de Kamp (1967), our condition equations forTWA22 AB were modified to include the photocentric move-ment. The condition equations are written for each star on eachof the N frames considered (including the master frame). Theseequations relate the measured coordinates to the stellar astromet-ric parameters: X + ∆ X + µ X ( t − t ) + π F X ( t ) + α Q α = a x ( t ) + a y ( t ) + a (1) Y + ∆ Y + µ Y ( t − t ) + π F Y ( t ) + α Q δ = b x ( t ) + b y ( t ) + b (2)where ( X , Y ) are the known standard coordinate of the star atthe central epoch t and ( x ( t ) , y ( t )) are the measured coordinateson the frame (epoch t ) that need to be transformed into the mas-ter frame system. ∆ X , ∆ Y , µ X , µ Y , π , and α are the unknown . Teixeira et al.: TWA22 AB kinematics 3 Table 3.
Heliocentric coordinates (X, Y, Z) and Galactic velocities (U, V, W) of TWA22 AB together with mean values for TWA, β Pic and Tuc-Hor.
Name X Y Z U V W Age dpc km / s Myr pcTWA22 3.5 ± ± ± ± ± ± ≤ ± ± ± ± ± ± ± ± β Pic 9.2 ± ± ± ± ± ± ± ± ± ± ± ± ± ± stellar astrometric parameters. Both ∆ X and ∆ Y yield correc-tions of the standard coordinates of the star on the master frame, µ X and µ Y are projected proper motions in right ascension anddeclination, π is the parallax, and α is a semi–major axis ofthe photocentric trajectory relative to a barycenter. Coe ffi cients( a i , b i ) are unknown frame parameters that describe the trans-formation to the master frame system, ( F α , F δ ) are the paral-lax factors, and ( Q α , Q δ ) are known orbital factors (based onBonnefoy et al. (2009) orbital data). The unknown coe ffi cient α is given by α = a ( R − β ) where a is the semi-major axisof TWA22 B’s orbit around TWA22 A, R is a fractional mass, R = M B M A + M B , β is the fractional distance of the primary to thephotocenter β = + − . ∆ m where ∆ m is the magnitude di ff erencebetween A and B.Although it is impossible to include the parameter α formallyas a variable in our equations, we could externally determineits value to correct X , Y for the orbital motion of photocenteraround barycenter. For this, we assumed the mass–luminosityrelations as: M ∝ ( L ) − . and used the extrapolated magni-tudes in the I-band adapted from Bonnefoy et al. (2009): ∆ m I = . − .
87 mag to determine α Q α and α Q δ and correct X , Y from these quantities. The resulting astrometric parameters forTWA22 AB are then: π = . ± . µ α cos ( δ ) = − . ± . / yr, and µ δ = − . ± . / yr.We note that the parallax value obtained from this study iswithin 1 σ π of the one given in Table 1 where it did not con-sider the e ff ect of photocenter’s periodic movement. On the otherhand, we observe a large variation in the proper motion in dec-lination. This suggests that our astrometric data may not cover along enough time interval to properly account for the 5.144 yr,orbital periodic signal from Bonnefoy et al. (2009). The influ-ence of this signal over 1.2 yr (duration of the observationalprogram of TWA22 AB) is mainly equivalent to an o ff set of theproper motion in declination. We therefore conservatively stickto the values given in Table 1 as the best fit to our data. TWA22 AB was observed with HARPS (Mayor et al. 2003)over 2 years. HARPS is a high-resolution (R = / V = . ≤ − ), and weperformed a precise nightly wavelength calibration from ThArspectra (Lovis & Pepe 2007). Out of these measurements, weestimated a heliocentric radial velocity V r = ± . − for the system. This radial velocity is likely to be a ff ected bythe SB1 status of TWA22 AB. We took the binary nature into account in our uncertainty value by simulating expected ampli-tudes from the binary orbital motion based on the parametersfrom Bonnefoy et al. (2009).
3. Kinematic analysis
Based on new trigonometric parallax, proper motion, and radialvelocity, we re-examine below the membership of TWA22 AB toTWA, β Pic, and Tuc–Hor. Membership in other young, nearbyassociations was rejected by more evident discrepancies in age,distances, etc.
To test the membership of TWA22 AB, our first approach is tostatistically compare its galactic space motion with the meanUVW values for TWA, β Pic, and Tuc-Hor members. Only starswith known trigonometric parallaxes were considered here be-cause accurate distances are crucial in the UVW calculation.For TWA, our sample set includes TWA 01, TWA 04, TWA 09,and TWA 11 with trigonometric parallaxes from the Hipparcoscatalog (ESA 1997)and 2M1207A from Ducourant et al. (2008).Although TWA19 has a Hipparcos parallax, we did not considerit here because Mamajek (2005) classified it as non TWA mem-ber. SSSPMJ1102-3431 TWA member (Teixeira et al. 2008) hasalso been excluded from our study because no radial velocitywas available. Their radial velocities were extracted from Table 1of Mamajek (2005) (Torres et al. 2003 data for TWA 01 andTWA9A; Torres et al. 1995 for TWA4; Reid 2003 for TWA11;and Mohanty et al. 2003 for 2M1207A). For β Pic, we used thelist of suggested members by Torres et al. (2006). Astrometricmeasurements and radial velocities were respectively obtainedfrom the Hipparcos catalog (ESA 1997) and the Table 6 ofTorres et al. (2006). Finally, for Tuc-Hor, astrometric measure-ments and radial velocities were respectively obtained fromthe Hipparcos catalog (ESA 1997) and Kharchenko et al. (2007)for suggested members by Zuckerman & Song (2004) andTorres et al. (2008). The selection of stars and the original dataused in our analysis are presented in Table 4 (only availablein the electronic edition). Calculated mean space motions ofTWA, β Pic, and Tuc-Hor are reported in Table 3, togetherwith their spatial heliocentric coordinates and velocities forTWA22 AB. In this Table positive X(U) points to the Galacticcenter, Y(V) is positive in the direction of Galactic rotationand Z(W) is positive toward the north Galactic pole. Agesare from (1) Song et al. (2003), (2) De la Reza et al. (2006), (3)Ortega et al. (2004), (4) Makarov (2007).The mean values derived here (Table 3) for TWA, β Pic,and Tuc-Hor are in good agreement with published values : (-11, -18, -5), (-11, -16, -9), and (-11, -21, 0) from Table 7 ofZuckerman & Song (2004) and ( − . ± . , − . ± . , − . ± . − . ± . , − . ± . , − . ± . − . ± . , − . ± . , − . ± .
9) from Table 1 of Torres et al. (2008).
R. Teixeira et al.: TWA22 AB kinematics
Fig. 2.
Number of β Pic members in a sphere of 2 σ radius in theUVW space around each member. Sigma is the velocity disper-sion for this association.Since Hipparcos proper motions were derived from obser-vations covering only a small time interval, we also calculatedmean spatial motions of these associations using Tycho-2 propermotions (Hoeg et al. 2000) and we obtained nearly the same re-sults: (-10.1, -17.3, -5.0), (-10.8,-16.0,-9.1), and (-9.6, -20.8, -0.5), respectively, for TWA, β Pic, and Tuc-Hor.To test the membership of TWA22 AB to TWA, β Pic, andTuc-Hor, based on its space motion, we applied a χ test with 3degrees of freedom using their space motion measurements. Wefind the probabilities that TWA22 AB space motion be compat-ible with the mean space motion of β Pic, TWA and Tuc-Horare 50%, 1% and 0.5% respectively. An alternative approach isto perform a k-NN analysis in the UVW space (implementedby Venables & Ripley 2002, R Development Core Team 2008)where we computed the distance of TWA22 to all members ofthese associations. Among the k nearest neighbors to TWA22,the fraction of members for a given association gives the mem-bership probability for that group. This k-NN analysis corrobo-rates that TWA22 is more likely a member of β Pic than TWAand Tuc-Hor. Both calculations tend to reject TWA and Tuc-Horas a host association for TWA22 AB.Our final approach is to count the number of β Pic, TWA,and Tuc-Hor members (or neighbors) within a sphere of fixedradius in the UVW space, centered at TWA22’s value and ateach individual member of these associations. Radii are selectedproportional to the velocity dispersions of the associations. Wefound that UVW spatial densities of TWA and Tuc-Hor mem-bers around TWA22 are significantly lower than the averagedone found in both associations. In contrary, the UVW spatialdensity of β Pic members around TWA22 (within 2 σ ) is similarto the average density in β Pic (see Fig. 2).Membership probabilities and association member densityaround TWA22 support a possible membership in the β Pic as-sociation. The membership of TWA22 in TWA cannot be firmlyevaluated because of the paucity of high-quality kinematic datafor most of its members.
Fig. 3.
Distances between TWA22 AB and three moving groups(TWA, β Pictoris, and Tucana-Horologium moving groups) forthe past 12 Myrs.
Another way to test the membership of TWA22 AB to TWA, β Pic, and Tuc-Hor is to use the trace-back technique to com-pare the Galactic space position of TWA22 AB and TWA, β Pic,and Tuc-Hor backward in time. To avoid using any uncertainvalues for the solar peculiar motion (Mihalas & Binney 1981;Dehnen & Binney 1998; Makarov 2007) by transforming helio-centric velocities into LSR velocities, we decided to work in areference system centered, along time, on TWA22 AB instead.We present, in Figure 3, the distance between TWA22 AB andthe center of each association in time. We note that TWA22 isalways closer to β Pic than to TWA and Tuc-Hor. Since the meanmotions of the associations derived here are in good agreementwith values from the literature, the few TWA members consid-ered here may not have seriously a ff ected the result.
4. Conclusions
Motivated by the importance of the young, very low-mass astro-metric binary TWA22 AB as an important calibration point forstellar theoretical calculations, we measured its precise trigono-metric parallax (57 . ± . − . ± . / yr, − . ± . / yr), and radial velocity ( V rad = . ± . / s). These parameters are fundamentals for determin thephysical properties of the tight binary system (Bonnefoy et al.2009).Our high-quality astrometric measurements along withHARPS radial velocity measurement allow us to discuss themembership of TWA22 AB to nearby associations. Our kine-matical study shows that membership by TWA22 AB in knownyoung, nearby associations can be excluded except for the β Pictoris and TW Hydrae associations. Membership probabilitiesbased on the system space motion or the use of trace-back tech-nique also support possible membership of TWA22 AB in the β Pictoris association. Membership in the TWA cannot be fullyexcluded because of the current lack of precise parallax mea-surements for most of its members. Our results are, to some ex-tent, inconclusive about the membership of TWA22 AB in TWA . Teixeira et al.: TWA22 AB kinematics 5 or β Pic, but they are consistent with that from an age analysis.The location of TWA22 AB on a color-magnitude diagram sup-ports its age being about 10 Myr but cannot be determined pre-cisely enough to distinguish from 8 (TWA age) and 12 Myr ( β Pic moving group age). Precisely known trigonometric distancesof many more TWA members, an aim of our larger astrometricprogram of observing all known TWA members, should improvethe situation soon.
Acknowledgements.
We thank Michel Rapaport for helpful comments. Wealso acknowledge partial financial support from the
Programmes Nationaux dePlan´etologie et de Physique Stellaire (PNP & PNPS) (in France), the Brazilianorganization FAPESP and CAPES, and the French organization COFECUB.
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HD B *180303 . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . C D - . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . P ZT e l . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . E t a T e l . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . A T M i c N . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . A T M i c S . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . AU M i c . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . WW P s A . - . . . ± . . ± . - . ± . . ± . . . - . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . M . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . . Teixeira et al.: TWA22 AB kinematics 7 i d e n t a l ph a d e lt a V π µ α c o s ( δ ) µ δ V r XY Z UV W ( h m s )( ◦ (cid:48)(cid:48)(cid:48) ) m a g ( m a s )( m a s / y r)( K m / s )( p c )( K m / s ) H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - ..
Barrado y Nevascu´es D., Stau ff er J.R., Song I. & Caillault J.P. 1999, ApJ, 520,L123Bonnefoy M., Chauvin G., Dumas C., et al. 2009, to be published in A&Ade Bruijne, J. H. J. 1999, MNRAS, 306, 381Dehnen, W., & Binney, J., J. 1998, MNRAS, 298, 387Cutri R.M., Skrustskie M.F., Van Dyk S. et al. 2003, (Pasadena:IPAC / Caltech)De la Reza R., Jilinski E. & Ortega V.G. 2006, AJ, 131, 2609-2614Ducourant C., Teixeira R., Chauvin G. et al. 2008, A&A, 477, L1-L4Ducourant C., Teixeira R., Hambly N. et al. 2007, A&A, 470, 387-394ESA 1997, HIPPARCOS and Tycho catalogues, ESA-SP-1200Fern´andez D., Figueras F. & Torra, J. 2008, A&A, 480, 735Hoeg E., Fabricius C., Makarov V. V. et al. 2000, A&A, 363, 385Kharchenko N.V., Scholz R.D., Piskunov A.E. et al. 2007, AN, 328, 889-896Kastner J.H., Zuckerman B., Weintraub D.A. & Forveille T. 1997, Science, 277,67Lovis C. & Pepe F. 2007, A&A , 468, 1115Mamajek E. 2005, ApJ, 634, 1385Makarov V.V. 2007, ApJS, 169, 105Mayor M., Pepe F., Queloz D., et al. 2003, The Messenger, 114, 20Mihalas, D., Binney, J., Galactic Astronomy, Structure and KinematicsMohanty S., Jayawardhana R. & Barrado y Navascu´es 2003, ApJ, 593, L109Mohanty S., Jayawardhana R., Hu´elamo N. & Mamajek E. 2007, ApJ, 657, 1064Ortega V. G., de la Reza R., Jilinski E. & Bazzanella B. 2004, ApJ, 609, 243Ortega V. G., de la Reza R., Jilinski E. & Bazzanella, B. 2002, ApJ, 575L, 75Robin A. C., Reyle C., Derriere S. & Picaud S. 2003, A&A 409, 523R Development Core Team, 2008. R: A language and environment for statisti-cal computing, reference index version 2.6.2, R Foundation for StatisticalComputing, Vienna, Austria. ISBN 3-900051-07-0, URL http: // R. Teixeira et al.: TWA22 AB kinematics T a b l e . O r i g i n a l d a t a f o r β P i c t o r i s , T W A a nd T u ca n a / H o r o l og i u mm e m b e r s u s e d i nou r k i n e m a ti ca l a n a l y s i s fr o m E S A , M a m a j e k ( ) , T o rr e s e t a l . ( ) a nd D u c ou r a n t e t a l . ( ) t og e t h e r w it h t h e d e r i v e dh e li o ce n t r i c s p a ti a l c oo r d i n a t e s a ndv e l o c iti e s d e r i v e d i n t h i s w o r k . i d e n t a l ph a d e lt a V π µ α c o s ( δ ) µ δ V r XY Z UV W ( h m s )( ◦ (cid:48)(cid:48)(cid:48) ) m a g ( m a s )( m a s / y r)( K m / s )( p c )( K m / s ) H I P . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . HD . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . AG T r i . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . B D + . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . G J . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . V O r i . + . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . C D - . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . + . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . B e t a P i c . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . AO M e n061828 . - . . . ± . - . ± . . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD B . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . V N o r *153857 . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . V A r a . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD C *171725 . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD B *180303 . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . C D - . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . P ZT e l . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . E t a T e l . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . A T M i c N . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . A T M i c S . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . AU M i c . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . WW P s A . - . . . ± . . ± . - . ± . . ± . . . - . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . M . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . . Teixeira et al.: TWA22 AB kinematics 7 i d e n t a l ph a d e lt a V π µ α c o s ( δ ) µ δ V r XY Z UV W ( h m s )( ◦ (cid:48)(cid:48)(cid:48) ) m a g ( m a s )( m a s / y r)( K m / s )( p c )( K m / s ) H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - .. ± ..
Barrado y Nevascu´es D., Stau ff er J.R., Song I. & Caillault J.P. 1999, ApJ, 520,L123Bonnefoy M., Chauvin G., Dumas C., et al. 2009, to be published in A&Ade Bruijne, J. H. J. 1999, MNRAS, 306, 381Dehnen, W., & Binney, J., J. 1998, MNRAS, 298, 387Cutri R.M., Skrustskie M.F., Van Dyk S. et al. 2003, (Pasadena:IPAC / Caltech)De la Reza R., Jilinski E. & Ortega V.G. 2006, AJ, 131, 2609-2614Ducourant C., Teixeira R., Chauvin G. et al. 2008, A&A, 477, L1-L4Ducourant C., Teixeira R., Hambly N. et al. 2007, A&A, 470, 387-394ESA 1997, HIPPARCOS and Tycho catalogues, ESA-SP-1200Fern´andez D., Figueras F. & Torra, J. 2008, A&A, 480, 735Hoeg E., Fabricius C., Makarov V. V. et al. 2000, A&A, 363, 385Kharchenko N.V., Scholz R.D., Piskunov A.E. et al. 2007, AN, 328, 889-896Kastner J.H., Zuckerman B., Weintraub D.A. & Forveille T. 1997, Science, 277,67Lovis C. & Pepe F. 2007, A&A , 468, 1115Mamajek E. 2005, ApJ, 634, 1385Makarov V.V. 2007, ApJS, 169, 105Mayor M., Pepe F., Queloz D., et al. 2003, The Messenger, 114, 20Mihalas, D., Binney, J., Galactic Astronomy, Structure and KinematicsMohanty S., Jayawardhana R. & Barrado y Navascu´es 2003, ApJ, 593, L109Mohanty S., Jayawardhana R., Hu´elamo N. & Mamajek E. 2007, ApJ, 657, 1064Ortega V. G., de la Reza R., Jilinski E. & Bazzanella B. 2004, ApJ, 609, 243Ortega V. G., de la Reza R., Jilinski E. & Bazzanella, B. 2002, ApJ, 575L, 75Robin A. C., Reyle C., Derriere S. & Picaud S. 2003, A&A 409, 523R Development Core Team, 2008. R: A language and environment for statisti-cal computing, reference index version 2.6.2, R Foundation for StatisticalComputing, Vienna, Austria. ISBN 3-900051-07-0, URL http: // R. Teixeira et al.: TWA22 AB kinematics T a b l e . O r i g i n a l d a t a f o r β P i c t o r i s , T W A a nd T u ca n a / H o r o l og i u mm e m b e r s u s e d i nou r k i n e m a ti ca l a n a l y s i s fr o m E S A , M a m a j e k ( ) , T o rr e s e t a l . ( ) a nd D u c ou r a n t e t a l . ( ) t og e t h e r w it h t h e d e r i v e dh e li o ce n t r i c s p a ti a l c oo r d i n a t e s a ndv e l o c iti e s d e r i v e d i n t h i s w o r k . i d e n t a l ph a d e lt a V π µ α c o s ( δ ) µ δ V r XY Z UV W ( h m s )( ◦ (cid:48)(cid:48)(cid:48) ) m a g ( m a s )( m a s / y r)( K m / s )( p c )( K m / s ) H I P . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . HD . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . AG T r i . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . B D + . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . G J . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . V O r i . + . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . C D - . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . + . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . B e t a P i c . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . AO M e n061828 . - . . . ± . - . ± . . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD B . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . V N o r *153857 . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . V A r a . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD C *171725 . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD B *180303 . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . C D - . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . P ZT e l . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . E t a T e l . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . A T M i c N . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . A T M i c S . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . AU M i c . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . WW P s A . - . . . ± . . ± . - . ± . . ± . . . - . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . M . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . . Teixeira et al.: TWA22 AB kinematics 7 i d e n t a l ph a d e lt a V π µ α c o s ( δ ) µ δ V r XY Z UV W ( h m s )( ◦ (cid:48)(cid:48)(cid:48) ) m a g ( m a s )( m a s / y r)( K m / s )( p c )( K m / s ) H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - .. ± .. - ..
Barrado y Nevascu´es D., Stau ff er J.R., Song I. & Caillault J.P. 1999, ApJ, 520,L123Bonnefoy M., Chauvin G., Dumas C., et al. 2009, to be published in A&Ade Bruijne, J. H. J. 1999, MNRAS, 306, 381Dehnen, W., & Binney, J., J. 1998, MNRAS, 298, 387Cutri R.M., Skrustskie M.F., Van Dyk S. et al. 2003, (Pasadena:IPAC / Caltech)De la Reza R., Jilinski E. & Ortega V.G. 2006, AJ, 131, 2609-2614Ducourant C., Teixeira R., Chauvin G. et al. 2008, A&A, 477, L1-L4Ducourant C., Teixeira R., Hambly N. et al. 2007, A&A, 470, 387-394ESA 1997, HIPPARCOS and Tycho catalogues, ESA-SP-1200Fern´andez D., Figueras F. & Torra, J. 2008, A&A, 480, 735Hoeg E., Fabricius C., Makarov V. 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Teixeira et al.: TWA22 AB kinematics T a b l e . O r i g i n a l d a t a f o r β P i c t o r i s , T W A a nd T u ca n a / H o r o l og i u mm e m b e r s u s e d i nou r k i n e m a ti ca l a n a l y s i s fr o m E S A , M a m a j e k ( ) , T o rr e s e t a l . ( ) a nd D u c ou r a n t e t a l . ( ) t og e t h e r w it h t h e d e r i v e dh e li o ce n t r i c s p a ti a l c oo r d i n a t e s a ndv e l o c iti e s d e r i v e d i n t h i s w o r k . i d e n t a l ph a d e lt a V π µ α c o s ( δ ) µ δ V r XY Z UV W ( h m s )( ◦ (cid:48)(cid:48)(cid:48) ) m a g ( m a s )( m a s / y r)( K m / s )( p c )( K m / s ) H I P . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . HD . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . AG T r i . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . B D + . + . . . ± . . ± . - . ± . . ± . - . . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . G J . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . V O r i . + . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . C D - . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . + . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . B e t a P i c . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . AO M e n061828 . - . . . ± . - . ± . . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD B . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . V N o r *153857 . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . V A r a . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD C *171725 . - . . . ± . - . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD B *180303 . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . C D - . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . P ZT e l . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . E t a T e l . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . HD . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . A T M i c N . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . A T M i c S . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . AU M i c . - . . . ± . . ± . - . ± . - . ± . . . - . - . ± . - . ± . - . ± . WW P s A . - . . . ± . . ± . - . ± . . ± . . . - . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . T W A . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . M . - . . . ± . - . ± . - . ± . . ± . . - . . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . . Teixeira et al.: TWA22 AB kinematics 7 i d e n t a l ph a d e lt a V π µ α c o s ( δ ) µ δ V r XY Z UV W ( h m s )( ◦ (cid:48)(cid:48)(cid:48) ) m a g ( m a s )( m a s / y r)( K m / s )( p c )( K m / s ) H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . - . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . - . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . - . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - . ± . . ± . H I P . - . . . ± . . ± . - . ± . . ± . . - . - . - . ± . - .. ± .. - .. ± ..