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ngc  5694 is a bright ( @xmath8 ) and remote ( @xmath9  kpc ) old and metal - poor galactic globular cluster ( gc ) , located in the hydra constellation . first discovered by w. herschel in 1784 , it has been recognised as a gc by @xcite . because of its distance and low apparent magnitude , the first photometric studies of giant stars in this cluster have been conducted only in relatively recent epoch @xcite . after the first integrated spectroscopic studies ( see , e.g. , * ? ? ? * ) spectroscopy of individual red giant stars in ngc  5694 have been carried out by @xcite and , more recently , by @xcite . the latter derived the chemical composition for one bright giant of the cluster from a high - resolution spectrum and found an abundance pattern different from ordinary stars and clusters in the galactic halo , more similar to those displayed by stars in dwarf spheroidal galaxies . the accretion of globular clusters into the halo of giant galaxies during the disruption of their parent dwarf galaxy is now established to have occurred in the milky way ( see , e.g. , * ? ? ? * ; * ? ? ? * ; * ? ? ? * and references therein ) and in m31 @xcite . dense nuclei of stripped dwarf satellites can also appear as massive gcs at the present epoch ( see * ? ? ? * ; * ? ? ? * ; * ? ? ? * for references and discussion ) . chemical tagging is one of the main technique to identify otherwise ordinary gcs as accreted from a former , and now fully disrupted , galactic satellite .    to follow - up the intriguing finding by @xcite we started a multi - instrument observational campaign that allowed us ( a ) to trace the surface brightness ( sb ) profile of the cluster down to @xmath10  mag / arcsec@xmath11 , finding that it extends smoothly much beyond the tidal radius of the best - fitting @xcite model and that it can not be adequately fit neither by a @xcite , @xcite nor @xcite model ( * ? ? ? * c11 hereafter ) , and ( b ) to perform accurate abundance analysis from high - resolution spectra for _ six _ cluster giants , fully confirming that the cluster has a chemical pattern different from the galactic halo , with nearly solar [ @xmath12/fe ] ratio and anomalously low abundances of y , ba , la and eu , at [ fe / h]@xmath13 ( * ? ? ? * mu13 hereafter ) .    here we present a study of the kinematics of the cluster , based on a large sample of medium - resolution spectra of stars selected to lie on the red giant branch ( rgb ) in the color magnitude diagram of the cluster . the plan of the paper is the following : in sect .  2 we present our observations and we describe the data reduction . in sect .  3 and 4 we describe how we derived our estimates of the radial velocity and metallicity , respectively , from the available spectra . in sect . 5 we present our criteria to select cluster members and the analysis of the cluster kinematics , including estimates of the dynamical mass . finally in sect . 6 we briefly summarise and discuss the results of the analysis . the data have been acquired with the multi - object facility flames@vlt @xcite in the combined medusa+uves mode , allowing the simultaneous allocation of 8 uves high - resolution fibres and 132 medusa mid - resolution fibres . for the uves spectra , discussed in details in mu13 , we employed the 580 red arm set - up , with spectral resolution @xmath1440000 and wavelength coverage @xmath1548006800  . the giraffe targets have been observed with the hr21 setup , with a resolving power of @xmath1516000 and a spectral coverage between @xmath1584809000   . this grating was chosen because it includes the prominent ca  ii triplet lines , which are ideal to measure radial velocities ( rv ) also in spectra of faint stars and to derive an estimate of their metallicity . two configurations of target stars have been used . a total of 4 exposures of 46 min each for each configuration has been secured in service mode during the period between april and july 2012 . a small overlap between the two configurations ( 12 stars ) has been secured in order to cross - check the stability of the rv when measured with different fibres . the target selection has been performed with the b , v photometric catalog by c11 obtained by combining vimos@vlt and wfpc2@hst data . we selected stars along the rgb with v@xmath1620 . stars with close ( within 2 arcsec ) companion stars of comparable or brighter magnitude have been discarded , to avoid spurious contaminations in the fibre . about 15 - 20 fibres in each configuration have been dedicated to sample the sky background , because this spectral range is affected by prominent @xmath17 and oh sky emission lines . [ cmd ] shows the ( v , b - v ) colour - magnitude diagram of ngc  5694 with with giraffe targets marked as red circles and the uves ones as blue asterisks . the spatial distribution of the targets with respect to the cluster center is shown in fig . [ map ] ; a circle with radius equal to the cluster tidal radius of the k66 model providing the best - fit to the sb profile of ngc  5694 , as derived in c11 , is also plotted , for reference .        ) with respect to the cluster center by @xcite . the black circle indicate the tidal radius of the k66 model providing the best - fit to the sb profile of ngc  5694 ( from c11).,width=317 ]    the data reduction has been performed using the last version of the eso pipeline , including bias - subtraction , flat - fielding , wavelength calibration with a standard th - ar lamp and spectral extraction . the accuracy of the zero - point of the wavelength calibration has been checked by measuring the position of several sky emission lines and comparing them with their rest - frame position taken from the sky lines atlas by @xcite . for each star the average difference between the measured and reference line positions is always smaller than 0.02  , corresponding to less than one half of a pixel . these shifts turns out to be compatible with 0 within the quoted uncertainties . hence , no relevant wavelengths shift is found . each individual stellar spectrum has been subtracted from the sky by using a master sky spectrum obtained as a median of the different sky spectra observed in that exposure . then the proper heliocentric correction has been applied . finally , individual spectra of the same target have been combined together . the typical snr per pixel ( measured at @xmath158550 @xmath18 ) is of @xmath15150 for the brightest targets ( v@xmath1516 ) and of @xmath1510 for the faintest stars ( v@xmath1520 ) . some targets have been discarded because of the poor quality of their spectra or due to some residuals of the sky lines that can affect the correct rv measurement . finally , the following analysis is based on 165 stars with reliable rv and metallicity estimates . rvs have been measured with the standard cross - correlation technique of the observed spectrum against a template of known rv , as implemented in the iraf task fxcor . as template , we adopted a synthetic spectrum calculated with the code synthe , adopting the entire atomic and molecular line - list by kurucz and castelli and a atlas9 model atmosphere calculated with the metallicity of the cluster , [ fe / h]@xmath152.0 dex and the typical atmospheric parameters of a giant star ( @xmath19=  4500 k , log(g)=  1.5 ) . uncertainties in the rv have been computed by fxcor according to @xcite , by taking into account the height and width of the cross - correlation function and the mean distance between its main peak and the nearest secondary peaks ( eq .  24 by * ? ? ? * ) .    as an additional sanity check , the rvs of the 12 stars observed in both configurations have been measured individually . the two sets of rv agree very well each other , with a mean difference of @xmath20   km / s , fully compatible with a null difference . [ rvdist ] shows the rv distribution of the entire sample of giraffe targets . the distribution ranges from 171 km / s to + 231 km / s , with a dominant peak around at @xmath15140 km / s and corresponding to the cluster stars ( the average rv derived from the 6 uves targets is of -140.4@xmath212.2 km / s ) . the inset panel shows a zoomed view of the region around the main peak of the rv distribution , with marked as a reference the average rv obtained from the uves targets ( red solid vertical line ) . abundances for all the target stars have been obtained by using the strength of the ca  ii triplet lines as a proxy of the metallicity . the lines of the ca  ii triplet lines have been fitted with a voigt profile , in order to reproduce the prominent pressure - broadened line wings , and then their equivalent widths ( ews ) obtained by direct integration of the best - fit profile . the metallicities have been obtained by adopting the calibration by @xcite and assuming @xmath22=  18.5 mag @xcite . uncertainties in the measured ews of the ca  ii triplet lines have been estimated by employing monte carlo simulations . a synthetic spectrum has been re - sampled at the pixel - size of the giraffe spectra ( 0.05   /pixel ) and then poissonian noise corresponding to four values of snr ( namely 10,50,100,150 ) has been injected in order to simulate the noise conditions of the observed spectra . for each value of snr , 1000 synthetic spectra have been generated following this approach , the ews of the ca  ii triplet lines have been measured and then the metallicity estimated as done for the observed spectra . for each snr , the uncertainty has been computed as 1@xmath23 of the derived [ fe / h ] distribution ; the abundance uncertainty is of 0.13 dex for snr=  10 and 0.01 dex for snr=  150 . a relation that provides @xmath24}$ ] as a function of snr has been derived and used to estimate the uncertainty in [ fe / h ] of all the targets interpolating at their value of the snr . additional sources of uncertainty are the error in v-@xmath22 ( a variation of @xmath210.05 mag translates in a variation in [ fe / h ] of @xmath250.01 dex ) and the uncertainty in the @xmath26[fe / h ] linear fit ( @xmath23=  0.08 dex , as quoted by * ? ? ? the distribution of the [ fe / h ] abundance ratios as derived from ca  ii triplet lines is shown in fig . [ iron ] as an empty histogram .      for 19 targets , the quality of the spectra ( snr@xmath2740 ) allows to determine the iron abundance directly from the measure of fe  i lines . we identify a ten of fe  i lines , unblended at the hr21 setup resolution and at the atmospheric parameters and metallicity of the targets ( see mu13 , for details ) . ews measurements have been performed by using the code daospec @xcite , iteratively launched by means of the package 4dao@xcite that allows an analysis cascade of a large sample of stellar spectra and a visual inspection of the gaussian fit obtained for all the investigated lines . the iron abundance has been derived with the package gala @xcite , by matching the measured and the theoretical ews . atmospheric parameters have been derived by using the b , v photometry by c11 . @xmath19 have been computed by means of the @xmath28@xmath19 transformation by @xcite based on the infrared flux method ; the de - reddened color @xmath28 is obtained adopting a color excess e(b - v)=  0.099 mag ( c11 ) and the extinction law by @xcite . surface gravities have been computed with the stefan - boltzmann relation , assuming the photometric @xmath19 , the distance modulus of 17.75@xmath210.10 mag ( c11 ) and an evolutive mass of 0.75 @xmath29 , according to an isochrone from the basti dataset @xcite with age of 12 gyr , z=  0.0003 and a solar - scaled chemical mixtures . the bolometric corrections are calculated according to eq . ( 17 ) of @xcite . micro - turbulent velocities can not be estimated from these spectra because of the small number of available lines and we adopted for all the targets the average value obtained by the uves spectra , @xmath30=  1.8 km / s . the average iron abundance of these 19 stars is [ fe / h]=2.04@xmath210.02 dex , in reasonable agreement with the value derived by the uves spectra , [ fe / h]=1.98@xmath210.03 dex ( mu13 ) . also , we highlight the good agreement between the abundances derived from ca  ii triplet and from fe  i lines : the average difference of the iron abundances for the 19 stars in common is @xmath31_{cat}-[fe / h]_{fe}=+0.02\pm 0.01 $ ] dex ( @xmath23=  0.08 dex ) . fig . [ iron ] shows the distribution of the 19 stars as a grey histogram , while the inset panel shows the difference between [ fe / h ] from fe  i lines and from ca  ii lines . we consider together the 25 stars for which a direct fe abundance has been derived , 19 giraffe and 6 uves targets . the mean abundance , together with the intrinsic spread @xmath32 and their uncertainties , have been calculated with the maximum likelihood algorithm described in @xcite . we obtain an average value of [ fe / h]=2.01@xmath210.02 dex ( @xmath32=  0.0@xmath210.03 dex ) that we recommended as the final value for the fe abundance . in comparison , the same algorithm applied on the [ fe / h ] derived from ca  ii triplet lines of the 83 member stars provides [ fe / h]=1.99@xmath210.01 dex ( @xmath32=  0.0@xmath210.02 dex ) . distribution of the targets as obtained from the ca  ii triplet lines ( empty histogram ) and from the direct measurement of fe  i lines ( uves+giraffe , grey - shaded histogram ) . the inset panel show the difference between the iron content from fe  i lines and from ca  ii triplet lines as a function of @xmath31_{fei}$ ] for 19 target stars observed with flames . the typical uncertainty in the difference is shown as the error - bar of the empty circle in the lower - right corner of the inset.,width=317 ]    [ cols="<,^,^,^,^,^,^,^,^ " , ]             in the lower panel of fig . [ disp ] we superimpose to the data the predictions of three models that fits the observed sb profile of the cluster ( at least in the innermost regions , see c11 and fig .  [ sbprof ] ) . the models have been normalised to best fit the observed velocity dispersion profile . the first two models are the single - mass isotropic ( * ? ? ? * k66 hereafter ) and ( * ? ? ? * w75 ) models that were proposed in c11 . in addition to these we adopt also a _ darkexp _ model ( * ? ? ? * hw10 ) that is shown , in fig . [ sbprof ] , to provide a reasonable fit of the sb profile over the whole extension of the cluster , in particular in the outermost region of the profile where k66 , w75 and @xcite models fail ( see c11 ) . darkexp models are theoretically derived maximum entropy equilibrium states of self - gravitating collision - less systems ( hw10 ) . @xcite have shown that in many cases ( including ngc  5694 ) they provide a better fit to the observed profiles of gcs , with respect to k66 models . the main difference between k66/w75 models and darkexp models is in the assumed distribution function ( df ; @xmath33 ) . k66 and w75 models adopt a df from the family of lowered maxwellian distributions , which reproduces the trend toward an isothermal condition driven by collisions . darkexp models , instead , adopt a df such that the corresponding energy distribution ( n(e)=@xmath34 ) is a lowered maxwellian distribution , with a proper treatment of the low - occupation - number regime ( see * ? ? ? * for details and discussion ) .    the comparisons displayed in the lower panel of fig . [ disp ] clearly show the inadequacy of k66 models to describe the kinematics of ngc  5694 . this is due to the tidal truncation that is built - in in k66 models : the sb profile is unable to fit the extended @xmath35 outer profile of the cluster and , consequently , it lacks sufficient mass in the outer regions to sustain a ( nearly ) flat dispersion profile beyond @xmath36 . the lack of a tidal truncation may be related to the fact that the cluster is under - filling its roche lobe by a significant amount ( see c11 and sect . [ sum ] , for further discussion ) . on the other hand both the w75 and darkexp models , that have much more extended sb profiles , provide a fair representation of the cluster kinematics . the central dispersion estimate by @xcite appears slightly low with respect to our innermost point and the extrapolation of all best - fitting models . it would be valuable to have an independent estimate of the dispersion in the innermost regions based on the velocities of individual stars , to obtain a robust validation of the estimate by @xcite from integrated spectroscopy . moreover , it has to be recalled that in this comparison we considered only isotropic single - mass and non - collisional models . in the innermost regions of the cluster collisional processes can be important and mass - segregation , as well as anisotropy , is expected to contribute in shaping the overall line - of - sight velocity dispersion profile .      to explore the possible role of orbital anisotropy and mass segregation in the dynamics of ngc  5694 we compare , in fig . [ aniso ] , the observed sb and @xmath23 profiles of the clusters with the predictions of a model including radial anisotropy , two multi - mass models and one multi - mass anisotropic model . the continuos lines in both panels of fig . [ aniso ] correspond to a single - mass king - michie ( k - m * ? ? ? * ) model with the maximum degree of radial anisotropy that still ensures stability ( see * ? ? ? * for a thorough discussion of this family of models ) . in these models , orbits are isotropic in the center and becomes radially biased at a characteristic radius @xmath37 . a rough criterion for stability is represented by the so - called fridman - polyachenko - shukhman parameter @xmath38 ( friedman & polyachenko 1984 ) , where @xmath39 and @xmath40 are the radial and tangential component of the kinetic energy tensor : a fully isotropic model have @xmath41 , while models with @xmath42 undergo bar instability on timescales of few tens of dynamical times ( nipoti et al . 2002 ) , where @xmath43 and @xmath44 are the tangential and radial components of the velocity , respectively , is not particularly informative for k - m models , since , by construction , they have @xmath45 at their center and @xmath46 in their outermost region , the shape of the distribution of @xmath47 being characterised by the anisotropy radius @xmath48 ( see * ? ? ? * and references therein ) . the maximum degree of radial anisotropy of the considered k - m model ( @xmath49 ) is required to obtain a reasonable reproduction of the extended outer branch of the sb profile . the velocity dispersion profile provides a good description of the nearly - flat branch of the observed profile but it fails to fit the central point by more than six times the error on the central dispersion by @xcite . it is interesting to note that excluding the central point to the best - fitting of the velocity normalisation leads to a nearly perfect fit to the profile , for @xmath50 , but , in this case , the predicted value of the central dispersion is as high as 14.0  km / s .    ; continuous line ) , and with the predictions for the distribution of star in the largest mass bin ( approximately corresponding to cluster giants ) of two multi - mass king models computed following g79 . the dotted lines correspond to a model with a single power law mf with index @xmath51 ; the short - dashed lines correspond to a model with @xcite mf . finally , the long - dashed dark grey lines correspond to a multi - mass model with @xcite mf and radial anisotropy . all the models have been normalised to best fit the observed velocity dispersion profile.,width=317 ]    in real clusters formed by stars with a mass spectrum and where the effects of collisions in the cluster center are non negligible , the density and velocity dispersion profiles are different for stars of different mass . broadly speaking , massive stars tend to transfer kinetic energy to less massive stars thus becoming kinematically cooler and sinking in the innermost region of the cluster on less energetic orbits . the amount of kinetic energy transferred by a given star is a function of the contrast between its mass and the average mass of cluster stars , therefore depending on the mass function ( mf ) . the three king multi - mass models shown in fig .  [ aniso ] as dotted , dashed and dot - dashed lines have been computed following ( * ? ? ? * g79 hereafter ) assuming 8 mass bins ( all covering equal - mass intervals at different ranges ) between 0.1 and 0.8 @xmath29 populated according to different assumption on the mf and degree of radial anisotropy : the dotted lines correspond to an isotropic model with a single power law mf ( in the form @xmath52 ) , with index @xmath51 , the short - dashed lines correspond to an isotropic model with a @xcite mf and the long - dashed lines correspond to a radially anisotropic model ( @xmath53 ) with a @xcite mf . dark remnants have been added to the original mf following the prescriptions by sollima , bellazzini & lee ( 2012 ) . since our sb profile , and especially the velocity dispersion profile , are mainly based on giant stars we derived the best - fit by comparing them with the predictions for the most massive mass bin . while both the isotropic multi - mass models fails to reproduce the outer branch of the sb profile , they provide a good fit to the dispersion profile over the whole radial range . an even better fit is provided by the anisotropic model ( with @xmath54 ) which well reproduce the shape of both the sb and the velocity dispersion profile along their entire extent . a gentler decline of the velocity dipersion curve with respect to isotropic k66 models is also predicted in the framework of the modified newtonian dynamics @xcite . however in this case one would expect a convex shape of the velocity dispersion profile in contrast with our data , unless a high degree of radial anisotropy is present ( i.e. , higher than that assumed here for king - michie models in newtonian dynamics , see * ? ? ? * ) . in general , given the good fit provided by darkexp and multi - mass anisotropic models described above , we conclude that there is no need to invoke a modification of the newtonian gravity to explain the observed structure and kinematics of this cluster . it is interesting to note that the masses of the three best - fitting isotropic single - mass models are fully consistent . for the k66 model we obtain @xmath55 , for the w75 model @xmath56 , and for the darkexp model @xmath57 , corresponding to @xmath58 . these values are in excellent agreement with the only previous dynamical mass estimate that can be found in the literature , i.e. , @xmath59 by @xcite , based on the central velocity dispersion from a preliminary analysis of the data of @xcite . the agreement is good also with the non - dynamical estimates by @xcite , who found @xmath60 for both k66 and w75 models , adopting @xmath61 and a total v luminosity lower than that estimated by c11 and used here ( @xmath62 instead of @xmath8 ) .    on the other hand , anisotropic and multi - mass models suggest a slightly larger mass , due to the fact that these models have a significant fraction of their kinetic energy in motions that are not accessible to a sampling of line - of - sight velocities of giants . the single - mass k - m anisotropic model gives @xmath63 , the isotropic multi - mass models give @xmath64 and @xmath65 for the power - law mf with @xmath51 and the kroupa ( 2002 ) mf , respectively , and the anisotropic multi - mass model gives @xmath66 . using the anisotropy - independent estimator of the mass enclosed within the half light radius by @xcite , integrating over the observed sb profile and interpolating the dispersion profile with a spline , we obtain @xmath67 . since in a star cluster the mass should approximately follow light ( modulo the mass segregation ) the total mass should be @xmath68 , also in reasonable agreement with the model - dependent estimates . we obtained rv and [ fe / h ] estimates from medium - resolution giraffe spectra for 165 stars selected to lie on the rgb of the remote globular cluster ngc  5694 . using both rv and [ fe / h ] we selected a sample of 89 bona - fide cluster members , 83 from the giraffe sample and six from the uves sample presented in mu13 . based on these data we derived a mean cluster metallicity of [ fe / h]@xmath69 , an intrinsic metallicity dispersion of @xmath70  dex and a systemic radial velocity of @xmath71  km / s . the cluster kinematics is characterised by a very weak systemic rotation , fully consistent with the _ rotation - metallicity _ and _ rotation - hb morphology _ relations derived by @xcite . the velocity dispersion profile flattens out at large radii . this is incompatible with isotropic single - mass k66 models but is reasonably reproduced by both w75 and darkexp models . however , w75 models provide an unsatisfactory fit to the the cluster sb profile , that , on the other hand is well reproduced by darkexp models over its whole extent . while anisotropic single - mass k - m models and multi - mass isotropic king models seem unable to provide an overall good representation of the structure and kinematics of the cluster , we showed that this result can be attained with multi - mass models including anisotropy . different models / mass estimators consistently converge on a mass between @xmath72 , and @xmath73 corresponding to @xmath74 quite typical for gcs @xcite . the two models providing the best representation of both the sb and the @xmath23 profiles lie at the extremes of this range , the darkexp isotropic non - collisional model at the lower end and the multi - mass anisotropic model ( g79-a ) at the upper end . the anisotropy - independent mass estimator by @xcite is in better agreement with the darkexp model , thus favouring mass ( and mass - to - light ) values toward the lower end . low values of the mass - to - light ratio ( @xmath75 ) are also in agreement with the predictions of population synthesis models , as derived by @xcite . we do not report the uncertainties on the individual mass estimates ( due to the errors in the input parameters , like , e.g. , distance , radii , etc . ) since they are significantly smaller than the the factor of @xmath76 systematic uncertainty that is associated to the choice of a given model ( darkexp or g79-a , in particular ) . lines at fixed @xmath77 ratio are also plotted for reference . ngc  5694 is plotted as an empty triangle when the k66 tidal radius is adopted , and as a filled triangle when the radius of the outermost point of our sb profile is adopted instead . the shaded area correspond to the region of over - filling clusters . , width=317 ]    as noted in c11 and clearly illustrated in fig . [ underf ] ( produced with the same assumptions as c11 , adopting @xmath78 , and taking tidal radii , total luminosities and galactocentric distances from @xcite ) ngc  5694 is largely under - filling its roche lobe , having a ratio between jacoby radius and tidal radius @xmath79 , independently on the actual assumption on the limiting radius ( i.e. , the tidal radius of the best - fitting k66 model or the outermost point of the observed profile ) . this holds also if the criterion by @xcite , based on the ratio between half - light radius and jacoby radius ( @xmath80 ) , is adopted : ngc  5694 has @xmath81 . these authors find that tidally under - filling clusters form a distinct family ( compact clusters ) with respect to tidally filling ones and concluded that they were likely born compact . the smooth nature of both the sb and the velocity dispersion profiles of ngc  5694 suggest that indeed it may be tidally undisturbed and may represent the typical status of a compact globular cluster evolved in isolation . this condition would also favour the permanence of an original radial anisotropic bias in the velocity distribution of cluster stars .    in this context , it is interesting to note that ( a ) virtually all the clusters shown in fig . [ underf ] and having @xmath79 display sb excesses in their outer regions , with respect to k66 models ( see , e.g. * ? ? ? * ; * ? ? ? * ) , and , in particular ( b ) many of the brightest among these clusters ( @xmath82 ) display smooth power - law profiles incompatible with k66 models in their outskirts , similar to ngc  5694 ( see , e.g. , * ? ? ? * ; * ? ? ? * for ngc  7006 , ngc  6229 , and ngc  5824 , respectively ) . deeper and more thorough analyses of the structure and kinematics of these clusters , extending into their low sb outskirts , seems timely . the study of a sample of distant _ compact _ clusters ( in the sense defined by * ? ? ? * ) may provide precious insight on the initial conditions of gcs whose evolution should be only weakly influenced by the interaction with the milky way . we are grateful to an anonymous referee for useful comments and suggestions . m.b . and a.s . acknowledges the financial support from prin miur , project : _ the chemical and dynamical evolution of the milky way and local group galaxies _ , prot . 2010ly5n2 t , ( pi f. matteucci ) . support for m.c . , p.a . , and c.c . is provided by the ministry for the economy , development , and tourism s programa iniciativa cientfica milenio through grant ic120009 , awarded to the millennium institute of astrophysics ( mas ) . m.c . also acknowledges support by proyecto basal pfb-06/2007 and by fondecyt grant # 1141141 .
we present a study of the kinematics of the remote globular cluster ngc  5694 based on giraffe@vlt medium resolution spectra . 
 a sample of 165 individual stars selected to lie on the red giant branch in the cluster color magnitude diagram was considered . using radial velocity and metallicity from calcium triplet 
 , we were able to select 83 bona - fide cluster members . 
 the addition of six previously known members leads to a total sample of 89 cluster giants with typical uncertainties @xmath0  km / s in their radial velocity estimates . 
 the sample covers a wide range of projected distances from the cluster center , from @xmath1 to @xmath2 half - light radii ( @xmath3 ) . 
 we find only very weak rotation , as typical of metal - poor globular clusters . 
 the velocity dispersion gently declines from a central value of @xmath4  km / s to @xmath5  km / s at @xmath6 , then it remainins flat out to the next ( and last ) measured point of the dispersion profile , at @xmath7 , at odds with the predictions of isotropic king models . 
 we show that both isotropic single - mass non - collisional models and multi - mass anisotropic models can reproduce the observed surface brightness and velocity dispersion profiles . 
 [ firstpage ]    ( galaxy : ) globular clusters : individual : ngc 5694  stars : abundances