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J/A+A/567/A69 Radial velocity + photometry in NGC 4372 (Kacharov+, 2014)
The following files can be converted to FITS (extension .fit or fit.gz)
kinemat.dat photom.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/567/A69
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Beginning of ReadMe :J/A+A/567/A69 Radial velocity and photometry in NGC 4372 (Kacharov+, 2014)
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A study of rotating globular clusters.
The case of the old, metal-poor globular cluster NGC 4372.
Kacharov N., Bianchini P., Koch A., Frank M.J., Martin N.F., van de Ven G.,
Puzia T.H., McDonald I., Johnson C.I., Zijlstra A.A.
<Astron. Astrophys. 567, A69 (2014)>
=2014A&A...567A..69K
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ADC_Keywords: Clusters, globular ; Photometry, UBVRI ; Reddening ;
Radial velocities
Keywords: Globular clusters: general - Globular clusters: individual: NGC4372 -
Galaxy: halo - Galaxy: kinematics and dynamics
Abstract:
We present the first in-depth study of the kinematic properties and
derive the structural parameters of NGC 4372 based on the fit of a
Plummer profile and a rotating, physical model. We explore the link
between internal rotation to different cluster properties and together
with similar studies of more GCs, we put these in the context of
globular cluster formation and evolution. We present radial velocities
for 131 cluster member stars measured from high-resolution
FLAMES/GIRAFFE observations. Their membership to the GC is
additionally confirmed from precise metallicity estimates. Using this
kinematic data set we build a velocity dispersion profile and a
systemic rotation curve. Additionally, we obtain an elliptical number
density profile of NGC 4372 based on optical images using a MCMC
fitting algorithm. From this we derive the cluster's half-light radius
and ellipticity as r_h_=3.4'+/-0.04' and e=0.08+/-0.01. Finally, we
give a physical interpretation of the observed morphological and
kinematic properties of this GC by fitting an axisymmetric,
differentially rotating, dynamical model. Our results show that NGC
4372 has an unusually high ratio of rotation amplitude to velocity
dispersion (1.2 vs. 4.5km/s) for its metallicity. This, however, puts
it in line with two other exceptional, very metal-poor GCs - M 15 and
NGC 4590. We also find a mild flattening of NGC 4372 in the direction
of its rotation. Given its old age, this suggests that the flattening
is indeed caused by the systemic rotation rather than tidal
interactions with the Galaxy. Additionally, we estimate the dynamical
mass of the GC M_dyn=2.0+/-0.5 x 10^5 M_Sun based on the dynamical
model, which constrains the mass-to-light ratio of NGC 4372 between
1.4 and 2.3 M_Sun/L_Sun, representative of an old, purely stellar
population.
Description:
We present the radial velocities of 220 stars in the field of the
globular cluster NGC 4372 measured from high resolution FLAMES/GIRAFFE
spectra. We have confirm 131 cluster member stars from radial velocity
and metallicity constraints. The rest are foreground contaminants. We
also present a BVI photometric catalogue in a field of view covering
30x30arcmin, centred on NGC 4372. We used archival imaging obtained
with the Wide Field Imager (WFI) at the 2.2m MPG/ESO telescope at La
Silla. We used the 2MASS point source catalog as astrometric
reference. Photometric zero points were fixed to standard stars in the
same field from the standard star database of Stetson
(2000PASP..112..925S, 2005PASP..117..563S). We have estimated
individual reddening for each star in the catalogue.