126 research outputs found
Central energy equipartition in multi-mass models of globular clusters
In the construction of multi-mass King-Michie models of globular clusters, an
approximated central energy equipartition between stars of different masses is
usually imposed by scaling the velocity parameter of each mass class inversely
with the stellar mass, as if the distribution function were isothermal. In this
paper, this 'isothermal approximation' (IA) has been checked and its
consequences on the model parameters studied by a comparison with models
including central energy equipartition correctly. It is found that, under the
IA, the 'temperatures' of a pair of components can differ to a non-negligible
amount for low concentration distributions. It is also found that, in general,
this approximation leads to a significantly reduced mass segregation in
comparison with that given under the exact energy equipartition at the centre.
As a representative example, an isotropic 3-component model fitting a given
projected surface brightness and line-of-sight velocity dispersion profiles is
discussed. In this example, the IA gives a cluster envelope much more
concentrated (central dimensionless potential W=3.3) than under the true
equipartition (W=0.059), as well as a higher logarithmic mass function slope.
As a consequence, the inferred total mass (and then the global mass-to-light
ratio) results a factor 1.4 times lower than the correct value and the amount
of mass in heavy dark remnants is 3.3 times smaller. Under energy
equipartition, the fate of stars having a mass below a certain limit is to
escape from the system. This limit is derived as a function of the mass and W
of the giants and turn-off stars component.Comment: LaTeX 2e, 9 pages with 7 figures. Accepted for publication in MNRA
Parallelization of a Code for the Simulation of Self-gravitating Systems in Astrophysics. Preliminary Speed-up Results
We have preliminary results on the parallelization of a Tree-Code for
evaluating gravitational forces in N-body astrophysical systems. For our Cray
T3D/CRAFT implementation, we have obtained an encouraging speed-up behavior,
which reaches a value of 37 with 64 processor elements (PEs). According to the
Amdahl'law, this means that about 99% of the code is actually parallelized. The
speed-up tests regarded the evaluation of the forces among N = 130,369
particles distributed scaling the actual distribution of a sample of galaxies
seen in the Northern sky hemisphere. Parallelization of the time integration of
the trajectories, which has not yet been taken into account, is both easier to
implement and not as fundamental.Comment: 14 pages LaTeX + 1 EPS figure + 2 EPS colour figures, epsf.sty and
aasms4.sty included; to be published in Science & Supercomputing at CINECA,
Report 1997 (Bologna, Italy
An efficient parallel tree-code for the simulation of self-gravitating systems
We describe a parallel version of our tree-code for the simulation of
self-gravitating systems in Astrophysics. It is based on a dynamic and adaptive
method for the domain decomposition, which exploits the hierarchical data
arrangement used by the tree-code. It shows low computational costs for the
parallelization overhead -- less than 4% of the total CPU-time in the tests
done -- because the domain decomposition is performed 'on the fly' during the
tree setting and the portion of the tree that is local to each processor
'enriches' itself of remote data only when they are actually needed.
The performances of an implementation of the parallel code on a Cray T3E are
presented and discussed. They exhibit a very good behaviour of the speedup (=15
with 16 processors and 10^5 particles) and a rather low load unbalancing (< 10%
using up to 16 processors), achieving a high computation speed in the forces
evaluation (>10^4 particles/sec with 8 processors).Comment: 10 pages, 8 figures, LaTeX2e, A&A class file needed (included),
submitted to A&A; corrected abstract word wrappin
A mass estimate of an intermediate-mass black hole in omega Centauri
Context. The problem of the existence of intermediate-mass black holes
(IMBHs) at the centre of globular clusters is a hot and controversial topic in
current astrophysical research with important implications in stellar and
galaxy formation.
Aims. In this paper, we aim at giving further support to the presence of an
IMBH in omega Centauri and at providing an independent estimate of its mass.
Methods. We employed a self-consistent spherical model with anisotropic
velocity distribution. It consists in a generalisation of the King model by
including the Bahcall-Wolf distribution function in the IMBH vicinity.
Results. By the parametric fitting of the model to recent HST/ACS data for
the surface brightness profile, we found an IMBH to cluster total mass ratio of
M_BH/M = 5.8(+0.9-1.2) x 10^(-3). It is also found that the model yields a fit
of the line-of-sight velocity dispersion profile that is better without mass
segregation than in the segregated case. This confirms the current thought of a
non-relaxed status for this peculiar cluster. The best fit model to the
kinematic data leads, moreover, to a cluster total mass estimate of M = (3.1
+/- 0.3) x 10^6 Msol, thus giving an IMBH mass in the range 13,000 < M_BH <
23,000 Msol (at 1-sigma confidence level). A slight degree of radial velocity
anisotropy in the outer region (r > 12') is required to match the outer surface
brightness profile.Comment: LateX, 5 pages, 5 figures. Accepted for publication by Astronomy &
Astrophysic
The surface density profile of NGC 6388: a good candidate for harboring an intermediate-mass black hole
We have used a combination of high resolution (HST ACS-HRC, ACS-WFC, and
WFPC2) and wide-field (ESO-WFI) observations of the galactic globular cluster
NGC 6388 to derive its center of gravity, projected density profile, and
central surface brightness profile. While the overall projected profiles are
well fit by a King model with intermediate concentration (c=1.8) and sizable
core radius (rc=7"), a significant power law (with slope \alpha=-0.2) deviation
from a flat core behavior has been detected within the inner 1 arcsecond. These
properties suggest the presence of a central intermediate mass black hole. The
observed profiles are well reproduced by a multi-mass isotropic, spherical
model including a black hole with a mass of ~5.7x10^3 Msol.Comment: ApJ Letter in pres
Evidence of tidal distortions and mass loss from the old open cluster NGC 6791
We present the first evidence of clear signatures of tidal distortions in the
density distribution of the fascinating open cluster NGC 6791. We used deep and
wide-field data obtained with the Canada-France-Hawaii-Telescope covering a 2x2
square degrees area around the cluster. The two-dimensional density map
obtained with the optimal matched filter technique shows a clear elongation and
an irregular distribution starting from ~300" from the cluster center. At
larger distances, two tails extending in opposite directions beyond the tidal
radius are also visible. These features are aligned to both the absolute proper
motion and to the Galactic center directions. Moreover, other overdensities
appear to be stretched in a direction perpendicular to the Galactic plane.
Accordingly to the behaviour observed in the density map, we find that both the
surface brightness and the star count density profiles reveal a departure from
a King model starting from ~600" from the center. These observational evidence
suggest that NGC 6791 is currently experiencing mass loss likely due to
gravitational shocking and interactions with the tidal field. We use this
evidence to argue that NGC 6791 should have lost a significant fraction of its
original mass. A larger initial mass would in fact explain why the cluster
survived so long. Using available recipes based on analytic studies and N-body
simulations, we derived the expected mass loss due to stellar evolution and
tidal interactions and estimated the initial cluster mass to be M_ini=(1.5-4) x
10^5 M_sun.Comment: Accepted for publication in the MNRAS (9 pages, 8 Figures
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