7,303 research outputs found
Dynamics of the Young Binary LMC Cluster NGC 1850
In this paper we have examined the age and internal dynamics of the young
binary LMC cluster NGC 1850 using BV CCD images and echelle spectra of 52
supergiants. Isochrone fits to a BV color-magnitude diagram revealed that the
primary cluster has an age of Myr while the secondary member
has Myr. BV surface brightness profiles were constructed out
to R 40 pc, and single-component King-Michie (KM) models were applied. The
total cluster luminosity varied from L = 2.60 - 2.65
L\sol\ and L = 1.25 - 1.35 as the anisotropy radius
varied from infinity to three times the scale radius with the isotropic models
providing the best agreement with the data. Of the 52 stars with echelle
spectra, a subset of 36 were used to study the cluster dynamics. The KM radial
velocity distributions were fitted to these velocities yielding total cluster
masses of 5.4 - 5.9 M\sol\ corresponding to M/L =
0.02 M\sol/L\sol\ or M/L = 0.05 M\sol/L\sol.
A rotational signal in the radial velocities has been detected at the 93\%
confidence level implying a rotation axis at a position angle of 100\deg. A
variety of rotating models were fit to the velocity data assuming cluster
ellipticities of . These models provided slightly better
agreement with the radial velocity data than the KM models and had masses that
were systematically lower by a few percent. The preferred value for the slope
of a power-law IMF is a relatively shallow, x = 0.29 \pmm{+0.3}{-0.8}
assuming the B-band M/L or x = 0.71 \pmm{+0.2}{-0.4} for the V-band.Comment: 41 pages (figures available via anonymous FTP as described below
The Optical Gravitational Lensing Experiment. Variable Stars in Globular Clusters - IV. Fields 104A-E in 47 Tuc
Five fields located close to the center of the globular cluster NGC 104=47
Tuc were surveyed in a search for variable stars. We present V-band light
curves for 42 variables. This sample includes 13 RR Lyr stars -- 12 of them
belong to the Small Magellanic Cloud (SMC) and 1 is a background object from
the galactic halo. Twelve eclipsing binaries were identified -- 9 contact
systems and 3 detached/semi-detached systems. Seven eclipsing binaries are
located in the blue straggler region on the cluster color-magnitude diagram
(CMD) and four binaries can be considered main-sequence systems. One binary is
probably a member of the SMC. Eight contact binaries are likely members of the
cluster and one is most probably a foreground star. We show that for the
surveyed region of 47 Tuc, the relative frequency of contact binaries is very
low as compared with other recently surveyed globular clusters. The sample of
identified variables also includes 15 red variables with periods ranging from
about 2 days to several weeks. A large fraction of these 15 variables probably
belong to the SMC but a few stars are likely to be red giants in 47 Tuc. VI
photometry for about 50 000 stars from the cluster fields was obtained as a by
product of our survey.Comment: Latex file, l-aa style, 10 pages, 7 ps figures included. Submitted to
A&A. Figure 8 available from
ftp://sirius.astrouw.edu.pl/pub/jka/47Tuc/fig8.ps.
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