2,129 research outputs found
Sizes of Confirmed Globular Clusters in NGC 5128: A Wide-Field High-Resolution Study
Using Magellan/IMACS images covering a 1.2 x 1.2 sq. degree FOV with seeing
of 0.4"-0.6", we have applied convolution techniques to analyse the light
distribution of 364 confirmed globular cluster in the field of NGC 5128 and to
obtain their structural parameters. Combining these parameters with existing
Washington photometry from Harris et al. (2004), we are able to examine the
size difference between metal-poor (blue) and metal-rich (red) globular
clusters. For the first time, this can be addressed on a sample of confirmed
clusters that extends to galactocentric distances about 8 times the effective
radius, R, of the galaxy. Within 1 R, red clusters are about
30% smaller on average than blue clusters, in agreement with the vast majority
of extragalactic globular cluster systems studied. As the galactocentric
distance increases, however, this difference becomes negligible. Thus, our
results indicate that the difference in the clusters' effective radii, r,
could be explained purely by projection effects, with red clusters being more
centrally concentrated than blue ones and an intrinsic r--R
dependence, like the one observed for the Galaxy.Comment: 4 figures, accepted for publication in ApJ
New g'r'i'z' Photometry of the NGC 5128 Globular Cluster System
We present new photometry for 323 of the globular clusters in NGC 5128
(Centaurus A), measured for the first time in the filter system. The
color indices are calibrated directly to standard stars in the
system and are used to establish the fiducial mean colors for the blue and red
(low and high metallicity) globular cluster sequences. We also use
spectroscopically measured abundances to establish the conversion between the
most metallicity-sensitive colors (, ) and metallicity,
[Fe/H].Comment: 14 pages, 9 figures, accepted in A
The Centaurus Group and the Outer Halo of NGC 5128: Are they Dynamically Connected?
NGC 5128, a giant elliptical galaxy only Mpc away, is the dominant
member of a galaxy group of over 80 probable members. The Centaurus group
provides an excellent sample for a kinematic comparison between the halo of NGC
5128 and its surrounding satellite galaxies. A new study, presented here, shows
no kinematic difference in rotation amplitude, rotation axis, and velocity
dispersion between the halo of NGC 5128, determined from over of its
globular clusters, and those of the Centaurus group as a whole. These results
suggest NGC 5128 could be behaving in part as the inner component to the galaxy
group, and could have begun as a large initial seed galaxy, gradually built up
by minor mergers and satellite accretions, consistent with simple cold dark
matter models. The mass and mass-to-light ratios in the B-band, corrected for
projection effects, are determined to be
M_{\sun} and M_{\sun}/L_{\sun} for NGC 5128 out to a
galactocentric radius of 45 kpc, and M_{\sun}
and M_{\sun}/L_{\sun} for the Centaurus group, consistent with
previous studies.Comment: 14 pages, 3 tables, 7 figures, Accepted for publication in A
Microscopic origin of the optical processes in blue sapphire
Al2O3 changes from transparent to a range of intense colours depending on the chemical impurities present. In blue sapphire, Fe and Ti are incorporated; however, the chemical process that gives rise to the colour has long been debated. Atomistic modelling identifies charge transfer from Ti(III) to Fe(III) as being responsible for the characteristic blue appearance
Radial Velocities of Newly Discovered Globular Clusters in NGC 5128
We present radial velocity measurements for 74 globular clusters (GCs) in the
nearby giant elliptical NGC 5128, of which 31 are newly discovered clusters.
All the GC candidates were taken from the list of possible new clusters given
in the Harris, Harris, & Geisler (2004) photometric survey. In addition to the
newly confirmed clusters, we identified 24 definite foreground stars and 31
probable background galaxies. From a combined list of 299 known GCs in NGC 5128
with measured radial velocities and metallicity-sensitive (C - T_1) photometric
indices, we construct a new metallicity distribution function (MDF) for the
cluster system. The MDF shows an approximately bimodal form, with centroids at
[Fe/H] = -1.46 and -0.53, and with nearly equal numbers of metal-poor and
metal-rich clusters in the two modes. However, there are many
intermediate-color clusters in the distribution, and the fainter clusters tend
to have a higher proportion of red clusters. These features of the MDF may
indicate a widespread age range within the cluster system as well as an
intrinsically broad metallicity spread.Comment: 10 pages, 7 figures, 4 tables - accepted in Astronomical Journa
Tuning Knobs for the NLC Final Focus
Compensation of optics errors at the Interaction Point (IP) is essential for
maintaining maximum luminosity at the NLC. Several correction systems (knobs)
using the Final Focus sextupoles have been designed to provide orthogonal
compensation of linear and the second order optics aberrations at IP. Tuning
effects of these knobs on the 250 GeV beam were verified using tracking
simulations.Comment: 4 pages, 3 figure
Globular Cluster Scale Sizes in Giant Galaxies: Orbital Anisotropy and Tidally Under-filling Clusters in M87, NGC 1399, and NGC 5128
We investigate the shallow increase in globular cluster half-light radii with
projected galactocentric distance observed in the giant galaxies M87,
NGC 1399, and NGC 5128. To model the trend in each galaxy, we explore the
effects of orbital anisotropy and tidally under-filling clusters. While a
strong degeneracy exists between the two parameters, we use kinematic studies
to help constrain the distance beyond which cluster orbits become
anisotropic, as well as the distance beyond which clusters are
tidally under-filling. For M87 we find kpc and kpc and kpc.
The connection of with each galaxy's mass profile indicates the
relationship between size and may be imposed at formation, with only
inner clusters being tidally affected. The best fitted models suggest the
dynamical histories of brightest cluster galaxies yield similar present-day
distributions of cluster properties. For NGC 5128, the central giant in a small
galaxy group, we find kpc and kpc. While we
cannot rule out a dependence on , NGC 5128 is well fitted by a tidally
filling cluster population with an isotropic distribution of orbits, suggesting
it may have formed via an initial fast accretion phase. Perturbations from the
surrounding environment may also affect a galaxy's orbital anisotropy profile,
as outer clusters in M87 and NGC 1399 have primarily radial orbits while outer
NGC 5128 clusters remain isotropic.Comment: 16 pages, 7 figures, 4 tables, Accepted for publication in MNRA
The Kinematics of the Globular Cluster System of NGC 5128 with a New, Large Sample of Radial Velocity Measurements
New radial velocity measurements for previously known and newly confirmed
globular clusters (GCs) in the nearby massive galaxy NGC 5128 are presented. We
have obtained spectroscopy from LDSS-2/Magellan, VIMOS/VLT, and Hydra/CTIO from
which we have measured the radial velocities of 218 known, and identified 155
new, GCs. The current sample of confirmed GCs in NGC 5128 is now 605 with 564
of these having radial velocity measurements. We have performed a new kinematic
analysis of the GC system that extends out to 45 arcmin in galactocentric
radius. We have examined the systemic velocity, projected rotation amplitude
and axis, and the projected velocity dispersion of the GCs as functions of
galactocentric distance and metallicity. Our results indicate that the
metal-poor GCs have a very mild rotation signature of (26 pm 15) km/s. The
metal-rich GCs are rotating with a higher, though still small signature of (43
pm 15) km/s around the isophotal major axis of NGC 5128 within 15 arcmin. Their
velocity dispersions are consistent within the uncertainties and the profiles
appear flat or declining within 20 arcmin. We note the small sample of
metal-rich GCs with ages less than 5 Gyr in the literature appear to have
different kinematic properties than the old, metal-rich GC subpopulation. The
mass and mass-to-light ratios have also been estimated using the GCs as tracer
particles for NGC 5128. Out to a distance of 20 arcmin, we have obtained a mass
of (5.9 pm 2.0) x 10^(11) M_(sun) and a mass-to-light ratio in the B-band of 16
M_(sun)/L_(B,sun). Combined with previous work on the ages and metallicities of
its GCs, as well as properties of its stellar halo, our findings suggest NGC
5128 formed via hierarchical merging over other methods of formation, such as
major merging at late times.Comment: Accepted for The Astronomical Journal, 14 pages plus 12 figures and 7
table
GULP: Capabilities and prospects
The current status and capabilities of the atomistic simulation code GULP are described. In particular, the differences between versions 1.3.2 and 3.0 are detailed, as well as a concise pointer to applications in computational crystallography
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