The Kinematics and Dynamics of the Globular Clusters and
Planetary Nebulae of NGC 5128
Kristin A. Woodley
Department of Physics & Astronomy, McMaster University, Hamilton ON L8S 4M1,
Canada
woodleka@physics.mcmaster.ca
William E. Harris
Department of Physics & Astronomy, McMaster University, Hamilton ON L8S 4M1,
Canada
harris@physics.mcmaster.ca
Michael A. Beasley
Instituto de Astrofisica de Canarias, Calle Vı́a Láctea, s/n E-38200, La Laguna Tenerife,
Spain
beasley@iac.es
Eric W. Peng
Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V8V 2X6,
Canada
eric.peng@nrc-cnrc.gc.ca
Terry J. Bridges
Department of Physics, Queen’s University, Kingston, ON K7L 3N6, Canada
tjb@astro.queensu.ca
Duncan A. Forbes
Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn, VIC 3122,
Australia
dforbes@astro.swin.edu.au
Gretchen L. H. Harris
http://arxiv.org/abs/0704.1189v2
– 2 –
Department of Physics & Astronomy, University of Waterloo, Waterloo ON N2L 3G1,
Canada
glharris@astro.uwaterloo.ca
ABSTRACT
A new kinematic and dynamic study of the halo of the giant elliptical galaxy
NGC 5128 is presented. From a spectroscopically confirmed sample of 340 glob-
ular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis,
velocity dispersion, and total dynamical mass are determined for the halo of
NGC 5128. The globular cluster kinematics were searched for both radial de-
pendence and metallicity dependence by subdividing the globular cluster sample
into 158 metal-rich ([Fe/H]> −1.0) and 178 metal-poor ([Fe/H]< −1.0) globular
clusters. Our results show that the kinematics of the metal-rich and metal-poor
subpopulations are quite similar: over a projected radius of 0−50 kpc, the mean
rotation amplitudes are 47±15 and 31±14 km s−1 for the metal-rich and metal-
poor populations, respectively. There is a indication within 0 − 5 kpc that the
metal-poor clusters have a lower rotation signal than in the outer regions of the
galaxy. The rotation axis shows an interesting twist at 5 kpc, agreeing with
the zero-velocity curve presented by Peng and coworkers. Within 5 kpc, both
metal-rich and metal-poor populations have a rotation axis nearly parallel to the
north-south direction, which is 0o, while beyond 5 kpc the rotation axis twists
∼ 180o. The velocity dispersion displays a steady increase with galactocentric
radius for both metallicity populations, with means of 111 ± 6 and 117 ± 6 km
s−1 within a projected radius of 15 kpc for the metal-rich and metal-poor pop-
ulations; however, the outermost regions suffer from low number statistics and
spatial biases. The planetary nebula kinematics are slightly different. Out to a
projected radius of 90 kpc from the center of NGC 5128, the planetary nebulae
have a higher rotation amplitude of 76±6 km s−1, and a rotation axis of 170±5o
east of north, with no significant radial deviation in either determined quantity.
The velocity dispersion decreases with galactocentric distance. The total mass
of NGC 5128 is found using the tracer mass estimator, described by Evans et al.,
to determine the mass supported by internal random motions and the spherical
component of the Jeans equation to determine the mass supported by rotation.
We find a total mass of 1.0 ± 0.2 × 1012 M⊙ from the planetary nebula data ex-
tending to a projected radius of 90 kpc. The similar kinematics of the metal-rich
and metal-poor globular clusters allow us to combine the two subpopulations
– 3 –
to determine an independent estimate of the total mass, giving 1.3 ± 0.5 × 1012
M⊙ out to a projected radius of 50 kpc. Lastly, we publish a new and homoge-
neous catalog of known globular clusters in NGC 5128. This catalog combines all
previous definitive cluster identifications from radial velocity studies and HST
imaging studies, as well as 80 new globular clusters with radial velocities from a
study of M.A. Beasley et al. (in preparation).
Subject headings: galaxies: elliptical and lenticular, cD — galaxies: individual
(NGC 5128) — galaxies: kinematics and dynamics — galaxies: star clusters —
globular clusters: general — planetary nebulae: general — catalogs
1. Introduction
Globular clusters (GCs), as single-age, single-metallicity objects, are excellent tracers of
the formation history of their host galaxies, through their dynamics, kinematics, metallicities,
and ages. For most galaxies within ≃ 20 Mpc, GCs can be identified through photometry
and image morphology, from which follow-up radial velocity studies can be carried out with
multi-object spectroscopy on 4 and 8 m class telescopes. The ability to target hundreds of
objects in a single field has vastly increased the observed samples of GCs confirmed in many
galaxies, providing the necessary basis for detailed kinematic and age studies.
Another benefit of using GCs as a kinematic tracer is that they provide a useful, inde-
pendent basis for comparison with results from planetary nebulae (PNe). This is particularly
true given the current debate surrounding the use of PN velocities and the implications for
low dark matter halos. For example, Romanowsky et al. (2003) reported, based on PN ve-
locities, that three low-luminosity ellipticals revealed declining velocity dispersion profiles
and little or no dark matter. However, subsequent simulations of merger-remnant ellipticals
suggested that the radial anisotropy of intermediate-age PNe could give rise to the observed
profiles within standard halos of dark matter (Dekel et al. 2005; Mamon &  Lokas 2005).
Flattening of the galaxy along the line of sight is another possible explanation. One of the
ellipticals studied by Romanowsky et al. (2003), NGC 3379, has also been investigated using
GC kinematics (Pierce et al. 2006; Bergond et al. 2006); both studies found evidence of a
dark matter halo. But the two studies of NGC 3379 suffered from small number statistics.
Clearly there is a need to directly compare PN and GC kinematics for the same elliptical
with sufficiently large numbers of tracer objects.
Previous velocity-based studies of globular cluster systems (GCSs) have shown an in-
triguing variety of results in their overall kinematics. Prominent recent examples include the
– 4 –
following:
1. Côté et al. (2001) performed a kinematic analysis of the GCS in M87 (NGC 4486),
the cD galaxy in the Virgo Cluster. With a sample of 280 GCs, they showed that the entire
GCS rotates on an axis matching the photometric minor axis of the galaxy, except for the
inner metal-poor sample. Inside the onset of the cD envelope, the metal-poor clusters appear
to rotate around the major axis of the galaxy instead. This study also found evidence for
an increase in velocity dispersion, σv, with radius, due to the larger scale Virgo Cluster
mass distribution. They also showed no strong evidence for a difference in σv between the
metal-poor and metal-rich groups. Using a Virgo mass model, they investigated anisotropy
and found that as a whole, the GCS had isotropy, but considered separately, the metal-poor
and metal-rich subpopulations had slight anisotropy.
2. Côté et al. (2003) performed a dynamical analysis for M49 (NGC 4472), the other
supergiant member of the Virgo Cluster. Using over 260 GCs, they found that the metal-
rich population shows no strong evidence for rotation, while the metal-poor population does
rotate about the minor axis of the galaxy. In addition, they found that the metal-poor
clusters had an overall higher dispersion than the metal-rich population.
3. Richtler et al. (2004) determined the kinematics for the GCS in NGC 1399, the
brightest elliptical in the Fornax Cluster of galaxies. Armed with a sample of over 460 GCs,
they found a marginal rotation signal for the entire GC sample and the outer metal-poor
sample, while no rotation was seen for the metal-rich subpopulation. Their projected velocity
dispersion showed no radial trend within their determined uncertainty, but the metal-poor
clusters had a higher dispersion than the metal-rich clusters. The kinematics of the PNe
in NGC 1399 have been most recently studied by Saglia et al. (2000) and Napolitano et al.
(2002) using a small sample of 37 PNe from Arnoaboldi et al. (1994). These studies do
not indicate any significant deviations in velocity dispersion with radius for the PNe, yet
interestingly, Napolitano et al. (2002) found stong rotation for the PNe in the inner region
of the galaxy.
4. Peng, Ford & Freeman (2004c) studied the GC kinematics of the giant elliptical
NGC 5128 from a total of 215 GCs. Their results showed definite rotation signals in both
metallicity groups beyond a 5 kpc distance from the center of the galaxy, as well as similar
velocity dispersions in both the metal-poor and the metal-rich populations within a 20 kpc
projected radius. A similar PN kinematic study in NGC 5128 (Peng, Ford & Freeman 2004b)
showed that the PNe population is rotating around a twisted axis that turns just beyond
the 5 kpc distance.
These few detailed kinematic studies of GCSs in elliptical galaxies, show results that
– 5 –
appear to differ on a galaxy-by-galaxy basis, without any clear global trends. The age
distributions of the GC populations in these same galaxies tend to show a consistent pattern
in which the blue, or metal-poor, population is found to be universally old. The red, or metal-
rich, population has also been shown to be old in the study of Strader et al. (2005). Their
study found that both the metal-poor and metal-rich GCs in a sample of eight galaxies ranging
from dwarf to massive ellipticals, all have ages as old as their Galactic GC counterparts.
Conversely, in a small sample of studies, the red GC population has also been found to be 2-4
Gyr younger than the metal-poor GC population, and with a wider spread in determined ages
(see the studies of Peng, Ford & Freeman 2004c; Puzia et al. 2005, among others), although
this is not yet a well-established trend. The GCs in NGC 5128 appear to be old, with an
intermediate-age population (Peng, Ford & Freeman 2004c; Beasley et al. 2006).
NGC 5128 (Centaurus A), the central giant in the Centaurus group of galaxies at a
distance of only ∼ 4 Mpc, is a prime candidate for both kinematic and age studies. Its GCS
has a specific frequency of SN ≃ 2.2±0.6 (Harris et al. 2006), toward the low end of the giant
elliptical range but about twice as high as in typical disk galaxies. Its optical features show
faint isophotal shells located in the halo (e.g. Peng et al. 2002), the prominent dust lane in the
inner 5 kpc, the presence of gas, and star formation, all of which suggest that NGC 5128 could
be a merger product. Baade & Minkowski (1954) first suggested that NGC 5128 could be
the result of a merger between two galaxies, a spiral and an elliptical. This idea was followed
by the general formation mechanism of disk-disk mergers proposed by Toomre & Toomre
(1972). Bekki, Harris, & Harris (2003) found that the metallicity distribution function of the
halo field stars could be reproduced by a gas-free (”dry”) disk-disk merger scenario. Recent
numerical simulations by Bekki & Peng (2006) also demonstrate that the PN kinematics
observed in NGC 5128 (Peng, Ford & Freeman 2004b) can be reproduced relatively well
from a merger of unequal-mass disk galaxies (with one galaxy half the mass of the other)
colliding on a highly inclined orbital configuration.
Alternatively, much of NGC 5128 could be a ”red and dead” galaxy, passively evolving
since its initial formation as a large seed galaxy (Woodley 2006), while undergoing later
minor mergers and satellite accretions. Evidence consistent with this scenario is in the halo
population of stars in NGC 5128, which have a mean age of 8+3.0
−3.5 Gyr (Rejkuba et al. 2005).
Its metal-poor GC ages have also been shown to have ages similar to Milky Way GCs,
while the metal-rich population appears younger (Peng, Ford & Freeman 2004c). Our new
spectroscopic study (Beasley et al. 2006) suggests that NGC 5128 has a trimodal distribution
of cluster ages: ∼ 50% of metal-rich clusters have ages of 6 − 8 Gyr, only a small handful
of metal-rich clusters have ages of 1 − 3 Gyr, and a large fraction of both metal-rich and
metal-poor clusters have ages of ≃ 12 Gyr. Lastly, the halo kinematics of NGC 5128 have
also been recently shown to match the surrounding satellite galaxies in the low-density
– 6 –
Centaurus group, suggesting that NGC 5128 acts like an inner component to its galaxy
group (Woodley 2006). Kinematic and age studies with large number of GCs are thus
starting to help disentangle the formation of this giant elliptical.
The confirmed GC population in NGC 5128 is now large enough to allow a new kine-
matic analysis subdivided to explore radial and metallicity dependence, while avoiding small
number statistics in almost all regions of the galaxy. The analysis presented here comple-
ments the detailed age distribution study provided by Beasley et al. (2006). The results
provide a broader picture of the formation scenario of NGC 5128.
The sections of this paper are divided as follows: § 2 contains the full catalog of NGC
5128 GCs with known photometry and radial velocities, § 3 contains the kinematic analysis of
GCSs, § 4 contains the kinematic analysis of the PN population, § 5 contains the discussion of
the dynamical mass of NGC 5128, and § 6 contains our final discussion, as well as concluding
remarks.
2. The Catalog of Globular Clusters in NGC 5128
Finding GCs in NGC 5128 is challenging. This process begins with photometric surveys
of the many thousands of objects projected onto the NGC 5128 field (e.g. Rejkuba 2001;
Harris et al. 2004); only a few percent of these are the GCs that we seek. This daunting task
is made difficult by the galactic latitude of NGC 5128 (b = 19o), which means that many
foreground stars are present in the field of NGC 5128. Background galaxies are another major
contaminant in the field, forcing the use of search criteria such as magnitude, color, and object
morphology to help build the necessary candidate list of GCs. Confirmation of such candidate
objects can then be done with spectroscopic radial velocity measurements. The GCs in NGC
5128 have radial velocities in the range vr = 200− 1000 km s
−1, while most foreground stars
have vr < 200 km s
−1. Background galaxies have radial velocities of many thousands of km
s−1 and can easily be eliminated (see the recent studies of Peng, Ford, & Freeman 2004a;
Woodley, Harris, & Harris 2005).
Over the past quarter century, there have been seven distinct radial velocity stud-
ies to identify GCs in NGC 5128 (van den Bergh, Hesser, & Harris 1981; Hesser et al. 1984;
Hesser, Harris, & Harris 1986; Harris et al. 1992; Peng, Ford, & Freeman 2004a; Woodley, Harris, & Harris
2005; Beasley et al. 2006). Although Harris et al. (1992) was not a radial velocity study it-
self, but rather a CCD photometric study of previously confirmed GCs, it does include the
GCs determined spectroscopically from Sharples (1988). A recent study with measured GC
radial velocities published by Rejkuba et al. (2007) has confirmed two new GCs, HCH15 and
– 7 –
R122, included in our catalog.
Within this catalog are 80 new GCs with radial velocity measurements from Beasley et al.
(2006). The combination of these studies now leads to a confirmed population of 342 GCs.1
Also included in our catalog are the new GC candidates from HST STIS imaging from
Harris et al. (2002), labelled C100-C106, and from HST ACS imaging from Harris et al.
(2006), labelled C111-C179. All these previous studies have their own internal numbering
systems, which makes the cluster identifications somewhat confusing at this point. Here we
define a new, homogeneous listing combining all this material and with a single numbering
system.
Our catalog of the GCs of NGC 5128 is given in Table 1. In successive columns, the Table
gives the new cluster name in order of increasing right ascension; the previous names of the
cluster in the literature; right ascension and declination (J2000); the projected radius from
the center of NGC 5128 in arcminutes; the U , B, V , R, and I photometric indices and their
measured uncertainties; the C, M , and T1 photometric indices and their uncertainties; the
colors U−B, B−V , V −R, V −I, M−T1, C−M , and C−T1; and, lastly, the weighted mean
velocity vr and its associated uncertainty from all previous studies. All UBV RI photometry
is from the imaging survey described in Peng, Ford, & Freeman (2004a). The CMT1 data
are from Harris et al. (2004).
The mean velocities are weighted averages with weights on each individual measurement
equal to ε−2v where εv is the quoted velocity uncertainty from each study. The uncertainty
in the mean velocity is then < εv >= (
ε−2i )
−1/2. There are no individual uncertainties
supplied for the velocities for clusters studied by Hesser, Harris, & Harris (1986), but their
study reports that the mean velocity uncertainty for clusters with Rgc < 11
′ is 25 km s−1
and for Rgc > 11
′ is 44 km s−1. We have adopted these values accordingly for their clusters.2
The study by Harris et al. (1992) also does not report velocity uncertainties; however,
these clusters have all been recently measured by Peng, Ford, & Freeman (2004a). The rms
1The confirmed GC list in Woodley (2006) containing 343 GCs has been reduced to 340 based on recent
spectroscopic and imaging studies. Object 304867 with a high radial velocity of 305± 56 km s−1 appears to
be an M-type star based on the strong molecular bands in its spectrum, see Beasley et al. (2006) for further
discussion. Objects pff gc-010 and 114993 are also rejected as GCs because of their starlike appearance
under HST ACS imaging; see Harris et al. (2006). However, newly confirmed GCs HCH15 and R122 have
now been added (Rejkuba et al. 2007).
2Hesser, Harris, & Harris (1986) report C32 at a distance of Rgc = 10.8
′, but more recently
Peng, Ford, & Freeman (2004a) claim a distance of Rgc = 11.25
′, so it has an adopted uncertainty of 44
km s−1 in the weighted mean.
– 8 –
scatter of the Harris et al. (1992) values from theirs was 58 km s−1. This value has been
adopted as the velocity uncertainty of the Harris et al. (1992) clusters in the weighted means.
The weighted mean velocity of cluster C10 does not include the measured value deter-
mined by Peng, Ford, & Freeman (2004a) which is significantly different from other mea-
surements. Also, cluster C27 does not include the measurement of vr = 1932 ± 203 km s
from Beasley et al. (2006), indicating that this object is a galaxy. We include C27 as a GC,
but with caution.
In the weighted velocity calculations, the velocities and uncertainties of the 27 GCs from
Rejkuba et al. (2007) have been rounded to the nearest whole number, with any velocity
uncertainty below 1 km s−1 rounded up to a value of 1.
Lastly, the GC pff gc-089 overlaps the previously existing confirmed cluster, C49, within
a 0.5” radius; pff gc-089 is therefore removed from the catalog of confirmed GCs.
The data in Table 1 provide the basis for the kinematic study presented in this paper.
We use them to derive the rotation amplitude, rotation axis and velocity dispersion in
the full catalog of clusters, as well as for the metal-poor ([Fe/H] < −1) and metal-rich
([Fe/H] > −1) subpopulations. For this purpose, we define the metallicity of the GCs by
transforming the dereddened colors (C − T1)o to [Fe/H] through the standard conversion
(Harris & Harris 2002), calibrated through Milky Way cluster data. A foreground reddening
value of E(B − V ) = 0.11 for NGC 5128, corresponding to E(C − T1) = 0.22, has been
adopted. The division of [Fe/H] = -1 between metal-rich and metal-poor GCs has been
shown as a good split between the two metallicity populations from [Fe/H] values converted
from C − T1 in Woodley, Harris, & Harris (2005) and Harris et al. (2004) for NGC 5128. If
no C and/or T1 values are available for the cluster, it is classified as metal-rich or metal-poor
through a transformation from (U − B)o to [Fe/H] from Reed, Harris, & Harris (1994).
In Figure 1 we show the spatial distributions of all the GCs from Table 1 (left) and the
distribution of the known PNe (right). Both systems are spatially biased to the major axis
of the galaxy because this is where most of the GC and PN searches have concentrated.
3. Kinematics of the Globular Cluster System
3.1. Velocity Field
For the present discussion we adopt a distance of 3.9 Mpc for NGC 5128. This value is
based on four stellar standard candles that each have internal precisions near ±0.2 mag: the
PN luminosity function, the tip of the old-halo red giant branch, the long-period variables,
– 9 –
and the Cepheids (Harris et al. 1999; Rejkuba 2004; Ferrarese et al. 2006).
HCH15 and R122 have not been included in our kinematic study, as our study was
completed before publication of these velocities. The weighted velocities used in this kine-
matic study do not include the most recent 25 velocities of previously known GCs published
in Rejkuba et al. (2007). Note that the velocities published in Table 1 do, however, in-
clude the Rejkuba et al. (2007) velocities in the quoted final weighted radial velocities for
completeness.
The velocity distribution of the entire sample of 340 is shown in Figure 2 (top left),
binned in 50 km s−1 intervals. A fit with a single Gaussian yields a mean velocity of 546± 7
km s−1, nicely matching the known systemic velocity of 541 ± 7 km s−1 (Hui et al. 1995).
There is a slight asymmetry at the low-velocity end that is likely due to contamination by
a few metal-poor Milky Way halo stars (also seen in the metal-poor subpopulation in the
bottom left panel, which has a mean velocity determined by the Gaussian fit as 532±13 km
s−1).
Selecting the clusters with radial velocity uncertainties less than 50 km s−1 leaves 226
clusters, plotted in Fig. 2 (top right). The close fit to a single Gaussian is consistent with
an isotropic distribution of orbits; the mean velocity is 554 ± 5 km s−1. The metal-rich
population, with a mean velocity determined by the Gaussian fit of 565 ± 11 km s−1, is
plotted in the bottom right panel, and also shows no strong asymmetries.
Looking closer at the metal-poor velocity asymmetry, we note that the 15 metal-poor
clusters between 250 and 300 km s−1 (in the region where contamination by Milky Way
field stars could occur) are balanced by only two GCs at the high-velocity end on reflec-
tion across the systemic velocity. The same velocity regions in the metal-rich population
are nearly equally balanced with four clusters between 250 and 300 km s−1 with three clus-
ters at the reflected high-velocity range. Interestingly, the four metal-rich clusters between
250 and 300 km s−1 have projected radii > 17 kpc even though the metal-rich popula-
tion is more centrally concentrated than the metal-poor (see Peng, Ford & Freeman 2004c;
Woodley, Harris, & Harris 2005, among others). The metal-poor clusters between 250 and
300 km s−1, conversely, are more evenly distributed, with five clusters between projected
radii of 5 and 10 kpc, five clusters between 10 and 20 kpc, and five clusters beyond 20 kpc
from the center of NGC 5128. Some of these low-velocity, metal-poor objects could be fore-
ground stars with velocities in the realm of GCs in NGC 5128 (vr & 250 km s
−1). However,
with only 340 GCs currently confirmed within ∼ 45’ from the center of NGC 5128, out of
an estimated ≃ 1500 total clusters within 25’ (Harris et al. 2006), these metal-poor, low-
velocity objects could simply be part of a very incomplete GC sample that is also spatially
biased. This potential bias is clearly shown in Figure 3, which shows the projected radial
– 10 –
distribution as a function of azimuthal angle for our GC sample. Beyond 12 kpc, the two
”voids” coincide with the photometric minor axis of the galaxy, attributed at least partly to
incomplete cluster surveys in these regions. These objects should, therefore, not be dropped
from the GC catalog without further spectroscopic analysis.
3.2. Rotation Amplitude, Rotation Axis, and Velocity Dispersion
3.2.1. Mathematic and Analytic Description
We determine the rotation amplitude and axis of the GCS of NGC 5128 from
vr(Θ) = vsys + ΩRsin(Θ − Θo) (1)
(see Côté et al. 2001; Richtler et al. 2004; Woodley 2006). In Equation 1, vr is the observed
radial velocity of the GCs in the system, vsys is the galaxy’s systemic velocity, R is the
projected radial distance of each GC from the center of the system assuming a distance
of 3.9 Mpc to NGC 5128, and Θ is the projected azimuthal angle of the GC measured in
degrees east of north. The systemic velocity of NGC 5128 is held constant at vsys = 541
km s−1 (Hui et al. 1995) for all kinematic calculations. The rotation axis of the GCs, Θo,
and the product ΩR, the rotation amplitude of the GCs in the system, are the values
obtained from the numerical solution. We use a Marquardt-Levenberg non-linear fitting
routine (Press et al. 1992).
Eqn. 1 assumes spherical symmetry. While this may be a decent assumption for the
inner 12 kpc region (it has a low ellipticity of ∼ 0.2; Peng, Ford & Freeman 2004b), true
ellipticities for the outer regions of the system are not well known because of the sample bias
(see Fig. 3). Future studies to remove these biases are vital to obtaining a sound kinematic
solution for the entire system. Eqn. 1 also assumes that Ω is only a function of the projected
radius and that the rotation axis lies in the plane of the sky. It is not entirely clear how these
assumptions, discussed thoroughly in Côté et al. (2001), apply to the GC and PN systems
of NGC 5128. The Ω we solve for is, therefore, only a lower limit to the true Ω if the true
rotation axis is not in the plane of the sky.
The projected velocity dispersion is also calculated from the normal condition,
σ2v =
(vfi − vsys)
where N is the number of clusters in the sample, vfi is the GC’s radial velocity after sub-
traction of the rotational component determined with Eqn. 1, and σv is the projected velocity
dispersion.
– 11 –
The GCs were assigned individual weights in the sums that combine in quadrature the
individual observational uncertainty, εv, in vr and the random velocity component, εrandom, of
the GCS. The dominance of the latter is evident by the large dispersion in the GC velocities
in the kinematic fitting (see Figure 4). In other words, the clusters have individual weights,
ωi = (ε
v + ε
random)
−1; the main purpose of this is to assign a bit more importance to the
clusters with more securely measured velocities. This random velocity term dominates in
nearly every case, leaving the GCs with very similar base weights in the kinematic fitting.
The three kinematic parameters - rotation amplitude, rotation axis, and velocity disper-
sion - are determined with three different binning methods. The first involves binning the
GCs in radially projected circular annuli from the center of NGC 5128. The chosen bins keep
a minimum of 15 clusters in each, ranging as high as 124 clusters. The bins are 0-5, 5-10,
10-15, 15-25, and 25-50 kpc. Also, we include 0-50 kpc to determine the overall kinematics
of the system.
The second method adopts bins with equal numbers of clusters. The entire population
of clusters had nine bins of 38 clusters each, the metal-poor clusters had nine bins of 20
clusters, and the metal-rich clusters had eight bins of 20 clusters. The base weighting is
applied to the clusters in both the first and second binning methods.
The third method uses an exponential weighting function, outlined in Bergond et al.
(2006), to generate a smoothed profile. This method determines each kinematic parameter
at the radial position, R, of every GC in the entire sample by exponentially weighting all
other GCs surrounding that position based on their radial separation, R− Ri, following
wi(R) =
−(R − Ri)
]. (3)
In Equation 3, wi is the determined weight on each GC in the sample, and σR is the
half-width of the window size. For this study, σR is incrementally varied in a linear fashion
for the total sample from σR = 1.0 kpc at the radius of the innermost GC in the sample
out to σR = 4.5 kpc at the radius of the outermost GC, where the population is lowest.
The metal-poor population was given a half-width window of σR = 1.0 − 6.5 kpc, and the
metal-rich population was given a half-width window of σR = 2 − 5.3 kpc, again from the
innermost to outermost cluster. The progressive radial increase in σR ensured that each
point R had roughly equal total weights.
– 12 –
3.2.2. Rotation Amplitude of the Globular Cluster System
The kinematic parameters were determined for the entire sample of 340 GCs, as well as
the subpopulations of 178 metal-poor and 158 metal-rich GCs (four clusters have unknown
metallicity). The kinematic results for the entire population of GCs are shown in Table 2,
reproduced almost in full from Woodley (2006), while the results for the metal-poor and
metal-rich clusters are shown in Tables 3 & 4, respectively. The columns give the radial bin,
the mean projected radius in the bin, the radius of the outermost cluster, the number of
clusters in the bin, the rotation amplitude, the rotation axis, and the velocity dispersion, with
associated uncertainties. These are followed by the mass correction, the pressure-supported
mass, the rotationally supported mass, and the total mass in units of solar mass (see § 5
for the mass discussion). The results for the alternate two methods, using an equal number
of GCs per bin and the exponentially weighted GCs, are not shown in tabular form but are
included in all of the figures.
Figure 4 shows the sine fit of Eqn. 1 for the total population and for the metal-poor
and metal-rich subpopulations. All three populations show rotation about a similar axis.
As discussed in § 3.1, the metal-poor population has more members with low velocities
(Vr ≤ 300 km s
−1) than the metal-rich population, suggesting possible contamination of
Milky Way foreground stars in the sample.
Figures 5 & 6 show the rotation amplitude results for the entire population and for
the metal-poor and metal-rich subpopulations, respectively. The three kinematic methods,
described in Section 3.2.1, appear to agree relatively well for all three populations of clusters.
While there appears to be no extreme difference in rotation amplitude between the cluster
populations, the metal-poor subpopulation of clusters has lower rotation in the inner 5 kpc
of NGC 5128 than the metal-rich subpopulation. The weighted average of the 0-5 kpc radial
bin and the innermost equal-numbered bin, shows that the entire population has a rotation
amplitude of ΩR = 31 ± 17 km s−1, while the metal-poor population has ΩR = 17 ± 26 km
s−1 and the metal-rich population has ΩR = 57±22 km s−1. Peng, Ford & Freeman (2004c)
show in their study that the metal-poor population has very little rotation in the central
regions, completely consistent with our findings. The rotation amplitude does not appear to
differ between the two populations outside of 5 kpc.
3.2.3. Rotation Axis of the Globular Cluster System
The results of the rotation axis solutions are shown in Figures 7 & 8, again for the
entire population and for the metal-poor and metal-rich subpopulations. The solution for
– 13 –
Θ0 agrees well for all three kinematic methods and all subgroups. The inner 5 kpc region
has a different rotation axis than the outer regions, demonstrated clearly in all three binning
methods. The innermost bin yields weighted averages of Θo = 369±24
o, Θo = 25±55
o, and
Θo = 352±18
o, all of which are equal within their uncertainties. Beyond 5 kpc, the rotation
axes for all three populations are in even closer agreement, with averages of Θo = 189 ± 6
Θo = 199 ± 7
o, and Θo = 196 ± 7
o for the entire population, the metal-poor subpopulation,
and the metal-rich subpopulation, respectively. The position angle of the photometric major
axis of NGC 5128 is Θ = 35o and 215o east of north and the photometric minor axis is
Θ = 119o and 299o east of north (Dufour et al. 1979). It appears the GCS is rotating about
an axis similar to the photometric major axis for the full extent of the galaxy, with a possible
axial twist or counterrotation within 5 kpc.
3.2.4. Velocity Dispersion of the Globular Cluster System
Figures 9 & 10 show the velocity dispersion for the entire population and for the metal-
poor and metal-rich subpopulations. Our results for σv show no significant differences be-
tween the metallicity subpopulations. All three show a relatively flat velocity dispersion
(σv = 119 ± 4, σv = 117 ± 6, and σv = 111 ± 6 km s
−1 within 15 kpc of the center of NGC
5128 for the entire population and for the metal-poor and metal-rich subpopulations, re-
spectively). These results match the previous study of NGC 5128 by Peng, Ford & Freeman
(2004c), whose determined velocity dispersion for the GCs within 20 kpc ranged between
75 and 150 km s−1. At a larger radius, we find that σv then slowly increases to σv > 150
km s−1 towards the outer regions of the halo for all populations. The velocity dispersion
of the metal-rich GCs, interestingly, appears higher than that of the metal-poor GCs in
the outer regions (although still consistent within the determined uncertainties). In most
previous studies, the velocity dispersion of the metal-poor GCs usually appears higher than
that of the metal-rich GCs, if there is a notable velocity dispersion difference between the
subpopulations (see the studies of Côté et al. 2003; Richtler et al. 2004, as examples).
To explore the cause of the distinct rise past 15 kpc a bit further, we have plotted
the actual velocity histograms in Figure 11 for the metal-poor and metal-rich subgroups,
subdivided further into inner (R < 15 kpc) and outer (R > 15 kpc) regions. In the inner 15
kpc, both samples show histograms strongly peaked near vf = 0 and with at least roughly
Gaussian falloff to both high and low velocities. By contrast, the histograms for the outer
regions (15−50 kpc) are noticeably flatter, so that the clusters with larger velocity residuals
have relatively more importance to the formal value of σv. Nominally, the flatter shape
of the velocity distribution would mean that the outer-halo clusters display anisotropy in
– 14 –
the direction of a bias towards more circular orbits. However, such a conclusion would be
premature at this point for two reasons. First, the sample size in the outer regions is still
too small to lead to high significance, and a direct comparison between the inner and outer
histograms (through a Kolmogorov-Smirnov test) does not show a statistically significant
difference between them larger than the 70% level. Second, the outer samples may still be
spatially biased in favor of objects along the major axis of the halo, as discussed above, and
this bias sets in strongly for R > 12 kpc (see Fig. 3), very near where we have set the radial
divisions in this Figure. This type of velocity distribution can also arise from the accretions
of satellite galaxies with their own small numbers of GCs (Bekki et al. 2003). We will need
to have a larger sample of the outer-halo clusters, and one in which these potential sample
biases have been removed, before we can draw any firmer conclusions. However, it needs to
be explicitly stated that the outermost point in the kinematic plots for the GCs representing
25 − 50 kpc suffers from very high spatial biases and low number statistics (< 40 GCs)
and covers a large radial interval. The rise in velocity dispersion could be driven purely by
systematic effects resulting from the radial gradient of the number density of GCs in this
outermost bin (Napolitano et al. 2001).
4. Kinematics of the Planetary Nebula System of NGC 5128
NGC 5128 has a large number, 780, of identified PNe with measured radial velocity from
the studies of Peng, Ford & Freeman (2004b) and Hui et al. (1995); these PNe are projected
out to 90 kpc assuming a distance to NGC 5128 of 3.9 Mpc. Since these are also old objects,
it is of obvious interest to compare them with the GCS. The PNe also have the advantage
of giving us the best available look at the kinematics of the halo field stars.
The PN kinematic results are listed in Table 5, with the same columns as Table 2. The
results are shown in Figures 5, 7, & 9 for the rotation amplitude, rotation axis, and velocity
dispersion, respectively. The spatial distribution of the known PNe is, like the GCS, biased
toward the major axis at large radii (see Fig. 1). Nevertheless, their kinematics closely
resemble the GCs.
The kinematics of the PN system are very consistent among all three binning methods.
The rotation amplitude and rotation axis show little radial trend, while the velocity disper-
sion appears relatively flat within the first 15 kpc at σv = 122 ± 7 km s
−1 and then slowly
decreases to σv ≃ 85 km s
−1 at large galactocentric radius. Peng, Ford, & Freeman (2004a)
show that the velocity dispersion of the PNe drops from a central value of 140 to 75 km s−1
in the outer regions of the galaxy, consistent with the findings of this study. Their velocity
field analysis led to the discovery of a ”zero-velocity curve” located between the photometric
– 15 –
minor axis, 119±5o east of north (Dufour et al. 1979), and the north-south direction, for the
innermost region of the galaxy. Just beyond 5 kpc, the zero-velocity curve turns and follows
a straight line at a 7o angle from the photometric major axis, 35o east of north (Dufour et al.
1979) (see Figure 7 of Peng, Ford & Freeman 2004c).
This study does not show a strong change in rotation axis for the PNe in the innermost
regions of the galaxy. However, it clearly shows in all three GC populations a significant
change in the rotation axis just beyond 5 kpc from the center of the galaxy. A change in
axis of 5 kpc outward (∼ 180o for the entire population and metal-poor subpopulation and
∼ 160o for the metal-rich subpopulation) has been found, as discussed in § 3.2.3. Similarly,
Peng, Ford & Freeman (2004c) show from their sample of 215 clusters that a clear sign
of rotation beyond 5 kpc about a misaligned axis appears particularly in their metal-rich
subpopulation. The kinematics of the GCs in this study matches the line of zero velocity
relatively nicely. Within 5 kpc the rotation axis of the GCS is nearly-parallel to the north-
south direction, and beyond 5 kpc the rotation axis is near 200o east of north, which is only
∼ 10o from the zero-velocity curve.
However, the velocity field of NGC 5128 is complex and not entirely captured by these
approximate solutions. The two-dimensional velocity field shown in Peng, Ford & Freeman
(2004b) (see their Figure 7), shows that the photometric major axis (which happens to be
very close to our maximum rotation as discussed above) is only 7o from the line of zero
velocity. This could lead to a very asymmetric velocity profile that may not be well fit by
the sine curve described in Equation 1. Biased kinematics, especially the rotation axis, may
develop from the sine fit that could lead to a higher estimated velocity dispersion.
Hui et al. (1995) similarly studied the kinematics of the PN system in NGC 5128 with
a sample of 433 PNe. They obtain a rotation axis of 344 ± 10o. Our result of 170 ± 5o
east of north is consistent with their findings on comparing their sine curve fit of their PN
data in their Figure 11 to our corresponding fit shown in Fig. 4 for the GCS, which shares a
similar axis to our PN sample (note that in their study, φ = 0o corresponds to our Θ = 305o
east of north). Our fits both correspond to a positive rotation amplitude for a rotation axis
near 170o east of north and a negative rotation axis near 350o east of north. Therefore,
the rotation axis quoted in Hui et al. (1995) of 344 ± 10o corresponds to a negative rotation
amplitude of approximately 70 − 75 km s−1 (taken from their Figure 11), nicely matching
our result of a positive 76 ± 6 km s−1 about an axis of 170 ± 5o east of north.
– 16 –
5. Dynamics of NGC 5128
Both GCs (Côté et al. 2001; Larsen et al. 2002; Evans et al. 2003; Côté et al. 2003;
Beasley et al. 2004; Peng, Ford & Freeman 2004c, among others) and PNe (Ciardullo et al.
1993; Hui et al. 1995; Arnaboldi et al. 1998; Peng, Ford & Freeman 2004b, among others)
can be used to estimate the total dynamical mass of their host galaxies. A variety of tools
are in use including derived mass models, the virial mass estimator (Bahcall & Tremaine
1981), the projected mass estimator (Heisler, Tremaine, & Bahcall 1985), and the tracer
mass estimator (Evans et al. 2003).
NGC 5128 does not have a large X-ray halo (detected by Kraft et al. 2003; O’Sullivan, Forbes, & Ponman
2001, the latter reporting a measurement of log Lx = 40.10 erg s
−1), such as is evident in
other giant ellipticals such as M87 (Côté et al. 2001) or NGC 4649 (Bridges et al. 2006).
Thus it is difficult to model the dark matter profile of NGC 5128 with a priori constraints.
Without such a mass model, we turn to the tracer mass estimator for the dynamical mass
determination. The tracer mass estimator has the distinct advantage over the virial and pro-
jected mass estimators that the tracer population does not have to follow the dark matter
density in the galaxy - an extremely useful feature for stellar subsystems such as GCs and
PNe that might, in principle, have significantly different radial distributions (see Evans et al.
(2003) for extensive discussion). Below, we determine the mass of NGC 5128 using the tracer
populations of GCs and PNe (our mass estimates do not include stellar kinematics in the
inner regions).
5.1. Mass Determination
The mass contributed by the random internal motion of the galaxy (pressure-supported
mass) is determined from the tracer mass estimator as
(vfi − vsys)
2Ri (4)
where N is the number of objects in the sample and vfi is the radial velocity of the tracer
object with the rotation component removed. For an isotropic population of tracer objects,
assumed in this study, the value of C is
4(α + γ)(4 − α− γ)(1 − ( rin
)(3−γ))
π(3 − γ)(1 − ( rin
)(4−α−γ))
where rin and rout are the three-dimensional radii corresponding to the two-dimensional
projected radii of the innermost, Rin, and outermost, Rout, tracers in the sample. The
– 17 –
parameter α is set to zero for an isothermal halo potential in which the system has a flat
rotation curve at large distances. Finally, γ is the slope of the volume density distribution,
which goes as r−γ, and is found by determining the surface density slope of the sample and
deprojecting the slope to three-dimensions. The tracer mass estimator uses a sample of tracer
objects defined between rin and rout, yet it is important to emphasize that it determines the
total enclosed mass within rout.
There is also a contribution to the total mass by the rotational component, as determined
in § 3.2.2 for the GCs and § 4 for the PNe. This mass component is determined from the
rotational component of the Jeans equation,
Routv
where Rout is the outermost tracer projected radius in the sample and vmax is the rotation
amplitude. Therefore, the total mass of NGC 5128, Mt, is determined by the addition of the
mass components supported by rotation, Mr, and random internal motion, Mp,
Mt = Mp + Mr. (7)
In the determination of the pressure-supported mass, one must estimate values for rin
and rout knowing Rin and Rout. Evans et al. (2003) suggest that rin ≃ Rin and rout ≃
Rout for distributions taken over a wide angle. However, in this study the inner and outer
radii of the chosen bins are at intermediate radial values within the distribution. Their
assumption would therefore lead to an underestimate of the determined mass, since the
true rout can be quite a bit larger than the projected Rout. To correct for this contributed
uncertainty, distributions of sample tracer populations were generated through Monte Carlo
simulations. In the simulations, 340 GCs were randomly placed in a spherically symmetric
system extending out to 50 kpc with an r−2 projected density, while 780 PNe were placed
in the same environment extending out to 90 kpc. From the generated distributions, the
value of C in Eqn. 5 was determined for both the real and projected positions of the tracer
populations in each designated radial bin. This correction factor, listed in Tables 3-5 as Mcorr,
multiplies the pressure-supported mass from Eqn. 4. The same correction was applied to the
full GC sample and the corresponding Mcorr values are listed in Table 1 of Woodley (2006).
These values are generally small, but in the worst case they triple Mp.
5.2. Surface Density Profiles
In Eqn. 5, the value of γ is determined for the tracer populations by deprojecting
the slope of the surface density profile to three-dimensions. Figure 12 shows the surface
– 18 –
density profiles for the entire, metal-poor, and metal-rich GC populations, along with the
PN profile. The populations were binned, following Máız Apellániz & Úbeda (2005), into
circular annuli of equal numbers of objects, providing the same statistical weight to each bin
(although spatial biases may still affect the GC population in the outer regions along the
major axis; see Fig. 3). In the inner 5 kpc of all tracer populations, incompleteness due to the
obscuration of the dust lane is evident by the flattening of the surface density profile. The
innermost objects were, therefore, excluded from the surface density profile fittings. Outside
of 5 kpc, the surface densities fit well to power laws, leading to γ = 3.65 ± 0.17, 3.49 ± 0.34,
3.37 ± 0.30, and 3.47 ± 0.12 for the entire GC population, the metal-poor and metal-rich
subpopulations of GCs, and the PNe in NGC 5128, respectively. These are all very similar
within their uncertainties.
5.3. Mass Results
The similar kinematics we find between the metal-poor and metal-rich subpopulations
of GCs in this study strongly justifies the combining of the two populations for the mass
determination performed in Woodley (2006). The GC population provides a total mass
estimate of (1.3 ± 0.5) × 1012 M⊙ from 340 clusters out to a projected radius of 50 kpc.
Removing the GCs in our sample with vr ≤ 300 km s
−1, which will remove all possible
contamination from foreground stars, discussed in § 3.1, leads to a total mass of (1.0±0.4)×
1012 M⊙. This mass agrees nicely with our mass determined from our entire GC sample.
The PN population provides a total mass of (1.0 ± 0.2) × 1012 M⊙ from 780 PNe out to 90
kpc in projected radius, agreeing with the GC value within the uncertainty.
We are also able to generate a mass profile of NGC 5128 from the total GC population
and the PNe, shown in Figure 13. The tracer mass estimator determines the total enclosed
mass for NGC 5128 within the outermost radius of a given tracer sample. It calculates this
total mass using a sample of objects defined within the radial range defined by the sample’s
inner and outermost radii. It is therefore possible to use a unique set of tracer objects,
denoted by the radial bin range, listed in the first column of Tables 2-5, to determine a mass
profile from independent mass estimates. The independent binning, leads to sample sizes in
the mass determination, in some cases generating higher uncertainties in the total enclosed
mass. The most certain mass is the one determined from the full sample of tracers.
In the mass determinations above, we have implicity assumed isotropy for the veloc-
ity distributions. But the possibility exists that the PNe (for example) might have radial
anisotropy which would produce their gradually falling σv(R) curve. Replacing Equation 5
– 19 –
in the tracer mass estimator by
16(α + γ − 2β)(4 − α− γ)(1 − ( rin
)(3−γ))
π(4 − 3β)(3 − γ)(1 − ( rin
)(4−α−γ))
which includes the anisotropy parameter, β, from Evans et al. (2003), we find that the mass
estimate from the PNe can be forced to agree with the mass estimate from the GCS for a
nominal β = 0.8. For perfect isotropy, β = 0. This would mean roughly 2:1 radial anisotropy
for the PNe in the outer halo. However, we find that any β in the wide range of −10 ≤ β ≤ 1
would still keep the two methods in agreement within their internal uncertainties, so we are
not yet in a position to tightly constrain any anisotropy. It is possible that the GCs may also
have anisotropy; it may therefore be too simplistic to find a range of β for the PNe for which
the masses of the PNe and GCs agree. However, the GCs are likelier to be nearly isotropic
than the PNe; the GCs are older, ”hotter” subsystems of the halo. In other studies, the
isotropy of the GCS orbits has also been shown to be a good assumption from mass profiles
of elliptical galaxies using X-ray observations (Côté et al. 2001, 2003; Bridges et al. 2006,
among others).
Both mass estimates can be compared to previous studies. First, we note the total
mass determined from the PN data with that of Peng, Ford & Freeman (2004b). While the
rotationally supported mass was determined here with different values of the mean rota-
tional velocity, they calculated the pressure supported mass using the identical tracer mass
estimator technique with exactly the same PN population. The total mass estimate given
by Peng, Ford & Freeman (2004b) is (5.3 ± 0.5) × 1011 M⊙. Subtracting their rotationally
supported mass leaves a pressure supported mass of ∼ 3.4×1011 M⊙, quite different from our
(8.46±1.72)×1011 M⊙. Recalculating our pressure supported mass estimate with γ = 2.54,
which was used in Peng, Ford & Freeman (2004b), we are able to reproduce their mass esti-
mate within the uncertainty. The values of γ differ between the two studies simply because
the γ used in Peng, Ford & Freeman (2004b) was the inverse of the surface density slope
instead of the inverse of the volume density slope. Using the correct value of γ = 3.54, their
pressure supported mass estimate would increase to 8.7× 1011M⊙, matching the mass found
in this study.
Second, we compare our total mass determined using the GC population with that from
Peng, Ford & Freeman (2004c). Using 215 GCs out to 40 kpc, they found a pressuresup-
ported mass of (3.4±0.8)×1011 M⊙, again much different from our pressure supported mass
of (1.26 ± 0.47) × 1012 M⊙ using 340 clusters out to 50 kpc. The large difference can again
be attributed to their using γ = 2.72 instead of deprojecting their surface density slope to
γ = 3.72. Using the correct value of γ, we find a pressure-supported mass of 7.5 × 1011 M⊙
using the same 215 clusters they used in their study. This corrected estimate is closer to the
– 20 –
pressure supported mass determined in our study, but it is not necessarily expected to agree
with our result, as our sample contains 130 more GCs and uses a slightly different γ that we
have independently redetermined.
Third, the mass determined by the H I shell study of NGC 5128 by Schiminovich et al.
(1994) found a mass of 2×1011 M⊙ within 15 kpc assuming a distance of 3.5 Mpc. With the
distance of 3.9 Mpc used in this study, the mass determined in their study would increase
to 2.2 × 1011 M⊙, which is 30% smaller than our total mass of 3.89± 0.94× 10
11 M⊙ within
15 kpc.
Lastly, we compare our determined mass to a recent study by Samurović (2006). Samurović
(2006) determined a total mass of NGC 5128 using GCs, PNe, and an X-ray data tech-
nique. The galaxy mass determined from the GC and PN data was obtained using the
tracer mass estimator and the spherical Jeans equation, as performed in our study. How-
ever, Samurović (2006) used the volume density slopes determined by Peng, Ford & Freeman
(2004b) and Peng, Ford & Freeman (2004c), for the PN and GC data, respectively. They ob-
tained mass estimates for NGC 5128 similar to those of Peng, Ford & Freeman (2004b) and
Peng, Ford & Freeman (2004c), discussed above, using an identical PN sample and slightly
increased GC sample. They also included an X-ray-modelling mass estimate for NGC 5128
from which they obtained masses of (7.0± 0.8)× 1011 M⊙ out to 50’ and (11.6± 1.0)× 10
M⊙ out to 80’. This mass estimate is similar to our PNe estimate out to the same radial
extent, but the author cautions that it is an overestimate of the true mass of NGC 5128
resulting from a lack of hydrostatic equilibrium in the outer region of the galaxy.
We note here that the mass estimates obtained are higher than those from Hui et al.
(1995), and Peng, Ford & Freeman (2004b) derived from the PNe using a two-component
mass model, as well as Samurović (2006), using an X-ray modelling technique. This dis-
crepancy is not fully understood and possibly lies in the assumptions that go into the mass
estimators with a spatially biased sample. We intend to pursue this issue further with an
upcoming larger sample of GCs with less spatial biases.
The mass of NGC 5128 that we find appears to be in the range of other giant elliptical
galaxies, such as NGC 1399 (∼ 2 × 1012 M⊙ out to 50 kpc; Richtler et al. 2004), M49
(∼ 2 × 1012 M⊙ out to their kinematically studied radius of 35 kpc; Côté et al. 2003), and
M87 (∼ 9 × 1011 M⊙ at 20 kpc, the onset of the projected cD envelope; Côté et al. 2001).
Clearly, it is legitimate to say that NGC 5128 is the largest, most massive galaxy in the
neighborhood of the Local Group, and one that can be talked about in the same category
as these other giants that reside in larger clusters.
The sample biases mentioned above in our currently available set of both GCs and PNe
– 21 –
place limitations on how much we can reasonably interpret the kinematic and dynamic data.
We are currently carrying out a set of new spectroscopic programs to increase the tracer
sample size and to remove the sample biases, leading to a more complete analysis of the halo
velocity field.
6. Discussion and Conclusions
Angular momentum is an essential quantity for characterizing the sizes, shapes, and
formation of galaxies and is often represented as the dimensionless spin parameter,
J |E|1/2
GM5/2
where J is the angular momentum, E is the binding energy, and M is the mass of the
galaxy. The spin parameter is representative of a galaxy’s angular momentum compared
to the amount of angular momentum needed for pure rotational support: the lower the Λ-
value, the less rotation and rotational support within the galaxy. For an elliptical galaxy in
gravitational equilibrium, the spin parameter simplifies to Λ ∼ 0.3 < (ΩR/σv) > (Fall 1979),
yielding Λ = 0.10 with (ΩR/σv) = 0.33 for the entire population of GCs in NGC 5128.
Table 6 shows the spin parameter for four giant galaxies with large GCS kinematic
studies, M87, M49, NGC 1399, and NGC 5128. The table columns give the galaxy name, the
rotation amplitude, the projected velocity dispersion, and the ratio of the rotation amplitude
to the velocity dispersion, followed by the spin parameter. These quantities are shown for
the metal-poor and metal-rich populations. What is clearly evident in Table 6 is the strong
galaxy to galaxy differences between these four galaxies, already hinted at in § 1. Though the
sample is still quite small, no obvious pattern emerges. There is an indication of metal-poor
and metal-rich GCSs having similar spin parameters within the same galaxy. M49 is the only
galaxy studied here where this may not be the case. Although the metal-poor and metal-rich
cluster spin parameters are consistent within the uncertainties, the metal-rich cluster spin
parameter of M49 is also consistent with zero.
In the monolithic collapse scenario, Peebles (1969) describes the angular momentum
within the galaxy as attributed to the tidal torque transferred from neighbouring proto-
galaxies during formation. In this scenario, Efstathiou & Jones (1979) found that a spin
parameter of Λ = 0.06 for elliptical systems is expected from simulations of the collapse of
an isolated protogalactic cloud. But NGC 5128, among many other giant elliptical galaxies,
is not in isolation, and therefore not necessarily expected to reproduce such a low spin
parameter. Also, the internal rotation axis changes at 5 kpc are not easily explained with
– 22 –
only the monolithic collapse scenario. In the monolithic collapse model, the inner regions
would be expected to have more pronounced rotations. Yet all four of the galaxies with
major kinematic studies presented here do not show a higher rotational signal in the inner
regions. In fact, for NGC 1399, the outer region (R > 6′) indicates rotation in the metal-poor
population that is not evident in the inner regions. Also, a slightly lower rotational signal
is present in the inner regions of NGC 5128 for the metal-poor population than in the outer
regions.
Hierarchical clustering of cold dark matter also relies on angular momentum in a galaxy
being produced by gravitational tidal torques during the growth of initial perturbations.
Sugerman, Summers, & Kamionkowski (2000) have demonstrated that the tidal torque the-
ory predicts an increase in angular momentum during the collapse, and with time, the
increase in angular momentum slows. Accretion of satellites and/or merger events is there-
fore a possible culprit for moving the angular momentum outward, as major mergers of disks
and bulges suggest that angular momentum resides largely in the outer regions of the galaxy
(Barnes 1992; Hernquist 1993).
Alternatively, Vitvitska et al. (2002) examine the change in spin parameter in a scenario
where the angular momentum in a galaxy is built up by mass accretion. Their results show
that the spin parameter changes sharply in major merger events in the galaxy and steadily
decreases with small satellite accretion events. They also show that the spin parameter for a
galaxy with a major merger after a redshift of z = 3 should be notably larger than a galaxy
that did not undergo such a major merger. Their study obtains an average of Λ = 0.045
from ΛCDM N -body simulations for galaxies with halo masses of (1.1 − 1.5) × 1012h−1 M⊙
with h = 0.7.
NGC 1399 and M49, with their weak rotation signals, are consistent with the model
predictions discussed above, whereby their major formation events could have occurred at
early times and with perhaps only minor accretions happening since then. However, NGC
5128 and M87 have spin parameters 2-3 times larger than predicted by the model averages.
For NGC 5128, this relatively large rotation (which is nearly independent of both metallicity
and radius) may, perhaps, be connected with its history within the Centaurus group envi-
ronment. The rotation speed and rotation axis for its extended group of satellite galaxies
are nearly identical to the NGC 5128 halo (Woodley 2006), much as if the accretion events
experienced by the central giant have been taking place preferentially along the main axis
of the entire group and in the same orientation. The GCS age distribution discussed by
Beasley et al. (2006) and the mean age for the halo field stars (Rejkuba et al. 2005) strongly
suggest that a high fraction of the stellar population in NGC 5128 formed long ago, with
particularly large bursts between 8 and 12 Gyr. Even if the galaxy underwent a significant
– 23 –
merger perhaps a few Gyr ago (the traces of which now appear in the halo arcs and shells),
the stars in it may already have been old at the time of the merger. Although a very few
younger GCs have formed since then, these make up a small minority of what is present, at
least for the R > 5 kpc halo outside the bulge region that now contains gas and dust.
The situation for M87, with its even larger rotation signature, may require a different
sort of individual history. Of the four galaxies compared here, it is at the dynamical center
of the richest environment (Virgo), has the most extensive cD-type envelope, and sits within
the most massive, extended, and dynamically evolved potential well. A single relatively
recent major merger could in principle have caused its present high rotation, but the lack of
distinctive tidal features does not necessarily favor such an interpretation and would at least
suggest that such a merger should have been with another large elliptical and nondissipative
galaxy. Côté et al. (2001) discuss an interpretation - at least partially resembling what we
suggest for NGC 5128 - that stellar material ”is gradually infalling onto M87 along the
so-called principal axis of the Virgo Cluster.”
In conclusion, we have presented a kinematic study of NGC 5128 that makes it now com-
parable to recent studies of the other giant galaxies, M87, M49, and NGC 1399. Using 340
GCs (158 metal-rich and 178 metal-poor GCs), we have calculated the rotation amplitude,
rotation axis, and velocity dispersion and have searched for radial and metallicity depen-
dences. Our findings show that both metallicity populations rotate with little dependence
on projected radius, with ΩR = 40±10, 31±14, and 47±15 km s−1 for the total, metal-poor,
and metal-rich populations, respectively. Perhaps the inner 5 kpc shows a slower rotation of
the metal-poor population, but more clusters would be needed to confirm this finding. The
rotation axis is 189±12o, 177±22o, and 202±15o east of north for the total, metal-poor, and
metal-rich populations out to a 50 kpc projected radius, assuming the velocity field is best
fit by a sine curve. The rotation axis does change at 5 kpc, following the zero-velocity curve
proposed by Peng, Ford & Freeman (2004b) or possibly full-on counterrotation. A study
with more GCs and lower uncertainties is needed to see what is happening in the innermost
5 kpc of NGC 5128. The velocity dispersion shows a modest increase with galactocentric
radius, although the outer regions (especially the metal-rich population) have less reliable
statistics; this increase could be driven purely by statistical effects. We find the velocity dis-
persion we find 123±5, 117±7, and 129±9 km s−1 for the total, metal-poor, and metal-rich
populations, respectively.
The PN data are also used to determine the kinematics of the halo of NGC 5128.
These show results that are encouragingly similar to those of the GC data, except that no
rotation axis change is noted with radius, and a decrease in velocity dispersion is found with
radius, possibly indicating a difference in orbital anisotropy compared with the GCs. A
– 24 –
very similar effect has been noted for the Leo elliptical NGC 3379, although with a much
smaller data sample (Romanowsky et al. 2003; Bergond et al. 2006; Pierce et al. 2006). We
also determine the total dynamical mass using both the GCs and the PNe by separately
calculating the pressure supported mass with the tracer mass estimator and the rotationally
supported mass using the spherical component of the Jeans equation. The total mass is
(1.3 ± 0.5) × 1012 M⊙ from the GC population out to a projected radius of 50 kpc, or
(1.0 ± 0.2) × 1012 M⊙ out to 90 kpc from the PNe.
Overall, we have enough evidence to cautiously conclude that a major episode of star
formation occurred about 8−10 Gyr ago (corresponding to a redshift z = 1.2 - 1.8) and this
may have been when the bulk of the visible galaxy was built. We still do not know just why
the most metal-poor clusters show up in such relatively large numbers and appear to have
ages of 10 − 12 Gyr, but this is a common issue in all big galaxies.
This kinematic study and the age study of Beasley et al. (2006) on the NGC 5128
cluster system indicate that additional spectroscopic studies to build up both the radial
velocity database and age distribution can lead to rich dividends. Large GC samples are
clearly needed to remove the current sample biases and to fully understand the complex
kinematics and history of this giant elliptical galaxy. It seems clear as well that each galaxy
needs to be individually studied to fully understand the different galaxy formation histories.
We are continuing these studies particularly for NGC 5128, with the eventual aim of at least
doubling the total GC sample size in this unique system.
Acknowledgements: WEH and GLHH acknowledge financial support from NSERC
through operating research grants. DAF thanks the ARC for financial support.
– 25 –
REFERENCES
Arnaboldi, M., Freeman, K.C., Capaccioli, M., & Ford, H. 1994, ESO Messanger, 76, 40
Arnaboldi, M., Freeman, K.C., Gerhard, O., Matthias, M., Kudritzki, R.P. Méndez, R.H.,
Capaccioli, M., & Ford, H. 1998, ApJ, 507, 759
Baade, W., & Minkowski, R. 1954, ApJ, 119, 215
Bahcall, J.N., & Tremaine, S. 1981, ApJ, 244, 805
Barnes, J.E. 1992, ApJ, 393, 484
Beasley, M.A., Forbes, D.A., Brodie, J.P., & Kissler-Patig, M. 2004, MNRAS, 347, 1150
Beasley, M.A., Bridges, T., Peng, E., Harris, W.E., Harris, G.L.H., Forbes, D.A., & Mackie,
G. 2006, in preparation
Bekki, K., Harris, W.E., & Harris, G.L.H. 2003, MNRAS, 338, 587
Bekki, K., Forbes, D.A., Beasley, M.A., & Couch, W.J. 2003, MNRAS, 334, 1334
Bekki, K., & Peng, E.W. 2006, MNRAS, 370, 1737
Bergond, G., Zepf, S.E., Romanowsky, A.J., Sharples, R.M., & Rhode, K.L. 2006, A&A,
448, 155
Bridges, T., Gebhardt, K., Sharples, R., Faifer, F.R., Forte, J.C., Beasley, M.A., Zepf, Z.E.,
Forbes, D.A., Pierce, M. 2006, MNRAS, 373, 157
Ciardullo, R., Jacoby, G.H., & Dejonghe, H.B. 1993, ApJ, 414, 454
Côté, P., McLaughlin, D.E., Hanes, D.A., Bridges, T.J., Geisler, D., Merritt, D., Hesser,
J.E., Harris, G.L.H., & Lee, M.G. 2001, ApJ, 559, 828
Côté, P., McLaughlin, D., Cohen, J.G., & Blakesless, J.P. 2003, ApJ, 591, 850
Dekel, A., Stoehr, F., Mamon, G.A., Cox, T.J., Novak, G.S., & Primak, J.R., 2005, Nature,
437, 707
Dufour, R.J., Harvel, C.A., Martins, D.M., Schiffer, F.H., Talent, D.L., Wells, D.C., van den
Bergh, S., & Talbot, R.J. 1979, AJ, 84, 284
Efstathiou, G., & Jones, B.J.T. 1979, MNRAS, 186, 133
– 26 –
Evans, N.W., Wilkinson, M.I., Perrett, K.M., & Bridges, T.J. 2003, ApJ, 583, 752
Fall, S.M. 1979, Rev. Mod. Phys., 51, 21
Ferrarese, L., Mould, J.R., Stetson, P.B., Tonry, J.L., Blakeslee, J.P., & Ajhar, E.A. 2006,
ApJ, in press (astro-ph/0605707)
Harris, G.L.H., Geisler, D., Harris, H.C., & Hesser, J.E. 1992, AJ, 104, 613
Harris, G.L.H., Harris, W.E., & Poole, G. 1999, AJ, 117, 855
Harris, W. E., & Harris, G. L. H. 2002, AJ, 123, 3108
Harris, W.E., Harris, G.L.H., Holland, S.T., & McLaughlin, D.E. 2002, AJ, 124, 1435
Harris, G.L.H., Harris, W.E., & Geisler, D. 2004, AJ, 128, 723
Harris, W.E., Harris, G.L.H., Barmby, P., McLaughlin, D.E., & Forbes, D. 2006, AJ, 132,
Heisler, J., Tremaine, S., & Bahcall, J.N. 1985, ApJ, 298, 8
Hernquist, I. 1993, ApJ, 409, 548
Hesser, J.E., Harris, H.C., van den Bergh, S., & Harris, G.L.H. 1984, ApJ, 276,491
Hesser, J.E., Harris, H.C., & Harris, G.L.H. 1986, ApJ, 303, L51
Hui, X., Ford, H.C., Freeman, K.C., & Dopita, M.A. 1995, ApJ, 449, 592
Kraft, R.P., Váquez, S.E., Forman, W.R., Jones, C., Murray, S.S., Hardcastle, M.J., Worrall,
D.M., Churazov, E. 2003, ApJ, 592, 129
Larsen, S.S., Brodie, J.P., Beasley, M.A., & Forbes, D.A. 2002, AJ, 124, 828
Lee, H., & Worthey, G. 2005, ApJS, 160, 176
Máız Apellániz, J. & Úbeda, L. 2005, ApJ, 629, 7873
Mamon, G.A., &  Lokas, E.L. 2005, MNRAS, 362, 95
Napolitano, N.R., Arnaboldi, M., Freeman, K.C., & Capaccioli, M. 2001, A&A, 377, 784
Napolitano, N.R., Arnaboldi, M., & Capaccioli, M. 2002, A&A, 383, 791
O’Sullivan, E., Forbes, D.A., & Ponman, T.J. 2001,MNRAS, 328, 461
http://arxiv.org/abs/astro-ph/0605707
– 27 –
Peebles, P.J.E. 1969, ApJ, 155, 393
Peng, E.W., Ford, H.C., Freeman, K.C., & White, R.L. 2002, AJ, 124, 3144
Peng, E.W., Ford, H.C., & Freeman, K.C. 2004, ApJS, 150, 367
Peng, E.W., Ford, H.C., & Freeman, K. 2004, ApJ, 602, 685
Peng, E.W., Ford, H.C., & Freeman, K. 2004, ApJ, 602, 705
Pierce, M., Beasley, M.A., Forbes, D.A., Bridges, T., Gebhardt, K., Faifer, F.R., Forte, J.C.,
Zepf, S.E., Sharples, R., Hanes, D.A., & Proctor, R. 2006, MNRAS, 366, 1253
Press, W.H., Teukolsky, S.A., Vetterling, W.T., & Flannery, B.P. 1992, Numerical Recipes
in Fortran (2nd Ed., Cambridge: Camdridge University Press)
Puzia, T.H., Kissler-Patig, M., Thomas, D., Maraston, C., Saglia, R.P., Bender, R., Goud-
frooij, P., & Hempel, M. 2005, A&A, 439, 997
Reed, L.G., Harris, G.L.H., & Harris, W.E. 1994, AJ, 107, 555
Rejkuba, M. 2001, A&A, 269, 812
Rejkuba, M. 2004, A&A, 413, 903
Rejkuba, M., Greggio, L., Harris, W.E., Harris, G.L.H., & Peng, E.W. 2005, ApJ, 631, 262
Rejkuba, M., Dubath, P., Minniti, D., & Meylan, G. 2007, A&A, in press (astro-ph/0703385)
Richtler, T., Dirsch, B., Gebhardt, K., Geisler, D., Hilker, M., Alonso, M. V., Forte, J. C,.
and Grebel, E. K., Infante, L., Larsen, S., Minniti, D., & Rejkuba, M. 2004, AJ, 127,
Romanowsky, A.J., Douglas, N.G., Arnaboldi, M., Kuijken, K., Merrifield, M.R., Napolitano,
N.R., Capaccioli, M., & Freeman, K.C., 2003, Science, 301, 1696
Saglia, R.P., Kronawitter, A., Gerhard, O., & Bender, R. 2000, AJ, 119, 153
Samurović, S. 2006, Serb. Astron. J., 173, 35
Schiminovich, D., van Gorkom, J.H., van der Hulst, J.M., & Kasow, S. 1994, ApJ, 423, L101
Sharples, R. 1988, IAU Symp. 126: The Harlow-Sharpley Symposium on Globular Cluster
Systems in Galaxies, 126, 245
http://arxiv.org/abs/astro-ph/0703385
– 28 –
Strader, J., Brodie, J.P., Cenarro, A.J., Beasley, M.A., & Forbes, D.A. 2005, AJ, 130, 1315
Sugerman, B., Summers, F.J., & Kamionkowski, M. 2000, MNRAS, 311, 762
Thomas, D., Maraston, C., & Korn, A. 2004, MNRAS, 351, 19
Toomre, A., & Toomre, J. 1972, ApJ, 178, 623
van den Bergh, S., Hesser, J.E., & Harris, G.L.H. 1981, AJ, 86, 24
Vitvitska, M., Klypin, A.A., Kravtsov, A.V., Wechsler, R.H., Primack, J.R., & Bullock, J.S.
2002, ApJ, 581, 799
Woodley, K.A., Harris, W.E., & Harris, G.L.H. 2005, AJ, 129, 2654
Woodley, K.A. 2006, AJ, 132, 2424
This preprint was prepared with the AAS LATEX macros v5.2.
Table 1. The Globular Cluster System Catalogue of NGC 5128
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0001 pff gc-028 13 20 01.16 -42 56 51.5 6.46 20.11 19.68 18.75 18.20 17.60 0.07 0.02 0.01 0.01 0.03 19.92 19.04 18.22 0.01 0.01 0.01 0.43 0.93 0.55 1.15 0.82 0.88 1.70 524±165
GC0002 HH-048 13 22 45.36 -43 07 08.8 30.26 - - - - - - - - - - - - - - - - - - - - - - - 856±507
GC0003 HH-080 13 23 38.33 -42 46 22.8 24.84 - - - - - - - - - - 19.45 18.72 17.98 0.02 0.01 0.01 - - - - 0.74 0.72 1.46 497±337
GC0004 HGHH-40/HH-044/C40 13 23 42.37 -43 09 37.8 21.02 19.37 19.01 18.12 17.59 17.03 0.04 0.01 0.01 0.01 0.03 20.12 19.28 18.49 0.02 0.01 0.01 0.35 0.89 0.53 1.10 0.79 0.84 1.63 365±244,5,7
GC0005 HGHH-01/C1 13 23 44.19 -43 11 11.8 21.41 - - - - - - - - - - 18.73 18.00 17.25 0.06 0.03 0.03 - - - - 0.76 0.72 1.48 642±11,5,7,8
GC0006 pff gc-001 13 23 49.62 -43 14 32.0 22.36 20.39 19.91 18.91 18.36 17.60 0.09 0.02 0.01 0.01 0.03 20.22 19.25 18.38 0.02 0.01 0.01 0.47 1.01 0.55 1.31 0.87 0.97 1.84 711±355,7
GC0007 AAT301956 13 23 54.52 -43 20 01.1 25.41 21.22 21.13 20.42 19.98 19.43 0.18 0.06 0.02 0.02 0.04 - - - - - - 0.09 0.71 0.44 0.98 - - - 287±1627
GC0008 HH-099 13 23 56.70 -42 59 59.8 16.66 - - - - - - - - - - 21.72 20.90 20.01 0.09 0.09 0.06 - - - - 0.89 0.82 1.71 798±497
GC0009 AAT101931 13 23 58.58 -42 57 17.0 16.73 20.58 20.57 19.88 19.43 18.96 0.06 0.02 0.01 0.01 0.03 20.60 20.09 19.45 0.01 0.01 - 0.02 0.68 0.45 0.92 0.64 0.51 1.15 590±1447
GC0010 AAT101906 13 23 58.76 -43 01 35.2 16.25 20.45 19.90 18.89 18.28 17.57 0.06 0.02 0.01 0.01 0.03 20.23 19.11 18.28 0.02 0.03 0.02 0.54 1.01 0.61 1.32 0.83 1.12 1.95 511±317
GC0011 pff gc-002 13 23 59.51 -43 17 29.1 22.94 20.70 20.43 19.55 19.02 18.44 0.07 0.02 0.01 0.01 0.03 20.61 19.83 19.07 0.03 0.03 0.01 0.27 0.88 0.53 1.11 0.76 0.78 1.55 653±375,7
GC0012 AAT102120 13 23 59.61 -42 55 19.4 17.11 20.60 20.59 19.92 19.49 19.03 0.06 0.02 0.01 0.01 0.03 20.61 20.13 19.49 0.01 0.01 0.01 0.02 0.67 0.44 0.89 0.64 0.48 1.12 293±837
GC0013 HH-001 13 24 02.67 -42 48 32.2 20.00 - - - - - - - - - - 22.52 21.20 19.89 0.08 0.05 0.03 - - - - 1.31 1.32 2.63 775±747
GC0014 pff gc-003 13 24 03.23 -43 28 13.9 31.17 20.39 20.18 19.31 18.80 18.21 0.15 0.02 0.01 0.01 0.03 20.39 19.64 18.80 0.02 0.02 0.02 0.21 0.87 0.51 1.09 0.84 0.76 1.59 704±225,7
GC0015 pff gc-004 13 24 03.74 -43 35 53.4 37.98 21.12 20.84 20.01 19.49 18.92 0.28 0.03 0.01 0.01 0.03 - - - - - - 0.28 0.83 0.52 1.09 - - - 571±385,7
GC0016 AAT103195 13 24 05.98 -43 03 54.7 15.18 21.57 21.10 20.13 19.58 18.98 0.14 0.03 0.01 0.01 0.03 21.34 20.39 19.50 0.01 0.01 0.01 0.47 0.97 0.56 1.15 0.89 0.95 1.84 277±677
GC0017 AAT30486710 13 24 08.62 -43 16 27.1 21.04 22.12 21.15 19.91 19.20 18.54 0.25 0.03 0.01 0.01 0.03 21.62 20.28 19.18 0.01 - - 0.97 1.24 0.71 1.36 1.10 1.34 2.44 305±567
GC0018 AAT305341 13 24 10.97 -43 12 52.8 18.27 22.13 21.54 20.51 19.88 19.19 0.23 0.04 0.01 0.01 0.03 21.87 20.80 19.90 0.01 0.01 0.01 0.59 1.03 0.63 1.31 0.89 1.07 1.97 440±1187
GC0019 HHH86-28/C28 13 24 18.06 -42 49 01.1 17.57 19.52 19.33 18.50 17.99 17.45 0.03 0.01 0.01 0.01 0.03 19.46 18.75 18.03 0.02 0.01 0.01 0.19 0.83 0.52 1.05 0.72 0.71 1.43 461±223,5,7
GC0020 pff gc-005 13 24 18.92 -43 14 30.1 18.33 21.89 21.31 20.29 19.71 19.07 0.18 0.04 0.01 0.01 0.03 21.63 20.64 19.72 0.02 0.02 0.01 0.58 1.02 0.58 1.22 0.91 1.00 1.91 750±335,7
GC0021 WHH-1/HH-096 13 24 21.40 -43 02 36.8 12.19 19.14 18.85 18.01 17.48 16.98 0.03 0.01 0.01 0.01 0.03 19.11 18.33 17.63 0.02 0.02 0.03 0.29 0.84 0.53 1.03 0.70 0.78 1.48 583±296,7
GC0022 pff gc-006 13 24 23.72 -43 07 52.1 13.48 20.22 20.00 19.22 18.70 18.20 0.05 0.02 0.01 0.01 0.03 20.10 19.46 18.73 0.01 0.01 0.01 0.21 0.78 0.52 1.02 0.73 0.65 1.37 644±285,7
GC0023 WHH-2 13 24 23.98 -42 54 10.7 13.56 20.57 20.45 19.67 19.17 18.65 0.06 0.02 0.01 0.01 0.03 20.54 19.94 19.27 0.03 0.03 0.02 0.12 0.78 0.50 1.02 0.68 0.59 1.27 582±816
GC0024 pff gc-007 13 24 24.15 -42 54 20.6 13.45 21.85 21.16 20.12 19.53 18.82 0.17 0.03 0.01 0.01 0.03 21.54 20.50 19.60 0.02 0.02 0.01 0.69 1.04 0.59 1.30 0.90 1.04 1.94 617±255,7
GC0025 AAT308432 13 24 25.55 -43 21 35.6 23.38 20.98 20.43 19.40 18.80 18.11 0.27 0.02 0.01 0.01 0.03 20.83 19.78 18.84 0.03 0.01 0.02 0.54 1.04 0.60 1.29 0.94 1.05 1.99 835±837
GC0026 C111 13 24 26.97 -43 17 20.0 19.62 - - - - - - - - - - 22.54 22.25 21.36 0.04 0.04 0.04 - - - - 0.89 0.29 1.17 -
GC0027 AAT106695 13 24 28.18 -42 53 04.3 13.54 20.95 20.75 19.63 18.96 18.30 0.09 0.03 0.01 0.01 0.03 21.16 20.17 19.19 0.06 0.06 0.04 0.20 1.12 0.67 1.33 0.98 0.99 1.96 835±837
GC0028 AAT106880 13 24 28.44 -42 57 52.9 11.30 21.11 20.94 20.14 19.61 19.11 0.10 0.03 0.01 0.01 0.03 21.06 20.43 19.65 0.01 0.01 0.01 0.18 0.80 0.53 1.03 0.79 0.63 1.41 558±987
GC0029 pff gc-008 13 24 29.20 -43 21 56.5 23.38 21.40 20.93 19.94 19.41 18.75 0.35 0.03 0.01 0.01 0.03 21.24 20.31 19.43 0.02 0.01 0.01 0.47 0.99 0.54 1.19 0.87 0.93 1.81 466±385,7
GC0030 AAT107060 13 24 29.23 -43 08 36.6 13.02 21.81 21.26 20.26 19.63 19.00 0.19 0.04 0.01 0.01 0.03 21.60 20.62 19.69 0.01 0.01 0.01 0.55 1.01 0.63 1.25 0.93 0.99 1.92 600±587
GC0031 AAT107145 13 24 29.73 -43 02 06.5 10.62 21.20 20.93 20.08 19.50 18.97 0.11 0.03 0.01 0.01 0.03 21.16 20.33 19.55 0.03 0.02 0.04 0.27 0.85 0.58 1.11 0.78 0.82 1.60 595±2027
GC0032 pff gc-009 13 24 31.35 -43 11 26.7 14.55 20.82 20.58 19.77 19.25 18.70 0.07 0.02 0.01 0.01 0.03 20.73 20.05 19.26 0.03 0.02 0.01 0.23 0.81 0.52 1.07 0.80 0.68 1.47 683±385,7
GC0033 WHH-3 13 24 32.17 -43 10 56.9 14.10 20.56 20.32 19.49 18.97 18.43 0.06 0.02 0.01 0.01 0.03 20.46 19.76 18.99 0.02 0.02 0.01 0.25 0.83 0.52 1.06 0.76 0.71 1.47 709±546,7
GC0034 C112 13 24 32.66 -43 18 48.8 20.32 - - - - - - - - - - 22.98 22.22 21.31 0.03 0.02 0.02 - - - - 0.91 0.75 1.67 -
GC0035 pff gc-0109 13 24 33.09 -43 18 44.8 20.23 20.45 20.36 19.68 19.26 18.84 0.06 0.02 0.01 0.01 0.03 20.45 19.91 19.24 0.01 0.01 0.01 0.09 0.68 0.42 0.85 0.67 0.54 1.21 344±585
GC0036 AAT107977 13 24 34.63 -43 12 50.5 15.18 21.73 21.18 20.18 19.57 18.89 0.17 0.04 0.01 0.01 0.03 21.52 20.54 19.59 0.02 0.02 0.01 0.54 1.01 0.60 1.28 0.95 0.98 1.93 517±1237
GC0037 pff gc-011 13 24 36.87 -43 19 16.2 20.36 20.01 19.82 19.03 18.53 18.00 0.13 0.02 0.01 0.01 0.03 19.95 19.33 18.55 0.01 0.01 0.01 0.18 0.79 0.50 1.04 0.78 0.62 1.40 616±415,7
GC0038 C113 13 24 37.75 -43 16 26.5 17.80 - - - - - - - - - - 20.50 19.87 19.12 0.02 0.02 0.01 - - - - 0.75 0.63 1.38 -
GC0039 pff gc-012 13 24 38.77 -43 06 26.6 10.38 21.24 20.51 19.45 18.83 18.15 0.13 0.02 0.01 0.01 0.03 20.92 19.78 18.85 0.01 0.01 0.01 0.73 1.06 0.62 1.30 0.93 1.14 2.07 573±215
GC0040 HGHH-41/C41 13 24 38.98 -43 20 06.4 20.94 20.20 19.59 18.59 17.94 17.32 0.06 0.02 0.01 0.01 0.03 19.95 18.92 17.97 0.02 0.01 0.01 0.61 1.00 0.65 1.27 0.95 1.03 1.98 363±14,5,7,8
GC0041 HGHH-29/C29 13 24 40.39 -43 18 05.3 19.01 19.77 19.15 18.15 17.54 16.89 0.04 0.01 0.01 0.01 0.03 19.46 18.37 17.53 0.04 0.03 0.02 0.62 1.00 0.61 1.26 0.84 1.09 1.92 726±13,5,7,8
GC0042 pff gc-013 13 24 40.42 -43 35 04.9 35.01 20.06 19.83 19.00 18.49 17.98 0.15 0.02 0.01 0.01 0.03 - - - - - - 0.24 0.83 0.51 1.03 - - - 727±315,7
GC0043 C114 13 24 40.48 -42 53 35.3 11.46 - - - - - - - - - - 23.46 22.39 21.42 0.05 0.04 0.03 - - - - 0.97 1.07 2.04 -
GC0044 WHH-4/HH-024 13 24 40.60 -43 13 18.1 14.89 20.71 20.12 19.12 18.50 17.85 0.07 0.02 0.01 0.01 0.03 20.46 19.40 18.53 0.03 0.02 0.01 0.60 1.00 0.62 1.27 0.87 1.06 1.93 688±256,7
GC0045 pff gc-014 13 24 41.05 -42 59 48.4 8.62 21.60 21.17 20.23 19.67 18.94 0.26 0.06 0.02 0.02 0.03 21.47 20.56 19.76 0.04 0.03 0.04 0.43 0.94 0.57 1.30 0.80 0.91 1.71 690±345,7
GC0046 pff gc-015 13 24 41.20 -43 01 45.6 8.51 20.27 20.01 19.22 18.74 18.15 0.06 0.02 0.01 0.01 0.03 20.12 19.40 18.70 0.05 0.04 0.05 0.26 0.79 0.47 1.06 0.70 0.72 1.42 533±255,7
GC0047 AAT109380 13 24 43.58 -43 08 43.2 11.05 19.64 19.52 18.80 18.32 17.87 0.04 0.01 0.01 0.01 0.03 19.60 19.02 18.30 0.01 - - 0.12 0.73 0.48 0.93 0.72 0.59 1.31 465±387
GC0048 pff gc-016 13 24 43.60 -42 53 07.3 11.36 21.38 20.87 19.85 19.26 18.58 0.12 0.03 0.01 0.01 0.03 21.19 20.21 19.33 0.02 0.02 0.01 0.51 1.02 0.60 1.27 0.88 0.98 1.85 505±175,7
GC0049 pff gc-017 13 24 43.63 -42 58 16.4 8.54 20.54 20.32 19.51 18.99 18.47 0.07 0.02 0.01 0.01 0.03 20.44 19.78 19.01 0.01 0.01 0.01 0.22 0.81 0.52 1.04 0.77 0.66 1.43 963±505
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0050 WHH-5 13 24 44.58 -43 02 47.3 8.04 20.47 20.03 19.06 18.49 17.87 0.08 0.02 0.01 0.01 0.03 20.29 19.19 18.90 0.05 0.04 0.04 0.44 0.97 0.57 1.19 0.29 1.09 1.39 671±416
GC0051 HH-054 13 24 45.22 -43 23 19.2 23.49 - - - - - - - - - - 20.92 20.08 19.25 0.05 0.03 0.04 - - - - 0.82 0.84 1.66 998±2507
GC0052 AAT109711 13 24 45.35 -42 59 33.5 7.89 19.88 19.87 19.30 18.90 18.33 0.06 0.02 0.01 0.01 0.03 19.84 19.48 18.91 0.02 0.02 0.04 0.02 0.56 0.40 0.98 0.58 0.36 0.94 276±597
GC0053 AAT109788 13 24 45.78 -43 02 24.5 7.75 21.82 21.02 19.89 19.23 18.56 0.25 0.04 0.01 0.01 0.03 21.39 20.17 19.43 0.02 0.02 0.03 0.80 1.14 0.65 1.33 0.74 1.22 1.96 527±307
GC0054 HGHH-G019/G19 13 24 46.46 -43 04 11.6 8.12 20.16 19.95 19.16 18.64 18.13 0.06 0.02 0.01 0.01 0.03 20.06 19.38 18.64 0.04 0.03 0.03 0.21 0.79 0.52 1.03 0.75 0.67 1.42 710±224,5,7
GC0055 HGHH-09/C9 13 24 46.72 -43 01 18.4 7.48 20.00 19.76 18.95 18.40 17.90 0.05 0.02 0.01 0.01 0.03 19.87 19.13 18.42 0.04 0.04 0.04 0.24 0.81 0.56 1.05 0.70 0.74 1.45 501±214,5
GC0056 pff gc-018 13 24 47.10 -43 06 01.7 8.87 20.90 20.03 18.91 18.25 17.54 0.10 0.02 0.01 0.01 0.03 20.45 19.23 18.28 0.02 0.01 0.01 0.87 1.12 0.66 1.37 0.95 1.22 2.17 534±155,6,7
GC0057 HGHH-G277/G277 13 24 47.37 -42 58 29.8 7.82 20.26 19.96 19.10 18.56 18.02 0.06 0.02 0.01 0.01 0.03 20.14 19.37 18.61 0.01 0.01 0.01 0.30 0.87 0.53 1.08 0.76 0.77 1.53 714±334,5,7
GC0058 WHH-6 13 24 47.37 -42 57 51.2 8.06 21.33 20.75 19.73 19.12 18.44 0.15 0.03 0.01 0.01 0.03 21.08 20.07 19.15 0.01 0.01 0.01 0.58 1.02 0.62 1.29 0.93 1.00 1.93 685±436,7
GC0059 AAT110138 13 24 47.61 -43 10 48.5 12.12 20.87 20.53 19.67 19.11 18.57 0.10 0.03 0.01 0.01 0.03 20.75 19.98 19.16 0.03 0.02 0.01 0.34 0.87 0.56 1.10 0.82 0.77 1.59 358±1377
GC0060 HHH86-10/C10 13 24 48.06 -43 08 14.2 10.13 19.87 19.44 18.49 17.91 17.33 0.05 0.01 0.01 0.01 0.03 19.66 18.75 17.93 0.03 0.03 0.01 0.44 0.95 0.58 1.16 0.81 0.91 1.73 829±222,5,6,7
GC0061 C115 13 24 48.71 -42 52 35.5 11.12 - - - - - - - - - - 20.88 20.23 19.51 0.02 0.02 0.01 - - - - 0.73 0.65 1.37 -
GC0062 pff gc-019 13 24 48.97 -42 57 48.4 7.81 20.10 19.87 19.05 18.53 18.00 0.05 0.02 0.01 0.01 0.03 20.00 19.31 18.57 0.03 0.03 0.01 0.23 0.81 0.53 1.05 0.74 0.69 1.43 607±275
GC0063 AAT110410 13 24 49.38 -43 08 17.7 10.00 21.47 21.18 20.34 19.79 19.23 0.16 0.04 0.02 0.01 0.03 21.37 20.66 19.81 0.03 0.02 0.01 0.29 0.84 0.55 1.11 0.85 0.71 1.56 580±817
GC0064 AAT110551 13 24 50.09 -43 07 36.2 9.42 21.43 21.08 20.44 20.04 19.49 0.16 0.04 0.02 0.02 0.03 21.19 20.70 20.03 0.02 0.02 0.01 0.35 0.64 0.41 0.96 0.67 0.49 1.16 615±767
GC0065 pff gc-020 13 24 50.48 -42 59 49.0 6.92 20.57 20.33 19.53 19.00 18.47 0.09 0.03 0.01 0.01 0.03 20.42 19.58 19.68 0.05 0.04 0.04 0.24 0.80 0.53 1.06 -0.11 0.85 0.74 331±475
GC0066 HGHH-42/C42 13 24 50.87 -43 01 22.9 6.72 20.53 19.91 18.86 18.24 17.53 0.09 0.02 0.01 0.01 0.03 20.21 19.11 18.21 0.04 0.03 0.05 0.62 1.05 0.63 1.33 0.90 1.10 2.00 552±124,5,7
GC0067 VHH81-02/C2 13 24 51.49 -43 12 11.1 12.86 19.64 19.33 18.50 18.01 17.42 0.04 0.01 0.01 0.01 0.03 19.48 18.72 17.94 0.04 0.03 0.01 0.31 0.83 0.49 1.07 0.78 0.77 1.55 628±222,5,6,7
GC0068 C100 13 24 51.80 -43 04 33.7 7.33 - - 20.08 - - - - - - - 20.44 19.72 19.03 0.08 0.08 0.10 - - - 1.28 0.69 0.72 1.41 -
GC0069 AAT111033 13 24 52.98 -43 11 55.8 12.50 21.17 20.93 20.12 19.66 19.13 0.11 0.03 0.01 0.01 0.03 21.10 20.40 19.64 0.01 0.01 0.01 0.24 0.81 0.46 0.99 0.76 0.70 1.47 302±1667
GC0070 HGHH-G302/G302 13 24 53.29 -43 04 34.8 7.15 20.30 20.01 19.20 18.69 18.16 0.07 0.02 0.01 0.01 0.03 20.18 19.50 18.73 0.02 0.01 0.01 0.28 0.81 0.52 1.04 0.77 0.68 1.45 558±434,5
GC0071 AAT111185 13 24 54.00 -43 04 24.4 6.96 20.92 20.76 19.92 19.41 18.92 0.11 0.03 0.01 0.01 0.03 20.90 20.28 19.37 0.02 0.02 0.02 0.16 0.84 0.51 1.00 0.91 0.62 1.53 466±877
GC0072 pff gc-021 13 24 54.18 -42 54 50.4 8.78 20.21 20.03 19.25 18.75 18.24 0.06 0.02 0.01 0.01 0.03 20.13 19.52 18.81 0.03 0.02 0.01 0.18 0.78 0.50 1.01 0.70 0.62 1.32 594±505
GC0073 pff gc-022 13 24 54.33 -43 03 15.5 6.44 20.72 20.58 19.84 19.37 18.90 0.11 0.03 0.01 0.01 0.03 20.69 20.09 19.37 0.03 0.02 0.02 0.14 0.74 0.48 0.95 0.72 0.60 1.32 619±445,7
GC0074 HHH86-30/C30 13 24 54.35 -42 53 24.8 9.84 18.76 18.24 17.25 16.67 16.02 0.03 0.01 0.01 0.01 0.03 18.47 17.49 16.68 0.03 0.04 0.02 0.52 0.98 0.58 1.23 0.81 0.98 1.79 778±133,5,6,7
GC0075 AAT111296 13 24 54.49 -43 05 34.7 7.50 21.70 20.99 19.96 19.31 18.61 0.23 0.04 0.01 0.01 0.03 21.40 20.28 19.33 0.02 0.01 0.01 0.71 1.03 0.65 1.35 0.96 1.11 2.07 695±457
GC0076 pff gc-023 13 24 54.55 -42 48 58.7 13.59 20.55 20.30 19.44 18.90 18.37 0.06 0.02 0.01 0.01 0.03 20.48 19.74 18.97 0.01 0.01 0.01 0.25 0.86 0.54 1.08 0.77 0.74 1.51 457±315,7
GC0077 HGHH-11/C11 13 24 54.73 -43 01 21.7 6.01 19.55 18.96 17.91 17.26 16.61 0.05 0.01 0.01 0.01 0.03 19.21 17.98 17.20 0.06 0.05 0.06 0.59 1.05 0.66 1.30 0.79 1.23 2.01 753±12,4,5,6,7,8
GC0078 AAT111406 13 24 55.29 -43 03 15.6 6.28 21.84 21.15 20.13 19.50 18.80 0.30 0.05 0.02 0.01 0.03 21.66 20.70 18.80 0.03 0.02 0.01 0.69 1.03 0.63 1.33 1.90 0.96 2.86 669±777
GC0079 C116 13 24 55.46 -43 09 58.5 10.61 - - - - - - - - - - 23.80 22.74 21.84 0.06 0.02 0.03 - - - - 0.90 1.07 1.97 -
GC0080 HH-052 13 24 55.71 -43 22 48.4 22.43 - - - - - - - - - - 22.58 21.61 20.42 0.05 0.03 0.03 - - - - 1.19 0.97 2.16 921±1467
GC0081 pff gc-024 13 24 55.71 -43 20 39.1 20.36 21.07 20.73 19.84 19.31 18.73 0.28 0.03 0.01 0.01 0.03 21.00 20.17 19.34 0.02 0.01 0.01 0.34 0.89 0.53 1.11 0.83 0.83 1.66 279±385,7
GC0082 C117 13 24 56.06 -42 54 29.6 8.80 - - - - - - - - - - 21.27 20.18 19.26 0.01 0.02 0.01 - - - - 0.92 1.09 2.01 -
GC0083 AAT111563 13 24 56.08 -43 10 16.4 10.79 21.34 21.03 20.45 20.05 19.62 0.15 0.04 0.02 0.02 0.03 21.14 20.73 20.05 0.02 0.01 0.02 0.31 0.58 0.41 0.83 0.68 0.41 1.09 649±1027
GC0084 HGHH-G279 13 24 56.27 -43 03 23.4 6.15 19.97 19.91 19.45 19.17 18.88 0.06 0.02 0.01 0.01 0.03 19.76 19.38 19.83 0.01 0.01 0.01 0.06 0.45 0.29 0.57 -0.45 0.38 -0.07 366±344,5,7
GC0085 C118 13 24 57.17 -43 08 42.6 9.39 - - - - - - - - - - 22.60 21.76 20.67 0.04 0.03 0.02 - - - - 1.08 0.84 1.92 -
GC0086 HGHH-31/C31 13 24 57.44 -43 01 08.1 5.52 20.09 19.42 18.38 17.75 17.06 0.08 0.02 0.01 0.01 0.03 19.73 18.59 17.71 0.04 0.03 0.04 0.67 1.04 0.62 1.31 0.88 1.14 2.02 690±183,5,7
GC0087 HGHH-G369 13 24 57.52 -42 59 23.3 5.78 19.82 19.58 18.74 18.22 17.69 0.06 0.02 0.01 0.01 0.03 19.67 18.96 18.24 0.04 0.03 0.05 0.24 0.83 0.53 1.06 0.72 0.71 1.44 512±174,5,6,7
GC0088 pff gc-025 13 24 57.56 -43 05 32.8 7.04 21.50 21.02 20.02 19.39 18.67 0.20 0.04 0.02 0.01 0.03 21.41 20.41 19.45 0.04 0.03 0.02 0.47 1.00 0.63 1.35 0.96 1.00 1.97 923±305
GC0089 C119 13 24 57.69 -42 55 48.4 7.64 - - - - - - - - - - 21.16 21.02 20.67 0.03 0.03 0.02 - - - - 0.35 0.14 0.49 -
GC0090 C120 13 24 57.95 -42 52 04.9 10.56 - - - - - - - - - - 23.26 22.34 21.43 0.04 0.04 0.03 - - - - 0.90 0.92 1.83 -
GC0091 VHH81-03/C3 13 24 58.21 -42 56 10.0 7.33 19.34 18.73 17.71 17.10 16.44 0.04 0.01 0.01 0.01 0.03 19.02 17.88 17.08 0.04 0.03 0.02 0.61 1.02 0.61 1.26 0.80 1.14 1.94 562±21,3,5,6,7,8
GC0092 C121 13 24 58.42 -43 08 21.2 8.97 - - - - - - - - - - 23.53 23.01 22.45 0.05 0.04 0.09 - - - - 0.56 0.52 1.08 -
GC0093 pff gc-026 13 24 58.45 -42 42 53.3 19.02 20.44 20.33 19.52 19.07 18.50 0.08 0.02 0.01 0.01 0.03 20.47 19.82 19.09 0.02 0.01 0.01 0.12 0.81 0.45 1.02 0.73 0.65 1.37 490±675,7
GC0094 C12211 13 24 59.01 -43 08 21.4 8.91 - - - - - - - - - - - - 22.33 - - - - - - - - - - -
GC0095 C123 13 24 59.92 -43 09 08.6 9.46 - - - - - - - - - - 21.88 21.10 20.24 0.02 0.01 0.01 - - - - 0.86 0.78 1.64 -
GC0096 AAT112158 13 25 00.15 -42 54 09.0 8.61 21.99 21.43 20.43 19.86 19.23 0.25 0.05 0.02 0.01 0.03 21.75 20.78 19.88 0.01 0.01 0.01 0.55 1.00 0.57 1.20 0.90 0.96 1.87 699±437
GC0097 C124 13 25 00.37 -43 10 46.9 10.85 - - - - - - - - - - 23.07 22.36 21.57 0.03 0.02 0.03 - - - - 0.78 0.71 1.50 -
GC0098 pff gc-027 13 25 00.64 -43 05 30.3 6.58 21.22 20.75 19.74 19.13 18.45 0.17 0.04 0.01 0.01 0.03 21.05 20.06 19.11 0.01 0.01 0.01 0.47 1.01 0.61 1.29 0.95 0.99 1.94 524±345,7
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0099 C125 13 25 00.83 -43 11 10.6 11.16 - - - - - - - - - - 22.34 21.55 20.66 0.03 0.02 0.02 - - - - 0.89 0.78 1.67 -
GC0100 C126 13 25 00.91 -43 09 14.5 9.45 - - - - - - - - - - 24.02 23.54 22.66 0.04 0.05 0.08 - - - - 0.88 0.48 1.35 -
GC0101 C127 13 25 01.32 -43 08 43.4 8.97 - - - - - - - - - - 23.21 22.42 21.62 0.04 0.02 0.03 - - - - 0.80 0.79 1.59 -
GC0102 C128 13 25 01.46 -43 08 33.0 8.81 - - - - - - - - - - 23.08 22.04 20.95 0.05 0.03 0.02 - - - - 1.09 1.04 2.13 -
GC0103 pff gc-029 13 25 01.60 -42 54 40.9 8.03 19.97 19.75 19.37 19.06 18.71 0.05 0.02 0.01 0.01 0.03 19.72 19.50 19.10 0.03 0.03 0.01 0.22 0.38 0.31 0.65 0.40 0.22 0.62 570±385
GC0104 C129 13 25 01.63 -42 50 51.3 11.34 - - - - - - - - - - 22.59 21.71 20.83 0.04 0.02 0.02 - - - - 0.88 0.88 1.76 -
GC0105 pff gc-030 13 25 01.73 -43 00 09.9 4.83 21.68 20.94 19.89 19.26 18.54 0.36 0.06 0.02 0.02 0.03 21.21 19.93 20.43 0.05 0.04 0.02 0.73 1.05 0.64 1.35 -0.50 1.29 0.78 357±295
GC0106 HGHH-04/C4 13 25 01.83 -43 09 25.4 9.52 19.10 18.86 18.04 17.50 16.98 0.03 0.01 0.01 0.01 0.03 18.95 18.24 17.50 0.04 0.03 0.01 0.23 0.82 0.54 1.06 0.74 0.71 1.45 689±161,3,5,6,7
GC0107 C130 13 25 01.86 -42 52 27.8 9.88 - - - - - - - - - - 21.22 20.58 19.85 0.01 0.01 0.01 - - - - 0.73 0.64 1.37 -
GC0108 pff gc-031 13 25 02.76 -43 11 21.2 11.17 20.51 20.29 19.48 18.99 18.42 0.07 0.02 0.01 0.01 0.03 20.43 19.75 18.95 0.03 0.02 0.01 0.23 0.81 0.49 1.06 0.80 0.68 1.48 444±335
GC0109 HGHH-G176 13 25 03.13 -42 56 25.1 6.51 20.47 19.94 18.93 18.32 17.67 0.09 0.02 0.01 0.01 0.03 20.24 19.23 18.36 0.01 0.02 0.01 0.54 1.01 0.61 1.26 0.87 1.01 1.88 551±134,5,7
GC0110 HGHH-G066 13 25 03.18 -43 03 02.5 4.85 20.26 19.67 18.68 18.15 17.44 0.09 0.02 0.01 0.01 0.03 19.94 18.96 18.05 0.01 0.01 0.02 0.59 0.99 0.52 1.24 0.91 0.98 1.89 576±84,5
GC0111 pff gc-032 13 25 03.24 -42 57 40.5 5.65 20.92 20.59 19.73 19.18 18.61 0.14 0.04 0.01 0.01 0.03 20.81 20.05 19.22 0.01 0.02 0.01 0.33 0.86 0.55 1.12 0.83 0.76 1.59 648±295,7
GC0112 pff gc-033 13 25 03.34 -43 15 27.4 14.98 21.10 20.49 19.46 18.89 18.21 0.33 0.03 0.01 0.01 0.03 20.83 19.79 18.90 0.02 0.02 0.01 0.61 1.02 0.57 1.25 0.89 1.04 1.93 531±185
GC0113 HHH86-32/C32 13 25 03.37 -42 50 46.2 11.28 20.22 19.50 18.44 17.81 17.15 0.05 0.01 0.01 0.01 0.03 19.86 18.71 17.85 0.03 0.03 0.01 0.72 1.06 0.63 1.29 0.85 1.15 2.01 718±113,5,6,7
GC0114 pff gc-034 13 25 03.37 -43 11 39.6 11.41 20.98 20.70 19.91 19.35 18.84 0.09 0.03 0.01 0.01 0.03 20.89 20.19 19.38 0.03 0.02 0.01 0.28 0.80 0.56 1.06 0.81 0.69 1.50 605±465
GC0115 C131 13 25 03.67 -42 51 21.7 10.72 - - - - - - - - - - 21.57 20.98 20.20 0.02 0.02 0.01 - - - - 0.78 0.59 1.36 -
GC0116 AAT112752 13 25 04.12 -43 00 19.6 4.37 20.51 20.16 19.34 18.88 18.44 0.15 0.04 0.02 0.01 0.03 20.35 19.58 18.87 0.02 0.02 0.03 0.35 0.82 0.46 0.90 0.72 0.76 1.48 679±827
GC0117 pff gc-035 13 25 04.48 -43 10 48.4 10.54 21.32 20.73 19.71 19.07 18.44 0.14 0.03 0.01 0.01 0.03 21.13 20.07 19.13 0.03 0.02 0.01 0.59 1.02 0.64 1.27 0.94 1.06 2.00 627±225,7
GC0118 AAT112964 13 25 04.61 -43 07 21.7 7.50 20.45 20.39 19.61 19.13 18.68 0.08 0.03 0.01 0.01 0.03 20.47 19.90 19.11 0.01 0.01 0.01 0.06 0.78 0.49 0.94 0.78 0.57 1.35 456±1187
GC0119 HGHH-43/C43 13 25 04.81 -43 09 38.8 9.47 19.74 19.45 18.60 18.07 17.53 0.04 0.01 0.01 0.01 0.03 19.59 18.85 18.07 0.03 0.02 0.01 0.29 0.85 0.53 1.07 0.78 0.74 1.52 518±254,5,7
GC0120 WHH-7 13 25 05.02 -42 57 15.0 5.68 18.96 18.39 17.41 16.81 16.19 0.04 0.01 0.01 0.01 0.03 18.69 17.60 16.83 0.02 0.03 0.01 0.57 0.98 0.60 1.22 0.77 1.09 1.86 722±206
GC0121 HGHH-G035 13 25 05.29 -42 58 05.8 5.09 21.02 20.59 19.62 19.01 18.41 0.17 0.04 0.01 0.01 0.03 20.87 19.95 19.08 0.01 0.02 0.01 0.43 0.97 0.61 1.21 0.87 0.92 1.80 776±264,5
GC0122 pff gc-036 13 25 05.46 -43 14 02.6 13.52 20.09 19.83 19.04 18.52 17.91 0.05 0.02 0.01 0.01 0.03 19.96 19.27 18.49 0.02 0.02 0.01 0.26 0.79 0.52 1.13 0.78 0.69 1.47 666±305,7
GC0123 HGHH-12/C12/R281 13 25 05.72 -43 10 30.7 10.18 - - - - - - - - - - 19.34 18.23 17.36 0.04 0.03 0.02 - - - - 0.87 1.11 1.98 440±12,5,8
GC0124 HGHH-G342 13 25 05.83 -42 59 00.6 4.52 19.65 19.14 18.18 17.57 16.96 0.08 0.02 0.01 0.01 0.03 - - - - - - 0.51 0.96 0.61 1.22 - - - 553±214,5,6,7
GC0125 HHH86-13/C13 13 25 06.25 -43 15 11.6 14.58 20.02 19.60 18.68 18.13 17.51 0.04 0.01 0.01 0.01 0.03 19.82 18.90 18.12 0.03 0.03 0.02 0.41 0.93 0.55 1.16 0.78 0.92 1.70 601±125,6,7
GC0126 R276 13 25 07.33 -43 08 29.6 8.23 21.93 21.62 20.78 20.26 19.73 0.26 0.07 0.02 0.02 0.04 21.88 21.16 20.32 0.03 0.03 0.02 0.31 0.83 0.52 1.05 0.84 0.71 1.55 550±285
GC0127 AAT113428 13 25 07.33 -43 06 20.6 6.38 21.25 20.92 20.04 19.49 18.93 0.16 0.04 0.01 0.01 0.03 21.14 20.36 19.51 0.02 0.01 0.01 0.33 0.88 0.54 1.11 0.85 0.78 1.63 657±677
GC0128 pff gc-037 13 25 07.48 -43 12 29.4 11.93 21.60 21.29 20.42 19.91 19.33 0.55 0.05 0.02 0.01 0.03 21.46 20.73 19.90 0.02 0.01 0.01 0.31 0.87 0.50 1.08 0.83 0.73 1.56 554±235
GC0129 WHH-8 13 25 07.62 -43 01 15.2 3.66 19.83 19.16 18.12 17.46 16.82 0.13 0.03 0.01 0.01 0.03 19.48 18.32 17.45 0.03 0.03 0.04 0.67 1.04 0.66 1.30 0.87 1.16 2.03 690±326
GC0130 WHH-9 13 25 08.51 -43 02 57.4 3.93 20.59 19.95 18.91 18.37 17.64 0.17 0.03 0.01 0.01 0.03 20.28 19.17 18.30 0.05 0.04 0.05 0.64 1.04 0.54 1.27 0.87 1.11 1.98 315±1006
GC0131 C132 13 25 08.79 -43 09 09.6 8.72 - - - - - - - - - - 20.38 19.69 18.90 0.02 0.02 0.01 - - - - 0.79 0.69 1.48 -
GC0132 R271 13 25 08.81 -43 09 09.5 8.72 20.49 20.23 19.42 18.91 18.39 0.08 0.02 0.01 0.01 0.03 20.38 19.69 18.90 0.02 0.02 0.01 0.26 0.80 0.52 1.03 0.79 0.69 1.48 436±455
GC0133 pff gc-038 13 25 08.82 -43 04 14.9 4.63 20.83 20.29 19.29 18.69 18.03 0.17 0.04 0.01 0.01 0.03 20.58 19.57 18.71 0.03 0.03 0.03 0.54 1.00 0.61 1.26 0.87 1.01 1.88 431±195
GC0134 pff gc-039 13 25 09.10 -42 24 00.9 37.29 20.01 19.77 18.95 18.44 17.91 0.17 0.02 0.01 0.01 0.03 19.92 19.22 18.50 0.01 0.01 0.01 0.23 0.82 0.51 1.04 0.72 0.70 1.42 387±275,7
GC0135 K-029 13 25 09.19 -42 58 59.2 4.00 19.13 18.65 17.71 17.13 16.55 0.08 0.02 0.01 0.01 0.03 - - - - - - 0.48 0.94 0.58 1.16 - - - 677±447
GC0136 pff gc-040 13 25 09.54 -42 55 18.5 6.71 20.09 19.89 19.12 18.60 18.11 0.06 0.02 0.01 0.01 0.03 20.00 19.37 18.66 0.02 0.02 0.01 0.20 0.76 0.52 1.01 0.71 0.62 1.34 504±355
GC0137 HGHH-G329 13 25 10.20 -43 02 06.7 3.33 21.73 20.89 19.71 19.07 18.38 0.69 0.11 0.03 0.02 0.03 21.34 20.04 19.07 0.02 0.01 0.03 0.84 1.18 0.64 1.33 0.97 1.29 2.26 502±164,5,7
GC0138 K-033 13 25 10.25 -42 55 09.5 6.78 21.07 20.47 19.46 18.90 18.21 0.13 0.03 0.01 0.01 0.03 20.78 19.77 18.86 0.01 0.01 0.01 0.60 1.01 0.57 1.25 0.91 1.02 1.93 582±337
GC0139 K-034 13 25 10.27 -42 53 33.1 8.23 19.33 18.79 17.80 17.26 16.55 0.04 0.01 0.01 0.01 0.03 19.14 18.03 17.25 0.03 0.03 0.02 0.55 0.99 0.54 1.25 0.79 1.11 1.89 464±427
GC0140 HHH86-14/C14 13 25 10.49 -42 44 52.6 16.57 19.23 18.84 17.94 17.40 16.79 0.03 0.01 0.01 0.01 0.03 19.06 18.16 17.41 0.01 0.02 0.01 0.39 0.90 0.54 1.15 0.75 0.90 1.65 705±102,5,6,7
GC0141 AAT113992 13 25 10.51 -43 03 24.0 3.85 21.95 21.39 20.40 19.79 19.19 0.58 0.11 0.03 0.03 0.04 21.77 20.78 19.82 0.03 0.03 0.01 0.57 0.99 0.61 1.20 0.97 0.99 1.95 648±587
GC0142 C13313 13 25 11.05 -43 01 32.3 3.05 - - - - - - - - - - - - 19.30 - - - - - - - - - - -
GC0143 HGHH-G348 13 25 11.10 -42 58 03.0 4.32 19.90 19.66 18.92 18.46 18.03 0.10 0.03 0.01 0.01 0.03 19.80 19.15 18.45 0.01 0.01 - 0.24 0.74 0.46 0.89 0.70 0.65 1.35 416±304,5,7
GC0144 pff gc-041 13 25 11.17 -43 03 09.6 3.62 20.57 20.32 19.51 18.99 18.48 0.19 0.05 0.02 0.02 0.03 20.48 19.77 19.01 0.02 0.02 0.02 0.24 0.81 0.52 1.03 0.76 0.71 1.47 456±295,7
GC0145 HGHH-G327 13 25 11.98 -43 04 19.3 4.27 21.46 20.83 19.78 19.16 18.56 0.34 0.06 0.02 0.02 0.03 21.16 20.11 19.19 0.01 0.01 0.01 0.63 1.05 0.61 1.22 0.92 1.05 1.97 608±194,5,7
GC0146 HGHH-G081 13 25 12.11 -42 57 25.2 4.68 19.90 19.52 18.62 18.05 17.49 0.08 0.02 0.01 0.01 0.03 19.72 18.88 18.10 0.03 0.03 0.01 0.38 0.90 0.57 1.13 0.77 0.85 1.62 536±434,5
GC0147 pff gc-042 13 25 12.21 -43 16 33.9 15.67 19.91 19.74 18.97 18.47 17.91 0.12 0.02 0.01 0.01 0.03 19.82 19.19 18.47 0.02 0.02 0.01 0.17 0.78 0.50 1.05 0.72 0.63 1.35 627±235,6,7
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0148 AAT114302 13 25 12.34 -42 58 07.7 4.11 21.87 21.39 20.44 19.90 19.35 0.53 0.11 0.03 0.03 0.04 21.64 20.76 19.97 0.02 0.01 0.01 0.47 0.95 0.55 1.09 0.79 0.88 1.67 754±1437
GC0149 pff gc-043 13 25 12.45 -43 14 07.4 13.27 20.51 20.22 19.40 18.89 18.33 0.20 0.02 0.01 0.01 0.03 20.38 19.67 18.90 0.03 0.02 0.01 0.29 0.82 0.52 1.07 0.77 0.70 1.48 527±335,7
GC0150 WHH-10 13 25 12.84 -42 56 59.8 4.95 20.62 20.36 19.57 19.07 18.48 0.12 0.03 0.01 0.01 0.03 20.43 19.90 19.10 0.03 0.02 0.01 0.26 0.79 0.50 1.09 0.80 0.54 1.33 664±1416
GC0151 R261 13 25 12.90 -43 07 59.1 7.35 19.65 19.15 18.20 17.60 17.03 0.05 0.01 0.01 0.01 0.03 19.42 18.49 17.62 0.02 0.01 0.01 0.51 0.94 0.60 1.17 0.88 0.93 1.81 615±45,7,8
GC0152 pff gc-044 13 25 13.19 -43 16 35.6 15.67 20.29 20.11 19.37 18.87 18.33 0.16 0.02 0.01 0.01 0.03 20.19 19.59 18.87 0.02 0.02 0.01 0.17 0.74 0.50 1.04 0.72 0.60 1.32 568±535
GC0153 C134 13 25 13.20 -43 02 31.3 2.97 - - - - - - - - - - 22.45 21.64 20.71 0.07 0.05 0.07 - - - - 0.93 0.80 1.74 -
GC0154 pff gc-045 13 25 13.31 -42 52 12.4 9.31 21.57 20.86 19.82 19.21 18.53 0.19 0.04 0.01 0.01 0.03 21.38 20.32 19.40 0.07 0.06 0.04 0.71 1.04 0.62 1.29 0.93 1.06 1.99 474±235
GC0155 R259 13 25 13.88 -43 07 32.5 6.87 22.13 21.70 20.70 20.11 19.48 0.37 0.08 0.02 0.02 0.03 21.96 21.07 20.10 0.02 0.01 0.01 0.43 1.00 0.60 1.23 0.96 0.89 1.85 628±485
GC0156 HGHH-G271 13 25 13.95 -42 57 42.6 4.25 19.45 19.36 18.72 18.32 17.90 0.07 0.02 0.01 0.01 0.03 19.40 18.92 18.30 0.01 0.01 - 0.09 0.63 0.40 0.82 0.62 0.47 1.09 353±274,5,6,7
GC0157 C13513 13 25 14.07 -43 00 51.8 2.49 - - - - - - - - - - - - 19.90 - - - - - - - - - - -
GC0158 C136 13 25 14.07 -43 03 35.0 3.47 - - - - - - - - - - 22.48 21.50 21.19 0.04 0.02 0.02 - - - - 0.30 0.99 1.29 -
GC0159 WHH-11/K-051 13 25 14.24 -43 07 23.5 6.71 21.26 20.63 19.55 18.90 18.21 0.18 0.04 0.01 0.01 0.03 21.02 19.95 18.95 0.03 0.02 0.01 0.64 1.07 0.65 1.34 1.00 1.06 2.07 582±306,7
GC0160 pff gc-046 13 25 14.83 -43 41 10.6 40.10 19.91 19.72 18.93 18.43 17.95 0.11 0.02 0.01 0.01 0.03 19.87 19.14 18.37 0.01 - 0.01 0.20 0.79 0.50 0.98 0.77 0.73 1.50 532±215,7
GC0161 pff gc-047 13 25 15.12 -42 50 30.4 10.88 20.92 20.72 19.87 19.37 18.87 0.09 0.03 0.01 0.01 0.03 20.87 20.22 19.41 0.02 0.02 0.01 0.20 0.85 0.50 0.99 0.81 0.65 1.46 717±555
GC0162 AAT114769 13 25 15.12 -42 57 45.7 4.08 21.20 21.00 20.25 19.76 19.25 0.30 0.09 0.03 0.03 0.04 21.11 20.52 19.80 0.02 0.02 0.01 0.20 0.75 0.49 1.00 0.71 0.59 1.30 650±1697
GC0163 R257 13 25 15.24 -43 08 39.2 7.84 22.29 21.77 20.78 20.18 19.58 0.35 0.07 0.02 0.02 0.03 22.02 21.09 20.16 0.02 0.02 0.02 0.51 1.00 0.60 1.20 0.92 0.93 1.85 339±515
GC0164 pff gc-048 13 25 15.79 -42 49 15.1 12.09 20.92 20.67 19.85 19.30 18.78 0.09 0.03 0.01 0.01 0.03 20.85 20.13 19.41 0.02 0.02 0.02 0.25 0.82 0.55 1.07 0.71 0.72 1.44 535±535,7
GC0165 AAT114913 13 25 15.93 -43 06 03.3 5.35 21.69 21.33 20.39 19.88 19.29 0.34 0.08 0.02 0.02 0.04 21.60 20.72 19.86 0.02 0.02 0.02 0.36 0.94 0.52 1.10 0.86 0.88 1.74 563±637
GC0166 pff gc-049 13 25 16.06 -43 05 06.5 4.49 20.74 20.45 19.59 19.05 18.50 0.15 0.04 0.01 0.01 0.03 20.64 19.85 19.07 0.03 0.03 0.03 0.29 0.86 0.54 1.09 0.78 0.79 1.57 674±325
GC0167 C13713 13 25 16.06 -43 02 19.3 2.42 - - - - - - - - - - - - 19.04 - - - - - - - - - - -
GC0168 VHH81-05/C5 13 25 16.12 -42 52 58.2 8.44 18.70 18.49 17.68 17.13 16.68 0.03 0.01 0.01 0.01 0.03 - - - - - - 0.21 0.81 0.55 1.00 - - - 555±31,2,3,5,7,8
GC0169 HCH01 13 25 16.22 -42 59 43.4 2.52 18.69 18.36 17.47 16.94 16.40 0.52 0.15 0.04 0.03 0.04 - - - - - - 0.33 0.89 0.53 1.07 - - - 649±455,7
GC0170 HHH86-33/C33 13 25 16.26 -42 50 53.3 10.47 19.58 19.34 18.50 18.02 17.50 0.04 0.01 0.01 0.01 0.03 - - - - - - 0.24 0.84 0.48 1.00 - - - 596±183,5,6,7
GC0171 AAT1149939 13 25 16.44 -43 03 33.1 3.16 22.49 21.50 20.44 19.82 19.32 1.41 0.19 .382 0.308 0.224 21.95 20.81 19.83 0.02 0.02 0.03 0.99 1.06 0.62 1.12 0.98 1.14 2.12 352±1367
GC0172 HCH02 13 25 16.69 -43 02 08.7 2.23 19.27 18.87 17.93 17.37 16.76 0.98 0.26 0.07 0.05 0.05 - - - - - - 0.40 0.94 0.56 1.17 - - - 300±25,7,8
GC0173 pff gc-050 13 25 16.73 -42 50 18.4 11.02 21.63 21.28 20.39 19.86 19.27 0.16 0.04 0.01 0.01 0.03 - - - - - - 0.35 0.89 0.54 1.12 - - - 688±705
GC0174 C138 13 25 16.91 -43 03 08.0 2.79 - - - - - - - - - - 21.53 20.79 19.97 0.02 0.02 0.03 - - - - 0.81 0.74 1.55 -
GC0175 R254 13 25 16.96 -43 09 28.0 8.54 20.52 20.26 19.43 18.91 18.33 0.09 0.03 0.01 0.01 0.03 20.42 19.65 18.91 0.04 0.03 0.03 0.27 0.82 0.52 1.10 0.73 0.77 1.51 561±275,7
GC0176 C139 13 25 17.06 -43 02 44.6 2.50 - - - - - - - - - - 20.73 19.62 18.86 0.03 0.02 0.04 - - - - 0.76 1.11 1.87 -
GC0177 HGHH-G219 13 25 17.31 -42 58 46.6 3.03 20.69 19.92 18.84 18.20 17.55 0.43 0.08 0.02 0.02 0.03 - - - - - - 0.77 1.09 0.63 1.29 - - - 535±244,5,7
GC0178 R253 13 25 17.33 -43 08 39.0 7.74 20.75 20.49 19.67 19.14 18.64 0.09 0.03 0.01 0.01 0.03 20.68 20.00 19.47 0.03 0.03 0.05 0.26 0.81 0.53 1.04 0.53 0.69 1.22 486±525,7
GC0179 C140 13 25 17.42 -43 03 25.2 2.94 - - - - - - - - - - 21.40 20.65 19.83 0.03 0.02 0.03 - - - - 0.82 0.75 1.57 -
GC0180 C141 13 25 18.14 -43 02 50.9 2.43 - - - - - - - - - - 22.23 21.55 20.95 0.06 0.05 0.06 - - - - 0.60 0.68 1.29 -
GC0181 WHH-12 13 25 18.27 -42 53 04.8 8.25 20.36 20.00 19.07 18.47 17.97 0.07 0.02 0.01 0.01 0.03 20.23 19.35 18.71 0.04 0.04 0.01 0.36 0.93 0.60 1.10 0.64 0.89 1.52 558±996
GC0182 AAT115339 13 25 18.44 -43 04 09.8 3.45 21.19 20.91 20.11 19.53 19.01 0.39 0.10 0.03 0.03 0.04 21.11 20.38 19.56 0.02 0.01 0.02 0.27 0.81 0.58 1.09 0.81 0.73 1.55 618±1087
GC0183 C142 13 25 18.50 -43 01 16.4 1.67 - - - - - - - - - - - - 17.64 - - - - - - - - - - -
GC0184 AAT320656 13 25 19.13 -43 12 03.8 11.03 20.61 20.50 19.81 19.35 18.89 0.08 0.03 0.01 0.01 0.03 20.57 20.01 19.35 0.02 0.01 0.02 0.10 0.70 0.46 0.92 0.66 0.56 1.22 453±2337
GC0185 HGHH-G331 13 25 19.50 -43 02 28.4 1.99 20.00 19.60 18.92 18.47 17.93 0.55 0.14 0.05 0.04 0.05 - - - - - - 0.40 0.68 0.44 0.99 - - - 371±224,5,7
GC0186 AAT115561 13 25 19.83 -42 58 27.2 3.05 22.13 21.47 20.50 19.92 19.29 1.44 0.26 0.07 0.06 0.06 - 20.98 20.15 1.00 0.04 0.02 0.66 0.98 0.57 1.20 0.83 - - 514±467
GC0187 R247 13 25 19.99 -43 07 44.1 6.73 21.86 21.20 20.11 19.40 18.62 0.28 0.05 0.02 0.01 0.03 21.73 20.65 19.75 0.05 0.04 0.04 0.66 1.10 0.70 1.49 0.90 1.08 1.98 662±485
GC0188 AAT115605 13 25 20.44 -42 54 08.5 7.13 21.44 21.22 20.47 20.00 19.50 0.18 0.05 0.02 0.02 0.03 21.36 20.76 20.11 0.01 0.03 0.01 0.22 0.75 0.47 0.97 0.66 0.60 1.25 713±1317
GC0189 AAT115679 13 25 20.72 -43 06 35.9 5.60 21.93 21.49 20.44 19.80 19.15 0.40 0.09 0.02 0.02 0.03 21.71 20.79 19.84 0.02 0.02 0.03 0.44 1.05 0.64 1.30 0.95 0.92 1.87 511±1657
GC0190 WHH-13/HH-090 13 25 21.29 -42 49 17.7 11.91 20.75 20.22 19.20 18.61 17.95 0.08 0.02 0.01 0.01 0.03 20.59 19.52 18.74 0.03 0.03 0.02 0.53 1.02 0.59 1.25 0.78 1.08 1.85 444±336,7
GC0191 AAT321194 13 25 21.32 -43 23 59.3 22.87 21.46 21.03 20.06 19.48 18.82 0.38 0.03 0.01 0.01 0.03 21.33 20.42 19.53 0.03 0.02 0.01 0.43 0.97 0.58 1.24 0.90 0.90 1.80 254±1697
GC0192 HGHH-06/C6 13 25 22.19 -43 02 45.6 1.89 18.65 18.17 17.21 16.61 16.03 0.24 0.06 0.02 0.01 0.03 - - - - - - 0.48 0.96 0.60 1.18 - - - 855±22,4,5,6,7,8
GC0193 pff gc-051 13 25 22.35 -43 15 00.1 13.89 21.15 20.73 19.79 19.20 18.61 0.10 0.02 0.01 0.01 0.03 21.00 20.10 19.22 0.03 0.03 0.02 0.42 0.94 0.59 1.18 0.88 0.90 1.78 468±395,7
GC0194 C143 13 25 23.20 -43 03 12.9 2.22 - - - - - - - - - - 21.87 21.35 20.52 0.05 0.04 0.06 - - - - 0.82 0.52 1.34 -
GC0195 AAT116025 13 25 23.46 -42 53 26.2 7.75 21.23 20.88 20.00 19.48 18.85 0.14 0.04 0.01 0.01 0.03 21.16 20.32 19.62 0.04 0.05 0.01 0.35 0.88 0.51 1.15 0.70 0.84 1.54 545±647
GC0196 AAT116220 13 25 24.40 -43 07 58.9 6.86 20.76 20.39 19.47 18.91 18.36 0.11 0.03 0.01 0.01 0.03 20.62 19.72 18.92 0.03 0.03 0.03 0.37 0.92 0.56 1.11 0.80 0.90 1.70 524±417
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0197 AAT116385 13 25 25.39 -42 58 21.5 2.82 21.71 21.23 20.26 19.59 18.99 1.22 0.26 0.07 0.05 0.06 21.58 20.68 19.94 0.02 0.02 0.01 0.48 0.97 0.66 1.27 0.74 0.90 1.64 550±407
GC0198 WHH-14 13 25 25.49 -42 56 31.2 4.64 20.99 20.83 20.06 19.56 19.05 0.18 0.05 0.02 0.02 0.03 20.98 20.36 19.68 0.02 0.03 0.01 0.15 0.77 0.50 1.01 0.68 0.62 1.30 461±756,7
GC0199 AAT204119 13 25 25.70 -42 37 40.9 23.47 20.59 20.49 19.81 19.35 18.93 0.18 0.02 0.01 0.01 0.03 20.60 20.04 19.42 0.01 - - 0.10 0.67 0.47 0.88 0.62 0.56 1.18 404±747
GC0200 pff gc-052 13 25 25.75 -43 05 16.5 4.14 20.88 20.70 19.88 19.39 18.86 0.19 0.06 0.02 0.02 0.03 20.86 20.17 19.42 0.03 0.03 0.03 0.18 0.82 0.48 1.01 0.75 0.69 1.44 462±525
GC0201 HGHH-46/C46 13 25 25.97 -43 03 25.7 2.30 19.74 19.71 19.10 18.74 18.30 0.37 0.12 0.04 0.04 0.05 19.77 19.30 18.64 0.01 0.02 0.22 0.03 0.61 0.36 0.80 0.66 0.47 1.13 508±194,5,7
GC0202 C144 13 25 26.28 -43 04 38.5 3.50 - - - - - - - - - - 23.22 22.36 21.96 0.06 0.05 0.05 - - - - 0.41 0.85 1.26 -
GC0203 AAT116531 13 25 26.75 -43 08 53.4 7.74 20.92 20.65 19.83 19.34 18.83 0.10 0.03 0.01 0.01 0.03 20.77 19.95 19.94 0.07 0.06 0.02 0.27 0.82 0.49 1.00 0.01 0.82 0.83 267±717
GC0204 WHH-15 13 25 26.78 -42 52 39.9 8.48 20.73 20.56 19.81 19.36 18.87 0.09 0.03 0.01 0.01 0.03 20.68 20.80 19.53 0.03 0.02 0.01 0.16 0.75 0.46 0.94 1.27 -0.12 1.15 513±536,7
GC0205 R235 13 25 26.82 -43 09 40.5 8.53 20.55 20.30 19.53 19.02 18.51 0.08 0.02 0.01 0.01 0.03 20.42 19.73 19.01 0.04 0.03 0.04 0.25 0.77 0.51 1.03 0.72 0.69 1.41 498±285,7
GC0206 WHH-16/K-102 13 25 27.97 -43 04 02.2 2.89 20.90 20.23 19.18 18.56 17.90 0.56 0.11 0.03 0.02 0.04 20.64 19.52 18.60 0.04 0.03 0.03 0.66 1.06 0.61 1.28 0.93 1.11 2.04 661±476,7
GC0207 HCH13 13 25 28.69 -43 02 55.0 1.78 21.32 20.82 19.89 19.30 18.63 2.53 0.55 0.15 0.12 0.12 - - - - - - 0.50 0.93 0.59 1.26 - - - 641±245,7
GC0208 C145 13 25 28.81 -43 04 21.6 3.22 - - - - - - - - - - 19.32 18.54 17.81 0.01 0.01 0.02 - - - - 0.73 0.78 1.51 -
GC0209 WHH-17 13 25 29.25 -42 57 47.1 3.38 19.68 19.39 18.57 18.06 17.48 0.15 0.04 0.02 0.01 0.03 19.54 18.77 18.13 0.02 0.03 - 0.29 0.82 0.51 1.09 0.65 0.76 1.41 619±456,7
GC0210 AAT116969 13 25 29.41 -42 53 25.6 7.73 21.55 21.28 20.46 20.10 19.48 0.21 0.06 0.02 0.02 0.03 21.45 20.77 20.10 0.03 0.02 0.01 0.27 0.82 0.35 0.98 0.68 0.68 1.36 446±617
GC0211 HGHH-G169 13 25 29.43 -42 58 09.9 3.00 21.39 20.58 19.49 18.92 18.12 0.81 0.13 0.03 0.03 0.04 21.00 19.80 18.94 0.01 0.02 0.01 0.81 1.10 0.57 1.37 0.86 1.21 2.07 643±244,5,7
GC0212 pff gc-053 13 25 29.62 -42 54 44.5 6.42 20.91 20.29 19.26 18.73 17.98 0.14 0.03 0.01 0.01 0.03 20.65 19.54 18.78 0.03 0.04 0.01 0.62 1.03 0.53 1.29 0.76 1.11 1.86 439±205
GC0213 R229 13 25 29.74 -43 11 42.8 10.57 20.70 20.49 19.72 19.20 18.69 0.08 0.02 0.01 0.01 0.03 20.62 19.94 19.22 0.04 0.03 0.04 0.21 0.77 0.52 1.03 0.73 0.68 1.41 517±665
GC0214 HCH15 13 25 29.80 -43 00 07.0 1.10 19.27 18.87 17.93 17.37 16.76 0.98 0.26 0.07 0.05 0.05 - - - - - - 0.04 0.94 0.56 1.17 - - - 519±18
GC0215 C146 13 25 29.87 -43 05 09.2 4.03 - - - - - - - - - - 21.71 20.78 19.94 0.03 0.02 0.02 - - - - 0.84 0.93 1.77 -
GC0216 WHH-18 13 25 30.07 -42 56 46.9 4.39 19.85 19.36 18.36 17.85 17.16 0.09 0.02 0.01 0.01 0.03 19.63 18.60 17.88 0.01 0.03 - 0.50 0.99 0.51 1.20 0.72 1.03 1.75 752±256,7
GC0217 pff gc-054 13 25 30.28 -43 41 53.6 40.75 20.65 20.60 19.99 19.57 19.09 0.19 0.03 0.01 0.01 0.03 - - - - - - 0.05 0.62 0.41 0.89 - - - 297±405,7
GC0218 HCH16 13 25 30.29 -42 59 34.8 1.64 - - - - - - - - - - - - - - - - - - - - - - - 458±25,7,8
GC0219 HHH86-15/C15/R226 13 25 30.41 -43 11 49.6 10.69 20.11 19.56 18.56 17.94 17.35 0.06 0.02 0.01 0.01 0.03 19.80 18.68 17.92 0.05 0.05 0.05 0.55 1.00 0.62 1.21 0.76 1.12 1.88 644±15,6,7,8
GC0220 C147 13 25 30.65 -43 03 47.1 2.70 - - - - - - - - - - 21.58 20.88 20.05 0.05 0.05 0.03 - - - - 0.83 0.69 1.52 -
GC0221 pff gc-055 13 25 30.72 -42 48 13.4 12.94 20.87 20.68 19.92 19.44 18.97 0.08 0.03 0.01 0.01 0.03 20.83 20.20 19.54 0.02 0.02 0.02 0.19 0.76 0.48 0.96 0.66 0.62 1.28 485±475,7
GC0222 AAT205071 13 25 30.74 -42 30 16.0 30.89 19.65 19.61 18.86 18.37 17.96 0.09 0.01 0.01 0.01 0.03 19.68 19.10 18.50 0.02 0.02 - 0.04 0.74 0.49 0.90 0.60 0.58 1.18 288±617
GC0223 WHH-19 13 25 31.03 -42 50 14.9 10.92 18.47 18.16 17.29 16.78 16.24 0.02 0.01 0.01 0.01 0.03 18.08 17.67 16.91 0.06 0.06 0.02 0.31 0.87 0.51 1.05 0.76 0.42 1.18 451±406,7
GC0224 AAT117287 13 25 31.08 -43 04 17.0 3.20 22.20 21.44 20.36 19.82 19.13 1.22 0.20 0.05 0.04 0.05 21.82 20.56 20.45 0.04 0.03 0.03 0.76 1.08 0.54 1.23 0.11 1.27 1.37 554±607
GC0225 HGHH-G292 13 25 31.48 -42 58 08.3 3.09 21.77 21.05 19.97 19.33 18.64 1.04 0.18 0.05 0.03 0.04 21.48 20.85 19.53 0.01 0.02 0.01 0.72 1.08 0.64 1.34 1.33 0.63 1.95 655±434,5
GC0226 HCH18 13 25 31.60 -43 00 02.8 1.32 21.06 20.99 19.93 19.20 18.43 2.42 0.76 0.19 0.13 0.12 - - - - - - 0.07 1.06 0.73 1.50 - - - 455±15,7,8
GC0227 AAT117322 13 25 31.73 -42 55 15.7 5.93 21.14 20.91 20.08 19.55 19.07 0.19 0.05 0.02 0.02 0.03 21.07 20.38 19.75 0.04 0.05 0.01 0.22 0.84 0.52 1.01 0.63 0.69 1.32 636±1337
GC0228 HGHH-44/C44 13 25 31.73 -43 19 22.6 18.25 19.76 19.50 18.69 18.14 17.66 0.04 0.01 0.01 0.01 0.03 19.59 18.85 18.15 0.03 0.02 0.01 0.26 0.80 0.55 1.03 0.70 0.74 1.44 505±14,5,6,7,8
GC0229 C148 13 25 31.75 -43 05 46.0 4.68 - - - - - - - - - - 21.25 20.79 20.21 0.07 0.06 0.05 - - - - 0.58 0.46 1.04 -
GC0230 R224/C149 13 25 32.33 -43 07 17.1 6.20 21.07 20.90 20.15 19.64 19.19 0.15 0.04 0.02 0.02 0.03 21.02 20.42 19.68 0.03 0.02 0.02 0.16 0.76 0.50 0.96 0.74 0.60 1.34 389±455
GC0231 HGHH-G359 13 25 32.42 -42 58 50.2 2.47 20.44 19.86 18.86 18.24 17.64 0.45 0.10 0.03 0.02 0.04 20.13 19.09 18.33 0.01 0.01 - 0.58 1.00 0.62 1.22 0.76 1.04 1.80 489±344,5,7
GC0232 pff gc-056 13 25 32.80 -42 56 24.4 4.83 19.62 19.43 18.64 18.15 17.64 0.06 0.02 0.01 0.01 0.03 19.51 18.82 18.22 0.03 0.04 - 0.19 0.79 0.48 1.00 0.60 0.69 1.29 306±275,6
GC0233 R223 13 25 32.80 -43 07 02.2 5.97 20.08 19.67 18.77 18.23 17.64 0.07 0.02 0.01 0.01 0.03 19.89 18.98 18.19 0.03 0.03 0.03 0.41 0.91 0.54 1.13 0.79 0.92 1.71 776±15,7,8
GC0234 K-131 13 25 32.88 -43 04 29.2 3.48 21.23 20.44 19.37 18.77 18.12 0.38 0.07 0.02 0.02 0.03 20.84 19.65 18.74 0.03 0.02 0.03 0.79 1.08 0.59 1.24 0.91 1.20 2.10 639±447
GC0235 pff gc-057 13 25 33.17 -42 59 03.2 2.33 22.21 21.38 20.35 19.75 18.95 2.11 0.37 0.09 0.07 0.07 21.67 20.75 19.86 0.03 0.02 0.01 0.82 1.04 0.60 1.40 0.90 0.91 1.81 515±125
GC0236 C15013 13 25 33.82 -43 02 49.6 2.03 - - - - - - - - - - - - 19.78 - - - - - - - - - - -
GC0237 C151 13 25 33.93 -43 03 51.4 2.94 - - - - - - - - - - 22.27 20.90 19.95 0.03 0.01 0.03 - - - - 0.95 1.37 2.32 -
GC0238 MAGJM-11 13 25 33.94 -42 59 39.4 1.89 19.80 19.64 18.87 18.44 17.83 0.80 0.25 0.07 0.06 0.07 - - - - - - 0.16 0.77 0.43 1.04 - - - 444±175,7
GC0239 HGHH-G206 13 25 34.10 -42 59 00.7 2.44 20.68 20.09 19.10 18.58 17.91 0.56 0.12 0.03 0.03 0.04 20.37 19.36 18.61 0.02 0.03 0.01 0.58 0.99 0.52 1.19 0.75 1.00 1.75 600±244,5
GC0240 HGHH-45/C45 13 25 34.25 -42 56 59.1 4.33 19.99 19.81 19.03 18.60 18.05 0.10 0.03 0.01 0.01 0.03 19.91 19.17 18.67 0.08 0.07 0.02 0.18 0.78 0.43 0.98 0.50 0.75 1.25 612±344,5,7
GC0241 WHH-20 13 25 34.36 -42 51 05.9 10.12 20.30 19.93 19.01 18.52 17.90 0.06 0.02 0.01 0.01 0.03 20.11 19.25 18.59 0.04 0.05 0.01 0.37 0.92 0.49 1.10 0.66 0.86 1.52 259±336,7
GC0242 C15213 13 25 34.64 -43 03 16.4 2.48 - - - - - - - - - - - - 17.82 - - - - - - - - - - -
GC0243 C15313 13 25 34.64 -43 03 27.8 2.65 - - - - - - - - - - - - 18.23 - - - - - - - - - - -
GC0244 HCH21 13 25 34.65 -43 03 27.7 2.65 - - - - - - - - - - - - - - - - - - - - - - - 663±25,7,8
GC0245 C15413 13 25 34.71 -43 03 30.2 2.69 - - - - - - - - - - - - 19.58 - - - - - - - - - - -
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0246 HHH86-16/C16 13 25 35.00 -42 36 05.0 25.10 20.01 19.57 18.59 18.00 17.41 0.12 0.01 0.01 0.01 0.03 19.85 18.83 18.12 0.03 0.03 0.01 0.44 0.98 0.59 1.19 0.70 1.02 1.73 538±162,4,7
GC0247 pff gc-058 13 25 35.12 -42 56 45.3 4.60 19.67 19.47 18.68 18.19 17.70 0.07 0.02 0.01 0.01 0.03 19.55 18.85 18.29 0.03 0.03 0.01 0.20 0.78 0.49 0.99 0.56 0.70 1.26 365±225,6,7
GC0248 K-144 13 25 35.16 -42 53 01.0 8.25 22.10 21.31 20.25 19.63 18.94 0.33 0.05 0.02 0.01 0.03 21.72 20.44 19.75 0.01 0.01 0.01 0.79 1.06 0.62 1.31 0.69 1.28 1.97 593±437
GC0249 WHH-21 13 25 35.22 -43 12 01.5 10.97 19.64 19.60 19.00 18.63 18.25 0.04 0.01 0.01 0.01 0.03 19.61 19.15 18.62 0.02 0.01 0.02 0.04 0.60 0.37 0.75 0.53 0.46 0.99 243±616
GC0250 WHH-22 13 25 35.31 -43 05 29.0 4.56 - - - - - - - - - - 19.66 18.80 18.03 0.04 0.04 0.04 - - - - 0.77 0.86 1.63 492±1266
GC0251 MAGJM-08 13 25 35.50 -42 59 35.2 2.12 20.76 20.18 19.17 18.68 17.94 1.15 0.24 0.06 0.05 0.05 - - - - - - 0.58 1.01 0.49 1.22 - - - 701±285,7
GC0252 R215 13 25 35.64 -43 08 36.8 7.61 22.06 21.68 20.80 20.27 19.70 0.27 0.06 0.02 0.02 0.03 21.98 21.18 20.35 0.03 0.03 0.04 0.38 0.87 0.53 1.11 0.83 0.79 1.63 543±575,7
GC0253 R213 13 25 35.93 -43 07 27.9 6.50 22.70 22.03 20.92 20.35 19.62 0.56 0.10 0.03 0.02 0.03 22.34 21.26 20.34 0.03 0.01 0.02 0.67 1.11 0.58 1.30 0.92 1.08 2.00 532±525,7
GC0254 AAT117899 13 25 36.05 -42 53 40.3 7.63 21.70 21.17 20.17 19.62 18.97 0.23 0.05 0.02 0.01 0.03 21.51 20.51 19.70 0.03 0.03 0.01 0.53 1.01 0.54 1.20 0.81 1.01 1.81 609±1167
GC0255 C155 13 25 36.47 -43 08 03.5 7.10 - - - - - - - - - - 22.98 22.21 21.36 0.06 0.05 0.05 - - - - 0.85 0.77 1.63 -
GC0256 MAGJM-06 13 25 36.69 -42 59 59.2 2.02 - - - - - - - - - - - - - - - - - - - - - - - 443±155,7
GC0257 AAT118198 13 25 37.47 -43 05 44.9 4.94 21.49 20.68 19.64 18.98 18.29 0.31 0.05 0.02 0.01 0.03 21.14 19.94 19.03 0.04 0.02 0.03 0.81 1.04 0.66 1.35 0.91 1.20 2.11 575±367
GC0258 AAT118314 13 25 38.03 -43 16 59.2 15.95 20.69 20.62 19.89 19.45 18.98 0.08 0.03 0.01 0.01 0.03 20.67 20.13 19.42 0.01 0.01 0.01 0.08 0.72 0.44 0.92 0.71 0.53 1.24 257±597
GC0259 R209 13 25 38.13 -43 13 02.2 12.04 21.92 21.51 20.62 20.05 19.43 0.20 0.05 0.02 0.01 0.03 21.91 20.95 20.13 0.04 0.04 0.04 0.41 0.90 0.57 1.19 0.83 0.96 1.79 558±405,7
GC0260 C156 13 25 38.43 -43 05 02.6 4.37 - - - - - - - - - - 19.76 18.55 17.65 0.02 0.02 0.03 - - - - 0.90 1.21 2.11 -
GC0261 C15712 13 25 38.45 -43 03 28.9 3.06 - - - - - - - - - - - - 19.21 - - - - - - - - - - -
GC0262 HGHH-G268 13 25 38.61 -42 59 19.6 2.71 20.23 19.83 18.93 18.36 17.79 0.34 0.08 0.03 0.02 0.04 20.05 19.15 18.44 0.02 0.02 - 0.40 0.91 0.56 1.13 0.71 0.91 1.62 436±434,5
GC0263 C158 13 25 38.76 -43 05 34.5 4.88 - - - - - - - - - - 21.67 20.86 20.06 0.05 0.04 0.05 - - - - 0.80 0.81 1.61 -
GC0264 C159 13 25 39.17 -43 04 33.8 4.02 - - - - - - - - - - 21.91 20.82 19.93 0.02 0.02 0.02 - - - - 0.90 1.09 1.99 -
GC0265 MAGJM-01 13 25 39.33 -43 00 48.8 2.17 19.90 19.52 18.61 18.06 17.50 0.32 0.08 0.02 0.02 0.03 - - - - - - 0.37 0.91 0.55 1.11 - - - 645±365,7
GC0266 pff gc-059 13 25 39.65 -43 04 01.4 3.62 21.53 20.97 19.96 19.35 18.73 0.55 0.11 0.03 0.02 0.04 21.42 20.33 19.48 0.05 0.04 0.04 0.56 1.01 0.61 1.23 0.86 1.09 1.94 525±275,7
GC0267 HGHH-17/C17 13 25 39.73 -42 55 59.2 5.62 18.82 18.51 17.63 17.10 16.57 0.04 0.01 0.01 0.01 0.03 18.61 17.72 17.19 0.04 0.05 0.01 0.32 0.88 0.53 1.06 0.53 0.89 1.42 782±22,5,6,7,8
GC0268 HHH86-18/C18/K-163 13 25 39.88 -43 05 01.9 4.49 18.79 18.42 17.53 16.97 16.43 0.04 0.01 0.01 0.01 0.03 18.49 17.51 16.89 0.05 0.04 0.05 0.38 0.89 0.56 1.10 0.62 0.99 1.60 480±22,5,6,7,8
GC0269 C16012 13 25 40.09 -43 03 07.1 3.01 - - - - - - - - - - - - 19.99 - - - - - - - - - - -
GC0270 C101 13 25 40.47 -42 56 02.7 5.65 - - 20.34 - - - - - - - 21.84 20.90 20.08 0.03 0.04 0.01 - - - - 0.82 0.94 1.76 -
GC0271 R204/C161 13 25 40.52 -43 07 17.9 6.59 21.58 20.84 19.80 19.16 18.41 0.21 0.04 0.01 0.01 0.03 21.21 20.15 19.26 0.04 0.03 0.03 0.74 1.05 0.63 1.39 0.89 1.06 1.95 425±325
GC0272 HGHH-34/C34 13 25 40.61 -43 21 13.6 20.22 19.37 19.01 18.12 17.59 17.03 0.04 0.01 0.01 0.01 0.03 19.64 18.54 17.76 0.04 0.03 0.02 0.35 0.89 0.53 1.10 0.77 1.10 1.87 669±183,5,7
GC0273 C162 13 25 40.87 -43 05 00.4 4.56 - - - - - - - - - - 21.95 21.41 20.91 0.06 0.05 0.01 - - - - 0.51 0.54 1.05 -
GC0274 R203 13 25 40.90 -43 08 16.0 7.52 20.66 20.56 19.84 19.36 18.88 0.09 0.03 0.01 0.01 0.03 20.62 20.08 19.38 0.04 0.03 0.03 0.09 0.73 0.48 0.96 0.70 0.54 1.24 455±355,7
GC0275 AAT118874 13 25 41.36 -42 58 08.9 3.91 21.55 21.02 19.99 19.43 18.81 0.44 0.09 0.03 0.02 0.04 21.49 20.30 19.57 0.05 0.02 - 0.53 1.03 0.56 1.18 0.73 1.19 1.92 570±827
GC0276 C163 13 25 41.63 -43 03 45.8 3.66 - - - - - - - - - - 21.98 21.25 20.43 0.05 0.04 0.04 - - - - 0.81 0.73 1.55 -
GC0277 R202 13 25 42.00 -43 10 42.2 9.91 20.34 20.08 19.26 18.72 18.22 0.06 0.02 0.01 0.01 0.03 20.35 19.74 18.94 0.07 0.03 0.06 0.27 0.81 0.54 1.05 0.80 0.61 1.41 286±455,7
GC0278 C16414 13 25 42.09 -43 03 19.5 3.43 - - - - - - - - - - - - 19.60 - - - - - - - - - - -
GC0279 HGHH-G370 13 25 42.25 -42 59 17.0 3.26 19.61 19.29 18.39 17.86 17.32 0.17 0.05 0.02 0.01 0.03 19.45 18.59 17.93 0.01 0.03 0.01 0.32 0.90 0.54 1.08 0.66 0.86 1.52 507±344,5,7
GC0280 pff gc-060 13 25 42.43 -42 59 02.6 3.43 20.11 19.74 18.81 18.24 17.66 0.20 0.05 0.02 0.01 0.03 19.96 19.02 18.33 0.02 0.03 0.01 0.37 0.93 0.57 1.15 0.69 0.95 1.63 890±195,6
GC0281 AAT119058 13 25 42.53 -43 03 41.5 3.73 21.85 21.42 20.39 19.77 19.18 0.60 0.13 0.04 0.03 0.04 21.69 20.74 19.86 0.04 0.03 0.04 0.43 1.03 0.62 1.21 0.88 0.95 1.83 385±877
GC0282 pff gc-061 13 25 42.62 -42 45 10.9 16.20 21.59 21.15 20.25 19.69 19.12 0.14 0.03 0.01 0.01 0.03 21.42 20.55 19.75 0.01 0.01 0.01 0.44 0.90 0.55 1.13 0.80 0.87 1.67 500±485,7
GC0283 pff gc-062 13 25 43.23 -42 58 37.4 3.81 21.13 20.46 19.42 18.83 18.18 0.34 0.06 0.02 0.02 0.03 20.79 19.71 18.92 0.01 0.01 0.01 0.67 1.04 0.59 1.24 0.80 1.08 1.88 697±375
GC0284 HGHH-19/C19 13 25 43.40 -43 07 22.8 6.87 19.37 19.01 18.12 17.59 17.03 0.04 0.01 0.01 0.01 0.03 18.96 17.83 18.64 0.05 0.04 0.01 0.35 0.89 0.53 1.10 -0.80 1.13 0.32 632±103,4,5,6,7
GC0285 C165 13 25 43.43 -43 04 56.5 4.77 - - - - - - - - - - 20.10 18.98 18.17 0.05 0.04 0.05 - - - - 0.81 1.12 1.93 -
GC0286 pff gc-063 13 25 43.80 -43 07 54.9 7.39 20.66 20.55 19.83 19.37 18.89 0.08 0.03 0.01 0.01 0.03 20.63 20.13 19.45 0.04 0.03 0.03 0.11 0.72 0.46 0.94 0.67 0.50 1.18 554±755
GC0287 pff gc-064 13 25 43.90 -42 50 42.7 10.85 21.16 20.67 19.66 19.07 18.41 0.11 0.03 0.01 0.01 0.03 20.96 19.97 19.20 0.02 0.03 0.01 0.50 1.01 0.59 1.25 0.76 0.99 1.76 560±245,6,7
GC0288 HGHH-35/C35 13 25 44.21 -42 58 59.4 3.72 19.92 19.51 18.58 18.01 17.43 0.13 0.03 0.01 0.01 0.03 19.74 18.79 18.11 0.02 0.02 0.01 0.41 0.93 0.57 1.14 0.68 0.94 1.63 544±133,4,5
GC0289 C16611 13 25 44.90 -43 04 21.1 4.50 - - - - - - - - - - - - 20.72 - - - - - - - - - - -
GC0290 AAT208065 13 25 45.77 -42 34 18.0 27.05 21.79 21.45 20.09 19.40 18.71 0.49 0.05 0.01 0.01 0.03 22.06 20.70 19.66 0.04 0.03 0.02 0.33 1.36 0.69 1.39 1.04 1.36 2.40 836±417
GC0291 WHH-23 13 25 45.90 -42 57 20.2 5.07 19.26 19.12 18.37 17.89 17.41 0.05 0.02 0.01 0.01 0.03 19.13 18.50 18.00 0.03 0.05 0.01 0.14 0.75 0.48 0.96 0.50 0.64 1.14 286±636
GC0292 C16713 13 25 45.97 -43 06 45.4 6.54 - - - - - - - - - - - - 20.41 - - - - - - - - - - -
GC0293 WHH-24 13 25 46.00 -42 56 53.0 5.43 20.64 20.43 19.63 19.12 18.62 0.12 0.04 0.01 0.01 0.03 20.54 19.91 19.25 0.02 0.03 0.01 0.21 0.80 0.51 1.01 0.66 0.63 1.29 566±486
GC0294 AAT119596 13 25 46.06 -43 08 24.5 8.01 21.19 20.69 19.70 19.10 18.51 0.12 0.03 0.01 0.01 0.03 - - - - - - 0.50 1.00 0.60 1.19 - - - 573±537
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0295 HGHH-G378 13 25 46.13 -43 01 22.9 3.39 21.30 20.59 19.53 18.86 18.22 0.55 0.10 0.03 0.02 0.03 - - - - - - 0.71 1.06 0.67 1.31 - - - 487±314,5,7
GC0296 AAT208206 13 25 46.49 -42 34 54.1 26.47 20.08 20.10 19.47 19.07 18.69 0.12 0.02 0.01 0.01 0.03 20.13 19.73 19.19 0.01 0.01 0.01 -0.02 0.63 0.40 0.78 0.55 0.40 0.94 293±1157
GC0297 HGHH-G284 13 25 46.59 -42 57 03.0 5.37 21.47 20.89 19.87 19.28 18.63 0.26 0.05 0.02 0.01 0.03 21.26 20.20 19.41 0.01 0.01 0.01 0.57 1.03 0.58 1.24 0.79 1.06 1.85 479±124,5,7
GC0298 AAT119697 13 25 46.68 -42 53 48.6 8.12 21.61 21.06 20.05 19.49 18.87 0.23 0.05 0.02 0.01 0.03 21.42 20.42 19.65 0.02 0.02 0.01 0.54 1.01 0.57 1.18 0.77 1.01 1.78 633±1087
GC0299 pff gc-065 13 25 46.92 -43 08 06.6 7.81 20.60 20.17 19.23 18.66 18.08 0.08 0.02 0.01 0.01 0.03 20.43 19.55 18.71 0.01 0.01 0.01 0.42 0.94 0.57 1.15 0.83 0.88 1.72 450±445
GC0300 HGHH-G204 13 25 46.99 -43 02 05.4 3.66 19.35 19.12 18.33 17.83 17.31 0.12 0.04 0.01 0.01 0.03 - - - - - - 0.23 0.79 0.51 1.02 - - - 690±184,5,7
GC0301 pff gc-066 13 25 47.14 -43 06 08.8 6.14 21.21 20.82 19.92 19.37 18.80 0.15 0.04 0.01 0.01 0.03 21.07 20.21 19.44 0.01 0.01 0.01 0.39 0.91 0.55 1.11 0.77 0.86 1.63 530±445,7
GC0302 HGHH-G357 13 25 47.78 -43 00 43.4 3.71 20.87 20.55 19.71 19.24 18.71 0.26 0.07 0.02 0.02 0.04 20.71 19.96 19.31 0.01 0.02 0.01 0.33 0.83 0.47 1.00 0.66 0.75 1.41 664±314,5
GC0303 AAT119894 13 25 47.92 -42 55 52.4 6.45 21.45 21.30 20.25 19.59 18.92 0.23 0.07 0.02 0.02 0.03 21.68 20.75 19.85 0.05 0.04 0.03 0.15 1.05 0.66 1.33 0.90 0.93 1.84 448±907
GC0304 C16815 13 25 48.46 -43 07 12.5 7.16 - - - - - - - - - - - - 19.71 - - - - - - - - - - -
GC0305 HGHH-G251 13 25 48.54 -42 57 41.2 5.16 20.50 19.93 18.93 18.33 17.69 0.13 0.03 0.01 0.01 0.03 20.23 19.22 18.46 0.02 0.01 0.01 0.57 1.00 0.60 1.24 0.76 1.01 1.77 574±274,5,7
GC0306 pff gc-067 13 25 48.77 -43 11 38.7 11.19 20.51 20.35 19.60 19.08 18.60 0.07 0.02 0.01 0.01 0.03 20.47 19.87 19.14 0.01 0.01 0.01 0.16 0.75 0.52 1.00 0.74 0.60 1.33 632±435,7
GC0307 pff gc-068 13 25 49.27 -43 02 20.4 4.13 20.73 20.41 19.55 18.99 18.48 0.20 0.05 0.02 0.02 0.03 20.65 20.17 19.13 0.03 0.04 0.01 0.32 0.85 0.56 1.08 1.04 0.48 1.52 393±265,7
GC0308 HGHH-20/C20 13 25 49.69 -42 54 49.3 7.50 19.18 18.83 17.95 17.43 16.88 0.04 0.01 0.01 0.01 0.03 19.01 18.19 17.54 0.03 0.02 0.01 0.35 0.88 0.53 1.07 0.65 0.82 1.47 744±92,5,6,7
GC0309 AAT120259 13 25 49.73 -43 05 04.7 5.64 21.95 21.16 20.12 19.51 18.80 0.35 0.06 0.02 0.01 0.03 21.57 20.48 19.56 0.01 0.01 0.01 0.79 1.04 0.62 1.32 0.92 1.09 2.01 477±547
GC0310 HGHH-48/C48 13 25 49.82 -42 50 15.3 11.62 19.63 19.46 18.67 18.16 17.67 0.04 0.01 0.01 0.01 0.03 19.56 18.92 18.28 0.02 0.02 0.01 0.17 0.79 0.51 1.01 0.64 0.64 1.28 547±194,5,6,7
GC0311 pff gc-069 13 25 49.93 -42 40 08.2 21.40 21.55 20.90 19.87 19.26 18.62 0.41 0.03 0.01 0.01 0.03 21.29 20.24 19.39 0.01 0.01 0.01 0.64 1.03 0.61 1.25 0.85 1.05 1.90 518±315,7
GC0312 HGHH-47/C47 13 25 49.95 -42 52 09.4 9.87 19.80 19.55 18.69 18.18 17.65 0.05 0.02 0.01 0.01 0.03 19.70 18.97 18.30 0.03 0.02 0.01 0.26 0.86 0.51 1.04 0.67 0.73 1.40 589±224,5,6
GC0313 AAT120336 13 25 50.22 -43 06 08.5 6.48 21.66 21.14 20.17 19.57 18.96 0.23 0.05 0.02 0.01 0.03 21.48 20.50 19.67 0.02 0.01 0.01 0.52 0.97 0.60 1.21 0.83 0.97 1.81 452±677
GC0314 WHH-25 13 25 50.34 -43 04 08.2 5.12 21.33 20.93 19.97 19.42 18.83 0.22 0.05 0.02 0.01 0.03 21.19 20.27 19.57 0.02 0.02 0.01 0.40 0.95 0.55 1.14 0.71 0.92 1.62 525±506,7
GC0315 AAT120355 13 25 50.37 -43 00 32.6 4.20 21.26 21.14 20.42 20.02 19.58 0.28 0.09 0.03 0.03 0.04 21.32 20.75 20.17 0.03 0.03 0.01 0.12 0.72 0.39 0.84 0.59 0.56 1.15 548±777
GC0316 pff gc-070 13 25 50.40 -42 58 02.3 5.20 20.39 20.23 19.42 18.94 18.45 0.12 0.04 0.01 0.01 0.03 20.35 19.67 19.06 0.01 0.01 0.01 0.16 0.81 0.48 0.97 0.61 0.68 1.29 556±495
GC0317 C169 13 25 51.01 -42 55 36.3 7.00 - - - - - - - - - - 21.60 21.00 20.39 0.03 0.03 0.02 - - - - 0.62 0.60 1.21 -
GC0318 AAT120515 13 25 51.31 -42 59 29.4 4.64 21.11 20.81 19.92 19.38 18.81 0.21 0.06 0.02 0.02 0.03 21.04 20.24 19.46 0.04 0.04 0.01 0.30 0.90 0.53 1.11 0.77 0.81 1.58 461±1417
GC0319 pff gc-071 13 25 51.54 -42 59 46.8 4.58 20.79 20.59 19.82 19.34 18.83 0.16 0.05 0.02 0.02 0.03 20.71 20.07 19.45 0.01 0.01 0.01 0.20 0.77 0.48 0.99 0.62 0.64 1.27 475±415
GC0320 C102 13 25 52.07 -42 59 14.4 4.87 - - 21.43 - - - - - - - 22.71 21.87 21.04 0.02 0.02 0.02 - - - - 0.83 0.84 1.67 -
GC0321 pff gc-072 13 25 52.14 -42 58 30.2 5.20 20.68 20.45 19.62 19.12 18.54 0.15 0.04 0.02 0.01 0.03 20.64 19.92 19.25 0.02 0.02 0.01 0.23 0.83 0.51 1.08 0.67 0.72 1.39 504±225
GC0322 HGHH-21/C21 13 25 52.74 -43 05 46.4 6.52 19.16 18.76 17.87 17.32 16.77 0.04 0.01 0.01 0.01 0.03 18.97 18.17 17.40 0.03 0.02 0.01 0.40 0.89 0.55 1.11 0.77 0.80 1.58 462±23,5,6,7,8
GC0323 pff gc-073 13 25 52.78 -42 58 41.7 5.21 21.36 20.94 19.97 19.38 18.74 0.25 0.06 0.02 0.02 0.03 21.25 20.29 19.50 0.02 0.01 0.01 0.42 0.98 0.58 1.22 0.79 0.97 1.76 401±295,6,7
GC0324 HGHH-G256 13 25 52.88 -43 02 00.0 4.70 20.69 20.18 19.00 18.35 17.65 0.18 0.04 0.01 0.01 0.03 20.50 19.31 18.44 0.03 0.04 0.01 0.51 1.17 0.65 1.36 0.87 1.20 2.06 495±184,5,7
GC0325 AAT209412 13 25 53.30 -42 30 52.7 30.63 21.94 21.23 20.22 19.60 18.97 0.52 0.04 0.01 0.01 0.03 21.69 20.64 19.76 0.01 0.01 0.01 0.71 1.01 0.62 1.25 0.88 1.05 1.92 998±1357
GC0326 pff gc-074 13 25 53.37 -42 51 12.4 11.00 21.16 20.83 20.00 19.48 18.90 0.11 0.03 0.01 0.01 0.03 21.04 20.27 19.56 0.01 0.01 0.01 0.33 0.83 0.52 1.10 0.71 0.77 1.48 471±245,7
GC0327 pff gc-075 13 25 53.50 -43 03 56.6 5.50 20.96 20.45 19.48 18.90 18.28 0.14 0.03 0.01 0.01 0.03 20.78 19.76 19.01 0.02 0.03 0.01 0.51 0.97 0.58 1.20 0.75 1.02 1.77 748±185,6,7
GC0328 HGHH-22/C22 13 25 53.57 -42 59 07.6 5.16 19.39 19.06 18.15 17.62 17.07 0.05 0.02 0.01 0.01 0.03 19.21 18.34 17.70 0.02 0.03 - 0.34 0.90 0.54 1.09 0.64 0.87 1.52 578±12,4,5,7,8
GC0329 pff gc-076 13 25 53.75 -43 19 48.6 19.26 20.67 20.06 19.07 18.41 17.78 0.08 0.02 0.01 0.01 0.03 20.44 19.44 18.52 0.02 0.01 0.01 0.62 0.99 0.66 1.29 0.92 1.00 1.92 368±155,6,7
GC0330 AAT120976 13 25 54.28 -42 56 20.6 6.84 21.51 21.23 20.38 19.84 19.27 0.23 0.06 0.02 0.02 0.03 21.50 20.73 19.99 0.03 0.02 0.02 0.28 0.85 0.54 1.11 0.74 0.77 1.51 595±697
GC0331 AAT328533 13 25 54.39 -43 18 40.1 18.19 21.79 21.26 20.31 19.74 19.09 0.16 0.04 0.01 0.01 0.03 21.62 20.64 19.77 0.01 0.01 0.01 0.53 0.95 0.58 1.23 0.87 0.98 1.85 577±897
GC0332 HGHH-23/C23 13 25 54.58 -42 59 25.4 5.22 18.92 18.29 17.22 16.62 15.95 0.04 0.01 0.01 0.01 0.03 18.59 17.44 16.69 0.01 0.03 - 0.63 1.07 0.60 1.28 0.75 1.15 1.90 674±12,3,5,7,8
GC0333 C103 13 25 54.98 -42 59 15.4 5.36 - - 18.88 - - - - - - - 20.43 20.44 18.44 0.01 0.02 0.02 - - - - 2.00 -0.01 1.99 -
GC0334 C170 13 25 56.11 -42 56 12.9 7.17 - - - - - - - - - - 23.31 22.83 22.16 0.05 0.04 0.06 - - - - 0.67 0.48 1.15 -
GC0335 AAT121367 13 25 56.26 -43 01 32.9 5.25 21.06 20.92 20.24 19.82 19.39 0.25 0.08 0.03 0.03 0.04 21.01 20.45 19.85 0.01 0.01 0.01 0.13 0.68 0.42 0.85 0.60 0.56 1.15 438±807
GC0336 WHH-26 13 25 56.59 -42 51 46.6 10.76 20.50 20.02 19.05 18.43 17.81 0.07 0.02 0.01 0.01 0.03 20.33 19.36 18.56 0.02 0.01 0.01 0.48 0.97 0.62 1.24 0.79 0.97 1.76 412±366
GC0337 AAT329209 13 25 57.28 -43 41 09.0 40.37 20.87 20.70 19.87 19.40 18.90 0.21 0.02 0.01 0.01 0.03 20.78 20.12 19.35 0.01 - 0.01 0.17 0.82 0.47 0.97 0.77 0.66 1.43 601±657
GC0338 C171 13 25 57.78 -42 55 36.1 7.82 - - - - - - - - - - 22.25 21.45 20.67 0.04 0.03 0.02 - - - - 0.78 0.79 1.58 -
GC0339 C172 13 25 57.95 -42 53 04.3 9.79 - - - - - - - - - - 22.15 21.45 20.91 0.02 0.01 0.01 - - - - 0.55 0.70 1.24 -
GC0340 pff gc-077 13 25 58.15 -42 31 38.2 30.03 20.57 20.32 19.50 18.96 18.47 0.16 0.02 0.01 0.01 0.03 20.55 19.83 19.09 0.02 0.01 0.01 0.24 0.83 0.53 1.03 0.74 0.71 1.45 675±415
GC0341 pff gc-078 13 25 58.47 -43 08 06.3 8.96 20.93 20.34 19.30 18.69 18.02 0.10 0.02 0.01 0.01 0.03 20.70 19.68 18.75 0.02 0.01 0.01 0.59 1.03 0.62 1.28 0.93 1.02 1.95 545±185,7
GC0342 HGHH-G143 13 25 58.69 -43 07 11.0 8.29 20.31 20.02 19.21 18.68 18.18 0.06 0.02 0.01 0.01 0.03 20.22 19.52 18.77 0.02 0.01 0.01 0.29 0.81 0.53 1.03 0.75 0.70 1.45 503±384,5,7
GC0343 pff gc-079 13 25 58.91 -42 53 18.9 9.70 20.74 20.43 19.58 19.06 18.52 0.10 0.03 0.01 0.01 0.03 20.62 19.86 19.14 0.02 0.01 0.01 0.30 0.86 0.51 1.06 0.72 0.77 1.48 410±215,7
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0344 AAT121826/C104 13 25 59.49 -42 55 30.8 8.10 20.91 20.65 19.81 19.28 18.73 0.13 0.03 0.01 0.01 0.03 20.81 20.15 19.40 0.02 0.02 0.01 0.26 0.83 0.53 1.08 0.74 0.66 1.40 448±987
GC0345 pff gc-080 13 25 59.55 -42 32 39.4 29.08 21.10 20.80 19.96 19.40 18.84 0.25 0.03 0.01 0.01 0.03 21.07 20.32 19.56 0.02 0.01 0.01 0.29 0.85 0.56 1.11 0.75 0.75 1.51 598±565,7
GC0346 C173 13 25 59.57 -42 55 01.5 8.46 - - - - - - - - - - 23.15 22.00 21.06 0.04 0.03 0.02 - - - - 0.94 1.15 2.09 -
GC0347 C174 13 25 59.63 -42 55 15.7 8.30 - - - - - - - - - - 23.24 22.42 21.42 0.04 0.04 0.03 - - - - 0.99 0.82 1.81 -
GC0348 pff gc-081 13 26 00.15 -42 49 00.7 13.51 20.43 20.17 19.34 18.80 18.28 0.07 0.02 0.01 0.01 0.03 20.36 19.61 18.93 0.02 0.01 0.01 0.26 0.83 0.53 1.05 0.69 0.75 1.43 304±315,7
GC0349 K-217 13 26 00.81 -43 09 40.1 10.46 21.63 21.09 20.09 19.54 18.91 0.16 0.03 0.01 0.01 0.03 21.42 20.48 19.57 0.01 0.01 0.01 0.54 0.99 0.56 1.19 0.91 0.94 1.85 315±1577
GC0350 C175 13 26 00.93 -42 58 28.9 6.65 - - - - - - - - - - 23.51 22.53 21.84 0.06 0.04 0.03 - - - - 0.69 0.97 1.67 -
GC0351 pff gc-082 13 26 00.98 -42 22 03.4 39.56 20.83 20.17 19.16 18.58 17.89 0.21 0.02 0.01 0.01 0.03 20.51 19.53 18.69 0.02 0.01 0.01 0.66 1.01 0.58 1.27 0.84 0.98 1.82 573±195,7
GC0352 AAT122146 13 26 01.00 -43 06 55.3 8.40 21.14 20.90 20.05 19.53 19.04 0.11 0.03 0.01 0.01 0.03 21.09 20.38 19.58 0.01 0.01 0.01 0.24 0.85 0.52 1.01 0.80 0.71 1.51 517±997
GC0353 HGHH-G221 13 26 01.11 -42 55 13.5 8.52 20.87 20.24 19.30 18.75 18.13 0.10 0.02 0.01 0.01 0.03 20.54 19.60 18.83 0.01 0.01 0.01 0.62 0.94 0.55 1.16 0.77 0.94 1.72 390±154,5
GC0354 AAT329848 13 26 01.29 -43 34 15.5 33.68 19.44 19.19 18.39 17.89 17.37 0.08 0.01 0.01 0.01 0.03 - - - - - - 0.25 0.79 0.50 1.03 - - - 558±467
GC0355 pff gc-083 13 26 01.83 -42 58 15.0 6.89 21.23 20.80 19.86 19.30 18.72 0.16 0.04 0.01 0.01 0.03 21.12 20.21 19.44 0.02 0.02 0.01 0.42 0.95 0.55 1.13 0.77 0.91 1.68 458±315,6,7
GC0356 pff gc-084 13 26 02.25 -43 08 55.6 10.03 21.31 20.80 19.84 19.24 18.63 0.12 0.03 0.01 0.01 0.03 21.13 20.19 19.32 0.02 0.01 0.01 0.51 0.97 0.59 1.21 0.87 0.93 1.80 458±385,7
GC0357 AAT122445 13 26 02.43 -43 00 11.7 6.43 21.13 20.99 20.28 19.81 19.42 0.15 0.05 0.02 0.02 0.03 21.08 20.50 19.92 0.01 0.02 0.01 0.14 0.71 0.47 0.86 0.58 0.58 1.16 342±987
GC0358 C176 13 26 02.79 -42 57 05.0 7.61 - - - - - - - - - - 22.35 21.92 21.30 0.02 0.02 0.03 - - - - 0.62 0.43 1.05 -
GC0359 HGHH-25/C25 13 26 02.85 -42 56 57.0 7.69 20.17 19.56 18.49 17.85 17.17 0.07 0.02 0.01 0.01 0.03 19.92 18.83 17.97 0.03 0.02 0.01 0.61 1.07 0.64 1.32 0.86 1.09 1.95 703±93,5,7
GC0360 AAT122526 13 26 02.90 -43 05 43.0 7.90 21.89 21.35 20.36 19.73 19.05 0.24 0.05 0.02 0.01 0.03 21.72 20.72 19.81 0.02 0.01 0.01 0.54 1.00 0.62 1.31 0.90 1.00 1.90 506±507
GC0361 C177 13 26 03.20 -42 54 30.1 9.30 - - - - - - - - - - 22.95 22.11 21.09 0.11 0.07 0.05 - - - - 1.02 0.84 1.87 -
GC0362 C178 13 26 03.85 -42 56 45.3 7.95 - - - - - - - - - - 23.02 22.32 21.53 0.04 0.04 0.03 - - - - 0.79 0.69 1.48 -
GC0363 HGHH-G293/G293 13 26 04.20 -42 55 44.7 8.60 20.11 19.90 19.10 18.61 18.11 0.06 0.02 0.01 0.01 0.03 20.04 19.36 18.69 0.01 0.01 0.01 0.21 0.80 0.49 0.99 0.67 0.69 1.35 581±154,5,7
GC0364 AAT122808 13 26 04.61 -43 09 10.2 10.49 21.05 20.87 20.12 19.66 19.18 0.10 0.03 0.01 0.01 0.03 21.00 20.45 19.69 0.01 0.01 0.01 0.18 0.75 0.46 0.94 0.76 0.55 1.31 264±1317
GC0365 AAT122794 13 26 04.69 -42 47 35.1 15.16 21.89 21.15 20.00 19.29 18.69 0.21 0.04 0.01 0.01 0.03 21.60 20.37 19.38 0.01 0.01 0.01 0.74 1.15 0.71 1.31 0.98 1.23 2.22 336±1617
GC0366 C105 13 26 05.12 -42 55 37.0 8.80 - - 22.01 - - - - - - - 23.68 22.58 21.76 0.07 0.04 0.04 - - - - 0.82 1.10 1.92 -
GC0367 HGHH-07/C7 13 26 05.41 -42 56 32.4 8.30 18.38 18.03 17.17 16.65 16.08 0.03 0.01 0.01 0.01 0.03 18.18 17.33 16.64 0.03 0.03 0.01 0.35 0.86 0.53 1.09 0.68 0.85 1.53 595±11,2,3,5,6,7,8
GC0368 C106 13 26 06.15 -42 56 45.4 8.32 - - 21.28 - - - - - - - 22.54 21.46 20.66 0.03 0.01 0.01 - - - - 0.80 1.08 1.88 -
GC0369 pff gc-085 13 26 06.42 -43 00 38.1 7.11 20.39 20.20 19.43 18.99 18.47 0.07 0.02 0.01 0.01 0.03 20.29 19.64 19.03 0.02 0.02 0.01 0.20 0.76 0.44 0.96 0.61 0.65 1.26 548±315,6,7
GC0370 pff gc-086 13 26 06.55 -43 06 14.5 8.75 21.48 20.93 19.95 19.37 18.76 0.16 0.03 0.01 0.01 0.03 21.29 20.32 19.45 0.02 0.01 0.01 0.56 0.97 0.59 1.20 0.87 0.97 1.84 440±265,7
GC0371 pff gc-087 13 26 06.87 -42 33 17.3 28.77 20.26 19.96 19.11 18.56 18.05 0.14 0.02 0.01 0.01 0.03 20.17 19.42 18.70 0.02 0.01 0.01 0.30 0.86 0.55 1.05 0.73 0.75 1.47 830±295,7
GC0372 HGHH-G170 13 26 06.93 -42 57 35.1 8.02 20.78 20.21 19.22 18.65 17.97 0.11 0.02 0.01 0.01 0.03 20.57 19.56 18.73 0.02 0.02 0.01 0.57 0.99 0.57 1.25 0.83 1.01 1.84 636±274,5,7
GC0373 AAT123188 13 26 06.94 -43 07 52.6 9.85 21.70 21.30 20.40 19.85 19.27 0.17 0.04 0.01 0.01 0.03 21.57 20.71 19.94 0.02 0.01 0.01 0.40 0.90 0.56 1.13 0.77 0.86 1.63 364±567
GC0374 HGHH-36/C36/R113 13 26 07.73 -42 52 00.3 11.72 19.42 19.19 18.35 17.81 17.33 0.04 0.01 0.01 0.01 0.03 19.32 18.61 17.94 0.02 0.01 0.01 0.23 0.84 0.54 1.03 0.67 0.71 1.38 703±13,5,6,7,8
GC0375 AAT123453 13 26 08.38 -42 59 18.9 7.67 21.29 20.95 20.09 19.55 19.03 0.17 0.04 0.02 0.01 0.03 21.20 20.40 19.67 0.03 0.02 0.01 0.34 0.86 0.54 1.06 0.73 0.80 1.53 257±1547
GC0376 pff gc-088 13 26 08.86 -43 01 21.4 7.54 19.99 19.79 18.99 18.46 18.00 0.05 0.02 0.01 0.01 0.03 19.86 19.14 18.59 0.03 0.03 0.01 0.20 0.80 0.53 0.99 0.55 0.72 1.27 554±295,7
GC0377 AAT123656 13 26 09.61 -43 07 05.9 9.71 21.77 21.13 20.08 19.46 18.79 0.19 0.04 0.01 0.01 0.03 21.57 20.51 19.59 0.03 0.02 0.02 0.64 1.05 0.63 1.29 0.92 1.07 1.99 380±937
GC0378 R111 13 26 09.71 -42 50 29.5 13.14 22.07 21.57 20.59 19.91 19.09 0.28 0.06 0.02 0.02 0.03 21.96 21.03 20.20 0.03 0.03 0.02 0.51 0.97 0.68 1.50 0.82 0.94 1.76 717±485,7
GC0379 C179 13 26 09.87 -42 56 36.0 8.96 - - - - - - - - - - 22.13 21.71 21.04 0.03 0.03 0.01 - - - - 0.67 0.42 1.09 -
GC0380 HGHH-37/C37/R116 13 26 10.58 -42 53 42.7 10.81 19.86 19.38 18.43 17.87 17.26 0.04 0.01 0.01 0.01 0.03 19.65 18.72 17.96 0.01 0.01 0.01 0.48 0.95 0.56 1.17 0.76 0.93 1.69 612±13,5,6,7,8
GC0381 WHH-27 13 26 12.82 -43 09 09.2 11.51 20.27 19.68 18.66 18.06 17.42 0.05 0.01 0.01 0.01 0.03 20.02 19.03 18.13 0.02 0.01 0.01 0.59 1.02 0.60 1.24 0.90 0.99 1.89 545±606
GC0382 WHH-28 13 26 14.18 -43 08 30.4 11.25 20.21 19.98 19.17 18.65 18.14 0.05 0.02 0.01 0.01 0.03 20.13 19.48 18.71 0.02 0.01 0.01 0.23 0.81 0.52 1.03 0.77 0.65 1.41 506±1236
GC0383 HHH86-26/C26 13 26 15.27 -42 48 29.4 15.36 19.99 19.26 18.13 17.47 16.77 0.05 0.01 0.01 0.01 0.03 19.66 18.45 17.59 0.04 0.03 0.02 0.73 1.13 0.66 1.35 0.86 1.21 2.07 377±142,5,6,7
GC0384 R122 13 26 15.95 -42 55 00.5 10.76 19.02 18.78 18.02 17.58 17.14 0.03 0.01 0.01 0.01 0.03 - - - - - - 0.24 0.76 0.44 0.88 - - - 588±28
GC0385 AAT125079 13 26 17.29 -43 06 39.3 10.62 21.13 20.90 20.09 19.59 19.06 0.10 0.03 0.01 0.01 0.03 21.07 20.41 19.64 0.02 0.01 0.01 0.23 0.81 0.51 1.03 0.77 0.66 1.43 513±1837
GC0386 C50/K-233 13 26 19.66 -43 03 18.6 9.76 20.09 19.68 18.74 18.17 17.57 0.05 0.02 0.01 0.01 0.03 19.91 18.92 18.28 0.04 0.04 0.01 0.41 0.93 0.58 1.17 0.64 1.00 1.63 615±586,7
GC0387 C49/pff gc-089 13 26 20.20 -43 10 35.7 13.48 19.90 19.73 18.95 18.45 17.95 0.12 0.02 0.01 0.01 0.03 19.85 19.30 18.53 0.03 0.02 0.01 0.17 0.78 0.50 1.00 0.77 0.56 1.32 538±305,6,7
GC0388 pff gc-090 13 26 20.53 -43 03 18.5 9.91 20.90 20.34 19.33 18.74 18.10 0.10 0.02 0.01 0.01 0.03 20.70 19.61 18.85 0.03 0.03 0.01 0.56 1.00 0.60 1.24 0.75 1.09 1.85 486±265,7
GC0389 AAT215171 13 26 20.66 -42 38 32.0 24.60 21.03 20.63 19.69 19.11 18.53 0.27 0.03 0.01 0.01 0.03 20.97 20.06 19.26 0.02 0.02 0.01 0.40 0.94 0.58 1.15 0.80 0.90 1.70 527±487
GC0390 R107 13 26 21.11 -42 48 41.1 15.84 21.53 20.82 19.75 19.13 18.48 0.16 0.03 0.01 0.01 0.03 21.23 20.16 19.30 0.05 0.03 0.02 0.71 1.07 0.62 1.27 0.86 1.06 1.92 405±285,7
GC0391 pff gc-091 13 26 21.14 -43 42 24.6 42.41 20.42 20.13 19.29 18.77 18.21 0.15 0.02 0.01 0.01 0.03 20.30 19.56 18.72 0.01 0.01 0.01 0.29 0.84 0.52 1.08 0.84 0.74 1.58 623±375,7
GC0392 pff gc-092 13 26 21.31 -42 57 19.1 10.53 21.36 20.86 19.92 19.35 18.76 0.14 0.03 0.01 0.01 0.03 21.18 20.27 19.46 0.02 0.02 0.01 0.50 0.93 0.57 1.16 0.81 0.92 1.73 462±275,7
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0393 R117 13 26 21.99 -42 53 45.5 12.38 20.52 20.41 19.68 19.23 18.75 0.07 0.02 0.01 0.01 0.03 20.50 19.98 19.32 0.02 0.02 0.01 0.10 0.73 0.45 0.93 0.66 0.53 1.18 484±265,7
GC0394 R118 13 26 22.01 -42 54 26.5 11.99 20.73 20.60 19.87 19.38 18.93 0.08 0.03 0.01 0.01 0.03 20.72 20.19 19.50 0.03 0.02 0.01 0.13 0.73 0.49 0.95 0.70 0.52 1.22 440±735
GC0395 WHH-29 13 26 22.08 -43 09 10.7 12.79 20.97 20.70 19.82 19.28 18.73 0.08 0.02 0.01 0.01 0.03 20.92 20.17 19.38 0.03 0.02 0.01 0.27 0.88 0.54 1.09 0.79 0.75 1.54 505±786
GC0396 pff gc-093 13 26 22.65 -42 46 49.8 17.50 20.58 20.39 19.62 19.13 18.66 0.08 0.03 0.01 0.01 0.03 20.52 19.91 19.23 0.02 0.01 0.01 0.20 0.77 0.48 0.96 0.69 0.61 1.30 576±425,7
GC0397 WHH-30 13 26 23.60 -43 03 43.9 10.55 20.56 20.25 19.38 18.83 18.30 0.10 0.03 0.01 0.01 0.03 20.45 19.62 18.96 0.03 0.03 0.01 0.31 0.87 0.55 1.08 0.65 0.83 1.49 470±666
GC0398 pff gc-094 13 26 23.66 -43 00 45.6 10.25 20.99 20.77 19.97 19.49 18.93 0.09 0.03 0.01 0.01 0.03 20.92 20.24 19.57 0.03 0.02 0.01 0.22 0.80 0.47 1.04 0.67 0.68 1.35 334±645,7
GC0399 HHH86-38/C38/R123 13 26 23.78 -42 54 01.1 12.50 19.67 19.30 18.41 17.87 17.32 0.04 0.01 0.01 0.01 0.03 19.51 18.68 17.96 0.02 0.02 0.01 0.37 0.89 0.54 1.09 0.72 0.83 1.54 405±13,5,6,8
GC0400 HGHH-51 13 26 23.86 -42 47 17.1 17.26 19.63 19.34 18.47 17.93 17.38 0.05 0.02 0.01 0.01 0.03 - - - - - - 0.29 0.87 0.54 1.09 - - - 343±434,5
GC0401 AAT335187 13 26 23.95 -43 17 44.4 19.53 21.19 21.11 20.46 20.04 19.60 0.10 0.03 0.01 0.01 0.03 21.20 20.72 20.08 0.01 0.01 0.01 0.08 0.65 0.42 0.86 0.64 0.49 1.12 277±1587
GC0402 pff gc-095 13 26 25.50 -42 57 06.2 11.33 21.13 20.60 19.60 19.02 18.40 0.11 0.02 0.01 0.01 0.03 20.97 19.97 19.17 0.04 0.03 0.02 0.53 1.00 0.58 1.20 0.80 0.99 1.79 405±185,7
GC0403 R124 13 26 28.87 -42 52 36.4 14.08 20.32 20.17 19.42 18.96 18.43 0.05 0.02 0.01 0.01 0.03 20.28 19.69 19.02 0.02 0.02 0.01 0.15 0.75 0.46 0.99 0.68 0.58 1.26 541±355,7
GC0404 pff gc-096 13 26 30.29 -42 34 41.7 28.83 21.24 20.73 19.73 19.10 18.42 0.31 0.03 0.01 0.01 0.03 21.08 20.09 19.24 0.01 0.01 0.01 0.52 1.00 0.63 1.30 0.85 0.99 1.83 532±255,7
GC0405 R105 13 26 33.55 -42 51 00.9 15.74 21.28 20.78 19.86 19.28 18.70 0.11 0.03 0.01 0.01 0.03 21.18 20.25 19.46 0.02 0.01 0.01 0.50 0.92 0.58 1.15 0.79 0.93 1.72 534±345,7
GC0406 HGHH-27/C27 13 26 37.99 -42 45 49.9 20.00 19.60 19.39 18.60 18.11 17.62 0.03 0.01 0.01 0.01 0.03 - - - - - - 0.21 0.78 0.49 0.98 - - - 492±372,5
GC0407 WHH-31 13 26 41.43 -43 11 25.0 16.96 20.76 20.44 19.50 18.94 18.36 0.07 0.02 0.01 0.01 0.03 20.67 19.89 19.05 0.03 0.02 0.02 0.32 0.94 0.56 1.14 0.85 0.77 1.62 573±676
GC0408 HHH86-39/C39 13 26 42.03 -43 07 44.8 15.12 18.72 18.33 17.43 16.91 16.42 0.02 0.01 0.01 0.01 0.03 18.57 17.73 16.92 0.01 0.01 - 0.39 0.89 0.53 1.01 0.81 0.83 1.65 271±203,5,6,7
GC0409 pff gc-097 13 26 45.40 -43 26 34.1 29.13 19.75 19.51 18.72 18.23 17.76 0.10 0.01 0.01 0.01 0.03 19.66 19.04 18.28 0.02 0.01 0.01 0.24 0.79 0.49 0.96 0.76 0.62 1.38 599±305,7
GC0410 HH-017 13 26 49.31 -43 04 57.8 15.41 23.21 22.54 20.80 19.87 19.06 0.67 0.11 0.02 0.01 0.03 23.32 21.63 20.13 0.05 0.03 0.02 0.67 1.75 0.93 1.73 1.50 1.68 3.19 839±637
GC0411 pff gc-098 13 26 53.94 -43 19 17.7 24.05 19.54 19.17 18.28 17.73 17.16 0.09 0.01 0.01 0.01 0.03 - - - - - - 0.37 0.89 0.55 1.12 - - - 631±185,7
GC0412 AAT222977 13 26 58.91 -42 38 53.4 27.82 21.18 21.02 20.34 19.84 19.38 0.28 0.03 0.01 0.01 0.03 21.16 20.64 20.02 0.02 0.01 0.01 0.17 0.68 0.50 0.96 0.62 0.52 1.14 655±1127
GC0413 HH-060 13 26 59.78 -42 55 26.5 17.79 - - - - - - - - - - 23.41 21.69 20.14 0.05 0.04 0.02 - - - - 1.55 1.72 3.26 811±327
GC0414 pff gc-099 13 26 59.82 -42 32 40.5 33.09 20.96 20.72 19.94 19.40 18.92 0.23 0.03 0.01 0.01 0.03 20.92 20.29 19.59 0.02 0.01 0.02 0.25 0.78 0.53 1.02 0.70 0.63 1.33 425±345,7
GC0415 pff gc-100 13 27 03.41 -42 27 17.2 38.12 19.92 19.37 18.41 17.81 17.17 0.11 0.01 0.01 0.01 0.03 - - - - - - 0.56 0.96 0.60 1.24 - - - 513±105,7
GC0416 pff gc-101 13 27 21.56 -42 38 41.4 30.63 19.89 19.51 18.72 18.20 17.74 0.10 0.01 0.01 0.01 0.03 19.74 19.02 18.39 0.01 0.01 - 0.38 0.79 0.51 0.97 0.63 0.72 1.35 263±165,7
GC0417 pff gc-102 13 28 18.45 -42 33 12.5 41.90 20.38 20.11 19.29 18.76 18.24 0.14 0.02 0.01 0.01 0.03 20.28 19.59 18.94 0.04 0.04 0.01 0.27 0.83 0.52 1.04 0.65 0.70 1.34 428±405,7
1Radial velocity measured by van den Bergh, Hesser, & Harris (1981).
2Radial velocity measured by Hesser et al. (1984).
3Radial velocity measured by Hesser, Harris, & Harris (1986).
4Radial velocity measured by Harris et al. (1992).
5Radial velocity measured by Peng, Ford, & Freeman (2004a).
6Radial velocity measured by Woodley, Harris, & Harris (2005).
7Radial velocity measured by Beasley et al. (2006).
8Radial velocity measured by Rejkuba et al. (2007).
9These objects appear starlike under HST/ACS imaging (Harris et al. 2006).
10This object appears to be a M-type star based on the strong molecular bands in its spectrum (Beasley et al. 2006).
11Faint globular (Harris et al. 2006).
12ocated in the inner bulge region which is very crowded (Harris et al. 2006).
13A very compact globular or star (Harris et al. 2006).
14A possible globular, but slightly elliptical (Harris et al. 2006).
15A globular next to a very bright star (Harris et al. 2006).
– 39 –
Table 2. Kinematic and Dynamic Solutions for the Globular Cluster System of NGC 51281
Radial Bin Rmean Rout N ΩR Θo σv Mcorr Mp Mr Mt
(kpc) (kpc) (kpc) (km s−1) (o E of N) (km s−1) (×1010M⊙) (×10
10M⊙) (×10
10M⊙)
0-50 12.9 48.8 340 40±10 189±12 123±5 1.0 125.8±46.52 3.1±1.3 128.9±46.5
0-5 3.64 4.96 54 24±21 334±59 120±12 - - - -
5-10 7.65 9.96 124 43±15 195±20 112±8 2.3 37.4±6.4 0.4±0.3 37.8±6.4
10-15 12.4 14.9 68 83±25 195±12 105±10 1.6 36.5±9.3 2.4±1.5 38.9±9.4
15-25 19.0 24.3 56 35±26 184±34 147±16 1.3 89.5±27.4 0.7±1.0 90.2±27.4
25-50 34.7 48.8 39 96±45 169±17 148±21 1.0 184.7±84.5 10.4±9.8 195.1±85.1
1This table is reproduced from Woodley (2006) for completeness.
2The Tracer Mass estimator determines the total mass enclosed within the outermost radius using a sample defined in the range of the
inner and outer radial bins.
Table 3. Kinematic and Dynamic Solutions for the Metal-Poor Globular Cluster System
of NGC 5128
Radial Bin Rmean Rout N ΩR Θo σv Mcorr Mp Mr Mt
(kpc) (kpc) (kpc) (km s−1) (o E of N) (km s−1) (×1010M⊙) (×10
10M⊙) (×10
10M⊙)
0-50 13.8 48.1 178 31±14 177±22 117±7 1.0 94.5±58.5 1.1±1.0 95.6 ±58.6
0-5 3.84 4.96 22 16±38 373±120 99±19 - - - -
5-10 7.76 9.96 66 30±21 223±39 116±12 2.1 38.9±12.4 0.2±0.3 39.1±12.4
10-15 12.7 14.8 41 97±38 199±13 102±15 1.5 31.4±15.1 3.3±2.5 34.6±15.3
15-25 18.8 24.3 26 45±31 139±49 112±20 1.3 59.7±32.7 1.2±1.6 60.8±32.7
25-50 36.7 48.1 23 61±43 137±50 141±24 1.0 122.4±82.9 4.2±5.9 126.7±83.1
Table 4. Kinematic and Dynamic Solutions for the Metal-Rich Globular Cluster System
of NGC 5128
Radial Bin Rmean Rout N ΩR Θo σv Mcorr Mp Mr Mt
(kpc) (kpc) (kpc) (km s−1) (o E of N) (km s−1) (×1010M⊙) (×10
10M⊙) (×10
10M⊙)
0-50 12.0 48.8 158 47±15 202±15 129±9 1.0 116.5±73.8 4.3±2.3 120.8±73.9
0-5 3.61 4.98 29 44±27 308±47 134±23 - - - -
5-10 7.52 9.93 58 65±22 180±19 105±11 1.5 17.4±7.7 1.0±0.7 18.3±7.7
10-15 12.0 14.9 27 74±34 186±22 108±17 1.2 23.8±11.3 1.9±1.8 25.7±13.3
15-25 19.3 24.3 30 50±36 223±32 168±24 1.1 72.1±46.2 1.2±1.7 73.3±46.3
25-50 31.7 48.8 15 102±96 191±21 146±65 1.0 219.1±174.6 11.8±22.2 230.9±176.0
– 40 –
Table 5. Kinematic and Dynamic Solutions for the Planetary Nebula System of NGC
Radial Bin Rmean Rout N ΩR Θo σv Mcorr Mp Mr Mt
(kpc) (kpc) (kpc) (km s−1) (o E of N) (km s−1) (×1010M⊙) (×10
10M⊙) (×10
10M⊙)
0-90 14.1 88.2 780 76±6 170±5 118±13 1.0 84.6±17.2 11.9±1.9 96.5±17.3
0-5 3.3 4.99 184 75±16 179±11 131±7 - - - -
5-10 7.6 9.98 211 82±12 177±8 120±6 3.0 43.9±3.6 1.6±0.5 45.4±3.6
10-15 11.8 14.8 138 76±15 171±10 118±7 2.0 42.3±5.0 2.0±0.8 44.2±5.1
15-20 17.4 20.0 71 96±24 169±12 116±10 1.7 47.7±5.6 4.3±2.1 52.0±6.9
20-30 24.6 30.0 87 76±17 157±17 108±8 1.5 53.2±8.4 4.0±1.8 57.2±8.6
30-40 34.6 39.8 50 44±15 132±38 87±9 1.3 40.7±7.4 1.8±1.2 42.3±7.5
40-80 48.7 71.2 36 61±45 183±22 85±11 1.0 48.6±11.5 6.2±9.1 54.8±14.7
Table 6. Spin Parameters for Giant Elliptical Galaxies
Galaxy ΩRMP σv,MP (ΩR/σv)MP ΛMP ΩRMR σv,MR (ΩR/σv)MR ΛMR
(km s−1) (km s−1) (km s−1) (km s−1)
NGC 5128 31±14 117±7 0.26±0.12 0.08±0.04 47±15 129±9 0.36±0.11 0.11±0.03
M878,9 186+58
397+36
0.47+0.13
−0.11 0.14
+0.04
−0.03 155
365+38
0.43+0.14
−0.12 0.13
+0.04
−0.04
M499 93+69
342+33
0.27+0.19
−0.11 0.08
+0.06
−0.03 -26
265+34
0.10+0.27
−0.25 0.03
+0.08
−0.08
NGC 139910 15±26 291±14 0.05±0.09 0.02±0.03 7±24 255±13 0.03±0.09 0.01±0.03
8Kinematic data taken from Côté et al. (2001).
9Kinematic data taken from Côté et al. (2003).
10Kinematic data taken from Richtler et al. (2004).
– 41 –
Fig. 1.— Positions of the GCS (left) totaling 340 objects and the PN system (right) totaling
780 objects in NGC 5128. The PN system has more than double the objects and extends
∼ 40 kpc further out from the center of NGC 5128. Both systems are spatially biased to the
major axis of the galaxy with a position angle of 35o east of north.
– 42 –
Fig. 2.— Velocity histograms fit with a Gaussian (mean velocity and standard deviation in
km s−1) for the samples. Top left, the entire GC (546.4 ± 7.3, 128.8 ± 7.3); top right, GCs
with a radial velocity uncertainty < 50 km s−1 (554.8 ± 5.3, 126.2 ± 7.3); bottom left, all
metal-poor GCs (532.5 ± 12.7, 123.8 ± 12.8); bottom right, all metal-rich GCs (565.5 ± 10.5,
140.3 ± 10.7).
– 43 –
Fig. 3.— Projected radial distribution as a function of projected angular position of all known
GCs in NGC 5128. The angular distribution of metal-poor (squares), metal-rich (crosses),
and unknown metallicity (circles) subpopulations of GCs clearly shows the observational
bias in GC searches along the photometric minor axis (Θ = 119 and 299o east of north,
Dufour et al. 1979) beyond 15 kpc.
– 44 –
Fig. 4.— Sine curve fit for the GCs in NGC 5128 (circles) with a fixed systemic velocity of
vsys = 541 km s
−1, for 0-50 kpc from the center of NGC 5128. The top panel shows all 340
GCs with rotation amplitude ΩR = 40± 10 km s−1 and rotation axis Θo = 189± 12
o east of
north. The middle panel shows the 178 metal-poor clusters with ΩR = 31 ± 14 km s−1 and
Θo = 177 ± 22
o east of north, and the bottom panel shows the 158 metal-rich clusters with
ΩR = 47± 15 km s−1 and Θo = 202± 15
o east of north. The squares represent the weighted
velocities in 72o bins.
– 45 –
Fig. 5.— Rotation amplitude as a function of projected galactocentric radius from the center
of NGC 5128, including all known GCs (left) and the 780 PNe (right). The data are binned
in radial bins (squares) of 0-5, 5-10, 10-15 15-25, and 25-50 kpc for the GCs or 0-5, 5-10,
10-15, 15-20, 20-30, 30-40, and 40-80 kpc for the PNe, in equal number of 38 GCs (filled
circles) or 60 PNe, and exponentially weighted GCs or PNe with varying bin width (solid
line) and 35% uncertainties of the weighted data (dashed lines). The radial distribution of
data is shown at the bottom (open circles).
– 46 –
Fig. 6.— Same as Fig. 5, but for the metal-poor subpopulation of GCs (left) and the metal-
rich subpopulation of GCs (right). The equal numbered bins (filled circles) consist of 20
metal-poor or metal-rich GCs.
– 47 –
Fig. 7.— Rotation axis as a function of projected galactocentric radius from the center of
NGC 5128, including all known GCs (left) and the 780 PNe (right). The symbols are the
same as in Fig. 5, but the uncertainty of the weighted data (dashed lines) is 25%.
– 48 –
Fig. 8.— Same as Fig. 7, but for the metal-poor (left) and metal-rich (right) subpopulations
of GCs.
– 49 –
Fig. 9.— Velocity dispersion as a function of projected galactocentric radius from the center
of NGC 5128 for all known GCs (left) and the 780 PNe (right). The symbols are the same as
in Fig. 7, but the uncertainties of the weighted data (dashed lines) are determined by Eqn 2.
– 50 –
Fig. 10.— Same as Fig. 9, but for the metal-poor (left) and metal-rich (right) subpopulations
of GCs.
– 51 –
Fig. 11.— Velocity histograms for the GCs, subdivided by both metallicity and radius,
binned in 50 km s−1 intervals. Here vf is the residual velocity after subtraction of the
systemic velocity of 541 km s−1 and the overall rotation component for either the metal-poor
or metal-rich subpopulation, determined from Eqn. 1. The histograms for the metal-poor
clusters (left panels) include 129 clusters between 0 and 15 kpc and 49 clusters between
15 and 50 kpc, while the histograms for the metal-rich clusters (right panels) include 114
clusters between 0 and 15 kpc and 44 clusters between 15 and 50 kpc.
– 52 –
Fig. 12.— Surface density of known GCs fit with a powerlaw for the entire population (solid
line), the metal-poor subpopulation (dotted line), and the metal-rich subpopulation (short-
dashed line) in NGC 5128 with the best-fit linear coefficients shown. The radial distribution
of the entire GC population is shown as filled squares, yet clusters with projected radii < 5
kpc are shown as open squares and are not included in the powerlaw fits. Also overplotted is
the surface density of the PN system (long-dashed line) fit from all PNe beyond 5 kpc with
the best-fit linear coefficients also shown.
– 53 –
Fig. 13.— Total mass profile for the radially binned estimates of the GC system (filled
squares) from Woodley (2006) and the PNe (filled triangles). The GC total mass from 0 to
50 kpc, shown as the open square, is 1.3 ± 0.5 × 1012M⊙, and the PN total mass from 0 to
90 kpc, shown as the open triangle, is 1.0± 0.2× 1012M⊙, agreeing within the uncertainties.
	Introduction
	The Catalog of Globular Clusters in NGC 5128
	Kinematics of the Globular Cluster System
	Velocity Field
	Rotation Amplitude, Rotation Axis, and Velocity Dispersion
	Mathematic and Analytic Description
	Rotation Amplitude of the Globular Cluster System
	Rotation Axis of the Globular Cluster System
	Velocity Dispersion of the Globular Cluster System
	Kinematics of the Planetary Nebula System of NGC 5128
	Dynamics of NGC 5128
	Mass Determination
	Surface Density Profiles
	Mass Results
	Discussion and Conclusions

  A new kinematic and dynamic study of the halo of the giant elliptical galaxy,
NGC 5128, is presented. From a spectroscopically confirmed sample of 340
globular clusters and 780 planetary nebulae, the rotation amplitude, rotation
axis, velocity dispersion, and the total dynamical mass are determined for the
halo of NGC 5128. The globular cluster kinematics were searched for both radial
dependence and metallicity dependence by subdividing the globular cluster
sample into 158 metal-rich ([Fe/H] > -1.0) and 178 metal-poor ([Fe/H] < -1.0)
globular clusters. Our results show the kinematics of the metal-rich and
metal-poor subpopulations are quite similar. The kinematics are compared to the
planetary nebula population where differences are apparent in the outer regions
of the halo. The total mass of NGC 5128 is found using the Tracer Mass
estimator (Evans et al. 2003), to determine the mass supported by internal
random motions, and the spherical component of the Jeans equation to determine
the mass supported by rotation. We find a total mass of (1.0+/-0.2) x 10^(12)
Msun from the planetary nebulae data out to a projected radius of 90 kpc and
(1.3+/-0.5) x 10^(12) Msun from the globular clusters out to a projected radius
of 50 kpc. Lastly, we present a new and homogeneous catalog of known globular
clusters in NGC 5128. This catalog combines all previous definitive cluster
identifications from radial velocity studies and HST imaging studies, as well
as 80 new globular clusters from a study of M.A. Beasley et al. (2007, in
preparation).

Introduction
Globular clusters (GCs), as single-age, single-metallicity objects, are excellent tracers of
the formation history of their host galaxies, through their dynamics, kinematics, metallicities,
and ages. For most galaxies within ≃ 20 Mpc, GCs can be identified through photometry
and image morphology, from which follow-up radial velocity studies can be carried out with
multi-object spectroscopy on 4 and 8 m class telescopes. The ability to target hundreds of
objects in a single field has vastly increased the observed samples of GCs confirmed in many
galaxies, providing the necessary basis for detailed kinematic and age studies.
Another benefit of using GCs as a kinematic tracer is that they provide a useful, inde-
pendent basis for comparison with results from planetary nebulae (PNe). This is particularly
true given the current debate surrounding the use of PN velocities and the implications for
low dark matter halos. For example, Romanowsky et al. (2003) reported, based on PN ve-
locities, that three low-luminosity ellipticals revealed declining velocity dispersion profiles
and little or no dark matter. However, subsequent simulations of merger-remnant ellipticals
suggested that the radial anisotropy of intermediate-age PNe could give rise to the observed
profiles within standard halos of dark matter (Dekel et al. 2005; Mamon &  Lokas 2005).
Flattening of the galaxy along the line of sight is another possible explanation. One of the
ellipticals studied by Romanowsky et al. (2003), NGC 3379, has also been investigated using
GC kinematics (Pierce et al. 2006; Bergond et al. 2006); both studies found evidence of a
dark matter halo. But the two studies of NGC 3379 suffered from small number statistics.
Clearly there is a need to directly compare PN and GC kinematics for the same elliptical
with sufficiently large numbers of tracer objects.
Previous velocity-based studies of globular cluster systems (GCSs) have shown an in-
triguing variety of results in their overall kinematics. Prominent recent examples include the
– 4 –
following:
1. Côté et al. (2001) performed a kinematic analysis of the GCS in M87 (NGC 4486),
the cD galaxy in the Virgo Cluster. With a sample of 280 GCs, they showed that the entire
GCS rotates on an axis matching the photometric minor axis of the galaxy, except for the
inner metal-poor sample. Inside the onset of the cD envelope, the metal-poor clusters appear
to rotate around the major axis of the galaxy instead. This study also found evidence for
an increase in velocity dispersion, σv, with radius, due to the larger scale Virgo Cluster
mass distribution. They also showed no strong evidence for a difference in σv between the
metal-poor and metal-rich groups. Using a Virgo mass model, they investigated anisotropy
and found that as a whole, the GCS had isotropy, but considered separately, the metal-poor
and metal-rich subpopulations had slight anisotropy.
2. Côté et al. (2003) performed a dynamical analysis for M49 (NGC 4472), the other
supergiant member of the Virgo Cluster. Using over 260 GCs, they found that the metal-
rich population shows no strong evidence for rotation, while the metal-poor population does
rotate about the minor axis of the galaxy. In addition, they found that the metal-poor
clusters had an overall higher dispersion than the metal-rich population.
3. Richtler et al. (2004) determined the kinematics for the GCS in NGC 1399, the
brightest elliptical in the Fornax Cluster of galaxies. Armed with a sample of over 460 GCs,
they found a marginal rotation signal for the entire GC sample and the outer metal-poor
sample, while no rotation was seen for the metal-rich subpopulation. Their projected velocity
dispersion showed no radial trend within their determined uncertainty, but the metal-poor
clusters had a higher dispersion than the metal-rich clusters. The kinematics of the PNe
in NGC 1399 have been most recently studied by Saglia et al. (2000) and Napolitano et al.
(2002) using a small sample of 37 PNe from Arnoaboldi et al. (1994). These studies do
not indicate any significant deviations in velocity dispersion with radius for the PNe, yet
interestingly, Napolitano et al. (2002) found stong rotation for the PNe in the inner region
of the galaxy.
4. Peng, Ford & Freeman (2004c) studied the GC kinematics of the giant elliptical
NGC 5128 from a total of 215 GCs. Their results showed definite rotation signals in both
metallicity groups beyond a 5 kpc distance from the center of the galaxy, as well as similar
velocity dispersions in both the metal-poor and the metal-rich populations within a 20 kpc
projected radius. A similar PN kinematic study in NGC 5128 (Peng, Ford & Freeman 2004b)
showed that the PNe population is rotating around a twisted axis that turns just beyond
the 5 kpc distance.
These few detailed kinematic studies of GCSs in elliptical galaxies, show results that
– 5 –
appear to differ on a galaxy-by-galaxy basis, without any clear global trends. The age
distributions of the GC populations in these same galaxies tend to show a consistent pattern
in which the blue, or metal-poor, population is found to be universally old. The red, or metal-
rich, population has also been shown to be old in the study of Strader et al. (2005). Their
study found that both the metal-poor and metal-rich GCs in a sample of eight galaxies ranging
from dwarf to massive ellipticals, all have ages as old as their Galactic GC counterparts.
Conversely, in a small sample of studies, the red GC population has also been found to be 2-4
Gyr younger than the metal-poor GC population, and with a wider spread in determined ages
(see the studies of Peng, Ford & Freeman 2004c; Puzia et al. 2005, among others), although
this is not yet a well-established trend. The GCs in NGC 5128 appear to be old, with an
intermediate-age population (Peng, Ford & Freeman 2004c; Beasley et al. 2006).
NGC 5128 (Centaurus A), the central giant in the Centaurus group of galaxies at a
distance of only ∼ 4 Mpc, is a prime candidate for both kinematic and age studies. Its GCS
has a specific frequency of SN ≃ 2.2±0.6 (Harris et al. 2006), toward the low end of the giant
elliptical range but about twice as high as in typical disk galaxies. Its optical features show
faint isophotal shells located in the halo (e.g. Peng et al. 2002), the prominent dust lane in the
inner 5 kpc, the presence of gas, and star formation, all of which suggest that NGC 5128 could
be a merger product. Baade & Minkowski (1954) first suggested that NGC 5128 could be
the result of a merger between two galaxies, a spiral and an elliptical. This idea was followed
by the general formation mechanism of disk-disk mergers proposed by Toomre & Toomre
(1972). Bekki, Harris, & Harris (2003) found that the metallicity distribution function of the
halo field stars could be reproduced by a gas-free (”dry”) disk-disk merger scenario. Recent
numerical simulations by Bekki & Peng (2006) also demonstrate that the PN kinematics
observed in NGC 5128 (Peng, Ford & Freeman 2004b) can be reproduced relatively well
from a merger of unequal-mass disk galaxies (with one galaxy half the mass of the other)
colliding on a highly inclined orbital configuration.
Alternatively, much of NGC 5128 could be a ”red and dead” galaxy, passively evolving
since its initial formation as a large seed galaxy (Woodley 2006), while undergoing later
minor mergers and satellite accretions. Evidence consistent with this scenario is in the halo
population of stars in NGC 5128, which have a mean age of 8+3.0
−3.5 Gyr (Rejkuba et al. 2005).
Its metal-poor GC ages have also been shown to have ages similar to Milky Way GCs,
while the metal-rich population appears younger (Peng, Ford & Freeman 2004c). Our new
spectroscopic study (Beasley et al. 2006) suggests that NGC 5128 has a trimodal distribution
of cluster ages: ∼ 50% of metal-rich clusters have ages of 6 − 8 Gyr, only a small handful
of metal-rich clusters have ages of 1 − 3 Gyr, and a large fraction of both metal-rich and
metal-poor clusters have ages of ≃ 12 Gyr. Lastly, the halo kinematics of NGC 5128 have
also been recently shown to match the surrounding satellite galaxies in the low-density
– 6 –
Centaurus group, suggesting that NGC 5128 acts like an inner component to its galaxy
group (Woodley 2006). Kinematic and age studies with large number of GCs are thus
starting to help disentangle the formation of this giant elliptical.
The confirmed GC population in NGC 5128 is now large enough to allow a new kine-
matic analysis subdivided to explore radial and metallicity dependence, while avoiding small
number statistics in almost all regions of the galaxy. The analysis presented here comple-
ments the detailed age distribution study provided by Beasley et al. (2006). The results
provide a broader picture of the formation scenario of NGC 5128.
The sections of this paper are divided as follows: § 2 contains the full catalog of NGC
5128 GCs with known photometry and radial velocities, § 3 contains the kinematic analysis of
GCSs, § 4 contains the kinematic analysis of the PN population, § 5 contains the discussion of
the dynamical mass of NGC 5128, and § 6 contains our final discussion, as well as concluding
remarks.
2. The Catalog of Globular Clusters in NGC 5128
Finding GCs in NGC 5128 is challenging. This process begins with photometric surveys
of the many thousands of objects projected onto the NGC 5128 field (e.g. Rejkuba 2001;
Harris et al. 2004); only a few percent of these are the GCs that we seek. This daunting task
is made difficult by the galactic latitude of NGC 5128 (b = 19o), which means that many
foreground stars are present in the field of NGC 5128. Background galaxies are another major
contaminant in the field, forcing the use of search criteria such as magnitude, color, and object
morphology to help build the necessary candidate list of GCs. Confirmation of such candidate
objects can then be done with spectroscopic radial velocity measurements. The GCs in NGC
5128 have radial velocities in the range vr = 200− 1000 km s
−1, while most foreground stars
have vr < 200 km s
−1. Background galaxies have radial velocities of many thousands of km
s−1 and can easily be eliminated (see the recent studies of Peng, Ford, & Freeman 2004a;
Woodley, Harris, & Harris 2005).
Over the past quarter century, there have been seven distinct radial velocity stud-
ies to identify GCs in NGC 5128 (van den Bergh, Hesser, & Harris 1981; Hesser et al. 1984;
Hesser, Harris, & Harris 1986; Harris et al. 1992; Peng, Ford, & Freeman 2004a; Woodley, Harris, & Harris
2005; Beasley et al. 2006). Although Harris et al. (1992) was not a radial velocity study it-
self, but rather a CCD photometric study of previously confirmed GCs, it does include the
GCs determined spectroscopically from Sharples (1988). A recent study with measured GC
radial velocities published by Rejkuba et al. (2007) has confirmed two new GCs, HCH15 and
– 7 –
R122, included in our catalog.
Within this catalog are 80 new GCs with radial velocity measurements from Beasley et al.
(2006). The combination of these studies now leads to a confirmed population of 342 GCs.1
Also included in our catalog are the new GC candidates from HST STIS imaging from
Harris et al. (2002), labelled C100-C106, and from HST ACS imaging from Harris et al.
(2006), labelled C111-C179. All these previous studies have their own internal numbering
systems, which makes the cluster identifications somewhat confusing at this point. Here we
define a new, homogeneous listing combining all this material and with a single numbering
system.
Our catalog of the GCs of NGC 5128 is given in Table 1. In successive columns, the Table
gives the new cluster name in order of increasing right ascension; the previous names of the
cluster in the literature; right ascension and declination (J2000); the projected radius from
the center of NGC 5128 in arcminutes; the U , B, V , R, and I photometric indices and their
measured uncertainties; the C, M , and T1 photometric indices and their uncertainties; the
colors U−B, B−V , V −R, V −I, M−T1, C−M , and C−T1; and, lastly, the weighted mean
velocity vr and its associated uncertainty from all previous studies. All UBV RI photometry
is from the imaging survey described in Peng, Ford, & Freeman (2004a). The CMT1 data
are from Harris et al. (2004).
The mean velocities are weighted averages with weights on each individual measurement
equal to ε−2v where εv is the quoted velocity uncertainty from each study. The uncertainty
in the mean velocity is then < εv >= (
ε−2i )
−1/2. There are no individual uncertainties
supplied for the velocities for clusters studied by Hesser, Harris, & Harris (1986), but their
study reports that the mean velocity uncertainty for clusters with Rgc < 11
′ is 25 km s−1
and for Rgc > 11
′ is 44 km s−1. We have adopted these values accordingly for their clusters.2
The study by Harris et al. (1992) also does not report velocity uncertainties; however,
these clusters have all been recently measured by Peng, Ford, & Freeman (2004a). The rms
1The confirmed GC list in Woodley (2006) containing 343 GCs has been reduced to 340 based on recent
spectroscopic and imaging studies. Object 304867 with a high radial velocity of 305± 56 km s−1 appears to
be an M-type star based on the strong molecular bands in its spectrum, see Beasley et al. (2006) for further
discussion. Objects pff gc-010 and 114993 are also rejected as GCs because of their starlike appearance
under HST ACS imaging; see Harris et al. (2006). However, newly confirmed GCs HCH15 and R122 have
now been added (Rejkuba et al. 2007).
2Hesser, Harris, & Harris (1986) report C32 at a distance of Rgc = 10.8
′, but more recently
Peng, Ford, & Freeman (2004a) claim a distance of Rgc = 11.25
′, so it has an adopted uncertainty of 44
km s−1 in the weighted mean.
– 8 –
scatter of the Harris et al. (1992) values from theirs was 58 km s−1. This value has been
adopted as the velocity uncertainty of the Harris et al. (1992) clusters in the weighted means.
The weighted mean velocity of cluster C10 does not include the measured value deter-
mined by Peng, Ford, & Freeman (2004a) which is significantly different from other mea-
surements. Also, cluster C27 does not include the measurement of vr = 1932 ± 203 km s
from Beasley et al. (2006), indicating that this object is a galaxy. We include C27 as a GC,
but with caution.
In the weighted velocity calculations, the velocities and uncertainties of the 27 GCs from
Rejkuba et al. (2007) have been rounded to the nearest whole number, with any velocity
uncertainty below 1 km s−1 rounded up to a value of 1.
Lastly, the GC pff gc-089 overlaps the previously existing confirmed cluster, C49, within
a 0.5” radius; pff gc-089 is therefore removed from the catalog of confirmed GCs.
The data in Table 1 provide the basis for the kinematic study presented in this paper.
We use them to derive the rotation amplitude, rotation axis and velocity dispersion in
the full catalog of clusters, as well as for the metal-poor ([Fe/H] < −1) and metal-rich
([Fe/H] > −1) subpopulations. For this purpose, we define the metallicity of the GCs by
transforming the dereddened colors (C − T1)o to [Fe/H] through the standard conversion
(Harris & Harris 2002), calibrated through Milky Way cluster data. A foreground reddening
value of E(B − V ) = 0.11 for NGC 5128, corresponding to E(C − T1) = 0.22, has been
adopted. The division of [Fe/H] = -1 between metal-rich and metal-poor GCs has been
shown as a good split between the two metallicity populations from [Fe/H] values converted
from C − T1 in Woodley, Harris, & Harris (2005) and Harris et al. (2004) for NGC 5128. If
no C and/or T1 values are available for the cluster, it is classified as metal-rich or metal-poor
through a transformation from (U − B)o to [Fe/H] from Reed, Harris, & Harris (1994).
In Figure 1 we show the spatial distributions of all the GCs from Table 1 (left) and the
distribution of the known PNe (right). Both systems are spatially biased to the major axis
of the galaxy because this is where most of the GC and PN searches have concentrated.
3. Kinematics of the Globular Cluster System
3.1. Velocity Field
For the present discussion we adopt a distance of 3.9 Mpc for NGC 5128. This value is
based on four stellar standard candles that each have internal precisions near ±0.2 mag: the
PN luminosity function, the tip of the old-halo red giant branch, the long-period variables,
– 9 –
and the Cepheids (Harris et al. 1999; Rejkuba 2004; Ferrarese et al. 2006).
HCH15 and R122 have not been included in our kinematic study, as our study was
completed before publication of these velocities. The weighted velocities used in this kine-
matic study do not include the most recent 25 velocities of previously known GCs published
in Rejkuba et al. (2007). Note that the velocities published in Table 1 do, however, in-
clude the Rejkuba et al. (2007) velocities in the quoted final weighted radial velocities for
completeness.
The velocity distribution of the entire sample of 340 is shown in Figure 2 (top left),
binned in 50 km s−1 intervals. A fit with a single Gaussian yields a mean velocity of 546± 7
km s−1, nicely matching the known systemic velocity of 541 ± 7 km s−1 (Hui et al. 1995).
There is a slight asymmetry at the low-velocity end that is likely due to contamination by
a few metal-poor Milky Way halo stars (also seen in the metal-poor subpopulation in the
bottom left panel, which has a mean velocity determined by the Gaussian fit as 532±13 km
s−1).
Selecting the clusters with radial velocity uncertainties less than 50 km s−1 leaves 226
clusters, plotted in Fig. 2 (top right). The close fit to a single Gaussian is consistent with
an isotropic distribution of orbits; the mean velocity is 554 ± 5 km s−1. The metal-rich
population, with a mean velocity determined by the Gaussian fit of 565 ± 11 km s−1, is
plotted in the bottom right panel, and also shows no strong asymmetries.
Looking closer at the metal-poor velocity asymmetry, we note that the 15 metal-poor
clusters between 250 and 300 km s−1 (in the region where contamination by Milky Way
field stars could occur) are balanced by only two GCs at the high-velocity end on reflec-
tion across the systemic velocity. The same velocity regions in the metal-rich population
are nearly equally balanced with four clusters between 250 and 300 km s−1 with three clus-
ters at the reflected high-velocity range. Interestingly, the four metal-rich clusters between
250 and 300 km s−1 have projected radii > 17 kpc even though the metal-rich popula-
tion is more centrally concentrated than the metal-poor (see Peng, Ford & Freeman 2004c;
Woodley, Harris, & Harris 2005, among others). The metal-poor clusters between 250 and
300 km s−1, conversely, are more evenly distributed, with five clusters between projected
radii of 5 and 10 kpc, five clusters between 10 and 20 kpc, and five clusters beyond 20 kpc
from the center of NGC 5128. Some of these low-velocity, metal-poor objects could be fore-
ground stars with velocities in the realm of GCs in NGC 5128 (vr & 250 km s
−1). However,
with only 340 GCs currently confirmed within ∼ 45’ from the center of NGC 5128, out of
an estimated ≃ 1500 total clusters within 25’ (Harris et al. 2006), these metal-poor, low-
velocity objects could simply be part of a very incomplete GC sample that is also spatially
biased. This potential bias is clearly shown in Figure 3, which shows the projected radial
– 10 –
distribution as a function of azimuthal angle for our GC sample. Beyond 12 kpc, the two
”voids” coincide with the photometric minor axis of the galaxy, attributed at least partly to
incomplete cluster surveys in these regions. These objects should, therefore, not be dropped
from the GC catalog without further spectroscopic analysis.
3.2. Rotation Amplitude, Rotation Axis, and Velocity Dispersion
3.2.1. Mathematic and Analytic Description
We determine the rotation amplitude and axis of the GCS of NGC 5128 from
vr(Θ) = vsys + ΩRsin(Θ − Θo) (1)
(see Côté et al. 2001; Richtler et al. 2004; Woodley 2006). In Equation 1, vr is the observed
radial velocity of the GCs in the system, vsys is the galaxy’s systemic velocity, R is the
projected radial distance of each GC from the center of the system assuming a distance
of 3.9 Mpc to NGC 5128, and Θ is the projected azimuthal angle of the GC measured in
degrees east of north. The systemic velocity of NGC 5128 is held constant at vsys = 541
km s−1 (Hui et al. 1995) for all kinematic calculations. The rotation axis of the GCs, Θo,
and the product ΩR, the rotation amplitude of the GCs in the system, are the values
obtained from the numerical solution. We use a Marquardt-Levenberg non-linear fitting
routine (Press et al. 1992).
Eqn. 1 assumes spherical symmetry. While this may be a decent assumption for the
inner 12 kpc region (it has a low ellipticity of ∼ 0.2; Peng, Ford & Freeman 2004b), true
ellipticities for the outer regions of the system are not well known because of the sample bias
(see Fig. 3). Future studies to remove these biases are vital to obtaining a sound kinematic
solution for the entire system. Eqn. 1 also assumes that Ω is only a function of the projected
radius and that the rotation axis lies in the plane of the sky. It is not entirely clear how these
assumptions, discussed thoroughly in Côté et al. (2001), apply to the GC and PN systems
of NGC 5128. The Ω we solve for is, therefore, only a lower limit to the true Ω if the true
rotation axis is not in the plane of the sky.
The projected velocity dispersion is also calculated from the normal condition,
σ2v =
(vfi − vsys)
where N is the number of clusters in the sample, vfi is the GC’s radial velocity after sub-
traction of the rotational component determined with Eqn. 1, and σv is the projected velocity
dispersion.
– 11 –
The GCs were assigned individual weights in the sums that combine in quadrature the
individual observational uncertainty, εv, in vr and the random velocity component, εrandom, of
the GCS. The dominance of the latter is evident by the large dispersion in the GC velocities
in the kinematic fitting (see Figure 4). In other words, the clusters have individual weights,
ωi = (ε
v + ε
random)
−1; the main purpose of this is to assign a bit more importance to the
clusters with more securely measured velocities. This random velocity term dominates in
nearly every case, leaving the GCs with very similar base weights in the kinematic fitting.
The three kinematic parameters - rotation amplitude, rotation axis, and velocity disper-
sion - are determined with three different binning methods. The first involves binning the
GCs in radially projected circular annuli from the center of NGC 5128. The chosen bins keep
a minimum of 15 clusters in each, ranging as high as 124 clusters. The bins are 0-5, 5-10,
10-15, 15-25, and 25-50 kpc. Also, we include 0-50 kpc to determine the overall kinematics
of the system.
The second method adopts bins with equal numbers of clusters. The entire population
of clusters had nine bins of 38 clusters each, the metal-poor clusters had nine bins of 20
clusters, and the metal-rich clusters had eight bins of 20 clusters. The base weighting is
applied to the clusters in both the first and second binning methods.
The third method uses an exponential weighting function, outlined in Bergond et al.
(2006), to generate a smoothed profile. This method determines each kinematic parameter
at the radial position, R, of every GC in the entire sample by exponentially weighting all
other GCs surrounding that position based on their radial separation, R− Ri, following
wi(R) =
−(R − Ri)
]. (3)
In Equation 3, wi is the determined weight on each GC in the sample, and σR is the
half-width of the window size. For this study, σR is incrementally varied in a linear fashion
for the total sample from σR = 1.0 kpc at the radius of the innermost GC in the sample
out to σR = 4.5 kpc at the radius of the outermost GC, where the population is lowest.
The metal-poor population was given a half-width window of σR = 1.0 − 6.5 kpc, and the
metal-rich population was given a half-width window of σR = 2 − 5.3 kpc, again from the
innermost to outermost cluster. The progressive radial increase in σR ensured that each
point R had roughly equal total weights.
– 12 –
3.2.2. Rotation Amplitude of the Globular Cluster System
The kinematic parameters were determined for the entire sample of 340 GCs, as well as
the subpopulations of 178 metal-poor and 158 metal-rich GCs (four clusters have unknown
metallicity). The kinematic results for the entire population of GCs are shown in Table 2,
reproduced almost in full from Woodley (2006), while the results for the metal-poor and
metal-rich clusters are shown in Tables 3 & 4, respectively. The columns give the radial bin,
the mean projected radius in the bin, the radius of the outermost cluster, the number of
clusters in the bin, the rotation amplitude, the rotation axis, and the velocity dispersion, with
associated uncertainties. These are followed by the mass correction, the pressure-supported
mass, the rotationally supported mass, and the total mass in units of solar mass (see § 5
for the mass discussion). The results for the alternate two methods, using an equal number
of GCs per bin and the exponentially weighted GCs, are not shown in tabular form but are
included in all of the figures.
Figure 4 shows the sine fit of Eqn. 1 for the total population and for the metal-poor
and metal-rich subpopulations. All three populations show rotation about a similar axis.
As discussed in § 3.1, the metal-poor population has more members with low velocities
(Vr ≤ 300 km s
−1) than the metal-rich population, suggesting possible contamination of
Milky Way foreground stars in the sample.
Figures 5 & 6 show the rotation amplitude results for the entire population and for
the metal-poor and metal-rich subpopulations, respectively. The three kinematic methods,
described in Section 3.2.1, appear to agree relatively well for all three populations of clusters.
While there appears to be no extreme difference in rotation amplitude between the cluster
populations, the metal-poor subpopulation of clusters has lower rotation in the inner 5 kpc
of NGC 5128 than the metal-rich subpopulation. The weighted average of the 0-5 kpc radial
bin and the innermost equal-numbered bin, shows that the entire population has a rotation
amplitude of ΩR = 31 ± 17 km s−1, while the metal-poor population has ΩR = 17 ± 26 km
s−1 and the metal-rich population has ΩR = 57±22 km s−1. Peng, Ford & Freeman (2004c)
show in their study that the metal-poor population has very little rotation in the central
regions, completely consistent with our findings. The rotation amplitude does not appear to
differ between the two populations outside of 5 kpc.
3.2.3. Rotation Axis of the Globular Cluster System
The results of the rotation axis solutions are shown in Figures 7 & 8, again for the
entire population and for the metal-poor and metal-rich subpopulations. The solution for
– 13 –
Θ0 agrees well for all three kinematic methods and all subgroups. The inner 5 kpc region
has a different rotation axis than the outer regions, demonstrated clearly in all three binning
methods. The innermost bin yields weighted averages of Θo = 369±24
o, Θo = 25±55
o, and
Θo = 352±18
o, all of which are equal within their uncertainties. Beyond 5 kpc, the rotation
axes for all three populations are in even closer agreement, with averages of Θo = 189 ± 6
Θo = 199 ± 7
o, and Θo = 196 ± 7
o for the entire population, the metal-poor subpopulation,
and the metal-rich subpopulation, respectively. The position angle of the photometric major
axis of NGC 5128 is Θ = 35o and 215o east of north and the photometric minor axis is
Θ = 119o and 299o east of north (Dufour et al. 1979). It appears the GCS is rotating about
an axis similar to the photometric major axis for the full extent of the galaxy, with a possible
axial twist or counterrotation within 5 kpc.
3.2.4. Velocity Dispersion of the Globular Cluster System
Figures 9 & 10 show the velocity dispersion for the entire population and for the metal-
poor and metal-rich subpopulations. Our results for σv show no significant differences be-
tween the metallicity subpopulations. All three show a relatively flat velocity dispersion
(σv = 119 ± 4, σv = 117 ± 6, and σv = 111 ± 6 km s
−1 within 15 kpc of the center of NGC
5128 for the entire population and for the metal-poor and metal-rich subpopulations, re-
spectively). These results match the previous study of NGC 5128 by Peng, Ford & Freeman
(2004c), whose determined velocity dispersion for the GCs within 20 kpc ranged between
75 and 150 km s−1. At a larger radius, we find that σv then slowly increases to σv > 150
km s−1 towards the outer regions of the halo for all populations. The velocity dispersion
of the metal-rich GCs, interestingly, appears higher than that of the metal-poor GCs in
the outer regions (although still consistent within the determined uncertainties). In most
previous studies, the velocity dispersion of the metal-poor GCs usually appears higher than
that of the metal-rich GCs, if there is a notable velocity dispersion difference between the
subpopulations (see the studies of Côté et al. 2003; Richtler et al. 2004, as examples).
To explore the cause of the distinct rise past 15 kpc a bit further, we have plotted
the actual velocity histograms in Figure 11 for the metal-poor and metal-rich subgroups,
subdivided further into inner (R < 15 kpc) and outer (R > 15 kpc) regions. In the inner 15
kpc, both samples show histograms strongly peaked near vf = 0 and with at least roughly
Gaussian falloff to both high and low velocities. By contrast, the histograms for the outer
regions (15−50 kpc) are noticeably flatter, so that the clusters with larger velocity residuals
have relatively more importance to the formal value of σv. Nominally, the flatter shape
of the velocity distribution would mean that the outer-halo clusters display anisotropy in
– 14 –
the direction of a bias towards more circular orbits. However, such a conclusion would be
premature at this point for two reasons. First, the sample size in the outer regions is still
too small to lead to high significance, and a direct comparison between the inner and outer
histograms (through a Kolmogorov-Smirnov test) does not show a statistically significant
difference between them larger than the 70% level. Second, the outer samples may still be
spatially biased in favor of objects along the major axis of the halo, as discussed above, and
this bias sets in strongly for R > 12 kpc (see Fig. 3), very near where we have set the radial
divisions in this Figure. This type of velocity distribution can also arise from the accretions
of satellite galaxies with their own small numbers of GCs (Bekki et al. 2003). We will need
to have a larger sample of the outer-halo clusters, and one in which these potential sample
biases have been removed, before we can draw any firmer conclusions. However, it needs to
be explicitly stated that the outermost point in the kinematic plots for the GCs representing
25 − 50 kpc suffers from very high spatial biases and low number statistics (< 40 GCs)
and covers a large radial interval. The rise in velocity dispersion could be driven purely by
systematic effects resulting from the radial gradient of the number density of GCs in this
outermost bin (Napolitano et al. 2001).
4. Kinematics of the Planetary Nebula System of NGC 5128
NGC 5128 has a large number, 780, of identified PNe with measured radial velocity from
the studies of Peng, Ford & Freeman (2004b) and Hui et al. (1995); these PNe are projected
out to 90 kpc assuming a distance to NGC 5128 of 3.9 Mpc. Since these are also old objects,
it is of obvious interest to compare them with the GCS. The PNe also have the advantage
of giving us the best available look at the kinematics of the halo field stars.
The PN kinematic results are listed in Table 5, with the same columns as Table 2. The
results are shown in Figures 5, 7, & 9 for the rotation amplitude, rotation axis, and velocity
dispersion, respectively. The spatial distribution of the known PNe is, like the GCS, biased
toward the major axis at large radii (see Fig. 1). Nevertheless, their kinematics closely
resemble the GCs.
The kinematics of the PN system are very consistent among all three binning methods.
The rotation amplitude and rotation axis show little radial trend, while the velocity disper-
sion appears relatively flat within the first 15 kpc at σv = 122 ± 7 km s
−1 and then slowly
decreases to σv ≃ 85 km s
−1 at large galactocentric radius. Peng, Ford, & Freeman (2004a)
show that the velocity dispersion of the PNe drops from a central value of 140 to 75 km s−1
in the outer regions of the galaxy, consistent with the findings of this study. Their velocity
field analysis led to the discovery of a ”zero-velocity curve” located between the photometric
– 15 –
minor axis, 119±5o east of north (Dufour et al. 1979), and the north-south direction, for the
innermost region of the galaxy. Just beyond 5 kpc, the zero-velocity curve turns and follows
a straight line at a 7o angle from the photometric major axis, 35o east of north (Dufour et al.
1979) (see Figure 7 of Peng, Ford & Freeman 2004c).
This study does not show a strong change in rotation axis for the PNe in the innermost
regions of the galaxy. However, it clearly shows in all three GC populations a significant
change in the rotation axis just beyond 5 kpc from the center of the galaxy. A change in
axis of 5 kpc outward (∼ 180o for the entire population and metal-poor subpopulation and
∼ 160o for the metal-rich subpopulation) has been found, as discussed in § 3.2.3. Similarly,
Peng, Ford & Freeman (2004c) show from their sample of 215 clusters that a clear sign
of rotation beyond 5 kpc about a misaligned axis appears particularly in their metal-rich
subpopulation. The kinematics of the GCs in this study matches the line of zero velocity
relatively nicely. Within 5 kpc the rotation axis of the GCS is nearly-parallel to the north-
south direction, and beyond 5 kpc the rotation axis is near 200o east of north, which is only
∼ 10o from the zero-velocity curve.
However, the velocity field of NGC 5128 is complex and not entirely captured by these
approximate solutions. The two-dimensional velocity field shown in Peng, Ford & Freeman
(2004b) (see their Figure 7), shows that the photometric major axis (which happens to be
very close to our maximum rotation as discussed above) is only 7o from the line of zero
velocity. This could lead to a very asymmetric velocity profile that may not be well fit by
the sine curve described in Equation 1. Biased kinematics, especially the rotation axis, may
develop from the sine fit that could lead to a higher estimated velocity dispersion.
Hui et al. (1995) similarly studied the kinematics of the PN system in NGC 5128 with
a sample of 433 PNe. They obtain a rotation axis of 344 ± 10o. Our result of 170 ± 5o
east of north is consistent with their findings on comparing their sine curve fit of their PN
data in their Figure 11 to our corresponding fit shown in Fig. 4 for the GCS, which shares a
similar axis to our PN sample (note that in their study, φ = 0o corresponds to our Θ = 305o
east of north). Our fits both correspond to a positive rotation amplitude for a rotation axis
near 170o east of north and a negative rotation axis near 350o east of north. Therefore,
the rotation axis quoted in Hui et al. (1995) of 344 ± 10o corresponds to a negative rotation
amplitude of approximately 70 − 75 km s−1 (taken from their Figure 11), nicely matching
our result of a positive 76 ± 6 km s−1 about an axis of 170 ± 5o east of north.
– 16 –
5. Dynamics of NGC 5128
Both GCs (Côté et al. 2001; Larsen et al. 2002; Evans et al. 2003; Côté et al. 2003;
Beasley et al. 2004; Peng, Ford & Freeman 2004c, among others) and PNe (Ciardullo et al.
1993; Hui et al. 1995; Arnaboldi et al. 1998; Peng, Ford & Freeman 2004b, among others)
can be used to estimate the total dynamical mass of their host galaxies. A variety of tools
are in use including derived mass models, the virial mass estimator (Bahcall & Tremaine
1981), the projected mass estimator (Heisler, Tremaine, & Bahcall 1985), and the tracer
mass estimator (Evans et al. 2003).
NGC 5128 does not have a large X-ray halo (detected by Kraft et al. 2003; O’Sullivan, Forbes, & Ponman
2001, the latter reporting a measurement of log Lx = 40.10 erg s
−1), such as is evident in
other giant ellipticals such as M87 (Côté et al. 2001) or NGC 4649 (Bridges et al. 2006).
Thus it is difficult to model the dark matter profile of NGC 5128 with a priori constraints.
Without such a mass model, we turn to the tracer mass estimator for the dynamical mass
determination. The tracer mass estimator has the distinct advantage over the virial and pro-
jected mass estimators that the tracer population does not have to follow the dark matter
density in the galaxy - an extremely useful feature for stellar subsystems such as GCs and
PNe that might, in principle, have significantly different radial distributions (see Evans et al.
(2003) for extensive discussion). Below, we determine the mass of NGC 5128 using the tracer
populations of GCs and PNe (our mass estimates do not include stellar kinematics in the
inner regions).
5.1. Mass Determination
The mass contributed by the random internal motion of the galaxy (pressure-supported
mass) is determined from the tracer mass estimator as
(vfi − vsys)
2Ri (4)
where N is the number of objects in the sample and vfi is the radial velocity of the tracer
object with the rotation component removed. For an isotropic population of tracer objects,
assumed in this study, the value of C is
4(α + γ)(4 − α− γ)(1 − ( rin
)(3−γ))
π(3 − γ)(1 − ( rin
)(4−α−γ))
where rin and rout are the three-dimensional radii corresponding to the two-dimensional
projected radii of the innermost, Rin, and outermost, Rout, tracers in the sample. The
– 17 –
parameter α is set to zero for an isothermal halo potential in which the system has a flat
rotation curve at large distances. Finally, γ is the slope of the volume density distribution,
which goes as r−γ, and is found by determining the surface density slope of the sample and
deprojecting the slope to three-dimensions. The tracer mass estimator uses a sample of tracer
objects defined between rin and rout, yet it is important to emphasize that it determines the
total enclosed mass within rout.
There is also a contribution to the total mass by the rotational component, as determined
in § 3.2.2 for the GCs and § 4 for the PNe. This mass component is determined from the
rotational component of the Jeans equation,
Routv
where Rout is the outermost tracer projected radius in the sample and vmax is the rotation
amplitude. Therefore, the total mass of NGC 5128, Mt, is determined by the addition of the
mass components supported by rotation, Mr, and random internal motion, Mp,
Mt = Mp + Mr. (7)
In the determination of the pressure-supported mass, one must estimate values for rin
and rout knowing Rin and Rout. Evans et al. (2003) suggest that rin ≃ Rin and rout ≃
Rout for distributions taken over a wide angle. However, in this study the inner and outer
radii of the chosen bins are at intermediate radial values within the distribution. Their
assumption would therefore lead to an underestimate of the determined mass, since the
true rout can be quite a bit larger than the projected Rout. To correct for this contributed
uncertainty, distributions of sample tracer populations were generated through Monte Carlo
simulations. In the simulations, 340 GCs were randomly placed in a spherically symmetric
system extending out to 50 kpc with an r−2 projected density, while 780 PNe were placed
in the same environment extending out to 90 kpc. From the generated distributions, the
value of C in Eqn. 5 was determined for both the real and projected positions of the tracer
populations in each designated radial bin. This correction factor, listed in Tables 3-5 as Mcorr,
multiplies the pressure-supported mass from Eqn. 4. The same correction was applied to the
full GC sample and the corresponding Mcorr values are listed in Table 1 of Woodley (2006).
These values are generally small, but in the worst case they triple Mp.
5.2. Surface Density Profiles
In Eqn. 5, the value of γ is determined for the tracer populations by deprojecting
the slope of the surface density profile to three-dimensions. Figure 12 shows the surface
– 18 –
density profiles for the entire, metal-poor, and metal-rich GC populations, along with the
PN profile. The populations were binned, following Máız Apellániz & Úbeda (2005), into
circular annuli of equal numbers of objects, providing the same statistical weight to each bin
(although spatial biases may still affect the GC population in the outer regions along the
major axis; see Fig. 3). In the inner 5 kpc of all tracer populations, incompleteness due to the
obscuration of the dust lane is evident by the flattening of the surface density profile. The
innermost objects were, therefore, excluded from the surface density profile fittings. Outside
of 5 kpc, the surface densities fit well to power laws, leading to γ = 3.65 ± 0.17, 3.49 ± 0.34,
3.37 ± 0.30, and 3.47 ± 0.12 for the entire GC population, the metal-poor and metal-rich
subpopulations of GCs, and the PNe in NGC 5128, respectively. These are all very similar
within their uncertainties.
5.3. Mass Results
The similar kinematics we find between the metal-poor and metal-rich subpopulations
of GCs in this study strongly justifies the combining of the two populations for the mass
determination performed in Woodley (2006). The GC population provides a total mass
estimate of (1.3 ± 0.5) × 1012 M⊙ from 340 clusters out to a projected radius of 50 kpc.
Removing the GCs in our sample with vr ≤ 300 km s
−1, which will remove all possible
contamination from foreground stars, discussed in § 3.1, leads to a total mass of (1.0±0.4)×
1012 M⊙. This mass agrees nicely with our mass determined from our entire GC sample.
The PN population provides a total mass of (1.0 ± 0.2) × 1012 M⊙ from 780 PNe out to 90
kpc in projected radius, agreeing with the GC value within the uncertainty.
We are also able to generate a mass profile of NGC 5128 from the total GC population
and the PNe, shown in Figure 13. The tracer mass estimator determines the total enclosed
mass for NGC 5128 within the outermost radius of a given tracer sample. It calculates this
total mass using a sample of objects defined within the radial range defined by the sample’s
inner and outermost radii. It is therefore possible to use a unique set of tracer objects,
denoted by the radial bin range, listed in the first column of Tables 2-5, to determine a mass
profile from independent mass estimates. The independent binning, leads to sample sizes in
the mass determination, in some cases generating higher uncertainties in the total enclosed
mass. The most certain mass is the one determined from the full sample of tracers.
In the mass determinations above, we have implicity assumed isotropy for the veloc-
ity distributions. But the possibility exists that the PNe (for example) might have radial
anisotropy which would produce their gradually falling σv(R) curve. Replacing Equation 5
– 19 –
in the tracer mass estimator by
16(α + γ − 2β)(4 − α− γ)(1 − ( rin
)(3−γ))
π(4 − 3β)(3 − γ)(1 − ( rin
)(4−α−γ))
which includes the anisotropy parameter, β, from Evans et al. (2003), we find that the mass
estimate from the PNe can be forced to agree with the mass estimate from the GCS for a
nominal β = 0.8. For perfect isotropy, β = 0. This would mean roughly 2:1 radial anisotropy
for the PNe in the outer halo. However, we find that any β in the wide range of −10 ≤ β ≤ 1
would still keep the two methods in agreement within their internal uncertainties, so we are
not yet in a position to tightly constrain any anisotropy. It is possible that the GCs may also
have anisotropy; it may therefore be too simplistic to find a range of β for the PNe for which
the masses of the PNe and GCs agree. However, the GCs are likelier to be nearly isotropic
than the PNe; the GCs are older, ”hotter” subsystems of the halo. In other studies, the
isotropy of the GCS orbits has also been shown to be a good assumption from mass profiles
of elliptical galaxies using X-ray observations (Côté et al. 2001, 2003; Bridges et al. 2006,
among others).
Both mass estimates can be compared to previous studies. First, we note the total
mass determined from the PN data with that of Peng, Ford & Freeman (2004b). While the
rotationally supported mass was determined here with different values of the mean rota-
tional velocity, they calculated the pressure supported mass using the identical tracer mass
estimator technique with exactly the same PN population. The total mass estimate given
by Peng, Ford & Freeman (2004b) is (5.3 ± 0.5) × 1011 M⊙. Subtracting their rotationally
supported mass leaves a pressure supported mass of ∼ 3.4×1011 M⊙, quite different from our
(8.46±1.72)×1011 M⊙. Recalculating our pressure supported mass estimate with γ = 2.54,
which was used in Peng, Ford & Freeman (2004b), we are able to reproduce their mass esti-
mate within the uncertainty. The values of γ differ between the two studies simply because
the γ used in Peng, Ford & Freeman (2004b) was the inverse of the surface density slope
instead of the inverse of the volume density slope. Using the correct value of γ = 3.54, their
pressure supported mass estimate would increase to 8.7× 1011M⊙, matching the mass found
in this study.
Second, we compare our total mass determined using the GC population with that from
Peng, Ford & Freeman (2004c). Using 215 GCs out to 40 kpc, they found a pressuresup-
ported mass of (3.4±0.8)×1011 M⊙, again much different from our pressure supported mass
of (1.26 ± 0.47) × 1012 M⊙ using 340 clusters out to 50 kpc. The large difference can again
be attributed to their using γ = 2.72 instead of deprojecting their surface density slope to
γ = 3.72. Using the correct value of γ, we find a pressure-supported mass of 7.5 × 1011 M⊙
using the same 215 clusters they used in their study. This corrected estimate is closer to the
– 20 –
pressure supported mass determined in our study, but it is not necessarily expected to agree
with our result, as our sample contains 130 more GCs and uses a slightly different γ that we
have independently redetermined.
Third, the mass determined by the H I shell study of NGC 5128 by Schiminovich et al.
(1994) found a mass of 2×1011 M⊙ within 15 kpc assuming a distance of 3.5 Mpc. With the
distance of 3.9 Mpc used in this study, the mass determined in their study would increase
to 2.2 × 1011 M⊙, which is 30% smaller than our total mass of 3.89± 0.94× 10
11 M⊙ within
15 kpc.
Lastly, we compare our determined mass to a recent study by Samurović (2006). Samurović
(2006) determined a total mass of NGC 5128 using GCs, PNe, and an X-ray data tech-
nique. The galaxy mass determined from the GC and PN data was obtained using the
tracer mass estimator and the spherical Jeans equation, as performed in our study. How-
ever, Samurović (2006) used the volume density slopes determined by Peng, Ford & Freeman
(2004b) and Peng, Ford & Freeman (2004c), for the PN and GC data, respectively. They ob-
tained mass estimates for NGC 5128 similar to those of Peng, Ford & Freeman (2004b) and
Peng, Ford & Freeman (2004c), discussed above, using an identical PN sample and slightly
increased GC sample. They also included an X-ray-modelling mass estimate for NGC 5128
from which they obtained masses of (7.0± 0.8)× 1011 M⊙ out to 50’ and (11.6± 1.0)× 10
M⊙ out to 80’. This mass estimate is similar to our PNe estimate out to the same radial
extent, but the author cautions that it is an overestimate of the true mass of NGC 5128
resulting from a lack of hydrostatic equilibrium in the outer region of the galaxy.
We note here that the mass estimates obtained are higher than those from Hui et al.
(1995), and Peng, Ford & Freeman (2004b) derived from the PNe using a two-component
mass model, as well as Samurović (2006), using an X-ray modelling technique. This dis-
crepancy is not fully understood and possibly lies in the assumptions that go into the mass
estimators with a spatially biased sample. We intend to pursue this issue further with an
upcoming larger sample of GCs with less spatial biases.
The mass of NGC 5128 that we find appears to be in the range of other giant elliptical
galaxies, such as NGC 1399 (∼ 2 × 1012 M⊙ out to 50 kpc; Richtler et al. 2004), M49
(∼ 2 × 1012 M⊙ out to their kinematically studied radius of 35 kpc; Côté et al. 2003), and
M87 (∼ 9 × 1011 M⊙ at 20 kpc, the onset of the projected cD envelope; Côté et al. 2001).
Clearly, it is legitimate to say that NGC 5128 is the largest, most massive galaxy in the
neighborhood of the Local Group, and one that can be talked about in the same category
as these other giants that reside in larger clusters.
The sample biases mentioned above in our currently available set of both GCs and PNe
– 21 –
place limitations on how much we can reasonably interpret the kinematic and dynamic data.
We are currently carrying out a set of new spectroscopic programs to increase the tracer
sample size and to remove the sample biases, leading to a more complete analysis of the halo
velocity field.
6. Discussion and Conclusions
Angular momentum is an essential quantity for characterizing the sizes, shapes, and
formation of galaxies and is often represented as the dimensionless spin parameter,
J |E|1/2
GM5/2
where J is the angular momentum, E is the binding energy, and M is the mass of the
galaxy. The spin parameter is representative of a galaxy’s angular momentum compared
to the amount of angular momentum needed for pure rotational support: the lower the Λ-
value, the less rotation and rotational support within the galaxy. For an elliptical galaxy in
gravitational equilibrium, the spin parameter simplifies to Λ ∼ 0.3 < (ΩR/σv) > (Fall 1979),
yielding Λ = 0.10 with (ΩR/σv) = 0.33 for the entire population of GCs in NGC 5128.
Table 6 shows the spin parameter for four giant galaxies with large GCS kinematic
studies, M87, M49, NGC 1399, and NGC 5128. The table columns give the galaxy name, the
rotation amplitude, the projected velocity dispersion, and the ratio of the rotation amplitude
to the velocity dispersion, followed by the spin parameter. These quantities are shown for
the metal-poor and metal-rich populations. What is clearly evident in Table 6 is the strong
galaxy to galaxy differences between these four galaxies, already hinted at in § 1. Though the
sample is still quite small, no obvious pattern emerges. There is an indication of metal-poor
and metal-rich GCSs having similar spin parameters within the same galaxy. M49 is the only
galaxy studied here where this may not be the case. Although the metal-poor and metal-rich
cluster spin parameters are consistent within the uncertainties, the metal-rich cluster spin
parameter of M49 is also consistent with zero.
In the monolithic collapse scenario, Peebles (1969) describes the angular momentum
within the galaxy as attributed to the tidal torque transferred from neighbouring proto-
galaxies during formation. In this scenario, Efstathiou & Jones (1979) found that a spin
parameter of Λ = 0.06 for elliptical systems is expected from simulations of the collapse of
an isolated protogalactic cloud. But NGC 5128, among many other giant elliptical galaxies,
is not in isolation, and therefore not necessarily expected to reproduce such a low spin
parameter. Also, the internal rotation axis changes at 5 kpc are not easily explained with
– 22 –
only the monolithic collapse scenario. In the monolithic collapse model, the inner regions
would be expected to have more pronounced rotations. Yet all four of the galaxies with
major kinematic studies presented here do not show a higher rotational signal in the inner
regions. In fact, for NGC 1399, the outer region (R > 6′) indicates rotation in the metal-poor
population that is not evident in the inner regions. Also, a slightly lower rotational signal
is present in the inner regions of NGC 5128 for the metal-poor population than in the outer
regions.
Hierarchical clustering of cold dark matter also relies on angular momentum in a galaxy
being produced by gravitational tidal torques during the growth of initial perturbations.
Sugerman, Summers, & Kamionkowski (2000) have demonstrated that the tidal torque the-
ory predicts an increase in angular momentum during the collapse, and with time, the
increase in angular momentum slows. Accretion of satellites and/or merger events is there-
fore a possible culprit for moving the angular momentum outward, as major mergers of disks
and bulges suggest that angular momentum resides largely in the outer regions of the galaxy
(Barnes 1992; Hernquist 1993).
Alternatively, Vitvitska et al. (2002) examine the change in spin parameter in a scenario
where the angular momentum in a galaxy is built up by mass accretion. Their results show
that the spin parameter changes sharply in major merger events in the galaxy and steadily
decreases with small satellite accretion events. They also show that the spin parameter for a
galaxy with a major merger after a redshift of z = 3 should be notably larger than a galaxy
that did not undergo such a major merger. Their study obtains an average of Λ = 0.045
from ΛCDM N -body simulations for galaxies with halo masses of (1.1 − 1.5) × 1012h−1 M⊙
with h = 0.7.
NGC 1399 and M49, with their weak rotation signals, are consistent with the model
predictions discussed above, whereby their major formation events could have occurred at
early times and with perhaps only minor accretions happening since then. However, NGC
5128 and M87 have spin parameters 2-3 times larger than predicted by the model averages.
For NGC 5128, this relatively large rotation (which is nearly independent of both metallicity
and radius) may, perhaps, be connected with its history within the Centaurus group envi-
ronment. The rotation speed and rotation axis for its extended group of satellite galaxies
are nearly identical to the NGC 5128 halo (Woodley 2006), much as if the accretion events
experienced by the central giant have been taking place preferentially along the main axis
of the entire group and in the same orientation. The GCS age distribution discussed by
Beasley et al. (2006) and the mean age for the halo field stars (Rejkuba et al. 2005) strongly
suggest that a high fraction of the stellar population in NGC 5128 formed long ago, with
particularly large bursts between 8 and 12 Gyr. Even if the galaxy underwent a significant
– 23 –
merger perhaps a few Gyr ago (the traces of which now appear in the halo arcs and shells),
the stars in it may already have been old at the time of the merger. Although a very few
younger GCs have formed since then, these make up a small minority of what is present, at
least for the R > 5 kpc halo outside the bulge region that now contains gas and dust.
The situation for M87, with its even larger rotation signature, may require a different
sort of individual history. Of the four galaxies compared here, it is at the dynamical center
of the richest environment (Virgo), has the most extensive cD-type envelope, and sits within
the most massive, extended, and dynamically evolved potential well. A single relatively
recent major merger could in principle have caused its present high rotation, but the lack of
distinctive tidal features does not necessarily favor such an interpretation and would at least
suggest that such a merger should have been with another large elliptical and nondissipative
galaxy. Côté et al. (2001) discuss an interpretation - at least partially resembling what we
suggest for NGC 5128 - that stellar material ”is gradually infalling onto M87 along the
so-called principal axis of the Virgo Cluster.”
In conclusion, we have presented a kinematic study of NGC 5128 that makes it now com-
parable to recent studies of the other giant galaxies, M87, M49, and NGC 1399. Using 340
GCs (158 metal-rich and 178 metal-poor GCs), we have calculated the rotation amplitude,
rotation axis, and velocity dispersion and have searched for radial and metallicity depen-
dences. Our findings show that both metallicity populations rotate with little dependence
on projected radius, with ΩR = 40±10, 31±14, and 47±15 km s−1 for the total, metal-poor,
and metal-rich populations, respectively. Perhaps the inner 5 kpc shows a slower rotation of
the metal-poor population, but more clusters would be needed to confirm this finding. The
rotation axis is 189±12o, 177±22o, and 202±15o east of north for the total, metal-poor, and
metal-rich populations out to a 50 kpc projected radius, assuming the velocity field is best
fit by a sine curve. The rotation axis does change at 5 kpc, following the zero-velocity curve
proposed by Peng, Ford & Freeman (2004b) or possibly full-on counterrotation. A study
with more GCs and lower uncertainties is needed to see what is happening in the innermost
5 kpc of NGC 5128. The velocity dispersion shows a modest increase with galactocentric
radius, although the outer regions (especially the metal-rich population) have less reliable
statistics; this increase could be driven purely by statistical effects. We find the velocity dis-
persion we find 123±5, 117±7, and 129±9 km s−1 for the total, metal-poor, and metal-rich
populations, respectively.
The PN data are also used to determine the kinematics of the halo of NGC 5128.
These show results that are encouragingly similar to those of the GC data, except that no
rotation axis change is noted with radius, and a decrease in velocity dispersion is found with
radius, possibly indicating a difference in orbital anisotropy compared with the GCs. A
– 24 –
very similar effect has been noted for the Leo elliptical NGC 3379, although with a much
smaller data sample (Romanowsky et al. 2003; Bergond et al. 2006; Pierce et al. 2006). We
also determine the total dynamical mass using both the GCs and the PNe by separately
calculating the pressure supported mass with the tracer mass estimator and the rotationally
supported mass using the spherical component of the Jeans equation. The total mass is
(1.3 ± 0.5) × 1012 M⊙ from the GC population out to a projected radius of 50 kpc, or
(1.0 ± 0.2) × 1012 M⊙ out to 90 kpc from the PNe.
Overall, we have enough evidence to cautiously conclude that a major episode of star
formation occurred about 8−10 Gyr ago (corresponding to a redshift z = 1.2 - 1.8) and this
may have been when the bulk of the visible galaxy was built. We still do not know just why
the most metal-poor clusters show up in such relatively large numbers and appear to have
ages of 10 − 12 Gyr, but this is a common issue in all big galaxies.
This kinematic study and the age study of Beasley et al. (2006) on the NGC 5128
cluster system indicate that additional spectroscopic studies to build up both the radial
velocity database and age distribution can lead to rich dividends. Large GC samples are
clearly needed to remove the current sample biases and to fully understand the complex
kinematics and history of this giant elliptical galaxy. It seems clear as well that each galaxy
needs to be individually studied to fully understand the different galaxy formation histories.
We are continuing these studies particularly for NGC 5128, with the eventual aim of at least
doubling the total GC sample size in this unique system.
Acknowledgements: WEH and GLHH acknowledge financial support from NSERC
through operating research grants. DAF thanks the ARC for financial support.
– 25 –
REFERENCES
Arnaboldi, M., Freeman, K.C., Capaccioli, M., & Ford, H. 1994, ESO Messanger, 76, 40
Arnaboldi, M., Freeman, K.C., Gerhard, O., Matthias, M., Kudritzki, R.P. Méndez, R.H.,
Capaccioli, M., & Ford, H. 1998, ApJ, 507, 759
Baade, W., & Minkowski, R. 1954, ApJ, 119, 215
Bahcall, J.N., & Tremaine, S. 1981, ApJ, 244, 805
Barnes, J.E. 1992, ApJ, 393, 484
Beasley, M.A., Forbes, D.A., Brodie, J.P., & Kissler-Patig, M. 2004, MNRAS, 347, 1150
Beasley, M.A., Bridges, T., Peng, E., Harris, W.E., Harris, G.L.H., Forbes, D.A., & Mackie,
G. 2006, in preparation
Bekki, K., Harris, W.E., & Harris, G.L.H. 2003, MNRAS, 338, 587
Bekki, K., Forbes, D.A., Beasley, M.A., & Couch, W.J. 2003, MNRAS, 334, 1334
Bekki, K., & Peng, E.W. 2006, MNRAS, 370, 1737
Bergond, G., Zepf, S.E., Romanowsky, A.J., Sharples, R.M., & Rhode, K.L. 2006, A&A,
448, 155
Bridges, T., Gebhardt, K., Sharples, R., Faifer, F.R., Forte, J.C., Beasley, M.A., Zepf, Z.E.,
Forbes, D.A., Pierce, M. 2006, MNRAS, 373, 157
Ciardullo, R., Jacoby, G.H., & Dejonghe, H.B. 1993, ApJ, 414, 454
Côté, P., McLaughlin, D.E., Hanes, D.A., Bridges, T.J., Geisler, D., Merritt, D., Hesser,
J.E., Harris, G.L.H., & Lee, M.G. 2001, ApJ, 559, 828
Côté, P., McLaughlin, D., Cohen, J.G., & Blakesless, J.P. 2003, ApJ, 591, 850
Dekel, A., Stoehr, F., Mamon, G.A., Cox, T.J., Novak, G.S., & Primak, J.R., 2005, Nature,
437, 707
Dufour, R.J., Harvel, C.A., Martins, D.M., Schiffer, F.H., Talent, D.L., Wells, D.C., van den
Bergh, S., & Talbot, R.J. 1979, AJ, 84, 284
Efstathiou, G., & Jones, B.J.T. 1979, MNRAS, 186, 133
– 26 –
Evans, N.W., Wilkinson, M.I., Perrett, K.M., & Bridges, T.J. 2003, ApJ, 583, 752
Fall, S.M. 1979, Rev. Mod. Phys., 51, 21
Ferrarese, L., Mould, J.R., Stetson, P.B., Tonry, J.L., Blakeslee, J.P., & Ajhar, E.A. 2006,
ApJ, in press (astro-ph/0605707)
Harris, G.L.H., Geisler, D., Harris, H.C., & Hesser, J.E. 1992, AJ, 104, 613
Harris, G.L.H., Harris, W.E., & Poole, G. 1999, AJ, 117, 855
Harris, W. E., & Harris, G. L. H. 2002, AJ, 123, 3108
Harris, W.E., Harris, G.L.H., Holland, S.T., & McLaughlin, D.E. 2002, AJ, 124, 1435
Harris, G.L.H., Harris, W.E., & Geisler, D. 2004, AJ, 128, 723
Harris, W.E., Harris, G.L.H., Barmby, P., McLaughlin, D.E., & Forbes, D. 2006, AJ, 132,
Heisler, J., Tremaine, S., & Bahcall, J.N. 1985, ApJ, 298, 8
Hernquist, I. 1993, ApJ, 409, 548
Hesser, J.E., Harris, H.C., van den Bergh, S., & Harris, G.L.H. 1984, ApJ, 276,491
Hesser, J.E., Harris, H.C., & Harris, G.L.H. 1986, ApJ, 303, L51
Hui, X., Ford, H.C., Freeman, K.C., & Dopita, M.A. 1995, ApJ, 449, 592
Kraft, R.P., Váquez, S.E., Forman, W.R., Jones, C., Murray, S.S., Hardcastle, M.J., Worrall,
D.M., Churazov, E. 2003, ApJ, 592, 129
Larsen, S.S., Brodie, J.P., Beasley, M.A., & Forbes, D.A. 2002, AJ, 124, 828
Lee, H., & Worthey, G. 2005, ApJS, 160, 176
Máız Apellániz, J. & Úbeda, L. 2005, ApJ, 629, 7873
Mamon, G.A., &  Lokas, E.L. 2005, MNRAS, 362, 95
Napolitano, N.R., Arnaboldi, M., Freeman, K.C., & Capaccioli, M. 2001, A&A, 377, 784
Napolitano, N.R., Arnaboldi, M., & Capaccioli, M. 2002, A&A, 383, 791
O’Sullivan, E., Forbes, D.A., & Ponman, T.J. 2001,MNRAS, 328, 461
http://arxiv.org/abs/astro-ph/0605707
– 27 –
Peebles, P.J.E. 1969, ApJ, 155, 393
Peng, E.W., Ford, H.C., Freeman, K.C., & White, R.L. 2002, AJ, 124, 3144
Peng, E.W., Ford, H.C., & Freeman, K.C. 2004, ApJS, 150, 367
Peng, E.W., Ford, H.C., & Freeman, K. 2004, ApJ, 602, 685
Peng, E.W., Ford, H.C., & Freeman, K. 2004, ApJ, 602, 705
Pierce, M., Beasley, M.A., Forbes, D.A., Bridges, T., Gebhardt, K., Faifer, F.R., Forte, J.C.,
Zepf, S.E., Sharples, R., Hanes, D.A., & Proctor, R. 2006, MNRAS, 366, 1253
Press, W.H., Teukolsky, S.A., Vetterling, W.T., & Flannery, B.P. 1992, Numerical Recipes
in Fortran (2nd Ed., Cambridge: Camdridge University Press)
Puzia, T.H., Kissler-Patig, M., Thomas, D., Maraston, C., Saglia, R.P., Bender, R., Goud-
frooij, P., & Hempel, M. 2005, A&A, 439, 997
Reed, L.G., Harris, G.L.H., & Harris, W.E. 1994, AJ, 107, 555
Rejkuba, M. 2001, A&A, 269, 812
Rejkuba, M. 2004, A&A, 413, 903
Rejkuba, M., Greggio, L., Harris, W.E., Harris, G.L.H., & Peng, E.W. 2005, ApJ, 631, 262
Rejkuba, M., Dubath, P., Minniti, D., & Meylan, G. 2007, A&A, in press (astro-ph/0703385)
Richtler, T., Dirsch, B., Gebhardt, K., Geisler, D., Hilker, M., Alonso, M. V., Forte, J. C,.
and Grebel, E. K., Infante, L., Larsen, S., Minniti, D., & Rejkuba, M. 2004, AJ, 127,
Romanowsky, A.J., Douglas, N.G., Arnaboldi, M., Kuijken, K., Merrifield, M.R., Napolitano,
N.R., Capaccioli, M., & Freeman, K.C., 2003, Science, 301, 1696
Saglia, R.P., Kronawitter, A., Gerhard, O., & Bender, R. 2000, AJ, 119, 153
Samurović, S. 2006, Serb. Astron. J., 173, 35
Schiminovich, D., van Gorkom, J.H., van der Hulst, J.M., & Kasow, S. 1994, ApJ, 423, L101
Sharples, R. 1988, IAU Symp. 126: The Harlow-Sharpley Symposium on Globular Cluster
Systems in Galaxies, 126, 245
http://arxiv.org/abs/astro-ph/0703385
– 28 –
Strader, J., Brodie, J.P., Cenarro, A.J., Beasley, M.A., & Forbes, D.A. 2005, AJ, 130, 1315
Sugerman, B., Summers, F.J., & Kamionkowski, M. 2000, MNRAS, 311, 762
Thomas, D., Maraston, C., & Korn, A. 2004, MNRAS, 351, 19
Toomre, A., & Toomre, J. 1972, ApJ, 178, 623
van den Bergh, S., Hesser, J.E., & Harris, G.L.H. 1981, AJ, 86, 24
Vitvitska, M., Klypin, A.A., Kravtsov, A.V., Wechsler, R.H., Primack, J.R., & Bullock, J.S.
2002, ApJ, 581, 799
Woodley, K.A., Harris, W.E., & Harris, G.L.H. 2005, AJ, 129, 2654
Woodley, K.A. 2006, AJ, 132, 2424
This preprint was prepared with the AAS LATEX macros v5.2.
Table 1. The Globular Cluster System Catalogue of NGC 5128
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0001 pff gc-028 13 20 01.16 -42 56 51.5 6.46 20.11 19.68 18.75 18.20 17.60 0.07 0.02 0.01 0.01 0.03 19.92 19.04 18.22 0.01 0.01 0.01 0.43 0.93 0.55 1.15 0.82 0.88 1.70 524±165
GC0002 HH-048 13 22 45.36 -43 07 08.8 30.26 - - - - - - - - - - - - - - - - - - - - - - - 856±507
GC0003 HH-080 13 23 38.33 -42 46 22.8 24.84 - - - - - - - - - - 19.45 18.72 17.98 0.02 0.01 0.01 - - - - 0.74 0.72 1.46 497±337
GC0004 HGHH-40/HH-044/C40 13 23 42.37 -43 09 37.8 21.02 19.37 19.01 18.12 17.59 17.03 0.04 0.01 0.01 0.01 0.03 20.12 19.28 18.49 0.02 0.01 0.01 0.35 0.89 0.53 1.10 0.79 0.84 1.63 365±244,5,7
GC0005 HGHH-01/C1 13 23 44.19 -43 11 11.8 21.41 - - - - - - - - - - 18.73 18.00 17.25 0.06 0.03 0.03 - - - - 0.76 0.72 1.48 642±11,5,7,8
GC0006 pff gc-001 13 23 49.62 -43 14 32.0 22.36 20.39 19.91 18.91 18.36 17.60 0.09 0.02 0.01 0.01 0.03 20.22 19.25 18.38 0.02 0.01 0.01 0.47 1.01 0.55 1.31 0.87 0.97 1.84 711±355,7
GC0007 AAT301956 13 23 54.52 -43 20 01.1 25.41 21.22 21.13 20.42 19.98 19.43 0.18 0.06 0.02 0.02 0.04 - - - - - - 0.09 0.71 0.44 0.98 - - - 287±1627
GC0008 HH-099 13 23 56.70 -42 59 59.8 16.66 - - - - - - - - - - 21.72 20.90 20.01 0.09 0.09 0.06 - - - - 0.89 0.82 1.71 798±497
GC0009 AAT101931 13 23 58.58 -42 57 17.0 16.73 20.58 20.57 19.88 19.43 18.96 0.06 0.02 0.01 0.01 0.03 20.60 20.09 19.45 0.01 0.01 - 0.02 0.68 0.45 0.92 0.64 0.51 1.15 590±1447
GC0010 AAT101906 13 23 58.76 -43 01 35.2 16.25 20.45 19.90 18.89 18.28 17.57 0.06 0.02 0.01 0.01 0.03 20.23 19.11 18.28 0.02 0.03 0.02 0.54 1.01 0.61 1.32 0.83 1.12 1.95 511±317
GC0011 pff gc-002 13 23 59.51 -43 17 29.1 22.94 20.70 20.43 19.55 19.02 18.44 0.07 0.02 0.01 0.01 0.03 20.61 19.83 19.07 0.03 0.03 0.01 0.27 0.88 0.53 1.11 0.76 0.78 1.55 653±375,7
GC0012 AAT102120 13 23 59.61 -42 55 19.4 17.11 20.60 20.59 19.92 19.49 19.03 0.06 0.02 0.01 0.01 0.03 20.61 20.13 19.49 0.01 0.01 0.01 0.02 0.67 0.44 0.89 0.64 0.48 1.12 293±837
GC0013 HH-001 13 24 02.67 -42 48 32.2 20.00 - - - - - - - - - - 22.52 21.20 19.89 0.08 0.05 0.03 - - - - 1.31 1.32 2.63 775±747
GC0014 pff gc-003 13 24 03.23 -43 28 13.9 31.17 20.39 20.18 19.31 18.80 18.21 0.15 0.02 0.01 0.01 0.03 20.39 19.64 18.80 0.02 0.02 0.02 0.21 0.87 0.51 1.09 0.84 0.76 1.59 704±225,7
GC0015 pff gc-004 13 24 03.74 -43 35 53.4 37.98 21.12 20.84 20.01 19.49 18.92 0.28 0.03 0.01 0.01 0.03 - - - - - - 0.28 0.83 0.52 1.09 - - - 571±385,7
GC0016 AAT103195 13 24 05.98 -43 03 54.7 15.18 21.57 21.10 20.13 19.58 18.98 0.14 0.03 0.01 0.01 0.03 21.34 20.39 19.50 0.01 0.01 0.01 0.47 0.97 0.56 1.15 0.89 0.95 1.84 277±677
GC0017 AAT30486710 13 24 08.62 -43 16 27.1 21.04 22.12 21.15 19.91 19.20 18.54 0.25 0.03 0.01 0.01 0.03 21.62 20.28 19.18 0.01 - - 0.97 1.24 0.71 1.36 1.10 1.34 2.44 305±567
GC0018 AAT305341 13 24 10.97 -43 12 52.8 18.27 22.13 21.54 20.51 19.88 19.19 0.23 0.04 0.01 0.01 0.03 21.87 20.80 19.90 0.01 0.01 0.01 0.59 1.03 0.63 1.31 0.89 1.07 1.97 440±1187
GC0019 HHH86-28/C28 13 24 18.06 -42 49 01.1 17.57 19.52 19.33 18.50 17.99 17.45 0.03 0.01 0.01 0.01 0.03 19.46 18.75 18.03 0.02 0.01 0.01 0.19 0.83 0.52 1.05 0.72 0.71 1.43 461±223,5,7
GC0020 pff gc-005 13 24 18.92 -43 14 30.1 18.33 21.89 21.31 20.29 19.71 19.07 0.18 0.04 0.01 0.01 0.03 21.63 20.64 19.72 0.02 0.02 0.01 0.58 1.02 0.58 1.22 0.91 1.00 1.91 750±335,7
GC0021 WHH-1/HH-096 13 24 21.40 -43 02 36.8 12.19 19.14 18.85 18.01 17.48 16.98 0.03 0.01 0.01 0.01 0.03 19.11 18.33 17.63 0.02 0.02 0.03 0.29 0.84 0.53 1.03 0.70 0.78 1.48 583±296,7
GC0022 pff gc-006 13 24 23.72 -43 07 52.1 13.48 20.22 20.00 19.22 18.70 18.20 0.05 0.02 0.01 0.01 0.03 20.10 19.46 18.73 0.01 0.01 0.01 0.21 0.78 0.52 1.02 0.73 0.65 1.37 644±285,7
GC0023 WHH-2 13 24 23.98 -42 54 10.7 13.56 20.57 20.45 19.67 19.17 18.65 0.06 0.02 0.01 0.01 0.03 20.54 19.94 19.27 0.03 0.03 0.02 0.12 0.78 0.50 1.02 0.68 0.59 1.27 582±816
GC0024 pff gc-007 13 24 24.15 -42 54 20.6 13.45 21.85 21.16 20.12 19.53 18.82 0.17 0.03 0.01 0.01 0.03 21.54 20.50 19.60 0.02 0.02 0.01 0.69 1.04 0.59 1.30 0.90 1.04 1.94 617±255,7
GC0025 AAT308432 13 24 25.55 -43 21 35.6 23.38 20.98 20.43 19.40 18.80 18.11 0.27 0.02 0.01 0.01 0.03 20.83 19.78 18.84 0.03 0.01 0.02 0.54 1.04 0.60 1.29 0.94 1.05 1.99 835±837
GC0026 C111 13 24 26.97 -43 17 20.0 19.62 - - - - - - - - - - 22.54 22.25 21.36 0.04 0.04 0.04 - - - - 0.89 0.29 1.17 -
GC0027 AAT106695 13 24 28.18 -42 53 04.3 13.54 20.95 20.75 19.63 18.96 18.30 0.09 0.03 0.01 0.01 0.03 21.16 20.17 19.19 0.06 0.06 0.04 0.20 1.12 0.67 1.33 0.98 0.99 1.96 835±837
GC0028 AAT106880 13 24 28.44 -42 57 52.9 11.30 21.11 20.94 20.14 19.61 19.11 0.10 0.03 0.01 0.01 0.03 21.06 20.43 19.65 0.01 0.01 0.01 0.18 0.80 0.53 1.03 0.79 0.63 1.41 558±987
GC0029 pff gc-008 13 24 29.20 -43 21 56.5 23.38 21.40 20.93 19.94 19.41 18.75 0.35 0.03 0.01 0.01 0.03 21.24 20.31 19.43 0.02 0.01 0.01 0.47 0.99 0.54 1.19 0.87 0.93 1.81 466±385,7
GC0030 AAT107060 13 24 29.23 -43 08 36.6 13.02 21.81 21.26 20.26 19.63 19.00 0.19 0.04 0.01 0.01 0.03 21.60 20.62 19.69 0.01 0.01 0.01 0.55 1.01 0.63 1.25 0.93 0.99 1.92 600±587
GC0031 AAT107145 13 24 29.73 -43 02 06.5 10.62 21.20 20.93 20.08 19.50 18.97 0.11 0.03 0.01 0.01 0.03 21.16 20.33 19.55 0.03 0.02 0.04 0.27 0.85 0.58 1.11 0.78 0.82 1.60 595±2027
GC0032 pff gc-009 13 24 31.35 -43 11 26.7 14.55 20.82 20.58 19.77 19.25 18.70 0.07 0.02 0.01 0.01 0.03 20.73 20.05 19.26 0.03 0.02 0.01 0.23 0.81 0.52 1.07 0.80 0.68 1.47 683±385,7
GC0033 WHH-3 13 24 32.17 -43 10 56.9 14.10 20.56 20.32 19.49 18.97 18.43 0.06 0.02 0.01 0.01 0.03 20.46 19.76 18.99 0.02 0.02 0.01 0.25 0.83 0.52 1.06 0.76 0.71 1.47 709±546,7
GC0034 C112 13 24 32.66 -43 18 48.8 20.32 - - - - - - - - - - 22.98 22.22 21.31 0.03 0.02 0.02 - - - - 0.91 0.75 1.67 -
GC0035 pff gc-0109 13 24 33.09 -43 18 44.8 20.23 20.45 20.36 19.68 19.26 18.84 0.06 0.02 0.01 0.01 0.03 20.45 19.91 19.24 0.01 0.01 0.01 0.09 0.68 0.42 0.85 0.67 0.54 1.21 344±585
GC0036 AAT107977 13 24 34.63 -43 12 50.5 15.18 21.73 21.18 20.18 19.57 18.89 0.17 0.04 0.01 0.01 0.03 21.52 20.54 19.59 0.02 0.02 0.01 0.54 1.01 0.60 1.28 0.95 0.98 1.93 517±1237
GC0037 pff gc-011 13 24 36.87 -43 19 16.2 20.36 20.01 19.82 19.03 18.53 18.00 0.13 0.02 0.01 0.01 0.03 19.95 19.33 18.55 0.01 0.01 0.01 0.18 0.79 0.50 1.04 0.78 0.62 1.40 616±415,7
GC0038 C113 13 24 37.75 -43 16 26.5 17.80 - - - - - - - - - - 20.50 19.87 19.12 0.02 0.02 0.01 - - - - 0.75 0.63 1.38 -
GC0039 pff gc-012 13 24 38.77 -43 06 26.6 10.38 21.24 20.51 19.45 18.83 18.15 0.13 0.02 0.01 0.01 0.03 20.92 19.78 18.85 0.01 0.01 0.01 0.73 1.06 0.62 1.30 0.93 1.14 2.07 573±215
GC0040 HGHH-41/C41 13 24 38.98 -43 20 06.4 20.94 20.20 19.59 18.59 17.94 17.32 0.06 0.02 0.01 0.01 0.03 19.95 18.92 17.97 0.02 0.01 0.01 0.61 1.00 0.65 1.27 0.95 1.03 1.98 363±14,5,7,8
GC0041 HGHH-29/C29 13 24 40.39 -43 18 05.3 19.01 19.77 19.15 18.15 17.54 16.89 0.04 0.01 0.01 0.01 0.03 19.46 18.37 17.53 0.04 0.03 0.02 0.62 1.00 0.61 1.26 0.84 1.09 1.92 726±13,5,7,8
GC0042 pff gc-013 13 24 40.42 -43 35 04.9 35.01 20.06 19.83 19.00 18.49 17.98 0.15 0.02 0.01 0.01 0.03 - - - - - - 0.24 0.83 0.51 1.03 - - - 727±315,7
GC0043 C114 13 24 40.48 -42 53 35.3 11.46 - - - - - - - - - - 23.46 22.39 21.42 0.05 0.04 0.03 - - - - 0.97 1.07 2.04 -
GC0044 WHH-4/HH-024 13 24 40.60 -43 13 18.1 14.89 20.71 20.12 19.12 18.50 17.85 0.07 0.02 0.01 0.01 0.03 20.46 19.40 18.53 0.03 0.02 0.01 0.60 1.00 0.62 1.27 0.87 1.06 1.93 688±256,7
GC0045 pff gc-014 13 24 41.05 -42 59 48.4 8.62 21.60 21.17 20.23 19.67 18.94 0.26 0.06 0.02 0.02 0.03 21.47 20.56 19.76 0.04 0.03 0.04 0.43 0.94 0.57 1.30 0.80 0.91 1.71 690±345,7
GC0046 pff gc-015 13 24 41.20 -43 01 45.6 8.51 20.27 20.01 19.22 18.74 18.15 0.06 0.02 0.01 0.01 0.03 20.12 19.40 18.70 0.05 0.04 0.05 0.26 0.79 0.47 1.06 0.70 0.72 1.42 533±255,7
GC0047 AAT109380 13 24 43.58 -43 08 43.2 11.05 19.64 19.52 18.80 18.32 17.87 0.04 0.01 0.01 0.01 0.03 19.60 19.02 18.30 0.01 - - 0.12 0.73 0.48 0.93 0.72 0.59 1.31 465±387
GC0048 pff gc-016 13 24 43.60 -42 53 07.3 11.36 21.38 20.87 19.85 19.26 18.58 0.12 0.03 0.01 0.01 0.03 21.19 20.21 19.33 0.02 0.02 0.01 0.51 1.02 0.60 1.27 0.88 0.98 1.85 505±175,7
GC0049 pff gc-017 13 24 43.63 -42 58 16.4 8.54 20.54 20.32 19.51 18.99 18.47 0.07 0.02 0.01 0.01 0.03 20.44 19.78 19.01 0.01 0.01 0.01 0.22 0.81 0.52 1.04 0.77 0.66 1.43 963±505
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0050 WHH-5 13 24 44.58 -43 02 47.3 8.04 20.47 20.03 19.06 18.49 17.87 0.08 0.02 0.01 0.01 0.03 20.29 19.19 18.90 0.05 0.04 0.04 0.44 0.97 0.57 1.19 0.29 1.09 1.39 671±416
GC0051 HH-054 13 24 45.22 -43 23 19.2 23.49 - - - - - - - - - - 20.92 20.08 19.25 0.05 0.03 0.04 - - - - 0.82 0.84 1.66 998±2507
GC0052 AAT109711 13 24 45.35 -42 59 33.5 7.89 19.88 19.87 19.30 18.90 18.33 0.06 0.02 0.01 0.01 0.03 19.84 19.48 18.91 0.02 0.02 0.04 0.02 0.56 0.40 0.98 0.58 0.36 0.94 276±597
GC0053 AAT109788 13 24 45.78 -43 02 24.5 7.75 21.82 21.02 19.89 19.23 18.56 0.25 0.04 0.01 0.01 0.03 21.39 20.17 19.43 0.02 0.02 0.03 0.80 1.14 0.65 1.33 0.74 1.22 1.96 527±307
GC0054 HGHH-G019/G19 13 24 46.46 -43 04 11.6 8.12 20.16 19.95 19.16 18.64 18.13 0.06 0.02 0.01 0.01 0.03 20.06 19.38 18.64 0.04 0.03 0.03 0.21 0.79 0.52 1.03 0.75 0.67 1.42 710±224,5,7
GC0055 HGHH-09/C9 13 24 46.72 -43 01 18.4 7.48 20.00 19.76 18.95 18.40 17.90 0.05 0.02 0.01 0.01 0.03 19.87 19.13 18.42 0.04 0.04 0.04 0.24 0.81 0.56 1.05 0.70 0.74 1.45 501±214,5
GC0056 pff gc-018 13 24 47.10 -43 06 01.7 8.87 20.90 20.03 18.91 18.25 17.54 0.10 0.02 0.01 0.01 0.03 20.45 19.23 18.28 0.02 0.01 0.01 0.87 1.12 0.66 1.37 0.95 1.22 2.17 534±155,6,7
GC0057 HGHH-G277/G277 13 24 47.37 -42 58 29.8 7.82 20.26 19.96 19.10 18.56 18.02 0.06 0.02 0.01 0.01 0.03 20.14 19.37 18.61 0.01 0.01 0.01 0.30 0.87 0.53 1.08 0.76 0.77 1.53 714±334,5,7
GC0058 WHH-6 13 24 47.37 -42 57 51.2 8.06 21.33 20.75 19.73 19.12 18.44 0.15 0.03 0.01 0.01 0.03 21.08 20.07 19.15 0.01 0.01 0.01 0.58 1.02 0.62 1.29 0.93 1.00 1.93 685±436,7
GC0059 AAT110138 13 24 47.61 -43 10 48.5 12.12 20.87 20.53 19.67 19.11 18.57 0.10 0.03 0.01 0.01 0.03 20.75 19.98 19.16 0.03 0.02 0.01 0.34 0.87 0.56 1.10 0.82 0.77 1.59 358±1377
GC0060 HHH86-10/C10 13 24 48.06 -43 08 14.2 10.13 19.87 19.44 18.49 17.91 17.33 0.05 0.01 0.01 0.01 0.03 19.66 18.75 17.93 0.03 0.03 0.01 0.44 0.95 0.58 1.16 0.81 0.91 1.73 829±222,5,6,7
GC0061 C115 13 24 48.71 -42 52 35.5 11.12 - - - - - - - - - - 20.88 20.23 19.51 0.02 0.02 0.01 - - - - 0.73 0.65 1.37 -
GC0062 pff gc-019 13 24 48.97 -42 57 48.4 7.81 20.10 19.87 19.05 18.53 18.00 0.05 0.02 0.01 0.01 0.03 20.00 19.31 18.57 0.03 0.03 0.01 0.23 0.81 0.53 1.05 0.74 0.69 1.43 607±275
GC0063 AAT110410 13 24 49.38 -43 08 17.7 10.00 21.47 21.18 20.34 19.79 19.23 0.16 0.04 0.02 0.01 0.03 21.37 20.66 19.81 0.03 0.02 0.01 0.29 0.84 0.55 1.11 0.85 0.71 1.56 580±817
GC0064 AAT110551 13 24 50.09 -43 07 36.2 9.42 21.43 21.08 20.44 20.04 19.49 0.16 0.04 0.02 0.02 0.03 21.19 20.70 20.03 0.02 0.02 0.01 0.35 0.64 0.41 0.96 0.67 0.49 1.16 615±767
GC0065 pff gc-020 13 24 50.48 -42 59 49.0 6.92 20.57 20.33 19.53 19.00 18.47 0.09 0.03 0.01 0.01 0.03 20.42 19.58 19.68 0.05 0.04 0.04 0.24 0.80 0.53 1.06 -0.11 0.85 0.74 331±475
GC0066 HGHH-42/C42 13 24 50.87 -43 01 22.9 6.72 20.53 19.91 18.86 18.24 17.53 0.09 0.02 0.01 0.01 0.03 20.21 19.11 18.21 0.04 0.03 0.05 0.62 1.05 0.63 1.33 0.90 1.10 2.00 552±124,5,7
GC0067 VHH81-02/C2 13 24 51.49 -43 12 11.1 12.86 19.64 19.33 18.50 18.01 17.42 0.04 0.01 0.01 0.01 0.03 19.48 18.72 17.94 0.04 0.03 0.01 0.31 0.83 0.49 1.07 0.78 0.77 1.55 628±222,5,6,7
GC0068 C100 13 24 51.80 -43 04 33.7 7.33 - - 20.08 - - - - - - - 20.44 19.72 19.03 0.08 0.08 0.10 - - - 1.28 0.69 0.72 1.41 -
GC0069 AAT111033 13 24 52.98 -43 11 55.8 12.50 21.17 20.93 20.12 19.66 19.13 0.11 0.03 0.01 0.01 0.03 21.10 20.40 19.64 0.01 0.01 0.01 0.24 0.81 0.46 0.99 0.76 0.70 1.47 302±1667
GC0070 HGHH-G302/G302 13 24 53.29 -43 04 34.8 7.15 20.30 20.01 19.20 18.69 18.16 0.07 0.02 0.01 0.01 0.03 20.18 19.50 18.73 0.02 0.01 0.01 0.28 0.81 0.52 1.04 0.77 0.68 1.45 558±434,5
GC0071 AAT111185 13 24 54.00 -43 04 24.4 6.96 20.92 20.76 19.92 19.41 18.92 0.11 0.03 0.01 0.01 0.03 20.90 20.28 19.37 0.02 0.02 0.02 0.16 0.84 0.51 1.00 0.91 0.62 1.53 466±877
GC0072 pff gc-021 13 24 54.18 -42 54 50.4 8.78 20.21 20.03 19.25 18.75 18.24 0.06 0.02 0.01 0.01 0.03 20.13 19.52 18.81 0.03 0.02 0.01 0.18 0.78 0.50 1.01 0.70 0.62 1.32 594±505
GC0073 pff gc-022 13 24 54.33 -43 03 15.5 6.44 20.72 20.58 19.84 19.37 18.90 0.11 0.03 0.01 0.01 0.03 20.69 20.09 19.37 0.03 0.02 0.02 0.14 0.74 0.48 0.95 0.72 0.60 1.32 619±445,7
GC0074 HHH86-30/C30 13 24 54.35 -42 53 24.8 9.84 18.76 18.24 17.25 16.67 16.02 0.03 0.01 0.01 0.01 0.03 18.47 17.49 16.68 0.03 0.04 0.02 0.52 0.98 0.58 1.23 0.81 0.98 1.79 778±133,5,6,7
GC0075 AAT111296 13 24 54.49 -43 05 34.7 7.50 21.70 20.99 19.96 19.31 18.61 0.23 0.04 0.01 0.01 0.03 21.40 20.28 19.33 0.02 0.01 0.01 0.71 1.03 0.65 1.35 0.96 1.11 2.07 695±457
GC0076 pff gc-023 13 24 54.55 -42 48 58.7 13.59 20.55 20.30 19.44 18.90 18.37 0.06 0.02 0.01 0.01 0.03 20.48 19.74 18.97 0.01 0.01 0.01 0.25 0.86 0.54 1.08 0.77 0.74 1.51 457±315,7
GC0077 HGHH-11/C11 13 24 54.73 -43 01 21.7 6.01 19.55 18.96 17.91 17.26 16.61 0.05 0.01 0.01 0.01 0.03 19.21 17.98 17.20 0.06 0.05 0.06 0.59 1.05 0.66 1.30 0.79 1.23 2.01 753±12,4,5,6,7,8
GC0078 AAT111406 13 24 55.29 -43 03 15.6 6.28 21.84 21.15 20.13 19.50 18.80 0.30 0.05 0.02 0.01 0.03 21.66 20.70 18.80 0.03 0.02 0.01 0.69 1.03 0.63 1.33 1.90 0.96 2.86 669±777
GC0079 C116 13 24 55.46 -43 09 58.5 10.61 - - - - - - - - - - 23.80 22.74 21.84 0.06 0.02 0.03 - - - - 0.90 1.07 1.97 -
GC0080 HH-052 13 24 55.71 -43 22 48.4 22.43 - - - - - - - - - - 22.58 21.61 20.42 0.05 0.03 0.03 - - - - 1.19 0.97 2.16 921±1467
GC0081 pff gc-024 13 24 55.71 -43 20 39.1 20.36 21.07 20.73 19.84 19.31 18.73 0.28 0.03 0.01 0.01 0.03 21.00 20.17 19.34 0.02 0.01 0.01 0.34 0.89 0.53 1.11 0.83 0.83 1.66 279±385,7
GC0082 C117 13 24 56.06 -42 54 29.6 8.80 - - - - - - - - - - 21.27 20.18 19.26 0.01 0.02 0.01 - - - - 0.92 1.09 2.01 -
GC0083 AAT111563 13 24 56.08 -43 10 16.4 10.79 21.34 21.03 20.45 20.05 19.62 0.15 0.04 0.02 0.02 0.03 21.14 20.73 20.05 0.02 0.01 0.02 0.31 0.58 0.41 0.83 0.68 0.41 1.09 649±1027
GC0084 HGHH-G279 13 24 56.27 -43 03 23.4 6.15 19.97 19.91 19.45 19.17 18.88 0.06 0.02 0.01 0.01 0.03 19.76 19.38 19.83 0.01 0.01 0.01 0.06 0.45 0.29 0.57 -0.45 0.38 -0.07 366±344,5,7
GC0085 C118 13 24 57.17 -43 08 42.6 9.39 - - - - - - - - - - 22.60 21.76 20.67 0.04 0.03 0.02 - - - - 1.08 0.84 1.92 -
GC0086 HGHH-31/C31 13 24 57.44 -43 01 08.1 5.52 20.09 19.42 18.38 17.75 17.06 0.08 0.02 0.01 0.01 0.03 19.73 18.59 17.71 0.04 0.03 0.04 0.67 1.04 0.62 1.31 0.88 1.14 2.02 690±183,5,7
GC0087 HGHH-G369 13 24 57.52 -42 59 23.3 5.78 19.82 19.58 18.74 18.22 17.69 0.06 0.02 0.01 0.01 0.03 19.67 18.96 18.24 0.04 0.03 0.05 0.24 0.83 0.53 1.06 0.72 0.71 1.44 512±174,5,6,7
GC0088 pff gc-025 13 24 57.56 -43 05 32.8 7.04 21.50 21.02 20.02 19.39 18.67 0.20 0.04 0.02 0.01 0.03 21.41 20.41 19.45 0.04 0.03 0.02 0.47 1.00 0.63 1.35 0.96 1.00 1.97 923±305
GC0089 C119 13 24 57.69 -42 55 48.4 7.64 - - - - - - - - - - 21.16 21.02 20.67 0.03 0.03 0.02 - - - - 0.35 0.14 0.49 -
GC0090 C120 13 24 57.95 -42 52 04.9 10.56 - - - - - - - - - - 23.26 22.34 21.43 0.04 0.04 0.03 - - - - 0.90 0.92 1.83 -
GC0091 VHH81-03/C3 13 24 58.21 -42 56 10.0 7.33 19.34 18.73 17.71 17.10 16.44 0.04 0.01 0.01 0.01 0.03 19.02 17.88 17.08 0.04 0.03 0.02 0.61 1.02 0.61 1.26 0.80 1.14 1.94 562±21,3,5,6,7,8
GC0092 C121 13 24 58.42 -43 08 21.2 8.97 - - - - - - - - - - 23.53 23.01 22.45 0.05 0.04 0.09 - - - - 0.56 0.52 1.08 -
GC0093 pff gc-026 13 24 58.45 -42 42 53.3 19.02 20.44 20.33 19.52 19.07 18.50 0.08 0.02 0.01 0.01 0.03 20.47 19.82 19.09 0.02 0.01 0.01 0.12 0.81 0.45 1.02 0.73 0.65 1.37 490±675,7
GC0094 C12211 13 24 59.01 -43 08 21.4 8.91 - - - - - - - - - - - - 22.33 - - - - - - - - - - -
GC0095 C123 13 24 59.92 -43 09 08.6 9.46 - - - - - - - - - - 21.88 21.10 20.24 0.02 0.01 0.01 - - - - 0.86 0.78 1.64 -
GC0096 AAT112158 13 25 00.15 -42 54 09.0 8.61 21.99 21.43 20.43 19.86 19.23 0.25 0.05 0.02 0.01 0.03 21.75 20.78 19.88 0.01 0.01 0.01 0.55 1.00 0.57 1.20 0.90 0.96 1.87 699±437
GC0097 C124 13 25 00.37 -43 10 46.9 10.85 - - - - - - - - - - 23.07 22.36 21.57 0.03 0.02 0.03 - - - - 0.78 0.71 1.50 -
GC0098 pff gc-027 13 25 00.64 -43 05 30.3 6.58 21.22 20.75 19.74 19.13 18.45 0.17 0.04 0.01 0.01 0.03 21.05 20.06 19.11 0.01 0.01 0.01 0.47 1.01 0.61 1.29 0.95 0.99 1.94 524±345,7
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0099 C125 13 25 00.83 -43 11 10.6 11.16 - - - - - - - - - - 22.34 21.55 20.66 0.03 0.02 0.02 - - - - 0.89 0.78 1.67 -
GC0100 C126 13 25 00.91 -43 09 14.5 9.45 - - - - - - - - - - 24.02 23.54 22.66 0.04 0.05 0.08 - - - - 0.88 0.48 1.35 -
GC0101 C127 13 25 01.32 -43 08 43.4 8.97 - - - - - - - - - - 23.21 22.42 21.62 0.04 0.02 0.03 - - - - 0.80 0.79 1.59 -
GC0102 C128 13 25 01.46 -43 08 33.0 8.81 - - - - - - - - - - 23.08 22.04 20.95 0.05 0.03 0.02 - - - - 1.09 1.04 2.13 -
GC0103 pff gc-029 13 25 01.60 -42 54 40.9 8.03 19.97 19.75 19.37 19.06 18.71 0.05 0.02 0.01 0.01 0.03 19.72 19.50 19.10 0.03 0.03 0.01 0.22 0.38 0.31 0.65 0.40 0.22 0.62 570±385
GC0104 C129 13 25 01.63 -42 50 51.3 11.34 - - - - - - - - - - 22.59 21.71 20.83 0.04 0.02 0.02 - - - - 0.88 0.88 1.76 -
GC0105 pff gc-030 13 25 01.73 -43 00 09.9 4.83 21.68 20.94 19.89 19.26 18.54 0.36 0.06 0.02 0.02 0.03 21.21 19.93 20.43 0.05 0.04 0.02 0.73 1.05 0.64 1.35 -0.50 1.29 0.78 357±295
GC0106 HGHH-04/C4 13 25 01.83 -43 09 25.4 9.52 19.10 18.86 18.04 17.50 16.98 0.03 0.01 0.01 0.01 0.03 18.95 18.24 17.50 0.04 0.03 0.01 0.23 0.82 0.54 1.06 0.74 0.71 1.45 689±161,3,5,6,7
GC0107 C130 13 25 01.86 -42 52 27.8 9.88 - - - - - - - - - - 21.22 20.58 19.85 0.01 0.01 0.01 - - - - 0.73 0.64 1.37 -
GC0108 pff gc-031 13 25 02.76 -43 11 21.2 11.17 20.51 20.29 19.48 18.99 18.42 0.07 0.02 0.01 0.01 0.03 20.43 19.75 18.95 0.03 0.02 0.01 0.23 0.81 0.49 1.06 0.80 0.68 1.48 444±335
GC0109 HGHH-G176 13 25 03.13 -42 56 25.1 6.51 20.47 19.94 18.93 18.32 17.67 0.09 0.02 0.01 0.01 0.03 20.24 19.23 18.36 0.01 0.02 0.01 0.54 1.01 0.61 1.26 0.87 1.01 1.88 551±134,5,7
GC0110 HGHH-G066 13 25 03.18 -43 03 02.5 4.85 20.26 19.67 18.68 18.15 17.44 0.09 0.02 0.01 0.01 0.03 19.94 18.96 18.05 0.01 0.01 0.02 0.59 0.99 0.52 1.24 0.91 0.98 1.89 576±84,5
GC0111 pff gc-032 13 25 03.24 -42 57 40.5 5.65 20.92 20.59 19.73 19.18 18.61 0.14 0.04 0.01 0.01 0.03 20.81 20.05 19.22 0.01 0.02 0.01 0.33 0.86 0.55 1.12 0.83 0.76 1.59 648±295,7
GC0112 pff gc-033 13 25 03.34 -43 15 27.4 14.98 21.10 20.49 19.46 18.89 18.21 0.33 0.03 0.01 0.01 0.03 20.83 19.79 18.90 0.02 0.02 0.01 0.61 1.02 0.57 1.25 0.89 1.04 1.93 531±185
GC0113 HHH86-32/C32 13 25 03.37 -42 50 46.2 11.28 20.22 19.50 18.44 17.81 17.15 0.05 0.01 0.01 0.01 0.03 19.86 18.71 17.85 0.03 0.03 0.01 0.72 1.06 0.63 1.29 0.85 1.15 2.01 718±113,5,6,7
GC0114 pff gc-034 13 25 03.37 -43 11 39.6 11.41 20.98 20.70 19.91 19.35 18.84 0.09 0.03 0.01 0.01 0.03 20.89 20.19 19.38 0.03 0.02 0.01 0.28 0.80 0.56 1.06 0.81 0.69 1.50 605±465
GC0115 C131 13 25 03.67 -42 51 21.7 10.72 - - - - - - - - - - 21.57 20.98 20.20 0.02 0.02 0.01 - - - - 0.78 0.59 1.36 -
GC0116 AAT112752 13 25 04.12 -43 00 19.6 4.37 20.51 20.16 19.34 18.88 18.44 0.15 0.04 0.02 0.01 0.03 20.35 19.58 18.87 0.02 0.02 0.03 0.35 0.82 0.46 0.90 0.72 0.76 1.48 679±827
GC0117 pff gc-035 13 25 04.48 -43 10 48.4 10.54 21.32 20.73 19.71 19.07 18.44 0.14 0.03 0.01 0.01 0.03 21.13 20.07 19.13 0.03 0.02 0.01 0.59 1.02 0.64 1.27 0.94 1.06 2.00 627±225,7
GC0118 AAT112964 13 25 04.61 -43 07 21.7 7.50 20.45 20.39 19.61 19.13 18.68 0.08 0.03 0.01 0.01 0.03 20.47 19.90 19.11 0.01 0.01 0.01 0.06 0.78 0.49 0.94 0.78 0.57 1.35 456±1187
GC0119 HGHH-43/C43 13 25 04.81 -43 09 38.8 9.47 19.74 19.45 18.60 18.07 17.53 0.04 0.01 0.01 0.01 0.03 19.59 18.85 18.07 0.03 0.02 0.01 0.29 0.85 0.53 1.07 0.78 0.74 1.52 518±254,5,7
GC0120 WHH-7 13 25 05.02 -42 57 15.0 5.68 18.96 18.39 17.41 16.81 16.19 0.04 0.01 0.01 0.01 0.03 18.69 17.60 16.83 0.02 0.03 0.01 0.57 0.98 0.60 1.22 0.77 1.09 1.86 722±206
GC0121 HGHH-G035 13 25 05.29 -42 58 05.8 5.09 21.02 20.59 19.62 19.01 18.41 0.17 0.04 0.01 0.01 0.03 20.87 19.95 19.08 0.01 0.02 0.01 0.43 0.97 0.61 1.21 0.87 0.92 1.80 776±264,5
GC0122 pff gc-036 13 25 05.46 -43 14 02.6 13.52 20.09 19.83 19.04 18.52 17.91 0.05 0.02 0.01 0.01 0.03 19.96 19.27 18.49 0.02 0.02 0.01 0.26 0.79 0.52 1.13 0.78 0.69 1.47 666±305,7
GC0123 HGHH-12/C12/R281 13 25 05.72 -43 10 30.7 10.18 - - - - - - - - - - 19.34 18.23 17.36 0.04 0.03 0.02 - - - - 0.87 1.11 1.98 440±12,5,8
GC0124 HGHH-G342 13 25 05.83 -42 59 00.6 4.52 19.65 19.14 18.18 17.57 16.96 0.08 0.02 0.01 0.01 0.03 - - - - - - 0.51 0.96 0.61 1.22 - - - 553±214,5,6,7
GC0125 HHH86-13/C13 13 25 06.25 -43 15 11.6 14.58 20.02 19.60 18.68 18.13 17.51 0.04 0.01 0.01 0.01 0.03 19.82 18.90 18.12 0.03 0.03 0.02 0.41 0.93 0.55 1.16 0.78 0.92 1.70 601±125,6,7
GC0126 R276 13 25 07.33 -43 08 29.6 8.23 21.93 21.62 20.78 20.26 19.73 0.26 0.07 0.02 0.02 0.04 21.88 21.16 20.32 0.03 0.03 0.02 0.31 0.83 0.52 1.05 0.84 0.71 1.55 550±285
GC0127 AAT113428 13 25 07.33 -43 06 20.6 6.38 21.25 20.92 20.04 19.49 18.93 0.16 0.04 0.01 0.01 0.03 21.14 20.36 19.51 0.02 0.01 0.01 0.33 0.88 0.54 1.11 0.85 0.78 1.63 657±677
GC0128 pff gc-037 13 25 07.48 -43 12 29.4 11.93 21.60 21.29 20.42 19.91 19.33 0.55 0.05 0.02 0.01 0.03 21.46 20.73 19.90 0.02 0.01 0.01 0.31 0.87 0.50 1.08 0.83 0.73 1.56 554±235
GC0129 WHH-8 13 25 07.62 -43 01 15.2 3.66 19.83 19.16 18.12 17.46 16.82 0.13 0.03 0.01 0.01 0.03 19.48 18.32 17.45 0.03 0.03 0.04 0.67 1.04 0.66 1.30 0.87 1.16 2.03 690±326
GC0130 WHH-9 13 25 08.51 -43 02 57.4 3.93 20.59 19.95 18.91 18.37 17.64 0.17 0.03 0.01 0.01 0.03 20.28 19.17 18.30 0.05 0.04 0.05 0.64 1.04 0.54 1.27 0.87 1.11 1.98 315±1006
GC0131 C132 13 25 08.79 -43 09 09.6 8.72 - - - - - - - - - - 20.38 19.69 18.90 0.02 0.02 0.01 - - - - 0.79 0.69 1.48 -
GC0132 R271 13 25 08.81 -43 09 09.5 8.72 20.49 20.23 19.42 18.91 18.39 0.08 0.02 0.01 0.01 0.03 20.38 19.69 18.90 0.02 0.02 0.01 0.26 0.80 0.52 1.03 0.79 0.69 1.48 436±455
GC0133 pff gc-038 13 25 08.82 -43 04 14.9 4.63 20.83 20.29 19.29 18.69 18.03 0.17 0.04 0.01 0.01 0.03 20.58 19.57 18.71 0.03 0.03 0.03 0.54 1.00 0.61 1.26 0.87 1.01 1.88 431±195
GC0134 pff gc-039 13 25 09.10 -42 24 00.9 37.29 20.01 19.77 18.95 18.44 17.91 0.17 0.02 0.01 0.01 0.03 19.92 19.22 18.50 0.01 0.01 0.01 0.23 0.82 0.51 1.04 0.72 0.70 1.42 387±275,7
GC0135 K-029 13 25 09.19 -42 58 59.2 4.00 19.13 18.65 17.71 17.13 16.55 0.08 0.02 0.01 0.01 0.03 - - - - - - 0.48 0.94 0.58 1.16 - - - 677±447
GC0136 pff gc-040 13 25 09.54 -42 55 18.5 6.71 20.09 19.89 19.12 18.60 18.11 0.06 0.02 0.01 0.01 0.03 20.00 19.37 18.66 0.02 0.02 0.01 0.20 0.76 0.52 1.01 0.71 0.62 1.34 504±355
GC0137 HGHH-G329 13 25 10.20 -43 02 06.7 3.33 21.73 20.89 19.71 19.07 18.38 0.69 0.11 0.03 0.02 0.03 21.34 20.04 19.07 0.02 0.01 0.03 0.84 1.18 0.64 1.33 0.97 1.29 2.26 502±164,5,7
GC0138 K-033 13 25 10.25 -42 55 09.5 6.78 21.07 20.47 19.46 18.90 18.21 0.13 0.03 0.01 0.01 0.03 20.78 19.77 18.86 0.01 0.01 0.01 0.60 1.01 0.57 1.25 0.91 1.02 1.93 582±337
GC0139 K-034 13 25 10.27 -42 53 33.1 8.23 19.33 18.79 17.80 17.26 16.55 0.04 0.01 0.01 0.01 0.03 19.14 18.03 17.25 0.03 0.03 0.02 0.55 0.99 0.54 1.25 0.79 1.11 1.89 464±427
GC0140 HHH86-14/C14 13 25 10.49 -42 44 52.6 16.57 19.23 18.84 17.94 17.40 16.79 0.03 0.01 0.01 0.01 0.03 19.06 18.16 17.41 0.01 0.02 0.01 0.39 0.90 0.54 1.15 0.75 0.90 1.65 705±102,5,6,7
GC0141 AAT113992 13 25 10.51 -43 03 24.0 3.85 21.95 21.39 20.40 19.79 19.19 0.58 0.11 0.03 0.03 0.04 21.77 20.78 19.82 0.03 0.03 0.01 0.57 0.99 0.61 1.20 0.97 0.99 1.95 648±587
GC0142 C13313 13 25 11.05 -43 01 32.3 3.05 - - - - - - - - - - - - 19.30 - - - - - - - - - - -
GC0143 HGHH-G348 13 25 11.10 -42 58 03.0 4.32 19.90 19.66 18.92 18.46 18.03 0.10 0.03 0.01 0.01 0.03 19.80 19.15 18.45 0.01 0.01 - 0.24 0.74 0.46 0.89 0.70 0.65 1.35 416±304,5,7
GC0144 pff gc-041 13 25 11.17 -43 03 09.6 3.62 20.57 20.32 19.51 18.99 18.48 0.19 0.05 0.02 0.02 0.03 20.48 19.77 19.01 0.02 0.02 0.02 0.24 0.81 0.52 1.03 0.76 0.71 1.47 456±295,7
GC0145 HGHH-G327 13 25 11.98 -43 04 19.3 4.27 21.46 20.83 19.78 19.16 18.56 0.34 0.06 0.02 0.02 0.03 21.16 20.11 19.19 0.01 0.01 0.01 0.63 1.05 0.61 1.22 0.92 1.05 1.97 608±194,5,7
GC0146 HGHH-G081 13 25 12.11 -42 57 25.2 4.68 19.90 19.52 18.62 18.05 17.49 0.08 0.02 0.01 0.01 0.03 19.72 18.88 18.10 0.03 0.03 0.01 0.38 0.90 0.57 1.13 0.77 0.85 1.62 536±434,5
GC0147 pff gc-042 13 25 12.21 -43 16 33.9 15.67 19.91 19.74 18.97 18.47 17.91 0.12 0.02 0.01 0.01 0.03 19.82 19.19 18.47 0.02 0.02 0.01 0.17 0.78 0.50 1.05 0.72 0.63 1.35 627±235,6,7
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0148 AAT114302 13 25 12.34 -42 58 07.7 4.11 21.87 21.39 20.44 19.90 19.35 0.53 0.11 0.03 0.03 0.04 21.64 20.76 19.97 0.02 0.01 0.01 0.47 0.95 0.55 1.09 0.79 0.88 1.67 754±1437
GC0149 pff gc-043 13 25 12.45 -43 14 07.4 13.27 20.51 20.22 19.40 18.89 18.33 0.20 0.02 0.01 0.01 0.03 20.38 19.67 18.90 0.03 0.02 0.01 0.29 0.82 0.52 1.07 0.77 0.70 1.48 527±335,7
GC0150 WHH-10 13 25 12.84 -42 56 59.8 4.95 20.62 20.36 19.57 19.07 18.48 0.12 0.03 0.01 0.01 0.03 20.43 19.90 19.10 0.03 0.02 0.01 0.26 0.79 0.50 1.09 0.80 0.54 1.33 664±1416
GC0151 R261 13 25 12.90 -43 07 59.1 7.35 19.65 19.15 18.20 17.60 17.03 0.05 0.01 0.01 0.01 0.03 19.42 18.49 17.62 0.02 0.01 0.01 0.51 0.94 0.60 1.17 0.88 0.93 1.81 615±45,7,8
GC0152 pff gc-044 13 25 13.19 -43 16 35.6 15.67 20.29 20.11 19.37 18.87 18.33 0.16 0.02 0.01 0.01 0.03 20.19 19.59 18.87 0.02 0.02 0.01 0.17 0.74 0.50 1.04 0.72 0.60 1.32 568±535
GC0153 C134 13 25 13.20 -43 02 31.3 2.97 - - - - - - - - - - 22.45 21.64 20.71 0.07 0.05 0.07 - - - - 0.93 0.80 1.74 -
GC0154 pff gc-045 13 25 13.31 -42 52 12.4 9.31 21.57 20.86 19.82 19.21 18.53 0.19 0.04 0.01 0.01 0.03 21.38 20.32 19.40 0.07 0.06 0.04 0.71 1.04 0.62 1.29 0.93 1.06 1.99 474±235
GC0155 R259 13 25 13.88 -43 07 32.5 6.87 22.13 21.70 20.70 20.11 19.48 0.37 0.08 0.02 0.02 0.03 21.96 21.07 20.10 0.02 0.01 0.01 0.43 1.00 0.60 1.23 0.96 0.89 1.85 628±485
GC0156 HGHH-G271 13 25 13.95 -42 57 42.6 4.25 19.45 19.36 18.72 18.32 17.90 0.07 0.02 0.01 0.01 0.03 19.40 18.92 18.30 0.01 0.01 - 0.09 0.63 0.40 0.82 0.62 0.47 1.09 353±274,5,6,7
GC0157 C13513 13 25 14.07 -43 00 51.8 2.49 - - - - - - - - - - - - 19.90 - - - - - - - - - - -
GC0158 C136 13 25 14.07 -43 03 35.0 3.47 - - - - - - - - - - 22.48 21.50 21.19 0.04 0.02 0.02 - - - - 0.30 0.99 1.29 -
GC0159 WHH-11/K-051 13 25 14.24 -43 07 23.5 6.71 21.26 20.63 19.55 18.90 18.21 0.18 0.04 0.01 0.01 0.03 21.02 19.95 18.95 0.03 0.02 0.01 0.64 1.07 0.65 1.34 1.00 1.06 2.07 582±306,7
GC0160 pff gc-046 13 25 14.83 -43 41 10.6 40.10 19.91 19.72 18.93 18.43 17.95 0.11 0.02 0.01 0.01 0.03 19.87 19.14 18.37 0.01 - 0.01 0.20 0.79 0.50 0.98 0.77 0.73 1.50 532±215,7
GC0161 pff gc-047 13 25 15.12 -42 50 30.4 10.88 20.92 20.72 19.87 19.37 18.87 0.09 0.03 0.01 0.01 0.03 20.87 20.22 19.41 0.02 0.02 0.01 0.20 0.85 0.50 0.99 0.81 0.65 1.46 717±555
GC0162 AAT114769 13 25 15.12 -42 57 45.7 4.08 21.20 21.00 20.25 19.76 19.25 0.30 0.09 0.03 0.03 0.04 21.11 20.52 19.80 0.02 0.02 0.01 0.20 0.75 0.49 1.00 0.71 0.59 1.30 650±1697
GC0163 R257 13 25 15.24 -43 08 39.2 7.84 22.29 21.77 20.78 20.18 19.58 0.35 0.07 0.02 0.02 0.03 22.02 21.09 20.16 0.02 0.02 0.02 0.51 1.00 0.60 1.20 0.92 0.93 1.85 339±515
GC0164 pff gc-048 13 25 15.79 -42 49 15.1 12.09 20.92 20.67 19.85 19.30 18.78 0.09 0.03 0.01 0.01 0.03 20.85 20.13 19.41 0.02 0.02 0.02 0.25 0.82 0.55 1.07 0.71 0.72 1.44 535±535,7
GC0165 AAT114913 13 25 15.93 -43 06 03.3 5.35 21.69 21.33 20.39 19.88 19.29 0.34 0.08 0.02 0.02 0.04 21.60 20.72 19.86 0.02 0.02 0.02 0.36 0.94 0.52 1.10 0.86 0.88 1.74 563±637
GC0166 pff gc-049 13 25 16.06 -43 05 06.5 4.49 20.74 20.45 19.59 19.05 18.50 0.15 0.04 0.01 0.01 0.03 20.64 19.85 19.07 0.03 0.03 0.03 0.29 0.86 0.54 1.09 0.78 0.79 1.57 674±325
GC0167 C13713 13 25 16.06 -43 02 19.3 2.42 - - - - - - - - - - - - 19.04 - - - - - - - - - - -
GC0168 VHH81-05/C5 13 25 16.12 -42 52 58.2 8.44 18.70 18.49 17.68 17.13 16.68 0.03 0.01 0.01 0.01 0.03 - - - - - - 0.21 0.81 0.55 1.00 - - - 555±31,2,3,5,7,8
GC0169 HCH01 13 25 16.22 -42 59 43.4 2.52 18.69 18.36 17.47 16.94 16.40 0.52 0.15 0.04 0.03 0.04 - - - - - - 0.33 0.89 0.53 1.07 - - - 649±455,7
GC0170 HHH86-33/C33 13 25 16.26 -42 50 53.3 10.47 19.58 19.34 18.50 18.02 17.50 0.04 0.01 0.01 0.01 0.03 - - - - - - 0.24 0.84 0.48 1.00 - - - 596±183,5,6,7
GC0171 AAT1149939 13 25 16.44 -43 03 33.1 3.16 22.49 21.50 20.44 19.82 19.32 1.41 0.19 .382 0.308 0.224 21.95 20.81 19.83 0.02 0.02 0.03 0.99 1.06 0.62 1.12 0.98 1.14 2.12 352±1367
GC0172 HCH02 13 25 16.69 -43 02 08.7 2.23 19.27 18.87 17.93 17.37 16.76 0.98 0.26 0.07 0.05 0.05 - - - - - - 0.40 0.94 0.56 1.17 - - - 300±25,7,8
GC0173 pff gc-050 13 25 16.73 -42 50 18.4 11.02 21.63 21.28 20.39 19.86 19.27 0.16 0.04 0.01 0.01 0.03 - - - - - - 0.35 0.89 0.54 1.12 - - - 688±705
GC0174 C138 13 25 16.91 -43 03 08.0 2.79 - - - - - - - - - - 21.53 20.79 19.97 0.02 0.02 0.03 - - - - 0.81 0.74 1.55 -
GC0175 R254 13 25 16.96 -43 09 28.0 8.54 20.52 20.26 19.43 18.91 18.33 0.09 0.03 0.01 0.01 0.03 20.42 19.65 18.91 0.04 0.03 0.03 0.27 0.82 0.52 1.10 0.73 0.77 1.51 561±275,7
GC0176 C139 13 25 17.06 -43 02 44.6 2.50 - - - - - - - - - - 20.73 19.62 18.86 0.03 0.02 0.04 - - - - 0.76 1.11 1.87 -
GC0177 HGHH-G219 13 25 17.31 -42 58 46.6 3.03 20.69 19.92 18.84 18.20 17.55 0.43 0.08 0.02 0.02 0.03 - - - - - - 0.77 1.09 0.63 1.29 - - - 535±244,5,7
GC0178 R253 13 25 17.33 -43 08 39.0 7.74 20.75 20.49 19.67 19.14 18.64 0.09 0.03 0.01 0.01 0.03 20.68 20.00 19.47 0.03 0.03 0.05 0.26 0.81 0.53 1.04 0.53 0.69 1.22 486±525,7
GC0179 C140 13 25 17.42 -43 03 25.2 2.94 - - - - - - - - - - 21.40 20.65 19.83 0.03 0.02 0.03 - - - - 0.82 0.75 1.57 -
GC0180 C141 13 25 18.14 -43 02 50.9 2.43 - - - - - - - - - - 22.23 21.55 20.95 0.06 0.05 0.06 - - - - 0.60 0.68 1.29 -
GC0181 WHH-12 13 25 18.27 -42 53 04.8 8.25 20.36 20.00 19.07 18.47 17.97 0.07 0.02 0.01 0.01 0.03 20.23 19.35 18.71 0.04 0.04 0.01 0.36 0.93 0.60 1.10 0.64 0.89 1.52 558±996
GC0182 AAT115339 13 25 18.44 -43 04 09.8 3.45 21.19 20.91 20.11 19.53 19.01 0.39 0.10 0.03 0.03 0.04 21.11 20.38 19.56 0.02 0.01 0.02 0.27 0.81 0.58 1.09 0.81 0.73 1.55 618±1087
GC0183 C142 13 25 18.50 -43 01 16.4 1.67 - - - - - - - - - - - - 17.64 - - - - - - - - - - -
GC0184 AAT320656 13 25 19.13 -43 12 03.8 11.03 20.61 20.50 19.81 19.35 18.89 0.08 0.03 0.01 0.01 0.03 20.57 20.01 19.35 0.02 0.01 0.02 0.10 0.70 0.46 0.92 0.66 0.56 1.22 453±2337
GC0185 HGHH-G331 13 25 19.50 -43 02 28.4 1.99 20.00 19.60 18.92 18.47 17.93 0.55 0.14 0.05 0.04 0.05 - - - - - - 0.40 0.68 0.44 0.99 - - - 371±224,5,7
GC0186 AAT115561 13 25 19.83 -42 58 27.2 3.05 22.13 21.47 20.50 19.92 19.29 1.44 0.26 0.07 0.06 0.06 - 20.98 20.15 1.00 0.04 0.02 0.66 0.98 0.57 1.20 0.83 - - 514±467
GC0187 R247 13 25 19.99 -43 07 44.1 6.73 21.86 21.20 20.11 19.40 18.62 0.28 0.05 0.02 0.01 0.03 21.73 20.65 19.75 0.05 0.04 0.04 0.66 1.10 0.70 1.49 0.90 1.08 1.98 662±485
GC0188 AAT115605 13 25 20.44 -42 54 08.5 7.13 21.44 21.22 20.47 20.00 19.50 0.18 0.05 0.02 0.02 0.03 21.36 20.76 20.11 0.01 0.03 0.01 0.22 0.75 0.47 0.97 0.66 0.60 1.25 713±1317
GC0189 AAT115679 13 25 20.72 -43 06 35.9 5.60 21.93 21.49 20.44 19.80 19.15 0.40 0.09 0.02 0.02 0.03 21.71 20.79 19.84 0.02 0.02 0.03 0.44 1.05 0.64 1.30 0.95 0.92 1.87 511±1657
GC0190 WHH-13/HH-090 13 25 21.29 -42 49 17.7 11.91 20.75 20.22 19.20 18.61 17.95 0.08 0.02 0.01 0.01 0.03 20.59 19.52 18.74 0.03 0.03 0.02 0.53 1.02 0.59 1.25 0.78 1.08 1.85 444±336,7
GC0191 AAT321194 13 25 21.32 -43 23 59.3 22.87 21.46 21.03 20.06 19.48 18.82 0.38 0.03 0.01 0.01 0.03 21.33 20.42 19.53 0.03 0.02 0.01 0.43 0.97 0.58 1.24 0.90 0.90 1.80 254±1697
GC0192 HGHH-06/C6 13 25 22.19 -43 02 45.6 1.89 18.65 18.17 17.21 16.61 16.03 0.24 0.06 0.02 0.01 0.03 - - - - - - 0.48 0.96 0.60 1.18 - - - 855±22,4,5,6,7,8
GC0193 pff gc-051 13 25 22.35 -43 15 00.1 13.89 21.15 20.73 19.79 19.20 18.61 0.10 0.02 0.01 0.01 0.03 21.00 20.10 19.22 0.03 0.03 0.02 0.42 0.94 0.59 1.18 0.88 0.90 1.78 468±395,7
GC0194 C143 13 25 23.20 -43 03 12.9 2.22 - - - - - - - - - - 21.87 21.35 20.52 0.05 0.04 0.06 - - - - 0.82 0.52 1.34 -
GC0195 AAT116025 13 25 23.46 -42 53 26.2 7.75 21.23 20.88 20.00 19.48 18.85 0.14 0.04 0.01 0.01 0.03 21.16 20.32 19.62 0.04 0.05 0.01 0.35 0.88 0.51 1.15 0.70 0.84 1.54 545±647
GC0196 AAT116220 13 25 24.40 -43 07 58.9 6.86 20.76 20.39 19.47 18.91 18.36 0.11 0.03 0.01 0.01 0.03 20.62 19.72 18.92 0.03 0.03 0.03 0.37 0.92 0.56 1.11 0.80 0.90 1.70 524±417
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0197 AAT116385 13 25 25.39 -42 58 21.5 2.82 21.71 21.23 20.26 19.59 18.99 1.22 0.26 0.07 0.05 0.06 21.58 20.68 19.94 0.02 0.02 0.01 0.48 0.97 0.66 1.27 0.74 0.90 1.64 550±407
GC0198 WHH-14 13 25 25.49 -42 56 31.2 4.64 20.99 20.83 20.06 19.56 19.05 0.18 0.05 0.02 0.02 0.03 20.98 20.36 19.68 0.02 0.03 0.01 0.15 0.77 0.50 1.01 0.68 0.62 1.30 461±756,7
GC0199 AAT204119 13 25 25.70 -42 37 40.9 23.47 20.59 20.49 19.81 19.35 18.93 0.18 0.02 0.01 0.01 0.03 20.60 20.04 19.42 0.01 - - 0.10 0.67 0.47 0.88 0.62 0.56 1.18 404±747
GC0200 pff gc-052 13 25 25.75 -43 05 16.5 4.14 20.88 20.70 19.88 19.39 18.86 0.19 0.06 0.02 0.02 0.03 20.86 20.17 19.42 0.03 0.03 0.03 0.18 0.82 0.48 1.01 0.75 0.69 1.44 462±525
GC0201 HGHH-46/C46 13 25 25.97 -43 03 25.7 2.30 19.74 19.71 19.10 18.74 18.30 0.37 0.12 0.04 0.04 0.05 19.77 19.30 18.64 0.01 0.02 0.22 0.03 0.61 0.36 0.80 0.66 0.47 1.13 508±194,5,7
GC0202 C144 13 25 26.28 -43 04 38.5 3.50 - - - - - - - - - - 23.22 22.36 21.96 0.06 0.05 0.05 - - - - 0.41 0.85 1.26 -
GC0203 AAT116531 13 25 26.75 -43 08 53.4 7.74 20.92 20.65 19.83 19.34 18.83 0.10 0.03 0.01 0.01 0.03 20.77 19.95 19.94 0.07 0.06 0.02 0.27 0.82 0.49 1.00 0.01 0.82 0.83 267±717
GC0204 WHH-15 13 25 26.78 -42 52 39.9 8.48 20.73 20.56 19.81 19.36 18.87 0.09 0.03 0.01 0.01 0.03 20.68 20.80 19.53 0.03 0.02 0.01 0.16 0.75 0.46 0.94 1.27 -0.12 1.15 513±536,7
GC0205 R235 13 25 26.82 -43 09 40.5 8.53 20.55 20.30 19.53 19.02 18.51 0.08 0.02 0.01 0.01 0.03 20.42 19.73 19.01 0.04 0.03 0.04 0.25 0.77 0.51 1.03 0.72 0.69 1.41 498±285,7
GC0206 WHH-16/K-102 13 25 27.97 -43 04 02.2 2.89 20.90 20.23 19.18 18.56 17.90 0.56 0.11 0.03 0.02 0.04 20.64 19.52 18.60 0.04 0.03 0.03 0.66 1.06 0.61 1.28 0.93 1.11 2.04 661±476,7
GC0207 HCH13 13 25 28.69 -43 02 55.0 1.78 21.32 20.82 19.89 19.30 18.63 2.53 0.55 0.15 0.12 0.12 - - - - - - 0.50 0.93 0.59 1.26 - - - 641±245,7
GC0208 C145 13 25 28.81 -43 04 21.6 3.22 - - - - - - - - - - 19.32 18.54 17.81 0.01 0.01 0.02 - - - - 0.73 0.78 1.51 -
GC0209 WHH-17 13 25 29.25 -42 57 47.1 3.38 19.68 19.39 18.57 18.06 17.48 0.15 0.04 0.02 0.01 0.03 19.54 18.77 18.13 0.02 0.03 - 0.29 0.82 0.51 1.09 0.65 0.76 1.41 619±456,7
GC0210 AAT116969 13 25 29.41 -42 53 25.6 7.73 21.55 21.28 20.46 20.10 19.48 0.21 0.06 0.02 0.02 0.03 21.45 20.77 20.10 0.03 0.02 0.01 0.27 0.82 0.35 0.98 0.68 0.68 1.36 446±617
GC0211 HGHH-G169 13 25 29.43 -42 58 09.9 3.00 21.39 20.58 19.49 18.92 18.12 0.81 0.13 0.03 0.03 0.04 21.00 19.80 18.94 0.01 0.02 0.01 0.81 1.10 0.57 1.37 0.86 1.21 2.07 643±244,5,7
GC0212 pff gc-053 13 25 29.62 -42 54 44.5 6.42 20.91 20.29 19.26 18.73 17.98 0.14 0.03 0.01 0.01 0.03 20.65 19.54 18.78 0.03 0.04 0.01 0.62 1.03 0.53 1.29 0.76 1.11 1.86 439±205
GC0213 R229 13 25 29.74 -43 11 42.8 10.57 20.70 20.49 19.72 19.20 18.69 0.08 0.02 0.01 0.01 0.03 20.62 19.94 19.22 0.04 0.03 0.04 0.21 0.77 0.52 1.03 0.73 0.68 1.41 517±665
GC0214 HCH15 13 25 29.80 -43 00 07.0 1.10 19.27 18.87 17.93 17.37 16.76 0.98 0.26 0.07 0.05 0.05 - - - - - - 0.04 0.94 0.56 1.17 - - - 519±18
GC0215 C146 13 25 29.87 -43 05 09.2 4.03 - - - - - - - - - - 21.71 20.78 19.94 0.03 0.02 0.02 - - - - 0.84 0.93 1.77 -
GC0216 WHH-18 13 25 30.07 -42 56 46.9 4.39 19.85 19.36 18.36 17.85 17.16 0.09 0.02 0.01 0.01 0.03 19.63 18.60 17.88 0.01 0.03 - 0.50 0.99 0.51 1.20 0.72 1.03 1.75 752±256,7
GC0217 pff gc-054 13 25 30.28 -43 41 53.6 40.75 20.65 20.60 19.99 19.57 19.09 0.19 0.03 0.01 0.01 0.03 - - - - - - 0.05 0.62 0.41 0.89 - - - 297±405,7
GC0218 HCH16 13 25 30.29 -42 59 34.8 1.64 - - - - - - - - - - - - - - - - - - - - - - - 458±25,7,8
GC0219 HHH86-15/C15/R226 13 25 30.41 -43 11 49.6 10.69 20.11 19.56 18.56 17.94 17.35 0.06 0.02 0.01 0.01 0.03 19.80 18.68 17.92 0.05 0.05 0.05 0.55 1.00 0.62 1.21 0.76 1.12 1.88 644±15,6,7,8
GC0220 C147 13 25 30.65 -43 03 47.1 2.70 - - - - - - - - - - 21.58 20.88 20.05 0.05 0.05 0.03 - - - - 0.83 0.69 1.52 -
GC0221 pff gc-055 13 25 30.72 -42 48 13.4 12.94 20.87 20.68 19.92 19.44 18.97 0.08 0.03 0.01 0.01 0.03 20.83 20.20 19.54 0.02 0.02 0.02 0.19 0.76 0.48 0.96 0.66 0.62 1.28 485±475,7
GC0222 AAT205071 13 25 30.74 -42 30 16.0 30.89 19.65 19.61 18.86 18.37 17.96 0.09 0.01 0.01 0.01 0.03 19.68 19.10 18.50 0.02 0.02 - 0.04 0.74 0.49 0.90 0.60 0.58 1.18 288±617
GC0223 WHH-19 13 25 31.03 -42 50 14.9 10.92 18.47 18.16 17.29 16.78 16.24 0.02 0.01 0.01 0.01 0.03 18.08 17.67 16.91 0.06 0.06 0.02 0.31 0.87 0.51 1.05 0.76 0.42 1.18 451±406,7
GC0224 AAT117287 13 25 31.08 -43 04 17.0 3.20 22.20 21.44 20.36 19.82 19.13 1.22 0.20 0.05 0.04 0.05 21.82 20.56 20.45 0.04 0.03 0.03 0.76 1.08 0.54 1.23 0.11 1.27 1.37 554±607
GC0225 HGHH-G292 13 25 31.48 -42 58 08.3 3.09 21.77 21.05 19.97 19.33 18.64 1.04 0.18 0.05 0.03 0.04 21.48 20.85 19.53 0.01 0.02 0.01 0.72 1.08 0.64 1.34 1.33 0.63 1.95 655±434,5
GC0226 HCH18 13 25 31.60 -43 00 02.8 1.32 21.06 20.99 19.93 19.20 18.43 2.42 0.76 0.19 0.13 0.12 - - - - - - 0.07 1.06 0.73 1.50 - - - 455±15,7,8
GC0227 AAT117322 13 25 31.73 -42 55 15.7 5.93 21.14 20.91 20.08 19.55 19.07 0.19 0.05 0.02 0.02 0.03 21.07 20.38 19.75 0.04 0.05 0.01 0.22 0.84 0.52 1.01 0.63 0.69 1.32 636±1337
GC0228 HGHH-44/C44 13 25 31.73 -43 19 22.6 18.25 19.76 19.50 18.69 18.14 17.66 0.04 0.01 0.01 0.01 0.03 19.59 18.85 18.15 0.03 0.02 0.01 0.26 0.80 0.55 1.03 0.70 0.74 1.44 505±14,5,6,7,8
GC0229 C148 13 25 31.75 -43 05 46.0 4.68 - - - - - - - - - - 21.25 20.79 20.21 0.07 0.06 0.05 - - - - 0.58 0.46 1.04 -
GC0230 R224/C149 13 25 32.33 -43 07 17.1 6.20 21.07 20.90 20.15 19.64 19.19 0.15 0.04 0.02 0.02 0.03 21.02 20.42 19.68 0.03 0.02 0.02 0.16 0.76 0.50 0.96 0.74 0.60 1.34 389±455
GC0231 HGHH-G359 13 25 32.42 -42 58 50.2 2.47 20.44 19.86 18.86 18.24 17.64 0.45 0.10 0.03 0.02 0.04 20.13 19.09 18.33 0.01 0.01 - 0.58 1.00 0.62 1.22 0.76 1.04 1.80 489±344,5,7
GC0232 pff gc-056 13 25 32.80 -42 56 24.4 4.83 19.62 19.43 18.64 18.15 17.64 0.06 0.02 0.01 0.01 0.03 19.51 18.82 18.22 0.03 0.04 - 0.19 0.79 0.48 1.00 0.60 0.69 1.29 306±275,6
GC0233 R223 13 25 32.80 -43 07 02.2 5.97 20.08 19.67 18.77 18.23 17.64 0.07 0.02 0.01 0.01 0.03 19.89 18.98 18.19 0.03 0.03 0.03 0.41 0.91 0.54 1.13 0.79 0.92 1.71 776±15,7,8
GC0234 K-131 13 25 32.88 -43 04 29.2 3.48 21.23 20.44 19.37 18.77 18.12 0.38 0.07 0.02 0.02 0.03 20.84 19.65 18.74 0.03 0.02 0.03 0.79 1.08 0.59 1.24 0.91 1.20 2.10 639±447
GC0235 pff gc-057 13 25 33.17 -42 59 03.2 2.33 22.21 21.38 20.35 19.75 18.95 2.11 0.37 0.09 0.07 0.07 21.67 20.75 19.86 0.03 0.02 0.01 0.82 1.04 0.60 1.40 0.90 0.91 1.81 515±125
GC0236 C15013 13 25 33.82 -43 02 49.6 2.03 - - - - - - - - - - - - 19.78 - - - - - - - - - - -
GC0237 C151 13 25 33.93 -43 03 51.4 2.94 - - - - - - - - - - 22.27 20.90 19.95 0.03 0.01 0.03 - - - - 0.95 1.37 2.32 -
GC0238 MAGJM-11 13 25 33.94 -42 59 39.4 1.89 19.80 19.64 18.87 18.44 17.83 0.80 0.25 0.07 0.06 0.07 - - - - - - 0.16 0.77 0.43 1.04 - - - 444±175,7
GC0239 HGHH-G206 13 25 34.10 -42 59 00.7 2.44 20.68 20.09 19.10 18.58 17.91 0.56 0.12 0.03 0.03 0.04 20.37 19.36 18.61 0.02 0.03 0.01 0.58 0.99 0.52 1.19 0.75 1.00 1.75 600±244,5
GC0240 HGHH-45/C45 13 25 34.25 -42 56 59.1 4.33 19.99 19.81 19.03 18.60 18.05 0.10 0.03 0.01 0.01 0.03 19.91 19.17 18.67 0.08 0.07 0.02 0.18 0.78 0.43 0.98 0.50 0.75 1.25 612±344,5,7
GC0241 WHH-20 13 25 34.36 -42 51 05.9 10.12 20.30 19.93 19.01 18.52 17.90 0.06 0.02 0.01 0.01 0.03 20.11 19.25 18.59 0.04 0.05 0.01 0.37 0.92 0.49 1.10 0.66 0.86 1.52 259±336,7
GC0242 C15213 13 25 34.64 -43 03 16.4 2.48 - - - - - - - - - - - - 17.82 - - - - - - - - - - -
GC0243 C15313 13 25 34.64 -43 03 27.8 2.65 - - - - - - - - - - - - 18.23 - - - - - - - - - - -
GC0244 HCH21 13 25 34.65 -43 03 27.7 2.65 - - - - - - - - - - - - - - - - - - - - - - - 663±25,7,8
GC0245 C15413 13 25 34.71 -43 03 30.2 2.69 - - - - - - - - - - - - 19.58 - - - - - - - - - - -
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0246 HHH86-16/C16 13 25 35.00 -42 36 05.0 25.10 20.01 19.57 18.59 18.00 17.41 0.12 0.01 0.01 0.01 0.03 19.85 18.83 18.12 0.03 0.03 0.01 0.44 0.98 0.59 1.19 0.70 1.02 1.73 538±162,4,7
GC0247 pff gc-058 13 25 35.12 -42 56 45.3 4.60 19.67 19.47 18.68 18.19 17.70 0.07 0.02 0.01 0.01 0.03 19.55 18.85 18.29 0.03 0.03 0.01 0.20 0.78 0.49 0.99 0.56 0.70 1.26 365±225,6,7
GC0248 K-144 13 25 35.16 -42 53 01.0 8.25 22.10 21.31 20.25 19.63 18.94 0.33 0.05 0.02 0.01 0.03 21.72 20.44 19.75 0.01 0.01 0.01 0.79 1.06 0.62 1.31 0.69 1.28 1.97 593±437
GC0249 WHH-21 13 25 35.22 -43 12 01.5 10.97 19.64 19.60 19.00 18.63 18.25 0.04 0.01 0.01 0.01 0.03 19.61 19.15 18.62 0.02 0.01 0.02 0.04 0.60 0.37 0.75 0.53 0.46 0.99 243±616
GC0250 WHH-22 13 25 35.31 -43 05 29.0 4.56 - - - - - - - - - - 19.66 18.80 18.03 0.04 0.04 0.04 - - - - 0.77 0.86 1.63 492±1266
GC0251 MAGJM-08 13 25 35.50 -42 59 35.2 2.12 20.76 20.18 19.17 18.68 17.94 1.15 0.24 0.06 0.05 0.05 - - - - - - 0.58 1.01 0.49 1.22 - - - 701±285,7
GC0252 R215 13 25 35.64 -43 08 36.8 7.61 22.06 21.68 20.80 20.27 19.70 0.27 0.06 0.02 0.02 0.03 21.98 21.18 20.35 0.03 0.03 0.04 0.38 0.87 0.53 1.11 0.83 0.79 1.63 543±575,7
GC0253 R213 13 25 35.93 -43 07 27.9 6.50 22.70 22.03 20.92 20.35 19.62 0.56 0.10 0.03 0.02 0.03 22.34 21.26 20.34 0.03 0.01 0.02 0.67 1.11 0.58 1.30 0.92 1.08 2.00 532±525,7
GC0254 AAT117899 13 25 36.05 -42 53 40.3 7.63 21.70 21.17 20.17 19.62 18.97 0.23 0.05 0.02 0.01 0.03 21.51 20.51 19.70 0.03 0.03 0.01 0.53 1.01 0.54 1.20 0.81 1.01 1.81 609±1167
GC0255 C155 13 25 36.47 -43 08 03.5 7.10 - - - - - - - - - - 22.98 22.21 21.36 0.06 0.05 0.05 - - - - 0.85 0.77 1.63 -
GC0256 MAGJM-06 13 25 36.69 -42 59 59.2 2.02 - - - - - - - - - - - - - - - - - - - - - - - 443±155,7
GC0257 AAT118198 13 25 37.47 -43 05 44.9 4.94 21.49 20.68 19.64 18.98 18.29 0.31 0.05 0.02 0.01 0.03 21.14 19.94 19.03 0.04 0.02 0.03 0.81 1.04 0.66 1.35 0.91 1.20 2.11 575±367
GC0258 AAT118314 13 25 38.03 -43 16 59.2 15.95 20.69 20.62 19.89 19.45 18.98 0.08 0.03 0.01 0.01 0.03 20.67 20.13 19.42 0.01 0.01 0.01 0.08 0.72 0.44 0.92 0.71 0.53 1.24 257±597
GC0259 R209 13 25 38.13 -43 13 02.2 12.04 21.92 21.51 20.62 20.05 19.43 0.20 0.05 0.02 0.01 0.03 21.91 20.95 20.13 0.04 0.04 0.04 0.41 0.90 0.57 1.19 0.83 0.96 1.79 558±405,7
GC0260 C156 13 25 38.43 -43 05 02.6 4.37 - - - - - - - - - - 19.76 18.55 17.65 0.02 0.02 0.03 - - - - 0.90 1.21 2.11 -
GC0261 C15712 13 25 38.45 -43 03 28.9 3.06 - - - - - - - - - - - - 19.21 - - - - - - - - - - -
GC0262 HGHH-G268 13 25 38.61 -42 59 19.6 2.71 20.23 19.83 18.93 18.36 17.79 0.34 0.08 0.03 0.02 0.04 20.05 19.15 18.44 0.02 0.02 - 0.40 0.91 0.56 1.13 0.71 0.91 1.62 436±434,5
GC0263 C158 13 25 38.76 -43 05 34.5 4.88 - - - - - - - - - - 21.67 20.86 20.06 0.05 0.04 0.05 - - - - 0.80 0.81 1.61 -
GC0264 C159 13 25 39.17 -43 04 33.8 4.02 - - - - - - - - - - 21.91 20.82 19.93 0.02 0.02 0.02 - - - - 0.90 1.09 1.99 -
GC0265 MAGJM-01 13 25 39.33 -43 00 48.8 2.17 19.90 19.52 18.61 18.06 17.50 0.32 0.08 0.02 0.02 0.03 - - - - - - 0.37 0.91 0.55 1.11 - - - 645±365,7
GC0266 pff gc-059 13 25 39.65 -43 04 01.4 3.62 21.53 20.97 19.96 19.35 18.73 0.55 0.11 0.03 0.02 0.04 21.42 20.33 19.48 0.05 0.04 0.04 0.56 1.01 0.61 1.23 0.86 1.09 1.94 525±275,7
GC0267 HGHH-17/C17 13 25 39.73 -42 55 59.2 5.62 18.82 18.51 17.63 17.10 16.57 0.04 0.01 0.01 0.01 0.03 18.61 17.72 17.19 0.04 0.05 0.01 0.32 0.88 0.53 1.06 0.53 0.89 1.42 782±22,5,6,7,8
GC0268 HHH86-18/C18/K-163 13 25 39.88 -43 05 01.9 4.49 18.79 18.42 17.53 16.97 16.43 0.04 0.01 0.01 0.01 0.03 18.49 17.51 16.89 0.05 0.04 0.05 0.38 0.89 0.56 1.10 0.62 0.99 1.60 480±22,5,6,7,8
GC0269 C16012 13 25 40.09 -43 03 07.1 3.01 - - - - - - - - - - - - 19.99 - - - - - - - - - - -
GC0270 C101 13 25 40.47 -42 56 02.7 5.65 - - 20.34 - - - - - - - 21.84 20.90 20.08 0.03 0.04 0.01 - - - - 0.82 0.94 1.76 -
GC0271 R204/C161 13 25 40.52 -43 07 17.9 6.59 21.58 20.84 19.80 19.16 18.41 0.21 0.04 0.01 0.01 0.03 21.21 20.15 19.26 0.04 0.03 0.03 0.74 1.05 0.63 1.39 0.89 1.06 1.95 425±325
GC0272 HGHH-34/C34 13 25 40.61 -43 21 13.6 20.22 19.37 19.01 18.12 17.59 17.03 0.04 0.01 0.01 0.01 0.03 19.64 18.54 17.76 0.04 0.03 0.02 0.35 0.89 0.53 1.10 0.77 1.10 1.87 669±183,5,7
GC0273 C162 13 25 40.87 -43 05 00.4 4.56 - - - - - - - - - - 21.95 21.41 20.91 0.06 0.05 0.01 - - - - 0.51 0.54 1.05 -
GC0274 R203 13 25 40.90 -43 08 16.0 7.52 20.66 20.56 19.84 19.36 18.88 0.09 0.03 0.01 0.01 0.03 20.62 20.08 19.38 0.04 0.03 0.03 0.09 0.73 0.48 0.96 0.70 0.54 1.24 455±355,7
GC0275 AAT118874 13 25 41.36 -42 58 08.9 3.91 21.55 21.02 19.99 19.43 18.81 0.44 0.09 0.03 0.02 0.04 21.49 20.30 19.57 0.05 0.02 - 0.53 1.03 0.56 1.18 0.73 1.19 1.92 570±827
GC0276 C163 13 25 41.63 -43 03 45.8 3.66 - - - - - - - - - - 21.98 21.25 20.43 0.05 0.04 0.04 - - - - 0.81 0.73 1.55 -
GC0277 R202 13 25 42.00 -43 10 42.2 9.91 20.34 20.08 19.26 18.72 18.22 0.06 0.02 0.01 0.01 0.03 20.35 19.74 18.94 0.07 0.03 0.06 0.27 0.81 0.54 1.05 0.80 0.61 1.41 286±455,7
GC0278 C16414 13 25 42.09 -43 03 19.5 3.43 - - - - - - - - - - - - 19.60 - - - - - - - - - - -
GC0279 HGHH-G370 13 25 42.25 -42 59 17.0 3.26 19.61 19.29 18.39 17.86 17.32 0.17 0.05 0.02 0.01 0.03 19.45 18.59 17.93 0.01 0.03 0.01 0.32 0.90 0.54 1.08 0.66 0.86 1.52 507±344,5,7
GC0280 pff gc-060 13 25 42.43 -42 59 02.6 3.43 20.11 19.74 18.81 18.24 17.66 0.20 0.05 0.02 0.01 0.03 19.96 19.02 18.33 0.02 0.03 0.01 0.37 0.93 0.57 1.15 0.69 0.95 1.63 890±195,6
GC0281 AAT119058 13 25 42.53 -43 03 41.5 3.73 21.85 21.42 20.39 19.77 19.18 0.60 0.13 0.04 0.03 0.04 21.69 20.74 19.86 0.04 0.03 0.04 0.43 1.03 0.62 1.21 0.88 0.95 1.83 385±877
GC0282 pff gc-061 13 25 42.62 -42 45 10.9 16.20 21.59 21.15 20.25 19.69 19.12 0.14 0.03 0.01 0.01 0.03 21.42 20.55 19.75 0.01 0.01 0.01 0.44 0.90 0.55 1.13 0.80 0.87 1.67 500±485,7
GC0283 pff gc-062 13 25 43.23 -42 58 37.4 3.81 21.13 20.46 19.42 18.83 18.18 0.34 0.06 0.02 0.02 0.03 20.79 19.71 18.92 0.01 0.01 0.01 0.67 1.04 0.59 1.24 0.80 1.08 1.88 697±375
GC0284 HGHH-19/C19 13 25 43.40 -43 07 22.8 6.87 19.37 19.01 18.12 17.59 17.03 0.04 0.01 0.01 0.01 0.03 18.96 17.83 18.64 0.05 0.04 0.01 0.35 0.89 0.53 1.10 -0.80 1.13 0.32 632±103,4,5,6,7
GC0285 C165 13 25 43.43 -43 04 56.5 4.77 - - - - - - - - - - 20.10 18.98 18.17 0.05 0.04 0.05 - - - - 0.81 1.12 1.93 -
GC0286 pff gc-063 13 25 43.80 -43 07 54.9 7.39 20.66 20.55 19.83 19.37 18.89 0.08 0.03 0.01 0.01 0.03 20.63 20.13 19.45 0.04 0.03 0.03 0.11 0.72 0.46 0.94 0.67 0.50 1.18 554±755
GC0287 pff gc-064 13 25 43.90 -42 50 42.7 10.85 21.16 20.67 19.66 19.07 18.41 0.11 0.03 0.01 0.01 0.03 20.96 19.97 19.20 0.02 0.03 0.01 0.50 1.01 0.59 1.25 0.76 0.99 1.76 560±245,6,7
GC0288 HGHH-35/C35 13 25 44.21 -42 58 59.4 3.72 19.92 19.51 18.58 18.01 17.43 0.13 0.03 0.01 0.01 0.03 19.74 18.79 18.11 0.02 0.02 0.01 0.41 0.93 0.57 1.14 0.68 0.94 1.63 544±133,4,5
GC0289 C16611 13 25 44.90 -43 04 21.1 4.50 - - - - - - - - - - - - 20.72 - - - - - - - - - - -
GC0290 AAT208065 13 25 45.77 -42 34 18.0 27.05 21.79 21.45 20.09 19.40 18.71 0.49 0.05 0.01 0.01 0.03 22.06 20.70 19.66 0.04 0.03 0.02 0.33 1.36 0.69 1.39 1.04 1.36 2.40 836±417
GC0291 WHH-23 13 25 45.90 -42 57 20.2 5.07 19.26 19.12 18.37 17.89 17.41 0.05 0.02 0.01 0.01 0.03 19.13 18.50 18.00 0.03 0.05 0.01 0.14 0.75 0.48 0.96 0.50 0.64 1.14 286±636
GC0292 C16713 13 25 45.97 -43 06 45.4 6.54 - - - - - - - - - - - - 20.41 - - - - - - - - - - -
GC0293 WHH-24 13 25 46.00 -42 56 53.0 5.43 20.64 20.43 19.63 19.12 18.62 0.12 0.04 0.01 0.01 0.03 20.54 19.91 19.25 0.02 0.03 0.01 0.21 0.80 0.51 1.01 0.66 0.63 1.29 566±486
GC0294 AAT119596 13 25 46.06 -43 08 24.5 8.01 21.19 20.69 19.70 19.10 18.51 0.12 0.03 0.01 0.01 0.03 - - - - - - 0.50 1.00 0.60 1.19 - - - 573±537
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0295 HGHH-G378 13 25 46.13 -43 01 22.9 3.39 21.30 20.59 19.53 18.86 18.22 0.55 0.10 0.03 0.02 0.03 - - - - - - 0.71 1.06 0.67 1.31 - - - 487±314,5,7
GC0296 AAT208206 13 25 46.49 -42 34 54.1 26.47 20.08 20.10 19.47 19.07 18.69 0.12 0.02 0.01 0.01 0.03 20.13 19.73 19.19 0.01 0.01 0.01 -0.02 0.63 0.40 0.78 0.55 0.40 0.94 293±1157
GC0297 HGHH-G284 13 25 46.59 -42 57 03.0 5.37 21.47 20.89 19.87 19.28 18.63 0.26 0.05 0.02 0.01 0.03 21.26 20.20 19.41 0.01 0.01 0.01 0.57 1.03 0.58 1.24 0.79 1.06 1.85 479±124,5,7
GC0298 AAT119697 13 25 46.68 -42 53 48.6 8.12 21.61 21.06 20.05 19.49 18.87 0.23 0.05 0.02 0.01 0.03 21.42 20.42 19.65 0.02 0.02 0.01 0.54 1.01 0.57 1.18 0.77 1.01 1.78 633±1087
GC0299 pff gc-065 13 25 46.92 -43 08 06.6 7.81 20.60 20.17 19.23 18.66 18.08 0.08 0.02 0.01 0.01 0.03 20.43 19.55 18.71 0.01 0.01 0.01 0.42 0.94 0.57 1.15 0.83 0.88 1.72 450±445
GC0300 HGHH-G204 13 25 46.99 -43 02 05.4 3.66 19.35 19.12 18.33 17.83 17.31 0.12 0.04 0.01 0.01 0.03 - - - - - - 0.23 0.79 0.51 1.02 - - - 690±184,5,7
GC0301 pff gc-066 13 25 47.14 -43 06 08.8 6.14 21.21 20.82 19.92 19.37 18.80 0.15 0.04 0.01 0.01 0.03 21.07 20.21 19.44 0.01 0.01 0.01 0.39 0.91 0.55 1.11 0.77 0.86 1.63 530±445,7
GC0302 HGHH-G357 13 25 47.78 -43 00 43.4 3.71 20.87 20.55 19.71 19.24 18.71 0.26 0.07 0.02 0.02 0.04 20.71 19.96 19.31 0.01 0.02 0.01 0.33 0.83 0.47 1.00 0.66 0.75 1.41 664±314,5
GC0303 AAT119894 13 25 47.92 -42 55 52.4 6.45 21.45 21.30 20.25 19.59 18.92 0.23 0.07 0.02 0.02 0.03 21.68 20.75 19.85 0.05 0.04 0.03 0.15 1.05 0.66 1.33 0.90 0.93 1.84 448±907
GC0304 C16815 13 25 48.46 -43 07 12.5 7.16 - - - - - - - - - - - - 19.71 - - - - - - - - - - -
GC0305 HGHH-G251 13 25 48.54 -42 57 41.2 5.16 20.50 19.93 18.93 18.33 17.69 0.13 0.03 0.01 0.01 0.03 20.23 19.22 18.46 0.02 0.01 0.01 0.57 1.00 0.60 1.24 0.76 1.01 1.77 574±274,5,7
GC0306 pff gc-067 13 25 48.77 -43 11 38.7 11.19 20.51 20.35 19.60 19.08 18.60 0.07 0.02 0.01 0.01 0.03 20.47 19.87 19.14 0.01 0.01 0.01 0.16 0.75 0.52 1.00 0.74 0.60 1.33 632±435,7
GC0307 pff gc-068 13 25 49.27 -43 02 20.4 4.13 20.73 20.41 19.55 18.99 18.48 0.20 0.05 0.02 0.02 0.03 20.65 20.17 19.13 0.03 0.04 0.01 0.32 0.85 0.56 1.08 1.04 0.48 1.52 393±265,7
GC0308 HGHH-20/C20 13 25 49.69 -42 54 49.3 7.50 19.18 18.83 17.95 17.43 16.88 0.04 0.01 0.01 0.01 0.03 19.01 18.19 17.54 0.03 0.02 0.01 0.35 0.88 0.53 1.07 0.65 0.82 1.47 744±92,5,6,7
GC0309 AAT120259 13 25 49.73 -43 05 04.7 5.64 21.95 21.16 20.12 19.51 18.80 0.35 0.06 0.02 0.01 0.03 21.57 20.48 19.56 0.01 0.01 0.01 0.79 1.04 0.62 1.32 0.92 1.09 2.01 477±547
GC0310 HGHH-48/C48 13 25 49.82 -42 50 15.3 11.62 19.63 19.46 18.67 18.16 17.67 0.04 0.01 0.01 0.01 0.03 19.56 18.92 18.28 0.02 0.02 0.01 0.17 0.79 0.51 1.01 0.64 0.64 1.28 547±194,5,6,7
GC0311 pff gc-069 13 25 49.93 -42 40 08.2 21.40 21.55 20.90 19.87 19.26 18.62 0.41 0.03 0.01 0.01 0.03 21.29 20.24 19.39 0.01 0.01 0.01 0.64 1.03 0.61 1.25 0.85 1.05 1.90 518±315,7
GC0312 HGHH-47/C47 13 25 49.95 -42 52 09.4 9.87 19.80 19.55 18.69 18.18 17.65 0.05 0.02 0.01 0.01 0.03 19.70 18.97 18.30 0.03 0.02 0.01 0.26 0.86 0.51 1.04 0.67 0.73 1.40 589±224,5,6
GC0313 AAT120336 13 25 50.22 -43 06 08.5 6.48 21.66 21.14 20.17 19.57 18.96 0.23 0.05 0.02 0.01 0.03 21.48 20.50 19.67 0.02 0.01 0.01 0.52 0.97 0.60 1.21 0.83 0.97 1.81 452±677
GC0314 WHH-25 13 25 50.34 -43 04 08.2 5.12 21.33 20.93 19.97 19.42 18.83 0.22 0.05 0.02 0.01 0.03 21.19 20.27 19.57 0.02 0.02 0.01 0.40 0.95 0.55 1.14 0.71 0.92 1.62 525±506,7
GC0315 AAT120355 13 25 50.37 -43 00 32.6 4.20 21.26 21.14 20.42 20.02 19.58 0.28 0.09 0.03 0.03 0.04 21.32 20.75 20.17 0.03 0.03 0.01 0.12 0.72 0.39 0.84 0.59 0.56 1.15 548±777
GC0316 pff gc-070 13 25 50.40 -42 58 02.3 5.20 20.39 20.23 19.42 18.94 18.45 0.12 0.04 0.01 0.01 0.03 20.35 19.67 19.06 0.01 0.01 0.01 0.16 0.81 0.48 0.97 0.61 0.68 1.29 556±495
GC0317 C169 13 25 51.01 -42 55 36.3 7.00 - - - - - - - - - - 21.60 21.00 20.39 0.03 0.03 0.02 - - - - 0.62 0.60 1.21 -
GC0318 AAT120515 13 25 51.31 -42 59 29.4 4.64 21.11 20.81 19.92 19.38 18.81 0.21 0.06 0.02 0.02 0.03 21.04 20.24 19.46 0.04 0.04 0.01 0.30 0.90 0.53 1.11 0.77 0.81 1.58 461±1417
GC0319 pff gc-071 13 25 51.54 -42 59 46.8 4.58 20.79 20.59 19.82 19.34 18.83 0.16 0.05 0.02 0.02 0.03 20.71 20.07 19.45 0.01 0.01 0.01 0.20 0.77 0.48 0.99 0.62 0.64 1.27 475±415
GC0320 C102 13 25 52.07 -42 59 14.4 4.87 - - 21.43 - - - - - - - 22.71 21.87 21.04 0.02 0.02 0.02 - - - - 0.83 0.84 1.67 -
GC0321 pff gc-072 13 25 52.14 -42 58 30.2 5.20 20.68 20.45 19.62 19.12 18.54 0.15 0.04 0.02 0.01 0.03 20.64 19.92 19.25 0.02 0.02 0.01 0.23 0.83 0.51 1.08 0.67 0.72 1.39 504±225
GC0322 HGHH-21/C21 13 25 52.74 -43 05 46.4 6.52 19.16 18.76 17.87 17.32 16.77 0.04 0.01 0.01 0.01 0.03 18.97 18.17 17.40 0.03 0.02 0.01 0.40 0.89 0.55 1.11 0.77 0.80 1.58 462±23,5,6,7,8
GC0323 pff gc-073 13 25 52.78 -42 58 41.7 5.21 21.36 20.94 19.97 19.38 18.74 0.25 0.06 0.02 0.02 0.03 21.25 20.29 19.50 0.02 0.01 0.01 0.42 0.98 0.58 1.22 0.79 0.97 1.76 401±295,6,7
GC0324 HGHH-G256 13 25 52.88 -43 02 00.0 4.70 20.69 20.18 19.00 18.35 17.65 0.18 0.04 0.01 0.01 0.03 20.50 19.31 18.44 0.03 0.04 0.01 0.51 1.17 0.65 1.36 0.87 1.20 2.06 495±184,5,7
GC0325 AAT209412 13 25 53.30 -42 30 52.7 30.63 21.94 21.23 20.22 19.60 18.97 0.52 0.04 0.01 0.01 0.03 21.69 20.64 19.76 0.01 0.01 0.01 0.71 1.01 0.62 1.25 0.88 1.05 1.92 998±1357
GC0326 pff gc-074 13 25 53.37 -42 51 12.4 11.00 21.16 20.83 20.00 19.48 18.90 0.11 0.03 0.01 0.01 0.03 21.04 20.27 19.56 0.01 0.01 0.01 0.33 0.83 0.52 1.10 0.71 0.77 1.48 471±245,7
GC0327 pff gc-075 13 25 53.50 -43 03 56.6 5.50 20.96 20.45 19.48 18.90 18.28 0.14 0.03 0.01 0.01 0.03 20.78 19.76 19.01 0.02 0.03 0.01 0.51 0.97 0.58 1.20 0.75 1.02 1.77 748±185,6,7
GC0328 HGHH-22/C22 13 25 53.57 -42 59 07.6 5.16 19.39 19.06 18.15 17.62 17.07 0.05 0.02 0.01 0.01 0.03 19.21 18.34 17.70 0.02 0.03 - 0.34 0.90 0.54 1.09 0.64 0.87 1.52 578±12,4,5,7,8
GC0329 pff gc-076 13 25 53.75 -43 19 48.6 19.26 20.67 20.06 19.07 18.41 17.78 0.08 0.02 0.01 0.01 0.03 20.44 19.44 18.52 0.02 0.01 0.01 0.62 0.99 0.66 1.29 0.92 1.00 1.92 368±155,6,7
GC0330 AAT120976 13 25 54.28 -42 56 20.6 6.84 21.51 21.23 20.38 19.84 19.27 0.23 0.06 0.02 0.02 0.03 21.50 20.73 19.99 0.03 0.02 0.02 0.28 0.85 0.54 1.11 0.74 0.77 1.51 595±697
GC0331 AAT328533 13 25 54.39 -43 18 40.1 18.19 21.79 21.26 20.31 19.74 19.09 0.16 0.04 0.01 0.01 0.03 21.62 20.64 19.77 0.01 0.01 0.01 0.53 0.95 0.58 1.23 0.87 0.98 1.85 577±897
GC0332 HGHH-23/C23 13 25 54.58 -42 59 25.4 5.22 18.92 18.29 17.22 16.62 15.95 0.04 0.01 0.01 0.01 0.03 18.59 17.44 16.69 0.01 0.03 - 0.63 1.07 0.60 1.28 0.75 1.15 1.90 674±12,3,5,7,8
GC0333 C103 13 25 54.98 -42 59 15.4 5.36 - - 18.88 - - - - - - - 20.43 20.44 18.44 0.01 0.02 0.02 - - - - 2.00 -0.01 1.99 -
GC0334 C170 13 25 56.11 -42 56 12.9 7.17 - - - - - - - - - - 23.31 22.83 22.16 0.05 0.04 0.06 - - - - 0.67 0.48 1.15 -
GC0335 AAT121367 13 25 56.26 -43 01 32.9 5.25 21.06 20.92 20.24 19.82 19.39 0.25 0.08 0.03 0.03 0.04 21.01 20.45 19.85 0.01 0.01 0.01 0.13 0.68 0.42 0.85 0.60 0.56 1.15 438±807
GC0336 WHH-26 13 25 56.59 -42 51 46.6 10.76 20.50 20.02 19.05 18.43 17.81 0.07 0.02 0.01 0.01 0.03 20.33 19.36 18.56 0.02 0.01 0.01 0.48 0.97 0.62 1.24 0.79 0.97 1.76 412±366
GC0337 AAT329209 13 25 57.28 -43 41 09.0 40.37 20.87 20.70 19.87 19.40 18.90 0.21 0.02 0.01 0.01 0.03 20.78 20.12 19.35 0.01 - 0.01 0.17 0.82 0.47 0.97 0.77 0.66 1.43 601±657
GC0338 C171 13 25 57.78 -42 55 36.1 7.82 - - - - - - - - - - 22.25 21.45 20.67 0.04 0.03 0.02 - - - - 0.78 0.79 1.58 -
GC0339 C172 13 25 57.95 -42 53 04.3 9.79 - - - - - - - - - - 22.15 21.45 20.91 0.02 0.01 0.01 - - - - 0.55 0.70 1.24 -
GC0340 pff gc-077 13 25 58.15 -42 31 38.2 30.03 20.57 20.32 19.50 18.96 18.47 0.16 0.02 0.01 0.01 0.03 20.55 19.83 19.09 0.02 0.01 0.01 0.24 0.83 0.53 1.03 0.74 0.71 1.45 675±415
GC0341 pff gc-078 13 25 58.47 -43 08 06.3 8.96 20.93 20.34 19.30 18.69 18.02 0.10 0.02 0.01 0.01 0.03 20.70 19.68 18.75 0.02 0.01 0.01 0.59 1.03 0.62 1.28 0.93 1.02 1.95 545±185,7
GC0342 HGHH-G143 13 25 58.69 -43 07 11.0 8.29 20.31 20.02 19.21 18.68 18.18 0.06 0.02 0.01 0.01 0.03 20.22 19.52 18.77 0.02 0.01 0.01 0.29 0.81 0.53 1.03 0.75 0.70 1.45 503±384,5,7
GC0343 pff gc-079 13 25 58.91 -42 53 18.9 9.70 20.74 20.43 19.58 19.06 18.52 0.10 0.03 0.01 0.01 0.03 20.62 19.86 19.14 0.02 0.01 0.01 0.30 0.86 0.51 1.06 0.72 0.77 1.48 410±215,7
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0344 AAT121826/C104 13 25 59.49 -42 55 30.8 8.10 20.91 20.65 19.81 19.28 18.73 0.13 0.03 0.01 0.01 0.03 20.81 20.15 19.40 0.02 0.02 0.01 0.26 0.83 0.53 1.08 0.74 0.66 1.40 448±987
GC0345 pff gc-080 13 25 59.55 -42 32 39.4 29.08 21.10 20.80 19.96 19.40 18.84 0.25 0.03 0.01 0.01 0.03 21.07 20.32 19.56 0.02 0.01 0.01 0.29 0.85 0.56 1.11 0.75 0.75 1.51 598±565,7
GC0346 C173 13 25 59.57 -42 55 01.5 8.46 - - - - - - - - - - 23.15 22.00 21.06 0.04 0.03 0.02 - - - - 0.94 1.15 2.09 -
GC0347 C174 13 25 59.63 -42 55 15.7 8.30 - - - - - - - - - - 23.24 22.42 21.42 0.04 0.04 0.03 - - - - 0.99 0.82 1.81 -
GC0348 pff gc-081 13 26 00.15 -42 49 00.7 13.51 20.43 20.17 19.34 18.80 18.28 0.07 0.02 0.01 0.01 0.03 20.36 19.61 18.93 0.02 0.01 0.01 0.26 0.83 0.53 1.05 0.69 0.75 1.43 304±315,7
GC0349 K-217 13 26 00.81 -43 09 40.1 10.46 21.63 21.09 20.09 19.54 18.91 0.16 0.03 0.01 0.01 0.03 21.42 20.48 19.57 0.01 0.01 0.01 0.54 0.99 0.56 1.19 0.91 0.94 1.85 315±1577
GC0350 C175 13 26 00.93 -42 58 28.9 6.65 - - - - - - - - - - 23.51 22.53 21.84 0.06 0.04 0.03 - - - - 0.69 0.97 1.67 -
GC0351 pff gc-082 13 26 00.98 -42 22 03.4 39.56 20.83 20.17 19.16 18.58 17.89 0.21 0.02 0.01 0.01 0.03 20.51 19.53 18.69 0.02 0.01 0.01 0.66 1.01 0.58 1.27 0.84 0.98 1.82 573±195,7
GC0352 AAT122146 13 26 01.00 -43 06 55.3 8.40 21.14 20.90 20.05 19.53 19.04 0.11 0.03 0.01 0.01 0.03 21.09 20.38 19.58 0.01 0.01 0.01 0.24 0.85 0.52 1.01 0.80 0.71 1.51 517±997
GC0353 HGHH-G221 13 26 01.11 -42 55 13.5 8.52 20.87 20.24 19.30 18.75 18.13 0.10 0.02 0.01 0.01 0.03 20.54 19.60 18.83 0.01 0.01 0.01 0.62 0.94 0.55 1.16 0.77 0.94 1.72 390±154,5
GC0354 AAT329848 13 26 01.29 -43 34 15.5 33.68 19.44 19.19 18.39 17.89 17.37 0.08 0.01 0.01 0.01 0.03 - - - - - - 0.25 0.79 0.50 1.03 - - - 558±467
GC0355 pff gc-083 13 26 01.83 -42 58 15.0 6.89 21.23 20.80 19.86 19.30 18.72 0.16 0.04 0.01 0.01 0.03 21.12 20.21 19.44 0.02 0.02 0.01 0.42 0.95 0.55 1.13 0.77 0.91 1.68 458±315,6,7
GC0356 pff gc-084 13 26 02.25 -43 08 55.6 10.03 21.31 20.80 19.84 19.24 18.63 0.12 0.03 0.01 0.01 0.03 21.13 20.19 19.32 0.02 0.01 0.01 0.51 0.97 0.59 1.21 0.87 0.93 1.80 458±385,7
GC0357 AAT122445 13 26 02.43 -43 00 11.7 6.43 21.13 20.99 20.28 19.81 19.42 0.15 0.05 0.02 0.02 0.03 21.08 20.50 19.92 0.01 0.02 0.01 0.14 0.71 0.47 0.86 0.58 0.58 1.16 342±987
GC0358 C176 13 26 02.79 -42 57 05.0 7.61 - - - - - - - - - - 22.35 21.92 21.30 0.02 0.02 0.03 - - - - 0.62 0.43 1.05 -
GC0359 HGHH-25/C25 13 26 02.85 -42 56 57.0 7.69 20.17 19.56 18.49 17.85 17.17 0.07 0.02 0.01 0.01 0.03 19.92 18.83 17.97 0.03 0.02 0.01 0.61 1.07 0.64 1.32 0.86 1.09 1.95 703±93,5,7
GC0360 AAT122526 13 26 02.90 -43 05 43.0 7.90 21.89 21.35 20.36 19.73 19.05 0.24 0.05 0.02 0.01 0.03 21.72 20.72 19.81 0.02 0.01 0.01 0.54 1.00 0.62 1.31 0.90 1.00 1.90 506±507
GC0361 C177 13 26 03.20 -42 54 30.1 9.30 - - - - - - - - - - 22.95 22.11 21.09 0.11 0.07 0.05 - - - - 1.02 0.84 1.87 -
GC0362 C178 13 26 03.85 -42 56 45.3 7.95 - - - - - - - - - - 23.02 22.32 21.53 0.04 0.04 0.03 - - - - 0.79 0.69 1.48 -
GC0363 HGHH-G293/G293 13 26 04.20 -42 55 44.7 8.60 20.11 19.90 19.10 18.61 18.11 0.06 0.02 0.01 0.01 0.03 20.04 19.36 18.69 0.01 0.01 0.01 0.21 0.80 0.49 0.99 0.67 0.69 1.35 581±154,5,7
GC0364 AAT122808 13 26 04.61 -43 09 10.2 10.49 21.05 20.87 20.12 19.66 19.18 0.10 0.03 0.01 0.01 0.03 21.00 20.45 19.69 0.01 0.01 0.01 0.18 0.75 0.46 0.94 0.76 0.55 1.31 264±1317
GC0365 AAT122794 13 26 04.69 -42 47 35.1 15.16 21.89 21.15 20.00 19.29 18.69 0.21 0.04 0.01 0.01 0.03 21.60 20.37 19.38 0.01 0.01 0.01 0.74 1.15 0.71 1.31 0.98 1.23 2.22 336±1617
GC0366 C105 13 26 05.12 -42 55 37.0 8.80 - - 22.01 - - - - - - - 23.68 22.58 21.76 0.07 0.04 0.04 - - - - 0.82 1.10 1.92 -
GC0367 HGHH-07/C7 13 26 05.41 -42 56 32.4 8.30 18.38 18.03 17.17 16.65 16.08 0.03 0.01 0.01 0.01 0.03 18.18 17.33 16.64 0.03 0.03 0.01 0.35 0.86 0.53 1.09 0.68 0.85 1.53 595±11,2,3,5,6,7,8
GC0368 C106 13 26 06.15 -42 56 45.4 8.32 - - 21.28 - - - - - - - 22.54 21.46 20.66 0.03 0.01 0.01 - - - - 0.80 1.08 1.88 -
GC0369 pff gc-085 13 26 06.42 -43 00 38.1 7.11 20.39 20.20 19.43 18.99 18.47 0.07 0.02 0.01 0.01 0.03 20.29 19.64 19.03 0.02 0.02 0.01 0.20 0.76 0.44 0.96 0.61 0.65 1.26 548±315,6,7
GC0370 pff gc-086 13 26 06.55 -43 06 14.5 8.75 21.48 20.93 19.95 19.37 18.76 0.16 0.03 0.01 0.01 0.03 21.29 20.32 19.45 0.02 0.01 0.01 0.56 0.97 0.59 1.20 0.87 0.97 1.84 440±265,7
GC0371 pff gc-087 13 26 06.87 -42 33 17.3 28.77 20.26 19.96 19.11 18.56 18.05 0.14 0.02 0.01 0.01 0.03 20.17 19.42 18.70 0.02 0.01 0.01 0.30 0.86 0.55 1.05 0.73 0.75 1.47 830±295,7
GC0372 HGHH-G170 13 26 06.93 -42 57 35.1 8.02 20.78 20.21 19.22 18.65 17.97 0.11 0.02 0.01 0.01 0.03 20.57 19.56 18.73 0.02 0.02 0.01 0.57 0.99 0.57 1.25 0.83 1.01 1.84 636±274,5,7
GC0373 AAT123188 13 26 06.94 -43 07 52.6 9.85 21.70 21.30 20.40 19.85 19.27 0.17 0.04 0.01 0.01 0.03 21.57 20.71 19.94 0.02 0.01 0.01 0.40 0.90 0.56 1.13 0.77 0.86 1.63 364±567
GC0374 HGHH-36/C36/R113 13 26 07.73 -42 52 00.3 11.72 19.42 19.19 18.35 17.81 17.33 0.04 0.01 0.01 0.01 0.03 19.32 18.61 17.94 0.02 0.01 0.01 0.23 0.84 0.54 1.03 0.67 0.71 1.38 703±13,5,6,7,8
GC0375 AAT123453 13 26 08.38 -42 59 18.9 7.67 21.29 20.95 20.09 19.55 19.03 0.17 0.04 0.02 0.01 0.03 21.20 20.40 19.67 0.03 0.02 0.01 0.34 0.86 0.54 1.06 0.73 0.80 1.53 257±1547
GC0376 pff gc-088 13 26 08.86 -43 01 21.4 7.54 19.99 19.79 18.99 18.46 18.00 0.05 0.02 0.01 0.01 0.03 19.86 19.14 18.59 0.03 0.03 0.01 0.20 0.80 0.53 0.99 0.55 0.72 1.27 554±295,7
GC0377 AAT123656 13 26 09.61 -43 07 05.9 9.71 21.77 21.13 20.08 19.46 18.79 0.19 0.04 0.01 0.01 0.03 21.57 20.51 19.59 0.03 0.02 0.02 0.64 1.05 0.63 1.29 0.92 1.07 1.99 380±937
GC0378 R111 13 26 09.71 -42 50 29.5 13.14 22.07 21.57 20.59 19.91 19.09 0.28 0.06 0.02 0.02 0.03 21.96 21.03 20.20 0.03 0.03 0.02 0.51 0.97 0.68 1.50 0.82 0.94 1.76 717±485,7
GC0379 C179 13 26 09.87 -42 56 36.0 8.96 - - - - - - - - - - 22.13 21.71 21.04 0.03 0.03 0.01 - - - - 0.67 0.42 1.09 -
GC0380 HGHH-37/C37/R116 13 26 10.58 -42 53 42.7 10.81 19.86 19.38 18.43 17.87 17.26 0.04 0.01 0.01 0.01 0.03 19.65 18.72 17.96 0.01 0.01 0.01 0.48 0.95 0.56 1.17 0.76 0.93 1.69 612±13,5,6,7,8
GC0381 WHH-27 13 26 12.82 -43 09 09.2 11.51 20.27 19.68 18.66 18.06 17.42 0.05 0.01 0.01 0.01 0.03 20.02 19.03 18.13 0.02 0.01 0.01 0.59 1.02 0.60 1.24 0.90 0.99 1.89 545±606
GC0382 WHH-28 13 26 14.18 -43 08 30.4 11.25 20.21 19.98 19.17 18.65 18.14 0.05 0.02 0.01 0.01 0.03 20.13 19.48 18.71 0.02 0.01 0.01 0.23 0.81 0.52 1.03 0.77 0.65 1.41 506±1236
GC0383 HHH86-26/C26 13 26 15.27 -42 48 29.4 15.36 19.99 19.26 18.13 17.47 16.77 0.05 0.01 0.01 0.01 0.03 19.66 18.45 17.59 0.04 0.03 0.02 0.73 1.13 0.66 1.35 0.86 1.21 2.07 377±142,5,6,7
GC0384 R122 13 26 15.95 -42 55 00.5 10.76 19.02 18.78 18.02 17.58 17.14 0.03 0.01 0.01 0.01 0.03 - - - - - - 0.24 0.76 0.44 0.88 - - - 588±28
GC0385 AAT125079 13 26 17.29 -43 06 39.3 10.62 21.13 20.90 20.09 19.59 19.06 0.10 0.03 0.01 0.01 0.03 21.07 20.41 19.64 0.02 0.01 0.01 0.23 0.81 0.51 1.03 0.77 0.66 1.43 513±1837
GC0386 C50/K-233 13 26 19.66 -43 03 18.6 9.76 20.09 19.68 18.74 18.17 17.57 0.05 0.02 0.01 0.01 0.03 19.91 18.92 18.28 0.04 0.04 0.01 0.41 0.93 0.58 1.17 0.64 1.00 1.63 615±586,7
GC0387 C49/pff gc-089 13 26 20.20 -43 10 35.7 13.48 19.90 19.73 18.95 18.45 17.95 0.12 0.02 0.01 0.01 0.03 19.85 19.30 18.53 0.03 0.02 0.01 0.17 0.78 0.50 1.00 0.77 0.56 1.32 538±305,6,7
GC0388 pff gc-090 13 26 20.53 -43 03 18.5 9.91 20.90 20.34 19.33 18.74 18.10 0.10 0.02 0.01 0.01 0.03 20.70 19.61 18.85 0.03 0.03 0.01 0.56 1.00 0.60 1.24 0.75 1.09 1.85 486±265,7
GC0389 AAT215171 13 26 20.66 -42 38 32.0 24.60 21.03 20.63 19.69 19.11 18.53 0.27 0.03 0.01 0.01 0.03 20.97 20.06 19.26 0.02 0.02 0.01 0.40 0.94 0.58 1.15 0.80 0.90 1.70 527±487
GC0390 R107 13 26 21.11 -42 48 41.1 15.84 21.53 20.82 19.75 19.13 18.48 0.16 0.03 0.01 0.01 0.03 21.23 20.16 19.30 0.05 0.03 0.02 0.71 1.07 0.62 1.27 0.86 1.06 1.92 405±285,7
GC0391 pff gc-091 13 26 21.14 -43 42 24.6 42.41 20.42 20.13 19.29 18.77 18.21 0.15 0.02 0.01 0.01 0.03 20.30 19.56 18.72 0.01 0.01 0.01 0.29 0.84 0.52 1.08 0.84 0.74 1.58 623±375,7
GC0392 pff gc-092 13 26 21.31 -42 57 19.1 10.53 21.36 20.86 19.92 19.35 18.76 0.14 0.03 0.01 0.01 0.03 21.18 20.27 19.46 0.02 0.02 0.01 0.50 0.93 0.57 1.16 0.81 0.92 1.73 462±275,7
Table 1—Continued
Name Old Name RA Dec. R U B V R I σU σB σV σR σI C M T1 σC σM σT1
U − B B − V V − R V − I M − T1 C − M C − T1 vr
(J2000) (J2000) (’) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (km s−1)
GC0393 R117 13 26 21.99 -42 53 45.5 12.38 20.52 20.41 19.68 19.23 18.75 0.07 0.02 0.01 0.01 0.03 20.50 19.98 19.32 0.02 0.02 0.01 0.10 0.73 0.45 0.93 0.66 0.53 1.18 484±265,7
GC0394 R118 13 26 22.01 -42 54 26.5 11.99 20.73 20.60 19.87 19.38 18.93 0.08 0.03 0.01 0.01 0.03 20.72 20.19 19.50 0.03 0.02 0.01 0.13 0.73 0.49 0.95 0.70 0.52 1.22 440±735
GC0395 WHH-29 13 26 22.08 -43 09 10.7 12.79 20.97 20.70 19.82 19.28 18.73 0.08 0.02 0.01 0.01 0.03 20.92 20.17 19.38 0.03 0.02 0.01 0.27 0.88 0.54 1.09 0.79 0.75 1.54 505±786
GC0396 pff gc-093 13 26 22.65 -42 46 49.8 17.50 20.58 20.39 19.62 19.13 18.66 0.08 0.03 0.01 0.01 0.03 20.52 19.91 19.23 0.02 0.01 0.01 0.20 0.77 0.48 0.96 0.69 0.61 1.30 576±425,7
GC0397 WHH-30 13 26 23.60 -43 03 43.9 10.55 20.56 20.25 19.38 18.83 18.30 0.10 0.03 0.01 0.01 0.03 20.45 19.62 18.96 0.03 0.03 0.01 0.31 0.87 0.55 1.08 0.65 0.83 1.49 470±666
GC0398 pff gc-094 13 26 23.66 -43 00 45.6 10.25 20.99 20.77 19.97 19.49 18.93 0.09 0.03 0.01 0.01 0.03 20.92 20.24 19.57 0.03 0.02 0.01 0.22 0.80 0.47 1.04 0.67 0.68 1.35 334±645,7
GC0399 HHH86-38/C38/R123 13 26 23.78 -42 54 01.1 12.50 19.67 19.30 18.41 17.87 17.32 0.04 0.01 0.01 0.01 0.03 19.51 18.68 17.96 0.02 0.02 0.01 0.37 0.89 0.54 1.09 0.72 0.83 1.54 405±13,5,6,8
GC0400 HGHH-51 13 26 23.86 -42 47 17.1 17.26 19.63 19.34 18.47 17.93 17.38 0.05 0.02 0.01 0.01 0.03 - - - - - - 0.29 0.87 0.54 1.09 - - - 343±434,5
GC0401 AAT335187 13 26 23.95 -43 17 44.4 19.53 21.19 21.11 20.46 20.04 19.60 0.10 0.03 0.01 0.01 0.03 21.20 20.72 20.08 0.01 0.01 0.01 0.08 0.65 0.42 0.86 0.64 0.49 1.12 277±1587
GC0402 pff gc-095 13 26 25.50 -42 57 06.2 11.33 21.13 20.60 19.60 19.02 18.40 0.11 0.02 0.01 0.01 0.03 20.97 19.97 19.17 0.04 0.03 0.02 0.53 1.00 0.58 1.20 0.80 0.99 1.79 405±185,7
GC0403 R124 13 26 28.87 -42 52 36.4 14.08 20.32 20.17 19.42 18.96 18.43 0.05 0.02 0.01 0.01 0.03 20.28 19.69 19.02 0.02 0.02 0.01 0.15 0.75 0.46 0.99 0.68 0.58 1.26 541±355,7
GC0404 pff gc-096 13 26 30.29 -42 34 41.7 28.83 21.24 20.73 19.73 19.10 18.42 0.31 0.03 0.01 0.01 0.03 21.08 20.09 19.24 0.01 0.01 0.01 0.52 1.00 0.63 1.30 0.85 0.99 1.83 532±255,7
GC0405 R105 13 26 33.55 -42 51 00.9 15.74 21.28 20.78 19.86 19.28 18.70 0.11 0.03 0.01 0.01 0.03 21.18 20.25 19.46 0.02 0.01 0.01 0.50 0.92 0.58 1.15 0.79 0.93 1.72 534±345,7
GC0406 HGHH-27/C27 13 26 37.99 -42 45 49.9 20.00 19.60 19.39 18.60 18.11 17.62 0.03 0.01 0.01 0.01 0.03 - - - - - - 0.21 0.78 0.49 0.98 - - - 492±372,5
GC0407 WHH-31 13 26 41.43 -43 11 25.0 16.96 20.76 20.44 19.50 18.94 18.36 0.07 0.02 0.01 0.01 0.03 20.67 19.89 19.05 0.03 0.02 0.02 0.32 0.94 0.56 1.14 0.85 0.77 1.62 573±676
GC0408 HHH86-39/C39 13 26 42.03 -43 07 44.8 15.12 18.72 18.33 17.43 16.91 16.42 0.02 0.01 0.01 0.01 0.03 18.57 17.73 16.92 0.01 0.01 - 0.39 0.89 0.53 1.01 0.81 0.83 1.65 271±203,5,6,7
GC0409 pff gc-097 13 26 45.40 -43 26 34.1 29.13 19.75 19.51 18.72 18.23 17.76 0.10 0.01 0.01 0.01 0.03 19.66 19.04 18.28 0.02 0.01 0.01 0.24 0.79 0.49 0.96 0.76 0.62 1.38 599±305,7
GC0410 HH-017 13 26 49.31 -43 04 57.8 15.41 23.21 22.54 20.80 19.87 19.06 0.67 0.11 0.02 0.01 0.03 23.32 21.63 20.13 0.05 0.03 0.02 0.67 1.75 0.93 1.73 1.50 1.68 3.19 839±637
GC0411 pff gc-098 13 26 53.94 -43 19 17.7 24.05 19.54 19.17 18.28 17.73 17.16 0.09 0.01 0.01 0.01 0.03 - - - - - - 0.37 0.89 0.55 1.12 - - - 631±185,7
GC0412 AAT222977 13 26 58.91 -42 38 53.4 27.82 21.18 21.02 20.34 19.84 19.38 0.28 0.03 0.01 0.01 0.03 21.16 20.64 20.02 0.02 0.01 0.01 0.17 0.68 0.50 0.96 0.62 0.52 1.14 655±1127
GC0413 HH-060 13 26 59.78 -42 55 26.5 17.79 - - - - - - - - - - 23.41 21.69 20.14 0.05 0.04 0.02 - - - - 1.55 1.72 3.26 811±327
GC0414 pff gc-099 13 26 59.82 -42 32 40.5 33.09 20.96 20.72 19.94 19.40 18.92 0.23 0.03 0.01 0.01 0.03 20.92 20.29 19.59 0.02 0.01 0.02 0.25 0.78 0.53 1.02 0.70 0.63 1.33 425±345,7
GC0415 pff gc-100 13 27 03.41 -42 27 17.2 38.12 19.92 19.37 18.41 17.81 17.17 0.11 0.01 0.01 0.01 0.03 - - - - - - 0.56 0.96 0.60 1.24 - - - 513±105,7
GC0416 pff gc-101 13 27 21.56 -42 38 41.4 30.63 19.89 19.51 18.72 18.20 17.74 0.10 0.01 0.01 0.01 0.03 19.74 19.02 18.39 0.01 0.01 - 0.38 0.79 0.51 0.97 0.63 0.72 1.35 263±165,7
GC0417 pff gc-102 13 28 18.45 -42 33 12.5 41.90 20.38 20.11 19.29 18.76 18.24 0.14 0.02 0.01 0.01 0.03 20.28 19.59 18.94 0.04 0.04 0.01 0.27 0.83 0.52 1.04 0.65 0.70 1.34 428±405,7
1Radial velocity measured by van den Bergh, Hesser, & Harris (1981).
2Radial velocity measured by Hesser et al. (1984).
3Radial velocity measured by Hesser, Harris, & Harris (1986).
4Radial velocity measured by Harris et al. (1992).
5Radial velocity measured by Peng, Ford, & Freeman (2004a).
6Radial velocity measured by Woodley, Harris, & Harris (2005).
7Radial velocity measured by Beasley et al. (2006).
8Radial velocity measured by Rejkuba et al. (2007).
9These objects appear starlike under HST/ACS imaging (Harris et al. 2006).
10This object appears to be a M-type star based on the strong molecular bands in its spectrum (Beasley et al. 2006).
11Faint globular (Harris et al. 2006).
12ocated in the inner bulge region which is very crowded (Harris et al. 2006).
13A very compact globular or star (Harris et al. 2006).
14A possible globular, but slightly elliptical (Harris et al. 2006).
15A globular next to a very bright star (Harris et al. 2006).
– 39 –
Table 2. Kinematic and Dynamic Solutions for the Globular Cluster System of NGC 51281
Radial Bin Rmean Rout N ΩR Θo σv Mcorr Mp Mr Mt
(kpc) (kpc) (kpc) (km s−1) (o E of N) (km s−1) (×1010M⊙) (×10
10M⊙) (×10
10M⊙)
0-50 12.9 48.8 340 40±10 189±12 123±5 1.0 125.8±46.52 3.1±1.3 128.9±46.5
0-5 3.64 4.96 54 24±21 334±59 120±12 - - - -
5-10 7.65 9.96 124 43±15 195±20 112±8 2.3 37.4±6.4 0.4±0.3 37.8±6.4
10-15 12.4 14.9 68 83±25 195±12 105±10 1.6 36.5±9.3 2.4±1.5 38.9±9.4
15-25 19.0 24.3 56 35±26 184±34 147±16 1.3 89.5±27.4 0.7±1.0 90.2±27.4
25-50 34.7 48.8 39 96±45 169±17 148±21 1.0 184.7±84.5 10.4±9.8 195.1±85.1
1This table is reproduced from Woodley (2006) for completeness.
2The Tracer Mass estimator determines the total mass enclosed within the outermost radius using a sample defined in the range of the
inner and outer radial bins.
Table 3. Kinematic and Dynamic Solutions for the Metal-Poor Globular Cluster System
of NGC 5128
Radial Bin Rmean Rout N ΩR Θo σv Mcorr Mp Mr Mt
(kpc) (kpc) (kpc) (km s−1) (o E of N) (km s−1) (×1010M⊙) (×10
10M⊙) (×10
10M⊙)
0-50 13.8 48.1 178 31±14 177±22 117±7 1.0 94.5±58.5 1.1±1.0 95.6 ±58.6
0-5 3.84 4.96 22 16±38 373±120 99±19 - - - -
5-10 7.76 9.96 66 30±21 223±39 116±12 2.1 38.9±12.4 0.2±0.3 39.1±12.4
10-15 12.7 14.8 41 97±38 199±13 102±15 1.5 31.4±15.1 3.3±2.5 34.6±15.3
15-25 18.8 24.3 26 45±31 139±49 112±20 1.3 59.7±32.7 1.2±1.6 60.8±32.7
25-50 36.7 48.1 23 61±43 137±50 141±24 1.0 122.4±82.9 4.2±5.9 126.7±83.1
Table 4. Kinematic and Dynamic Solutions for the Metal-Rich Globular Cluster System
of NGC 5128
Radial Bin Rmean Rout N ΩR Θo σv Mcorr Mp Mr Mt
(kpc) (kpc) (kpc) (km s−1) (o E of N) (km s−1) (×1010M⊙) (×10
10M⊙) (×10
10M⊙)
0-50 12.0 48.8 158 47±15 202±15 129±9 1.0 116.5±73.8 4.3±2.3 120.8±73.9
0-5 3.61 4.98 29 44±27 308±47 134±23 - - - -
5-10 7.52 9.93 58 65±22 180±19 105±11 1.5 17.4±7.7 1.0±0.7 18.3±7.7
10-15 12.0 14.9 27 74±34 186±22 108±17 1.2 23.8±11.3 1.9±1.8 25.7±13.3
15-25 19.3 24.3 30 50±36 223±32 168±24 1.1 72.1±46.2 1.2±1.7 73.3±46.3
25-50 31.7 48.8 15 102±96 191±21 146±65 1.0 219.1±174.6 11.8±22.2 230.9±176.0
– 40 –
Table 5. Kinematic and Dynamic Solutions for the Planetary Nebula System of NGC
Radial Bin Rmean Rout N ΩR Θo σv Mcorr Mp Mr Mt
(kpc) (kpc) (kpc) (km s−1) (o E of N) (km s−1) (×1010M⊙) (×10
10M⊙) (×10
10M⊙)
0-90 14.1 88.2 780 76±6 170±5 118±13 1.0 84.6±17.2 11.9±1.9 96.5±17.3
0-5 3.3 4.99 184 75±16 179±11 131±7 - - - -
5-10 7.6 9.98 211 82±12 177±8 120±6 3.0 43.9±3.6 1.6±0.5 45.4±3.6
10-15 11.8 14.8 138 76±15 171±10 118±7 2.0 42.3±5.0 2.0±0.8 44.2±5.1
15-20 17.4 20.0 71 96±24 169±12 116±10 1.7 47.7±5.6 4.3±2.1 52.0±6.9
20-30 24.6 30.0 87 76±17 157±17 108±8 1.5 53.2±8.4 4.0±1.8 57.2±8.6
30-40 34.6 39.8 50 44±15 132±38 87±9 1.3 40.7±7.4 1.8±1.2 42.3±7.5
40-80 48.7 71.2 36 61±45 183±22 85±11 1.0 48.6±11.5 6.2±9.1 54.8±14.7
Table 6. Spin Parameters for Giant Elliptical Galaxies
Galaxy ΩRMP σv,MP (ΩR/σv)MP ΛMP ΩRMR σv,MR (ΩR/σv)MR ΛMR
(km s−1) (km s−1) (km s−1) (km s−1)
NGC 5128 31±14 117±7 0.26±0.12 0.08±0.04 47±15 129±9 0.36±0.11 0.11±0.03
M878,9 186+58
397+36
0.47+0.13
−0.11 0.14
+0.04
−0.03 155
365+38
0.43+0.14
−0.12 0.13
+0.04
−0.04
M499 93+69
342+33
0.27+0.19
−0.11 0.08
+0.06
−0.03 -26
265+34
0.10+0.27
−0.25 0.03
+0.08
−0.08
NGC 139910 15±26 291±14 0.05±0.09 0.02±0.03 7±24 255±13 0.03±0.09 0.01±0.03
8Kinematic data taken from Côté et al. (2001).
9Kinematic data taken from Côté et al. (2003).
10Kinematic data taken from Richtler et al. (2004).
– 41 –
Fig. 1.— Positions of the GCS (left) totaling 340 objects and the PN system (right) totaling
780 objects in NGC 5128. The PN system has more than double the objects and extends
∼ 40 kpc further out from the center of NGC 5128. Both systems are spatially biased to the
major axis of the galaxy with a position angle of 35o east of north.
– 42 –
Fig. 2.— Velocity histograms fit with a Gaussian (mean velocity and standard deviation in
km s−1) for the samples. Top left, the entire GC (546.4 ± 7.3, 128.8 ± 7.3); top right, GCs
with a radial velocity uncertainty < 50 km s−1 (554.8 ± 5.3, 126.2 ± 7.3); bottom left, all
metal-poor GCs (532.5 ± 12.7, 123.8 ± 12.8); bottom right, all metal-rich GCs (565.5 ± 10.5,
140.3 ± 10.7).
– 43 –
Fig. 3.— Projected radial distribution as a function of projected angular position of all known
GCs in NGC 5128. The angular distribution of metal-poor (squares), metal-rich (crosses),
and unknown metallicity (circles) subpopulations of GCs clearly shows the observational
bias in GC searches along the photometric minor axis (Θ = 119 and 299o east of north,
Dufour et al. 1979) beyond 15 kpc.
– 44 –
Fig. 4.— Sine curve fit for the GCs in NGC 5128 (circles) with a fixed systemic velocity of
vsys = 541 km s
−1, for 0-50 kpc from the center of NGC 5128. The top panel shows all 340
GCs with rotation amplitude ΩR = 40± 10 km s−1 and rotation axis Θo = 189± 12
o east of
north. The middle panel shows the 178 metal-poor clusters with ΩR = 31 ± 14 km s−1 and
Θo = 177 ± 22
o east of north, and the bottom panel shows the 158 metal-rich clusters with
ΩR = 47± 15 km s−1 and Θo = 202± 15
o east of north. The squares represent the weighted
velocities in 72o bins.
– 45 –
Fig. 5.— Rotation amplitude as a function of projected galactocentric radius from the center
of NGC 5128, including all known GCs (left) and the 780 PNe (right). The data are binned
in radial bins (squares) of 0-5, 5-10, 10-15 15-25, and 25-50 kpc for the GCs or 0-5, 5-10,
10-15, 15-20, 20-30, 30-40, and 40-80 kpc for the PNe, in equal number of 38 GCs (filled
circles) or 60 PNe, and exponentially weighted GCs or PNe with varying bin width (solid
line) and 35% uncertainties of the weighted data (dashed lines). The radial distribution of
data is shown at the bottom (open circles).
– 46 –
Fig. 6.— Same as Fig. 5, but for the metal-poor subpopulation of GCs (left) and the metal-
rich subpopulation of GCs (right). The equal numbered bins (filled circles) consist of 20
metal-poor or metal-rich GCs.
– 47 –
Fig. 7.— Rotation axis as a function of projected galactocentric radius from the center of
NGC 5128, including all known GCs (left) and the 780 PNe (right). The symbols are the
same as in Fig. 5, but the uncertainty of the weighted data (dashed lines) is 25%.
– 48 –
Fig. 8.— Same as Fig. 7, but for the metal-poor (left) and metal-rich (right) subpopulations
of GCs.
– 49 –
Fig. 9.— Velocity dispersion as a function of projected galactocentric radius from the center
of NGC 5128 for all known GCs (left) and the 780 PNe (right). The symbols are the same as
in Fig. 7, but the uncertainties of the weighted data (dashed lines) are determined by Eqn 2.
– 50 –
Fig. 10.— Same as Fig. 9, but for the metal-poor (left) and metal-rich (right) subpopulations
of GCs.
– 51 –
Fig. 11.— Velocity histograms for the GCs, subdivided by both metallicity and radius,
binned in 50 km s−1 intervals. Here vf is the residual velocity after subtraction of the
systemic velocity of 541 km s−1 and the overall rotation component for either the metal-poor
or metal-rich subpopulation, determined from Eqn. 1. The histograms for the metal-poor
clusters (left panels) include 129 clusters between 0 and 15 kpc and 49 clusters between
15 and 50 kpc, while the histograms for the metal-rich clusters (right panels) include 114
clusters between 0 and 15 kpc and 44 clusters between 15 and 50 kpc.
– 52 –
Fig. 12.— Surface density of known GCs fit with a powerlaw for the entire population (solid
line), the metal-poor subpopulation (dotted line), and the metal-rich subpopulation (short-
dashed line) in NGC 5128 with the best-fit linear coefficients shown. The radial distribution
of the entire GC population is shown as filled squares, yet clusters with projected radii < 5
kpc are shown as open squares and are not included in the powerlaw fits. Also overplotted is
the surface density of the PN system (long-dashed line) fit from all PNe beyond 5 kpc with
the best-fit linear coefficients also shown.
– 53 –
Fig. 13.— Total mass profile for the radially binned estimates of the GC system (filled
squares) from Woodley (2006) and the PNe (filled triangles). The GC total mass from 0 to
50 kpc, shown as the open square, is 1.3 ± 0.5 × 1012M⊙, and the PN total mass from 0 to
90 kpc, shown as the open triangle, is 1.0± 0.2× 1012M⊙, agreeing within the uncertainties.
	Introduction
	The Catalog of Globular Clusters in NGC 5128
	Kinematics of the Globular Cluster System
	Velocity Field
	Rotation Amplitude, Rotation Axis, and Velocity Dispersion
	Mathematic and Analytic Description
	Rotation Amplitude of the Globular Cluster System
	Rotation Axis of the Globular Cluster System
	Velocity Dispersion of the Globular Cluster System
	Kinematics of the Planetary Nebula System of NGC 5128
	Dynamics of NGC 5128
	Mass Determination
	Surface Density Profiles
	Mass Results
	Discussion and Conclusions
