85 research outputs found
Bimodal Infrared Colors of the M87 Globular Cluster System: Peaks in the Metallicity Distribution
The globular cluster (GC) systems of many galaxies reveal bimodal optical
color distributions. Based on stellar evolutionary models and the bimodal
colors and metallicities of Galactic GCs this is thought to reflect an
underlying bimodal metallicity distribution. However, stars at many different
phases of stellar evolution contribute to optical light. The I-H color is a
much cleaner tracer of metallicity because it primarily samples the metallicity
sensitive giant branch. Therefore, we use deep HST-NICMOS H, and WFPC2 optical
observations, of M87 GCs to study their metallicity distribution. The M87
clusters are bimodal in I-H, for which there is no known physical explanation
other than a bimodal metallicity distribution. Moreover, the two modes defined
by the B-I and I-H colors are comprised of roughly the same two sets of
objects, confirming that optical colors also primarily trace the metallicity.
This is inconsistent with a recent suggestion based on one model of metallicity
effects on the horizontal branch that bimodality arises from an underlying
unimodal metallicity distribution due to a specific color-metallicity relation.
We also find no discernable variation in the peak colors of the M87 GCs out to
roughly 75 kpc due to the declining ratio of red-to-blue GCs, as implied by
this model. Similarly, there is no evidence that the bimodal peaks are bluer
for systems with large blue-to-red GC ratio. Our observations confirm that the
primary cause of bimodality in cluster systems is an underlying bimodal
metallicity distribution, and not the specific color-metallicity relationship
defined by this horizontal branch model.Comment: Accepted for publication in ApJ Letters. 5 pages, 4 figs. Version 2
is identical to version
The Luminosity Functions of Old and Intermediate-Age Globular Clusters in NGC 3610
The WFPC2 Camera on board HST has been used to obtain high-resolution images
of NGC 3610, a dynamically young elliptical galaxy. These observations
supersede shorter, undithered HST observations where an intermediate-age
population of globular clusters was first discovered. The new observations show
the bimodal color distribution of globular clusters more clearly, with peaks at
(V-I)o = 0.95 and 1.17. The luminosity function (LF) of the blue, metal-poor
population of clusters in NGC 3610 turns over, consistent with a Gaussian
distribution with a peak Mv ~= -7.0, similar to old globular-cluster
populations in ellipticals. The red, metal-rich population of clusters has a LF
that is more extended toward both the bright and faint ends, as expected for a
cluster population of inter-mediate age. It is well fit by a power law with an
exponent of alpha = -1.78 +-0.05, or -1.90+-0.07 when corrected for
observational scatter. A Kolmogorov-Smirnov test confirms the significant
difference between the LFs of the red and blue clusters, with a probability of
less than 0.1% that they come from the same population. A comparison with the
Fall & Zhang cluster disruption models shows marginal agreement with the
observed LF, although there are differences in detail. In particular, there is
no clear evidence of the predicted turnover at the faint end. A by-product of
the analysis is the demonstration that, at any given metallicity, the peak of
the LF should remain nearly constant from 1.5 Gyr to 12 Gyr, since the effect
of the disruption of faint clusters is almost perfectly balanced by the fading
of the clusters. This may help explain the apparent universality of the peak of
the globular cluster luminosity function. (Abridged)Comment: 32 pages, LaTeX, 13 PS figures, 1 table; to appear in AJ (July 2002
Some Constraints On the Effects of Age and Metallicity on the Low Mass X-ray Binary Formation Rate
We have studied the low mass X-ray binary (LMXB) populations within and
outside globular clusters (GC) in NGC 4365 and NGC 3115. Using published age
and metallicity constraints from optical and IR observations of their GCs, we
do not find any evidence for an increase in the LMXB formation rate in the
intermediate age cluster population of NGC 4365, as has been proposed in some
scenarios of dynamical LMXB formation in GCs. The old, metal-rich, red
population of GCs in NGC 3115 on the other hand is {\it at least} three times
as efficient at creating LMXBs as the old, metal-poor, blue clusters. These
data suggest that the higher formation efficiency of LMXBs in the red GC
subsystems of many galaxies is largely a consequence of their higher
metallicity. A comparison of the densities of field LMXBs in different galaxies
does not reveal an obvious correlation with the age of the field stars as
predicted by models in which the LMXB formation rate in the field drops
monotonically with time after an initial burst. This suggests that either a
significant fraction of the field LMXBs are created in GCs and subsequently
injected into the field, or the LMXB formation rate has a more complex time
evolution pattern.Comment: Accepted for publication in ApJ Letters. 7 pages including 5 figure
Hubble Space Telescope FUV observations of M31's globular clusters suggest a spatially homogeneous helium-enriched sub population
We present high spatial resolution, far ultraviolet (FUV) F140LP observations
of 12 massive globular clusters in M 31 obtained using the ACS/SBC on the
Hubble Space Telescope (HST). These observations resolve the cluster profiles
to scales similar to their core radii and enable the study of the spatial
distribution of blue and extreme horizontal branch (HB) stars, which dominate
the emission in the F140LP images. We confirm that some of these clusters have
excess FUV emission, suggesting additional hot populations beyond those
expected by canonical single stellar populations models. We find no evidence
that the hot populations are spatially distinct from the majority populations
in these clusters, as would be expected if the excess FUV emission is a result
of a dynamically enhanced population of extreme-HB stars. We conclude that a
second population of stars with significantly enhanced helium abundance is a
viable explanation for the observed FUV emission which is both bright and
distributed similarly to the rest of the cluster light. Our results support the
use of FUV observations as a path to characterising helium enhanced sub
populations in extragalactic clusters. These M31 clusters also show a
correlation such that more massive and denser clusters are relatively FUV
bright. Similar to extant Milky Way results, this may indicate the degree of
helium enrichment, or second population fraction increases with cluster mass.Comment: 12 pages, 7 figures, 1 table, accepted for publication in MNRA
Global Properties of the Globular Cluster Systems of Four Spiral Galaxies
We present results from a wide-field imaging study of the globular cluster
(GC) systems of a sample of edge-on, Sb-Sc spiral galaxies ~7-20 Mpc away. This
study is part of a larger survey of the ensemble properties of the GC
populations of giant galaxies. We imaged the galaxies in BVR filters with
large-format CCD detectors on the WIYN 3.5-m telescope, to projected radii of
~20-40 kpc. For four galaxies (NGC 2683, NGC 3556, NGC 4157, and NGC 7331), we
quantify the radial distributions of the GC systems and estimate the total
number, luminosity- and mass-normalized specific frequencies (S_N and T), and
blue (metal-poor) fraction of GCs. A fifth galaxy (NGC 3044) was apparently too
distant for us to have detected its GC system. Our S_N for NGC 2683 is 2.5
times smaller than the previously-published value, likely due in part to
reduced contamination from non-GCs. For the spiral galaxies analyzed for the
survey to date, the average number of GCs is 170+/-40 and the weighted mean
values of S_N and T are 0.8+/-0.2 and 1.4+/-0.3. We use the survey data to
derive a relationship between radial exent of the GC system and host galaxy
mass over a factor of 20 in mass. Finally, we confirm the trend, identified in
previous survey papers, of increasing specific frequency of metal-poor GCs with
increasing galaxy mass. We compare the data with predictions from a simple
model and show that carefully quantifying the numbers of metal-poor GCs in
galaxies can constrain the formation redshifts of the GCs and their host
galaxies.Comment: 30 pages, including 14 figures and 13 tables; accepted for
publication in The Astronomical Journal, Oct 2007 issu
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