The Dependence of Globular Cluster Number on Density for Abell Cluster Central Galaxies

A study of the globular cluster systems of 23 brightest, or central, galaxies in 19 Abell clusters has recently been completed. This Letter presents some of the newly discovered correlations of the globular cluster specific frequency $S_N$ in these galaxies with other galaxy and cluster properties and puts forth an interpretation of these results. $S_N$ is found to correlate strongly with measures of the cluster density, such as the velocity dispersion of the cluster galaxies and the cluster X-ray temperature and luminosity (especially ``local'' X-ray luminosity). Within a cluster, galaxies at smaller projected distances from the X-ray center are found to have higher values of $S_N$. Taken together, the scaling of $S_N$ with cluster density and the relative constancy of central galaxy luminosity suggest a scenario in which globular clusters form in proportionate numbers to the available mass, but galaxy luminosity ``saturates'' at a maximum threshold, resulting in higher \sn\ values for central galaxies in denser clusters as well as the suitability of these galaxies as ``standard candles.'' Thus, these galaxies do not have too many globular clusters for their luminosity; rather, they are underluminous for their number of globular clusters.Comment: 10 pages, with 4 included postscript figures; AASTeX (aaspp4.sty); to appear in ApJ Letter

Stellar Populations and Surface Brightness Fluctuations: New Observations and Models

We examine the use of surface brightness fluctuations (SBF) for both stellar population and distance studies. New V-band SBF data are reported for five Fornax cluster galaxies and combined with literature data to define a new V-band SBF distance indicator. We use new stellar population models, based on the latest Padua isochrones transformed empirically to the observational plane, to predict SBF magnitudes and integrated colours for a wide range of population ages and metallicities. We examine the sensitivity of the predictions to changes in the isochrones, transformations, and IMF. The new models reproduce the SBF data for globular clusters fairly well, especially if higher metallicity globulars are younger. The models also give a good match to the "fluctuation colors" of elliptical galaxies. In order to obtain theoretical calibrations of the SBF distance indicators, we combine our single-burst models into composite population models. These models reproduce the observed behavior of the SBF magnitudes as a function of stellar population parameters, including the steep colour dependence found for HST/WFPC2 F814W SBF data. Because the theoretical SBF calibrations are fairly sensitive to uncertain details of stellar evolution, the empirical calibrations are more secure. However, the sensitivity of SBF to these finer details potentially makes it a powerful constraint for stellar evolution and population synthesis. [abbridged]Comment: 24 pages with 17 embedded figures. MNRAS, in pres

Simulating CCD images of elliptical galaxies

We introduce a procedure developed by the ``Teramo Stellar Populations Tools'' group (Teramo-SPoT), specifically optimized to obtain realistic simulations of CCD images of elliptical galaxies. Particular attention is devoted to include the Surface Brightness Fluctuation (SBF) signal observed in ellipticals and to simulate the Globular Cluster (GC) system in the galaxy, and the distribution of background galaxies present in real CCD frames. In addition to the physical properties of the simulated objects - galaxy distance and brightness profile, luminosity function of GC and background galaxies, etc. - the tool presented allows the user to set some of the main instrumental properties - FoV, zero point magnitude, exposure time, etc.Comment: Presented at From Stars to Galaxies: Building the Pieces to Build up the Universe (StarGal 2006), Venice, Italy, 16-20 Oct 200

Structural Parameters of the M87 Globular Clusters

We derive structural parameters for ~2000 globular clusters in the giant Virgo elliptical M87 using extremely deep Hubble Space Telescope images in F606W (V) and F814W (I) taken with the ACS/WFC. The cluster scale sizes (half-light radii r_h) and ellipticities are determined from PSF-convolved King-model profile fitting. We find that the r_h distribution closely resembles the inner Milky Way clusters, peaking at r_h~2.5 pc and with virtually no clusters more compact than r_h ~ 1 pc. The metal-poor clusters have on average an r_h 24% larger than the metal-rich ones. The cluster scale size shows a gradual and noticeable increase with galactocentric distance. Clusters are very slightly larger in the bluer waveband V a possible hint that we may be beginning to see the effects of mass segregation within the clusters. We also derived a color magnitude diagram for the M87 globular cluster system which show a striking bimodal distribution.Comment: ApJ accepte