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-Our final calibration sample (81 galaxies, plus VCC 21; see text) is shown, together with the fitted relations. Elliptical galaxies are represented by open squares, S0 by open triangles, dwarf ellipticals by filled squares, and dwarfs S0 by filled triangles. The straight line is the fit to the full sample, while the thick continuous lines are, respectively, fits for the red and blue ends. At the top left, the typical SBF magnitude error (0.12 mag, including the uncertainty due to the Virgo cluster depth and intrinsic SBF dispersion) is shown.

-Our final calibration sample (81 galaxies, plus VCC 21; see text) is shown, together with the fitted relations. Elliptical galaxies are represented by open squares, S0 by open triangles, dwarf ellipticals by filled squares, and dwarfs S0 by filled triangles. The straight line is the fit to the full sample, while the thick continuous lines are, respectively, fits for the red and blue ends. At the top left, the typical SBF magnitude error (0.12 mag, including the uncertainty due to the Virgo cluster depth and intrinsic SBF dispersion) is shown.

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Fig. 1.-The fit of total external source counts as a function of...
Fig. 2.— Our SBF galaxy sample (85 galaxies) is shown. Elliptical...
Fig. 3.-Our final calibration sample (81 galaxies, plus VCC 21; see...
The ACS Virgo Cluster Survey V: SBF Calibration for Giant and Dwarf Early-type Galaxies
Article
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  • Jun 2005
As part of the Advanced Camera for Survey (ACS) Virgo Cluster Survey, we have measured Surface Brightness Fluctuations (SBF) in a sample of 100 early-type Virgo galaxies. Distances derived from these measurements are needed to explore the three-dimensional structure of the Virgo Cluster, study the intrinsic parameters of globular clusters associate...
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... Fig. 3 our final galaxy sample and an overall fit (the continuous straight line) are shown. Both uncertainties on magnitude and color have been included in the fit χ 2 estima- tion. We ...

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