Globular Cluster Luminosity Functions and the Hubble Constant from WFPC2 Imaging: The Dominant Group Elliptical NGC 5846

Details Globular Cluster Luminosity Functions and the Hubble Constant from WFPC2 Imaging: The Dominant Group Elliptical NGC 5846 Globular Cluster Luminosity Functions and the Hubble Constant from WFPC2 Imaging: The Dominant Group Elliptical NGC 5846

1996-11-18

arxiv.org/abs/astro-ph/9611141v1

Astronomy and Astrophysics

Astrophysics

12 pages, Plate 1 in JPEG format, Latex, full paper also available at http://www.ucolick.org/~forbes/home.html

Scientific paper

10.1086/118194

The HST's WFPC2 has several advantages over ground--based observations for the study of globular cluster luminosity functions (GCLFs) and distance determination. Here we present WFPC2 data on the globular clusters associated with NGC 5846. This giant elliptical is the dominant galaxy in a small, compact group located ~ 13 Mpc beyond the Virgo cluster. We have detected over 1200 globular clusters in three (central, north and south) separate pointings. The luminosity function in each of these pointings are statistically the same, indicating that the mean luminosity (mass) does not vary between ~ 3 and 30 kpc from the galaxy center. This suggests that dynamical friction and bulge shocking destruction processes are insignificant. We have fit a Gaussian and t_5 profile to the GCLF (of the combined pointings) and find that it is well represented by a turnover magnitude of m^0_V = 25.05 +/- 0.10 and a dispersion of sigma = 1.34 +/- 0.06. Our 50% completeness level is ~ 1 mag fainter than the turnover. After applying a metallicity correction to the `universal' GCLF turnover magnitude, we derive a distance modulus of (m--M) = 32.32 +/- 0.23. For a group velocity V_{CMB} = 1883 +/- 28 km/s, the Hubble constant is H_o = 65 +/- 8 km/s/Mpc.

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