|Authors||Cristiano Da Rocha1, Claudia Mendes de Oliveira1, Michael Bolte2, Bodo L. Ziegler3 and Thomas H. Puzia4|
|Affiliation||1Instituto de Astronomia, Geofísica e Ciéncias Atmosféricas, Universidade de São Paulo, São Paulo -- SP, Brazil |
2UCO/Lick Observatory, Dept. of Astronomy and Astrophysics, University of California, Santa Cruz, California 9 5064
3Universitätssternwarte Göttingen, Geismarlandstr. 11, 37083 Göttingen, Germany
4Universitätssternwarte München, Scheinerstr. 1, D-81679 M\"unchen, Germany
|Accepted by||Astronomical Journal|
Our analysis of B and R images uncovered a population of globular clusters around both galaxies, with total (and local) specific frequency SN = 3.6 ± 1.8 (3.4 ± 1.5) for NGC 1199 and SN = 1.8 ± 1.1 (0.8 ± 0.4) for NGC 6868. The radial profile of the globulars of NGC 1199 follows the light distribution of the galaxy and can be fitted by a power-law and a ``core model'' with a very steep slope (alpha = 2.5 ± 0.3). In the case of NGC 6868, the profile of the globulars is well fitted by a power-law and a ``core model'' profile of slope 1.4 ± 0.3 and is shallower than the galaxy light distribution. Maximum-likelihood fitting of two Gaussians to the globular cluster color distribution yields a high significance for multi-modality with peaks centered at (B-R)0 = 1.13 ± 0.04 and 1.42 ± 0.04 (NGC 1199) and (B-R)0=1.12 ± 0.07 and 1.42 ± 0.07 (NGC 6868).
NGC 1199 and NGC 6868 are good examples of galaxies where the group environment are likely to have affected their dynamical evolution. We find that for NGC 1199, the properties of the globular cluster system are similar to those for other systems around external elliptical galaxies located in less dense environments, but with a very steep radial profile. In the case of NGC 6868, we find a regular radial profile and color distribution and a comparatively low specific frequency for the globular cluster system of the galaxy.