We have obtained deep photometry of NGC 1199 ( in the compact group HCG 22 ) and NGC 6868 ( in the Telescopium loose group ) with the Keck II and the VLT-I telescopes .
Both galaxies are the optically brightest galaxy of their groups .
NGC 1199 has two companion galaxies at a median projected distance of only 33 ~ { } kpc and , based in its peculiar internal structure and large X-ray halo , NGC 6868 has been proposed to be a merger remnant .

Our analysis of B and R images uncovered a population of globular clusters around both galaxies , with total ( and local ) specific frequency S _ { N } = 3.6 \pm 1.8 ( 3.4 \pm 1.5 ) for NGC 1199 and S _ { N } = 1.8 \pm 1.1 ( 0.8 \pm 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 \pm 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 \pm 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 \pm 0.04 and 1.42 \pm 0.04 ( NGC 1199 ) and ( B - R ) _ { 0 } = 1.12 \pm 0.07 and 1.42 \pm 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 .