Tracing the Assembly History of NGC 1395 through its Globular Cluster
  System
  We used deep Gemini-South/GMOS g'r'i'z' images to study the globular cluster
(GC) system of the massive elliptical galaxy NGC 1395, located in the Eridanus
supergroup. The photometric analysis of the GC candidates reveals a clear
colour bimodality distribution, indicating the presence of "blue" and "red" GC
subpopulations. While a negative radial colour gradient is detected in the
projected spatial distribution of the red GCs, the blue GCs display a shallow
colour gradient. The blue GCs also display a remarkable shallow and extended
surface density profile, suggesting a significant accretion of low-mass
satellites in the outer halo of the galaxy. In addition, the slope of the
projected spatial distribution of the blue GCs in the outer regions of the
galaxy, is similar to that of the X-ray halo emission. Integrating up to 165
kpc the profile of the projected spatial distribution of the GCs, we estimated
a total GC population and specific frequency of 6000$\pm$1100 and
$S_N$=7.4$\pm$1.4, respectively. Regarding NGC 1395 itself, the analysis of the
deep Gemini/GMOS images shows a low surface brightness umbrella-like structure
indicating, at least, one recent merger event. Through relations recently
published in the literature, we obtained global parameters, such as
$M_\mathrm{stellar}=9.32\times10^{11}$ M$\odot$ and $M_h=6.46\times10^{13}$
M$\odot$. Using public spectroscopic data, we derive stellar population
parameters of the central region of the galaxy by the full spectral fitting
technique. We have found that, this region, seems to be dominated for an old
stellar population, in contrast to findings of young stellar populations from
the literature.
