NGC 5044 Group is one of the brightest Galaxy Groups in X-rays. Due to its proximity (redshift=0.0087), it has been studied extensively in X-rays and in other wavebands. To trace the Dark Matter (DM) Profile of this interesting group down to the core, the high-resolution Chandra data had been used. However, its field-of-view is limited to the central region (r<100 kpc). To better constrain the DM profile from the core up to a radius of 250 kpc, a Chandra-ROSAT simultaneous analysis had been performed. Within 250 kpc, the total mass is found to be ~1.6 x 1013 solar mass, 12% of which comes from baryons (gas and stars) while 88% presumably comes from dark matter. Within the inner central regions, the total mass profile exhibits a double structure, typical for groups containing a central Dominant (cD) galaxy. The onset of this double structure seems to signify likely interface between stellar-dominated and DM-dominated regimes. For NGC 5044, this interface occur around 7.5 kpc. Beyond this radius, DM dominates the total mass. The DM profile is reasonably fitted with the popular NFW model yielding results consistent with observed scatter expected for Cold Dark Matter (CDM) halos. A Power-law fit to the DM profile gives α=1.88+0.32. This slope is within the observed range, but is significantly larger than that of Low Surface Brightness (LSB) galaxies and self-interacting DM halos. <br />