ner_tags: O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O B-Model I-Model O O O O O O O O O O O O O O B-Model O O O O O O O B-Model I-Model O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O
tokens: In the case of ErisMod Low simulation pair the first replacement was made at redshift 1.1 and the last at redshift 0.1. In total, there were four replacement epochs. The final count of high-resolution objects in each of the ErisMod Low runs was 17. The progenitors as well as other halos found in the proximity of the main halo at an epoch of replacement went through a process of selection. If the respective dark matter cloud was found to be monolithic, not elongated, not part of a group of overlapping halos, and with no identifiable satellites, then a high-resolution model will be generated and used as a replacement. This procedure leads to the exclusions of between 40% and 60% of all considered halos at a certain epoch of replacement. Thus, the objects that are replaced are in general more resilient to the tides due to their compactness. The two simulation pairs ErisMod High and ErisMod Low should be seen as complementary since they are both derived from the same simulation ErisDARK and the first epoch of replacement for ErisMod Low starts after the last epoch of replacement in the ErisMod High simulation. Information regarding the orbits, the original virial mass, as well as the redshift of the first pericenter passage for all replaced objects is available in Figure 1 . Figure 1. Dwarf galaxy distances from host ranges for the four ErisMod simulations are plotted as bars. The dwarf galaxy number is sorted by halo mass at infall. At the top of each bar, the marked number (blue color) denotes the pre-infall virial mass of the objects in units of 10 9 M ⊙ . Near the bottom of each bar, the neighboring number (red color) indicates the count of the pericenter passages done by the galaxy until redshift zero. 3. RESULTS For the following analysis we consider subsets of the satellite populations presented in Figure 1 . We are interested in objects that at z = 0 are within 247 kpc of the center of the main halo, namely, inside the virial volume of the host halo. This was done in order to achieve consistency with previous analysis of the TBTF problem from the literature. Moreover, we exclude from analysis all the objects that have lost more than 99% of their mass before redshift zero, as the low number of particles will make the results of the analysis not trustworthy. This class of objects includes galaxies that have lost such a large fraction of their mass that they become irrelevant for the TBTF problem. The circular velocity of the satellites is defined as the function of distance from center: The results are shown in Figures 1 and 2 . In Figure 1 , the profiles of the halos at the epoch of replacement are plotted for comparison. Moreover, in Figure 2 , we have added the estimated circular velocities at the half-light radius available for the MW dSph satellites based on the data compiled by McConnachie ( 2012 ). They are derived from the line of sight velocity dispersion data using the equation:originally proposed by Klypin et al. ( 1999 ) and later