La política agraria: objetivos y evolución

Unlike central galaxies, the∆Σprofiles of the satellites galaxies are_notexpected to be mono-

tonically decreasing functions of the separation from the centre. For a single satellite galaxy the profile should become negative at the projected separation from the center of the host halo (Yang et al. 2006). This effect is due to the surface density at the center of the host halo being larger than the mean internal surface density,Σ(rhalo

p,center)>Σ¯(<rphalo,center). At larger separations than the distance to the host halo, the∆Σprofile first increases due to the inclusion of the

center of the host halo in the termΣ(<_rp), before decreasing again at still larger separations.

Stacking the∆Σof satellites in a given stellar mass bin averages out the negative parts of the

profiles since the distances between each satellite and its host halo are different. On the other hand, the increase in the signal at larger radii is preserved by the stacking; the amplitude of the satellite bump can be used as a proxy for the typical mass of the host haloes in which satellites reside.

The left panel of Fig. 5.3 shows the excess surface density as a function of the projected distance from the center of the satellite galaxy. The small scale (rp =0.05h−1Mpc) normal- ization of the∆Σprofile is an increasing function of the stellar mass of the satellite. The three

lowest stellar mass bins show a comparable amplitude of the satellite bump. This similarity can be explained by the fact that the richness cut effectively selects host haloes by mass. In fact, most of the satellites with stellar mass 10 < log10(Mstar[ M_⊙]) < 10.9 reside in host haloes of comparable masses (log10(Mcrit

200[h−1M⊙])≈13.8; see also Table 5.1, column (3)). The prominence of the satellite bump decreases up to log10(Mstar[ M_⊙])=11.2, a trend that is

explained by the fact that the ratio M_subsat/M₂₀₀crit increases from 0.04 to 0.09 in the considered mass range (see Table 5.1, column 6). For higher stellar mass bins, the relative importance of the satellite bump decreases.

The radius at which the excess surface density profile starts to be dominated by the host halo mass (the satellite bump) increases with stellar mass up to log10(Mstar[ M_⊙])=11.2. This

effect is driven by the increasing average distance between satellites and their host haloes raising from ∼ 500h−1kpc to∼ 800h−1kpc in the mass range considered (see table 5.1, column (7)).

The right panel of Fig. 5.3 shows∆Σ for satellite galaxies at a separationr_p=0.05h−1_Mpc (blue continuous curve) and at separationrp=0.5h−1Mpc (blue dashed curve), as a function of stellar mass, normalized by their values in the stellar mass bin 10 <log10(Mstar[ M_⊙]) < 10.3. The mean Msub (black continuous curve) and the host halo mass M₂₀₀crit (black dashed curve) are also shown as a function of stellar mass.

At smaller separations (rp =0.05h−1Mpc), the ESD of satellite galaxies increases with stellar mass. The same trend is shared by the average subhalo mass for satellite galaxies since satellites with higher stellar masses are hosted by more massive dark matter subhaloes. As in the case of central galaxies, the similar dependence on the stellar mass suggests that the amplitude of∆Σ at small separations can be considered a proxy for the subhalo mass hosting

the satellite galaxy.

For larger separations (rp = 0.5h−1Mpc), the∆Σprofile starts to be dominated by the contribution of the halo hosting the satellite galaxy. In this case∆Σshares a similar trend

with stellar mass as the mean host halo mass for satellite galaxies, M₂₀₀crit. The dependence on stellar mass is remarkably similar for both quantities and shows very little variation up to log10(Mstar[ M⊙]) = 10.9 since, as discussed before, the richness cut effectively results in a selection in host halo mass as well. The similar dependence of∆Σwith halo mass at larger

radii highlights the fact that the amplitude of the satellite bump is tightly correlated to the host halo mass. In principle the amplitude of the satellite bump should depend on the satellite’s subhalo mass as well as on the host halo mass. In practice the satellite’s subhalo mass is

Figure 5.3: As in Fig. 5.1 but for satellite galaxies. To ease the comparison in the left panel, the results for the central galaxies are reported with gray curves. In the right panel the value of∆Σ(_rp=0_.5_h−1_{Mpc) is} reported as a function of the stellar mass (blue dashed curve) along with the mean host halo massMcrit₂₀₀ (black dashed curve). The slope of a linear fit of the∆Σvalues at a separation_rp=0_.05_h−1_{Mpc is 0.65} whereas forMsubthe slope is 1.10.

always around∼5% of the host halo mass and therefore it plays a minor role in setting the

amplitude of the satellite bump. We note that the ratioM_sub/Mcrit₂₀₀is often inferred in N-body simulations or in semi-analytical models of infalling satellite galaxies (e.g. van den Bosch et al. 2005; Jiang & van den Bosch 2014) and it has been recently measured via galaxy-galaxy lensing by Sifón et al. (2015) who report values ranging from 0.005 to 0.015, in agreement with our results.

Comparison with observations

Fig. 5.4 shows the comparison between the observed∆Σ profile of satellite galaxies in KiD-

SxGAMA (black squares) and the corresponding signal in the EAGLE simulations (blue curves) for 6 stellar mass bins. For all stellar masses there is good agreement between simula- tion and observation in both the predicted normalization of the ESD profile and in the location and the amplitude of the satellite bump.

For stellar masses 10.6<log10(Mstar[ M_⊙])<10.9 the data show a dip in the∆Σprofile

atrp ∼100h−1kpc that is not present in the simulations. This unreproduced feature can be due to a different radial distribution of satellite galaxies in the simulation and observations. For example, if a large part of the satellites in the observations are located in a very narrow range of distances from their host haloes this can produce a similar dip in the observed signal. On the other hand, it is quite unlikely that satellites of different host haloes are preferentially located at a particular distance from their hosts. The richness is likely to play a role since the dip is less pronounced in the signal computed using the full sample of galaxies without a richness cut (cf. Fig. 5.10). Understanding this feature in the observations would require a comparison of the radial distribution of satellites in both the simulation and observations. We leave this comparison to future work. The amplitude of the signal at small and large radii for this mass bin is well reproduced by the simulation.

Figure 5.4: As in Fig. 5.2 but for satellite galaxies.