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tokens: with mass loadings of . This leads to disks at high redshift with baryon fractions depleted relative to those at low redshift. This feedback effect is clear when a single galaxy, g 1536, is compared to the same galaxy simulated without SNe feedback. As Figure 3 shows, the redshift trend is nearly nonexistent without SNe feedback. Even at z = 2, the galaxy without feedback falls within the scatter of the SPARC observations, and within the scatter of the z = 0 MUGS2 relation. This tells us that we need not invoke feedback processes to explain the z = 0 SPARC RAR. Simple dissipational collapse of gas is sufficient to produce a similar relation. The evolution as a function of redshift is therefore dominated primarily by the stronger effect of feedback at higher redshift. Figure 2. The simulated relation is not constant with redshift. As this figure shows, at higher redshift the low g bar slope is much shallower than at z = 0. This shows that for high-redshift galaxies, their disks can be depleted of baryons compared with z = 0. We have focused on the low g bar end of the relation here, where the changes are most significant. Figure 3. The evolution seen in Figure 2 is primarily driven by feedback. This can be seen when looking at the same galaxy with and without feedback. Without feedback, the baryon fraction within the disk increases slightly from z = 0 to z = 2, but still roughly follows the RAR. At z = 2, strong outflows in the galaxy expel most of the baryons from the disk, flattening the acceleration relation. This effect is sensitive to the frequent merger-driven starbursts at high redshift, which can drive bursty outflows. 4. Discussion This Letter is the first work to show that the RAR’s acceleration scale and tight scatter, as reported by McGaugh et al. ( 2016 ), can arise from fully self-consistent hydrodynamical simulations. Efforts have been made in the past to explain related acceleration relations (the MDAR; the Baryonic Tully–Fisher, BTFR; McGaugh et al. 2000 , etc.) with analytic arguments (van den Bosch Dalcanton 2000 ; Kaplinghat Turner 2002 ), existing scaling relations (Di Cintio Lelli 2016 ), or hydrodynamical simulations (Santos-Santos et al. 2016 ). Analytic studies have found that the MOND-like scaling relations can arise as a consequence of exponential disks living within an NFW halo (van den Bosch Dalcanton 2000 ). van den Bosch Dalcanton ( 2000 ) showed that this can explain not only Tully–Fisher relation’s relatively tight scaling over a large range of masses and surface densities (McGaugh de Blok 1998 ), but even explain the appearance of a characteristic acceleration in disk galaxy rotation curves (McGaugh 1999 ). Subsequent studies have suggested that an even harder constraint for Λ CDM to match is the tight scatter in the MDAR (Wu Kroupa 2015 ) or the RAR (Milgrom 2016 ). A semi-empirical model recently published by Di Cintio Lelli ( 2016 ) showed that both the BTFR and the MDAR can arise as a result of galaxies that