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At fixed stellar mass, satellite galaxies show higher passive fractions thancentrals, suggesting that environment is directly quenching their starformation. Here, we investigate whether satellite quenching is accompanied bychanges in stellar spin (quantified by the ratio of the rotational todispersion velocity V/$\sigma$) for a sample of massive ($M_{*}>$10$^{10}$M$_{\odot}$) satellite galaxies extracted from the SAMI Galaxy Survey. Thesesystems are carefully matched to a control sample of main sequence, high$V/\sigma$ central galaxies. As expected, at fixed stellar mass andellipticity, satellites have lower star formation rate (SFR) and spin than thecontrol centrals. However, most of the difference is in SFR, whereas the spindecreases significantly only for satellites that have already reached the redsequence. We perform a similar analysis for galaxies in the EAGLEhydro-dynamical simulation and recover differences in both SFR and spin similarto those observed in SAMI. However, when EAGLE satellites are matched to their`true' central progenitors, the change in spin is further reduced and galaxiesmainly show a decrease in SFR during their satellite phase. The difference inspin observed between satellites and centrals at $z\sim$0 is primarily due tothe fact that satellites do not grow their angular momentum as fast as centralsafter accreting into bigger halos, not to a reduction of $V/\sigma$ due toenvironmental effects. Our findings highlight the effect of progenitor bias inour understanding of galaxy transformation and they suggest that satellitesundergo little structural change before and during their quenching phase.

The SAMI Galaxy Survey: Satellite galaxies undergo little structural change during their quenching phase