A New Method to Constrain the Appearance and Disappearance of Observed Jellyfish Galaxy Tails

We present a new approach to observationally constrain where the tails of Jellyfish (JF) galaxies in groups and clusters first appear how long they remain visible with respect moment their orbital pericenter. This is accomplished by measuring distribution tail directions host's center, projected velocity-radius phase-diagram. then model these observed distributions using fast flexible JF are painted onto dark matter halos according simple parameterised prescription, perform Bayesian analysis estimate parameters. demonstrate effectiveness our observational mocks, apply it known sample 106 radio continuum located inside 68 hosts such as clusters. find that, typically, become on infall when galaxy reaches roughly three quarters r$_{200}$, for few hundred Myr after pericenter passage. Lower mass more massive tend form further out disappear quickly argue that this indicates sensitive ram pressure stripping. With upcoming large area surveys progress, promising method environmental conditions which exist.