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tokens: (Dubois et al. 2014 ; Codis et al. 2018 ; Wang et al. 2018 ; Ganeshaiah Veena et al. 2019 ; Kraljic, Davé Pichon 2020b ). The mass dependence of the spin alignment signal is however debated. While some works confirmed the existence of a galaxy spin transition from parallel to perpendicular with respect to the filament’s direction (Dubois et al. 2014 ; Codis et al. 2018 ; Kraljic et al. 2020b ), and analogously with respect to walls (Codis et al. 2018 ; Kraljic et al. 2020b ), others (Ganeshaiah Veena et al. 2019 ; Krolewski et al. 2019 ) found preferential perpendicular orientation with respect to filaments at all masses with no sign of a spin transition. A possible interpretation of this lack of detection of a clear transition is the nature of the filaments, with galaxies in thinner filaments having their spins more likely perpendicular to the filament’s axis, compared to galaxies of similar mass in thicker filaments (Ganeshaiah Veena et al. 2019 ). This can be in turn understood recalling the multiscale nature of the problem and the conditional TTT (Codis et al. 2015 ) predicting larger transition mass for denser, thus thicker, filaments. Further support for this interpretation was provided by the findings of stronger impact of large-scale tides on the galaxy spin orientation in denser filaments (Kraljic et al. 2020b , using filament density as a proxy for the thickness of filaments). In addition to the stellar mass, the spin-filament alignment was shown to depend on other internal properties of galaxies. Blue or rotation-supported galaxies were found to dominate the alignment signal at low stellar mass, while red or dispersion-dominated galaxies tend to show a preferential perpendicular alignment (Codis et al. 2018 ; Wang et al. 2018 ; Kraljic et al. 2020b ). The orientation of the galaxies’ spin with respect to their large-scale environment has been quite extensively studied also on the observational side. When focusing on disc galaxies, some groups find preferentially parallel orientation for spirals (Tempel Libeskind 2013 ; Tempel, Stoica Saar 2013 ), Scd types (Hirv et al. 2017 ), or both red and blue galaxies (Zhang et al. 2013 ). Others report a tendency for a perpendicular orientation for spirals (Lee Erdogdu 2007 ; Jones, van de Weygaert Aragón-Calvo 2010 ; Zhang et al. 2015 ) and Sab galaxies (Hirv et al. 2017 ), or no evidence for a clear signal (Pahwa et al. 2016 ; Krolewski et al. 2019 ). A much better agreement seems to exist for elliptical/S0 galaxies, for which a preferential orthogonal orientation of their spin (or minor axis) with respect to their host filaments is found (Tempel et al. 2013 ; Pahwa et al. 2016 ), in agreement with with results of shape measurements (e.g. Okumura Jing 2009 ; Joachimi et al. 2011 ; Singh, Mandelbaum More 2015 ; Chen et al. 2019 ; Johnston et al. 2019 ). More recently, Welker et al. ( 2020 ) studied the alignment of galactic spin in projection with respect to the filaments of the cosmic