Abstract
ABSTRACT We investigate the 3D spin alignment of galaxies with respect to the large-scale filaments using the MaNGA survey. The cosmic web is reconstructed from the Sloan Digital Sky Survey using disperse and the 3D spins of MaNGA galaxies are estimated using the thin disc approximation with integral field spectroscopy kinematics. Late-type spiral galaxies are found to have their spins parallel to the closest filament’s axis. The alignment signal is found to be dominated by low-mass spirals. Spins of S0-type galaxies tend to be oriented preferentially in perpendicular direction with respect to the filament’s axis. This orthogonal orientation is found to be dominated by S0s that show a notable misalignment between their kinematic components of stellar and ionized gas velocity fields and/or by low-mass S0s with lower rotation support compared to their high-mass counterparts. Qualitatively similar results are obtained when splitting galaxies based on the degree of ordered stellar rotation, such that galaxies with high spin magnitude have their spin aligned, and those with low spin magnitude in perpendicular direction to the filaments. In the context of conditional tidal torque theory, these findings suggest that galaxies’ spins retain memory of their larger scale environment. In agreement with measurements from hydrodynamical cosmological simulations, the measured signal at low redshift is weak, yet statistically significant. The dependence of the spin-filament orientation of galaxies on their stellar mass, morphology, and kinematics highlights the importance of sample selection to detect the signal.
Highlights
UNL Angular momentum of galaxies is one of the key ingredients to understand their morphological diversity
The misalignment between the tidal and the R inertia tensors constrained to the vicinity of filament-type saddle Opoints implies a spin aligned with filaments for low mass halos, and a perpendicular spin orientation for more massive halos, in agreement with findings from cosmological N-body simulations (e.g. Aragón-Calvo et al 2007; Hahn et al 2007; Codis et al 2012; Trowland et al 2013; Wang & Kang 2017; Ganeshaiah Veena et al 2018)
Results are broadly in agreement with the trends seen in hydrodynamical simulations (Codis et al 2018; Kraljic et al 2020b) showing that at fixed stellar mass the alignment signal is dominated by galaxies with high v/σ, while the perpendicular orientation is mostly dominated by galaxies with low values of v/σ
Summary
L Angular momentum of galaxies is one of the key ingredients to understand their morphological diversity. The misalignment between the tidal and the R inertia tensors constrained to the vicinity of filament-type saddle Opoints implies a spin aligned with filaments for low mass halos, and a perpendicular spin orientation for more massive halos, in agreement with findings from cosmological N-body simulations (e.g. Aragón-Calvo et al 2007; Hahn et al 2007; Codis et al 2012; Trowland et al 2013; Wang & Kang 2017; Ganeshaiah Veena et al 2018). Galaxies seem to retain a memory of their spin orientation with respect to the cosmic web filaments and walls, as suggested by the results from large-scale cosmological hydrodynamical simulations (Dubois et al 2014; Codis et al 2018; Wang et al 2018; Ganeshaiah Veena et al 2019; Kraljic et al 2020b). 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 galax-
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