SDSS-IV MaNGA: 3D spin alignment of spiral and S0 galaxies

Kraljic, Katarina; Duckworth, Christopher; Tojeiro, Rita; Alam, Shadab; Bizyaev, Dmitry; Weijmans, Anne-Marie; Boardman, Nicholas Fraser; Lane, Richard R.

doi:10.1093/mnras/stab1109

SDSS-IV MaNGA: 3D spin alignment of spiral and S0 galaxies

Journal Article · Wed Apr 21 00:00:00 EDT 2021 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stab1109· OSTI ID:1806348

^[1]; ^[2]; ^[2]; Alam, Shadab ^[3]; ^[4]; Weijmans, Anne-Marie ^[2]; Boardman, Nicholas Fraser ^[5]; Lane, Richard R. ^[6]

Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK, Aix Marseille Université, CNRS, CNES, UMR 7326, Laboratoire d’Astrophysique de Marseille, F-13388 Marseille, France
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK
Aix Marseille Université, CNRS, CNES, UMR 7326, Laboratoire d’Astrophysique de Marseille, F-13388 Marseille, France
Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, NM 88349-0059, USA, Sternberg Astronomical Institute, Moscow State University, 119899 Moscow, Russia
Department of Physics & Astronomy, University of Utah, Salt Lake City, UT 84112, USA
Instituto de Astronomía y Ciencias Planetarias de Atacama, Universidad de Atacama, Copayapu 485, 1531772 Copiapó, Chile, Centro de Investigación en Astronomía, Universidad Bernardo O’Higgins, Avenida Viel 1497, 8370993 Santiago, Chile

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.

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Sponsoring Organization:: USDOE

OSTI ID:: 1806348

Journal Information:: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 3 Vol. 504; ISSN 0035-8711

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United Kingdom

Language:: English

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