2015/09/09 by Daniel Pomarède, Daniel Pomarede, R. Brent Tully +3 · 24 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Disc galaxy #Electrical and Electromagnetic Research #Galactic nuclei #Galaxies: Formation, Evolution, Phenomena #Galaxy #Luminosity #Radio galaxy #Red shift #Stars #astro-ph.CO
paper · pdf · doi:10.1088/0004-637x/812/1/17
published in The Astrophysical Journal 812(1), 17 (IOP Publishing) · Accepted for publication in The Astrophysical Journal. Video can be viewed at http://irfu.cea.fr/arrowhead
arxiv created 2015/09/09 · openalex publication_date 2015/10/05 · arxiv updated 2015/10/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
Superclusters of galaxies can be defined kinematically from local evaluations of the velocity shear tensor. The location where the smallest eigenvalue of the shear is positive and maximal defines the center of a basin of attraction. Velocity and density fields are reconstructed with Wiener Filter techniques. Local velocities due to the density field in a restricted region can be separated from external tidal flows, permitting the identification of boundaries separating inward flows toward a basin of attraction and outward flows. This methodology was used to define the Laniakea Supercluster that includes the Milky Way. Large adjacent structures include Perseus–Pisces, Coma, Hercules, and Shapley but current kinematic data are insufficient to capture their full domains. However, there is a small region trapped between Laniakea, Perseus–Pisces, and Coma that is close enough to be reliably characterized and that satisfies the kinematic definition of a supercluster. Because of its shape, it is given the name the Arrowhead Supercluster. This entity does not contain any major clusters. A characteristic dimension is ∼25 Mpc and the contained mass is only