The Arrowhead Mini-Supercluster of Galaxies

Abstract

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 ~10^15 Msun.

Accepted for publication in The Astrophysical Journal. Video can be viewed at http://irfu.cea.fr/arrowhead

References in corpus (4)

• The Laniakea supercluster of galaxies
• Galaxy Groups: A 2MASS Catalog
• Cosmic Bulk Flow and the Local Motion from Cosmicflows-2
• Midlife Crises in Dwarf Galaxies in the NGC 5353/4 Group

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• Identification of Basins of Attraction in the Local Universe
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• Does the Corona Borealis Supercluster form a giant binary-like system?
• Galaxy Superclusters and Their Complexes in the Cosmic Web
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