The observed properties of dwarf galaxies in and around the Local Group

TL;DR

This paper compiles and discusses detailed observational data on over 100 dwarf galaxies within 3Mpc of the Sun, covering their properties, environments, and implications for galaxy formation and evolution.

Contribution

It provides a comprehensive, homogenized dataset of dwarf galaxy parameters in the Local Group, including new insights into their morphological diversity and scaling relations.

Findings

Dwarf galaxies exhibit a wide range of morphologies and properties.

Scaling relations and metallicity trends are characterized for the sample.

Evidence suggests a possible floor in central surface brightness at faint magnitudes.

Abstract

Positional, structural and dynamical parameters for all dwarf galaxies in and around the Local Group are presented, and various aspects of our observational understanding of this volume-limited sample are discussed. Over 100 nearby galaxies that have distance estimates placing them within 3Mpc of the Sun are identified. This distance threshold samples dwarfs in a large range of environments, from the satellite systems of the MW and M31, to the dwarfs in the outer regions of the Local Group, to the numerous isolated galaxies found in its surroundings. It extends to, but does not include, the galaxies associated with the next nearest groups. Our basic knowledge of this important galactic subset and their resolved stellar populations will continue to improve dramatically over the coming years with existing and future observational capabilities, and they will continue to provide the most detailed information available on numerous aspects of dwarf galaxy formation and evolution. Basic observational parameters, such as distances, velocities, magnitudes, mean metallicities, as well as structural and dynamical characteristics, are collated, homogenized (as far as possible), and presented in tables that will be continually updated to provide a convenient and current on-line resource. As well as discussing the provenance of the tabulated values and uncertainties affecting their usage, the membership and spatial extent of the MW and M31 subgroups and the Local Group are explored. The morphological diversity of the entire sample and sub-groups is discussed, and time-scales are derived for the Local Group members in the context of their orbital histories. The scaling relations and mean stellar metallicity trends defined by the dwarfs are presented, and the origin of a possible floor in central surface brightness (and, more speculatively, stellar mean metallicity) at faint magnitudes is considered.