A galaxy is a massive, gravitationally bound system that consists of stars, stellar remnants, interstellar gas, dust, dark matter, and an important but poorly understood component tentatively dubbed dark energy. The word galaxy is derived from the Greek galaxias (γαλαξίας), literally "milky", a reference to the Milky Way galaxy.
There are three main types of galaxies: elliptical, spiral, and irregular. Each of these types is further divided into subcategories based on their specific characteristics.
Elliptical galaxies are shaped like ellipsoids and have a smooth, featureless appearance. They are categorized by their elongation, ranging from nearly spherical to highly elongated. Elliptical galaxies are composed mainly of older, low-mass stars and contain very little interstellar matter.
Spiral galaxies are characterized by their spiral arms, which contain a mix of population I and population II stars, as well as a significant amount of interstellar matter. The Milky Way is a prime example of a spiral galaxy.
Irregular galaxies do not have a distinct regular shape and do not fit into the classification of elliptical or spiral galaxies. They often contain large amounts of interstellar matter and are sites of active star formation.
A typical galaxy consists of a central bulge, a disk, and a halo. The central bulge contains older stars and is surrounded by a flattened disk where star formation occurs. The halo contains globular clusters and extends beyond the main body of the galaxy.
Galaxies evolve over time through interactions with other galaxies, star formation, and the accretion of intergalactic gas. Understanding the processes of galactic evolution helps scientists comprehend the formation and development of different types of galaxies.
Scientists study galaxies using various tools and techniques, such as telescopes, spectroscopy, and computer simulations. By analyzing the light emitted by galaxies, researchers can determine their composition, distance, and motion.