Messier 60 Galaxy is an elliptical-type galaxy located in the direction of the Virgo constellation. Discovered on April 15, 1779, by Johann Gottfried Koehler, the celestial object was also independently observed the same year by Charles Messier and included in the Messier Catalog as number 60. M60 is one of the giant elliptical galaxies in the Virgo Cluster and attracts the attention of the scientific community with its structural features, particularly its mass, size, and the supermassive black hole at its center.
Messier 60 Galaxy (NASA)
Location and Observability
M60 is located approximately 55 million light-years (17 megaparsecs) from Earth. It can be observed with a telescope from the northern hemisphere during the spring months. Its coordinates are as follows:
- Right Ascension (RA): 12h 43m 40.0s
- Declination (Dec): +11° 33′ 10″
- Galactic Longitude: 287.43°
- Galactic Latitude: +71.17°
Its apparent brightness is about +8.8 magnitude and can be studied in detail with large telescopes.
Morphological and Physical Characteristics
Messier 60 is classified as an E2-type elliptical galaxy. This classification refers to the degree of elongation of the galaxy from the center outward. An E2 type indicates a slightly elliptical, nearly circular galaxy shape.
The diameter of M60 is estimated to be about 120,000 light-years. This size is comparable to the Milky Way Galaxy. However, it has a more compact structure in terms of stellar density. The total mass of the galaxy is approximately 10¹² solar masses (M☉). A significant portion of this mass is composed of dark matter.
M60 is a typical elliptical galaxy dominated by an old stellar population. New star formation is quite low. This is due to the low amounts of gas and dust in the galaxy. Observations show that the galaxy is mostly composed of red giants and old non-main sequence stars.
Messier 60 Galaxy (NASA)
Structural Features
Central Supermassive Black Hole
The supermassive black hole at the center of M60 is estimated to have a mass of approximately 4.5 billion solar masses (M☉). This value is near the upper limit of typical supermassive black hole masses in galaxies. The existence of the black hole has been inferred indirectly through the motion of surrounding stars.
Globular Cluster System
M60 hosts thousands of globular star clusters. It is estimated to contain between 5,000 and 6,000 globular clusters. This number is several times greater than the number of globular clusters in the Milky Way. These globular clusters provide information about the formation and evolution of the galaxy.
X-ray and Radio Emissions
Observations made by the Chandra X-ray Observatory and other space telescopes have shown strong X-ray emissions at the center of M60. These emissions are caused by both the activity of the supermassive black hole and the hot gases present in the interstellar medium. Additionally, low-level radio frequency emissions have also been detected.
Companion Galaxy: NGC 4647
Messier 60 is located close to the spiral galaxy NGC 4647. Although the two galaxies appear close together in the sky, it is not yet fully agreed upon whether they are interacting. However, some observations suggest signs of gravitational interaction between the two galaxies.
Astrophysical Significance
M60 is one of the example galaxies studied in search of answers to various astrophysical questions concerning the formation and evolution of large structures in the universe, due to its large mass, central black hole, globular cluster system, and its position within the Virgo Cluster. It holds particular scientific importance in terms of supermassive black hole formation and the consequences of galactic mergers. Due to its contribution to the dynamic structure of the Virgo Cluster, it is also considered a reference in cosmological studies.
