NGC 1365 is a barred spiral galaxy located in the direction of the Eridanus constellation. Discovered by James Dunlop in the 19th century, the galaxy is approximately 56 million light-years away and is a member of the Eridanus Galaxy Cluster.

^{NGC 1365 (NASA)}

Main Characteristics

NGC 1365 is classified as an SBb-type barred spiral galaxy according to the Hubble classification. This classification indicates the presence of a prominent bar structure extending along the center of the galaxy and two main spiral arms. The visible diameter of the galaxy is approximately 200,000 light-years. Its heliocentric radial velocity is about 1,636 km/s.

Structural Features

The bar structure extending from the center of the galaxy plays a role in directing gas and dust toward the central regions. This structure is associated with central star formation and the feeding of the supermassive black hole located in the core. The spiral arms begin at the ends of the bar and extend outward, and star-forming regions have been observed in these areas. The galaxy’s disk contains clusters of young and hot stars.

Active Galactic Nucleus (AGN) and X-Ray Observations

NGC 1365 hosts a Seyfert Type I active galactic nucleus. A supermassive black hole resides in the core. X-ray observations indicate the accumulation of matter around the core, which can sometimes be obscured by clouds of dust and gas. Observations by ESA’s XMM-Newton and NASA’s Chandra X-ray Observatory have revealed that the X-ray emissions from the core are variable.

Star Formation and Galactic Evolution

There are star formation centers in the gas regions spread along the spiral arms and the bar. Observations in infrared and radio wavelengths indicate the presence of young star clusters and H II regions in these areas. These data show that the galaxy’s star formation process is ongoing.

^{NGC 1365 in Visible and Infrared Light (NASA)}

Galactic Environment and Interactions

NGC 1365 is located within the Fornax-II Galaxy Cluster, which is part of the Eridanus Supercluster. Due to gravitational interactions with surrounding galaxies, asymmetric structures have been observed in the outer regions of the galaxy. These interactions are thought to influence the star formation rate.

Spectral Features and Chemical Composition

Spectral analyses show that metal richness increases near the central bar region and decreases in the outer parts of the spiral arms. This metallicity gradient indicates that earlier generations of stars formed in the inner regions, while younger stellar populations are found in the outer regions.