NGC 7582

Central region

Nuclear region

The nuclear region of NGC 7582 is complex with an estimated total mass of about 3×10⁻³ M_☉. It is highly inclined being at an angle of 58°. The galaxy hosts an active galactic nucleus (AGN) that is driven by biconical ionized outflow. The supermassive black hole at the core has a mass of 5.5+2.6
−1.9×10⁷ M_☉.

Circumnuclear region

Surrounding the nucleus is an circumnuclear star-forming disc with a total mass of around 3×10⁶ M_☉. The disc has a radius of approximately 190-200 parsecs with a asymmetric ring located at a distance of around 30-40 parsecs. Bright emission regions are also seen which are caused by star formation which in turn is powered by a ring of molecular gas. The star formation rate in this galaxy is around 0.23-0.28 solar masses a year. This region is young being around 5 million years old. Temperatures of circumnuclear dust is around 1050 Kelvin at distances closer than 25 parsecs from the nucleus.

It seems that the outflow of gas does not originate from the AGN but instead originates from gas in the circumnuclear region. This gas is being pushed away from the galaxy by outflow from the nuclear region.

Central bar

The central bar of NGC 7582 has a prominent boxy-shaped morphology. The central bar and its box-shaped was discovered in 1997 by Quillen et al. (1997). The study showed that the boxiness of NGC 7582 was prominent even compared to other galaxies with a box-shaped central bar. The bar is dusty and is similar to the central bar of NGC 7552.