Hubble Telescope: What is The forbidden Light

Reading Time: 2 minutesThe forbidden light from the nucleus of the galaxy MCG-01-24-014…

Reading Time: 2 minutes

The forbidden light from the nucleus of the galaxy MCG-01-24-014 refers to specific spectral lines that are not normally allowed based on quantum mechanics.

These forbidden lines indicate the presence of certain elements in a highly excited state, and their occurrence is often associated with the presence of an active galactic nucleus (AGN) at the center of the galaxy.

The forbidden lines arise when electrons in the atoms of the gas surrounding the AGN undergo transitions that are typically prohibited under normal conditions. Studying these forbidden lines provides valuable insights into the energetic processes and conditions near the galactic center, shedding light on the nature and properties of the AGN in MCG-01-24-014.

MCG-01-24-014 exhibits forbidden light from the galactic nucleus. This forbidden light originates from an active galactic nucleus (AGN) in the center of the galaxy, which is part of the intriguing Seyfert Type-2 galaxy class. Seyfert galaxies are characterized by the presence of an AGN, which represents one of the most fascinating and mysterious phenomena in the universe.

Active Galactic Nuclei (AGNs) are among the most enigmatic events in the cosmos. They involve regions located at the centers of galaxies where massive outbursts of energy occur, affecting the brightness in those regions differently from the rest of the galaxy. The primary question is, why does this happen, and how can we study it?

  • The image of MCG-01-24-014, taken by NASA’s Hubble Space Telescope from approximately 275 million light-years away, reveals a bright, active nucleus with two prominent branches extending from a bright core. MCG-01-24-014 is classified as a Type 2 Seyfert galaxy, a designation named after the American astronomer Carl Seyfert, who first discovered their distinctive features. Seyfert galaxies are further divided into Type 1 and Type 2 based on differences in their spectra, particularly in the distribution of intensity at certain wavelengths.

In Type 1 Seyfert galaxies, there is a broad emission line that indicates fast motion of material toward the center. In Type 2 Seyfert galaxies, a narrow emission line suggests that the material is moving more slowly.

Additionally, Type 2 Seyferts exhibit forbidden emission lines, which are lines that, according to quantum physics, should not occur. These forbidden lines indicate the presence of a thin region of gas near the galactic center strongly influenced by energy.

The most likely source of this energy is a supermassive black hole, which surrounds itself with an accretion disk, gas, and dust, creating a torus.

However, not all light emitted from the accretion disk reaches us. In some cases, it is obscured by a dusty torus, a thick, toroidal structure of dust surrounding the center, creating a dense bulge of material.

This torus may only emit energy at specific wavelengths, obscuring the rest of the visible spectrum. The torus’s orientation determines whether we observe the accretion disk and the extended emission lines directly or at an oblique angle.

Therefore, Type 1 and Type 2 Seyfert galaxies likely represent the same phenomenon, but their emission characteristics depend on the orientation of the viewing observer, leading to differences in the observed spectrum. This scenario is known as the Unified AGN model, assuming variations in the orientation of the torus in different Seyfert galaxies.

While the Unified AGN model has gained support through many observations, challenges and uncertainties persist, making AGN research one of the most relevant and captivating fields in astrophysics.

Source : Quora

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