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--- courses:ast403:unified-model [2026/03/07 21:00] – shuvo
+++ courses:ast403:unified-model [2026/03/07 22:00] (current) – [Observational Evidence for Unification] shuvo
@@ Line 4: / Line 4: @@
 The unified model of Active Galactic Nuclei (AGNs) proposes that the diverse observational classifications of active galaxies—such as Seyfert galaxies, quasars, radio galaxies, and blazars—are fundamentally the same type of physical system viewed from different orientations. This model explains the variety of observed spectra and luminosities as a result of geometric and projection effects rather than intrinsic physical differences between the objects.
-**Core Components of the Model**
+===== Core Components of the Model =====
 The unified model consists of several key physical structures powered by a central supermassive black hole (SMBH).
@@ Line 17: / Line 17: @@
 *   **Relativistic Jets:** In some AGNs, highly collimated beams of plasma are ejected at near-light speeds along the rotation axis of the accretion disk.
-**Classification by Orientation**
+[{{ :courses:ast403:agn_unified.jpg?600 | Fig 1: A sketch of a unified model of an active galactic nucleus. The jets would be present in a radio-loud AGN. A typical observer’s point of view is indicated for AGNs of various types.}}]
+===== Classification by Orientation =====
 According to the unified scheme, the specific type of AGN observed depends on the angle between the line of sight and the axis of the accretion disk.
-//Type 1 AGNs (Seyfert 1s and Quasars):// These are seen from a direction closer to the symmetry axis of the disk. In this orientation, the observer has a **direct view** of the central continuum source and the fast-moving clouds in the **Broad-Line Region**.
+**Type 1 AGNs (Seyfert 1s and Quasars):** These are seen from a direction closer to the symmetry axis of the disk. In this orientation, the observer has a **direct view** of the central continuum source and the fast-moving clouds in the **Broad-Line Region**.
-//Type 2 AGNs (Seyfert 2s and Narrow-Line Radio Galaxies):// These are viewed from a large angle, close to the equatorial plane of the disk. The **obscuring torus** blocks the view of the central engine and the BLR, leaving only the more distant **Narrow-Line Region** visible.
+**Type 2 AGNs (Seyfert 2s and Narrow-Line Radio Galaxies):** These are viewed from a large angle, close to the equatorial plane of the disk. The **obscuring torus** blocks the view of the central engine and the BLR, leaving only the more distant **Narrow-Line Region** visible.
-//Blazars:// These are AGNs where the observer is looking directly down the axis of a relativistic jet. Because of relativistic beaming (Doppler favoritism), the jet's radiation is enormously amplified, often outshining the rest of the galaxy and the emission lines.
+**Blazars:** These are AGNs where the observer is looking directly down the axis of a relativistic jet. Because of relativistic beaming (Doppler favoritism), the jet's radiation is enormously amplified, often outshining the rest of the galaxy and the emission lines.
-**Observational Evidence for Unification**
+===== Observational Evidence for Unification =====
 Several key discoveries support the validity of the unified model:
-**Hidden Broad Lines in Polarized Light: Observations of the Seyfert 2 galaxy NGC 1068 in polarized light revealed broad emission lines that are invisible in total flux. This indicates that a BLR exists but is obscured; its light is only visible when **reflected (and thus polarized)** by dust or electrons into our line of sight.
+**Hidden Broad Lines in Polarized Light:** Observations of the Seyfert 2 galaxy NGC 1068 in polarized light revealed broad emission lines that are invisible in total flux. This indicates that a BLR exists but is obscured; its light is only visible when reflected (and thus polarized) by dust or electrons into our line of sight.
 **Ionization Cones:** High-resolution images of the NLR in Seyfert 2 galaxies often reveal cone-shaped regions of ionized gas. This suggests that the ionizing radiation from the nucleus is not emitted isotropically but is instead channeled into cones by the obscuring torus.
-**X-ray Absorption:** Type 2 AGNs typically show significantly higher levels of **intrinsic X-ray absorption** than Type 1 AGNs. This is consistent with the line of sight passing through the dense material of the torus.
+**X-ray Absorption:** Type 2 AGNs typically show significantly higher levels of intrinsic X-ray absorption than Type 1 AGNs. This is consistent with the line of sight passing through the dense material of the torus.
 **Relativistic Beaming:** The fact that jets are frequently observed to be one-sided is explained by beaming; the jet approaching the observer is brightened by a factor of thousands, while the receding counter-jet is dimmed by the same factor.
+[{{ :courses:ast403:agn_hst.jpg?600 | Fig 2: Two views of NGC 4261. Left: a composite optical and radio image from the ground, showing the radio jets. Right: an optical image from the HST , showing the dusty torus around the nucleus. (Courtesy of NASA.)}}]