The Fanaroff–Riley classification is a scheme created by B.L. Fanaroff and J.M. Riley in 1974, which is used to distinguish radio galaxies with active nuclei based on their radio luminosity or brightness of their radio emissions in relation to their hosting environment. Fanaroff and Riley noticed that the relative positions high/low surface brightness regions in the lobes of extragalactic radio sources are correlated with their radio luminosity. Their conclusion was based on a set of 57 radio galaxies and quasars that were clearly resolved at 1.4 GHz or 5 GHz into two or more components. Fanaroff and Riley divided this sample into two classes using the ratio of the distance between the regions of highest surface brightness on opposite sides of the central galaxy or quasar to the total exte
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| - Fanaroff–Riley classification (en)
- Classification Fanaroff-Riley (fr)
- Классификация Фанарова — Райли (ru)
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| - La classification Fanaroff-Riley est une classification servant à distinguer les radiogalaxies des galaxies actives selon leur luminosité dans les ondes radio selon leur environnement. Elle a été inventée en 1974 par (en) et (en). (fr)
- The Fanaroff–Riley classification is a scheme created by B.L. Fanaroff and J.M. Riley in 1974, which is used to distinguish radio galaxies with active nuclei based on their radio luminosity or brightness of their radio emissions in relation to their hosting environment. Fanaroff and Riley noticed that the relative positions high/low surface brightness regions in the lobes of extragalactic radio sources are correlated with their radio luminosity. Their conclusion was based on a set of 57 radio galaxies and quasars that were clearly resolved at 1.4 GHz or 5 GHz into two or more components. Fanaroff and Riley divided this sample into two classes using the ratio of the distance between the regions of highest surface brightness on opposite sides of the central galaxy or quasar to the total exte (en)
- Классификация Фанарова — Райли — это классификация радиогалактик, созданная Б. Фанаровым и Ю. Райли в 1974 году и основанная на распределении яркости радиоизлучения по отношению к поверхностной яркости галактики. Фанаров и Райли провели исследование 57 радиогалактик и квазаров, излучение которых чётко регистрировалось на частоте 1,4 ГГц или 5 ГГц. Астрономы смогли разделить их на 2 класса, используя отношение расстояния между областями самой высокой поверхностной яркостью на противоположных сторонах центральной галактики или квазара к общей протяжённости источника. (ru)
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| - The Fanaroff–Riley classification is a scheme created by B.L. Fanaroff and J.M. Riley in 1974, which is used to distinguish radio galaxies with active nuclei based on their radio luminosity or brightness of their radio emissions in relation to their hosting environment. Fanaroff and Riley noticed that the relative positions high/low surface brightness regions in the lobes of extragalactic radio sources are correlated with their radio luminosity. Their conclusion was based on a set of 57 radio galaxies and quasars that were clearly resolved at 1.4 GHz or 5 GHz into two or more components. Fanaroff and Riley divided this sample into two classes using the ratio of the distance between the regions of highest surface brightness on opposite sides of the central galaxy or quasar to the total extent of the source up to the lowest brightness contour. Class I (abbreviated FR-I) are sources whose luminosity decreases as the distance from the central galaxy or quasar host increase, while Class II (FR-II) sources exhibit increasing luminosity in the lobes. This distinction is important because it presents a direct link between the galaxy's luminosity and the way in which energy is transported from the central region and converted to radio emission in the outer parts. (en)
- La classification Fanaroff-Riley est une classification servant à distinguer les radiogalaxies des galaxies actives selon leur luminosité dans les ondes radio selon leur environnement. Elle a été inventée en 1974 par (en) et (en). (fr)
- Классификация Фанарова — Райли — это классификация радиогалактик, созданная Б. Фанаровым и Ю. Райли в 1974 году и основанная на распределении яркости радиоизлучения по отношению к поверхностной яркости галактики. Фанаров и Райли провели исследование 57 радиогалактик и квазаров, излучение которых чётко регистрировалось на частоте 1,4 ГГц или 5 ГГц. Астрономы смогли разделить их на 2 класса, используя отношение расстояния между областями самой высокой поверхностной яркостью на противоположных сторонах центральной галактики или квазара к общей протяжённости источника. Класс I (сокращённо FR-I) — это класс радиоисточников, светимость которых уменьшается с увеличением расстояния от центральной галактики или квазара. Класс II (FR-II) — это класс радиоисточников, светимость которых увеличивается к краям галактики. Это различие важно, потому что оно представляет прямую связь между светимостью галактики и тем, как энергия переносится из центральной области и преобразуется в радиоизлучение во внешних частях. (ru)
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