NGC 4194 | |
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Observation data ( J2000 epoch) | |
Constellation | Ursa Major |
Right ascension | 12h 14m 09.64s [1] |
Declination | +54° 31′ 34.60″ [1] |
Redshift | 0.008433 [2] |
Heliocentric radial velocity | 2,511±12 km/s [3] |
Distance | 128 Mly (39.1 Mpc) [4] |
Apparent magnitude (V) | 13.30 [5] |
Apparent magnitude (B) | 13.79 [5] |
Characteristics | |
Type | Imeger [2] |
Apparent size (V) | 0.14 ′ × 0.13 ′ [6] |
Notable features | Interacting, starburst |
Other designations | |
Medusa galaxy merger, NGC 4194, Arp 160, UGC 7241, Mrk 201, PGC 39068 [7] |
NGC 4194, the Medusa merger, is a galaxy merger in the constellation Ursa Major about 128 million light-years (39.1 Mpc) away. [4] It was discovered on April 2, 1791 by German-British astronomer William Herschel. [8] Due to its disturbed appearance, it is object 160 in Halton Arp's 1966 Atlas of Peculiar Galaxies. [7]
The morphological classification of NGC 4194 is Imeger, [2] indicating an irregular form. This galaxy consists of a brighter central region spanning an angular size 9″ across, with an accompanying system of loops and arcs. Additional material is thinly spread out to a radius of 75″ from the central region. [9] There is a tidal tail and regions undergoing high levels of star formation, making this a starburst galaxy. It is a source for strong infrared and radio emission. [10] [11] These features indicate NGC 4194 is a late-stage galaxy merger. [12] A region of extreme star formation 500 ly (150 pc) across exists in the center of the Eye of Medusa, the central gas-rich region. [13]
Within 1.2 kpc (3.9 kly) of the dynamic center of NGC 4194, star formation is occurring at a rate of 8 M☉·yr−1. The star forming regions in this volume range from 5 to 9 million years in age, with the youngest occurring in areas of the highest star formation rate. [14] As of 2014, no galactic nucleus has been detected based on radio emissions, nor have the respective nuclei of the merger galaxies. [15] However, X-ray emission from a black hole in the tidal tail was detected by Chandra in 2009. [16]
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cite journal}}
: CS1 maint: multiple names: authors list (
link)NGC 4194 | |
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![]() | |
Observation data ( J2000 epoch) | |
Constellation | Ursa Major |
Right ascension | 12h 14m 09.64s [1] |
Declination | +54° 31′ 34.60″ [1] |
Redshift | 0.008433 [2] |
Heliocentric radial velocity | 2,511±12 km/s [3] |
Distance | 128 Mly (39.1 Mpc) [4] |
Apparent magnitude (V) | 13.30 [5] |
Apparent magnitude (B) | 13.79 [5] |
Characteristics | |
Type | Imeger [2] |
Apparent size (V) | 0.14 ′ × 0.13 ′ [6] |
Notable features | Interacting, starburst |
Other designations | |
Medusa galaxy merger, NGC 4194, Arp 160, UGC 7241, Mrk 201, PGC 39068 [7] |
NGC 4194, the Medusa merger, is a galaxy merger in the constellation Ursa Major about 128 million light-years (39.1 Mpc) away. [4] It was discovered on April 2, 1791 by German-British astronomer William Herschel. [8] Due to its disturbed appearance, it is object 160 in Halton Arp's 1966 Atlas of Peculiar Galaxies. [7]
The morphological classification of NGC 4194 is Imeger, [2] indicating an irregular form. This galaxy consists of a brighter central region spanning an angular size 9″ across, with an accompanying system of loops and arcs. Additional material is thinly spread out to a radius of 75″ from the central region. [9] There is a tidal tail and regions undergoing high levels of star formation, making this a starburst galaxy. It is a source for strong infrared and radio emission. [10] [11] These features indicate NGC 4194 is a late-stage galaxy merger. [12] A region of extreme star formation 500 ly (150 pc) across exists in the center of the Eye of Medusa, the central gas-rich region. [13]
Within 1.2 kpc (3.9 kly) of the dynamic center of NGC 4194, star formation is occurring at a rate of 8 M☉·yr−1. The star forming regions in this volume range from 5 to 9 million years in age, with the youngest occurring in areas of the highest star formation rate. [14] As of 2014, no galactic nucleus has been detected based on radio emissions, nor have the respective nuclei of the merger galaxies. [15] However, X-ray emission from a black hole in the tidal tail was detected by Chandra in 2009. [16]
{{
cite journal}}
: CS1 maint: multiple names: authors list (
link)