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Galaxy in the constellation Boötes From Wikipedia, the free encyclopedia
NGC 5665 is a spiral galaxy in the northern constellation of Boötes. It was discovered on January 30, 1784 by German-British astronomer William Herschel.[8] This galaxy is located at a distance of 53.6 ± 7.7 million light-years (16.44 ± 2.37 Mpc),[3] and is receding with a heliocentric radial velocity of 2,237 km/s.[3] It is cataloged in Halton Arp's Atlas of Peculiar Galaxies as object number 49.[5]
| NGC 5665 | |
|---|---|
Hubble Space Telescope view of NGC 5665 | |
| Observation data (J2000 epoch) | |
| Constellation | Boötes |
| Right ascension | 14h 32m 25.796s[1] |
| Declination | +08° 04′ 42.43″[1] |
| Redshift | 0.007431±0.000017[2] |
| Heliocentric radial velocity | 2,237 km/s[3] |
| Distance | 53.6 ± 7.7 Mly (16.44 ± 2.37 Mpc)[3] |
| Apparent magnitude (V) | 12.7[4] |
| Apparent magnitude (B) | 12.50[5] |
| Characteristics | |
| Type | SAB(rs)c pec?[6] |
| Mass | 6×1010[5] M☉ |
| Apparent size (V) | 1.653′ × 1.257′[1] |
| Other designations | |
| GC 3923, IRAS F14299+0818, 2MASX J14322579+0804424, NGC 5665, UGC 9352, LEDA 51953, MCG +01-37-024, PGC 51953, CGCG 047.084, VV 412[7] | |
The morphological classification of NGC 5665 is unclear and differs by author.[5] In the De Vaucouleurs system it was classified as SAB(rs)c pec?,[6] which indicates a weakly-barred spiral galaxy (SAB) with a transitional inner ring structure (rs), loosely wound spiral arms (c), and suspected peculiarities (pec?). The galactic plane is inclined at an angle of 53°±5° to the plane of the sky,[3] with the major axis aligned along a position angle of 145°.[5]
Evidence suggests that NGC 5665 underwent a gravitational interaction with another galaxy some 500 million years ago, swallowing a smaller companion.[5] It is somewhat asymmetrical in appearance,[6] retaining a single main spiral arm and the remains of several others. The galaxy is rich in dust and gas with a small bar at the center. There are numerous sites of star formation in the arm that match the age of the interaction.[5] The spectrum of the core is a blend between a LINER and an H II region.[6]
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