| NGC 266 | |
|---|---|
 NGC 266 is the galaxy in the center-left of this photo. The bright star in the center is SAO 54174. | |
| Observation data (J2000epoch) | |
| Constellation | Pisces |
| Right ascension | 00h 49m 47.81400s[1] |
| Declination | +32° 16′ 39.8067″[1] |
| Redshift | 0.015547[2] |
| Heliocentric radial velocity | 4,565.3±15.3[3] km/s |
| Distance | 197 Mly (60.3 Mpc)[4] |
| Group orcluster | NGC 315 Group |
| Apparent magnitude (V) | 12.54[2] |
| Characteristics | |
| Type | SB(rs)ab[4] |
| Size | 223,150ly (68.45kpc) (estimated)[2] |
| Apparent size (V) | 3.0' × 2.9'[2] |
| Other designations | |
| IRAS 00471+3200,2MASX J00494779+3216398,UGC 508,MCG +05-03-009,PGC 2901,CGCG 501-022[2] | |
NGC 266 is a massive[4]barred spiral galaxy in the constellationPisces. NGC 266 is located at a distance of 197megalight-years from theMilky Way.[4] It was discovered on September 12, 1784, byWilliam Herschel.[5] The form of this barred galaxy is described by itsmorphological classification of SB(rs)ab,[4] which indicates a quasi-ring-like structure (rs) and moderate-to-tightly woundspiral arms (ab).
According to A.M. Garcia, NGC 266 is a member of theNGC 315 Group (also known asLGG 14). This group contains 42 galaxies, includingNGC 226,NGC 243,NGC 262,NGC 311, NGC 315,NGC 338,IC 43,IC 66, ANDIC 69, among others.[6] Also, a 2013 paper lists NGC 266 as the dominant member of a smallgroup with six low-mass galaxies.[4]
NGC 266 is anLINER-typeactive galaxy.[7] It has a moderate star formation rate estimated at2.4 M☉·yr−1.[4] A diffuseX-ray emission from hot gas has been detected around this galaxy, extending out to a radius of at least 70,000 light years. This emission not being driven by winds from astarburst region, so the root cause is unknown.[4]
Onesupernova has been observed in NGC 266. On 5 October 2005,Tim Puckett, Peter Ceravolo, and Yasuo Sano discoveredSN 2005gl (type IIn, mag. 18.2).[8] It was positioned29.8″ east and16.7″ north of the galactic nucleus. An image of the galaxy taken on September 10 showed no supernova event, so this explosion occurred after that date.[9] The progenitor was identified as a massive hypergiant star that was most likely aluminous blue variable.[10]
Media related toNGC 266 at Wikimedia Commons
