| NGC 3226 | |
|---|---|
 NGC 3227 (left) and NGC 3226 (right) | |
| Observation data (J2000epoch) | |
| Constellation | Leo |
| Right ascension | 10h 23m 27.0s[1] |
| Declination | +19° 53′ 55″[1] |
| Redshift | 1151 ± 10 km/s[1] |
| Apparent magnitude (V) | 12.3[1] |
| Characteristics | |
| Type | E2 pec[1] |
| Apparent size (V) | 3.2′ × 2.8′[1] |
| Other designations | |
| HOLM 187B,Arp 94,UGC 5617,MCG +03-27-015,PGC 30440,CGCG 094-026,VV 209b[1] | |
NGC 3226 is adwarf elliptical galaxy that is interacting with thespiral galaxyNGC 3227. They were both discovered byGerman-British astronomerWilliam Herschel on 15 February 1784.[2] The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in theAtlas of Peculiar Galaxies.[3] Both galaxies may be found in theconstellationLeo. It is a member of theNGC 3227 Group of galaxies, which is a member of theLeo II Groups, a series of galaxies andgalaxy clusters strung out from the right edge of theVirgo Supercluster.[4]
Onesupernova has been observed in NGC 3226: SN 1976K (type unknown, mag. 17) was discovered byArnold Klemola on 21 December 1976.[5][6]
NGC 3226 contains alow-ionization nuclear emission-line region (LINER), a type of region that is characterized byspectral line emission from weaklyionized atoms.[7] In general, the energy source for LINER emission has been a subject of debate among astronomers. Some astronomers have asserted that LINERs are powered bystar formation regions, while other have asserted that LINERs are powered byactive galactic nuclei (AGN) which containsupermassive black holes.
The nucleus of NGC 3226 appears to contain an AGN. The nucleus is a strong source of bothradio[8][9] andX-ray[10] emission that appears to besynchrotron emission, which is generated whenelectrons moving at high speeds oscillate withinmagnetic fields. Such synchrotron emission is expected from the environment around asupermassive black hole. TheX-ray emission may also be variable, which is also expected in the environment of a supermassive black hole.[10]
It is possible that NGC 3226 may be acquiring gas from NGC 3227 during the interaction process, which would enhancestar formation within NGC 3226. However, millimeter observations of NGC 3226 failed to detect any molecular gas within the galaxy. These results not only demonstrate that NGC 3226 contains little molecular gas but also demonstrate that the galaxy has acquired no gas from NGC 3227.[11]
