| NGC 7412 | |
|---|---|
 NGC 7412 by Legacy Surveys | |
| Observation data (J2000epoch) | |
| Constellation | Grus |
| Right ascension | 22h 55m 45.8108s[1] |
| Declination | −42° 38′ 30.718″[1] |
| Redshift | 0.005704 ± 0.000013[1] |
| Heliocentric radial velocity | 1,710 ± 4 km/s[1] |
| Distance | 34.8 ± 15.5Mly (10.7 ± 4.7Mpc)[1] |
| Apparent magnitude (V) | 11.1[2] |
| Characteristics | |
| Type | SAB(s)c[1] |
| Size | ~39,000 ly (12.1 kpc) (estimated)[1] |
| Apparent size (V) | 3.9′ × 2.9′[1] |
| Other designations | |
| ESO 290- G 024, 2252-425,IRAS 22529-4254,MCG -07-47-004,PGC 70027[1] | |
NGC 7412 is aspiral galaxy in the constellationGrus. The galaxy lies about 35 millionlight years away from Earth based on redshift independent methods, which means, given its apparent dimensions, that NGC 7412 is approximately 40,000 light years across.[1] However, based on redshift the galaxy lies about 80 million light years away.[1] It was discovered byJohn Herschel on September 2, 1836.[3]
NGC 7412 is characterised as anintermediate spiral galaxy, meaning it has a weak bar embedded in itsbulge. The bulge is small and lies in a smooth inner disk. The galaxy has two well defined arms in agrand design pattern.[4] The inner part of the north arm appears complex. After about 60° of revolution the arm splits in two, with the higher surface brightness branc being more tightly wound. Both branches can be traced for about a quarter of a revolution. The south arm also splits in two, after about 60° of revolution. The inner branch is of higher surface brightness and can be traced for about 150° of revolution while the outer branch fades after about 60°. Star formation regions are visible at the outer branch.[4] A dust lane runs across the brighter parts of each arm.HII regions are visible, but are smaller than 1.5 arcseconds across.[5] The hydrogen disk of the galaxy extends beyond the optical one. The total hydrogen mass is estimated to be109.46 M☉.[6] The outer regions of the galaxy appear warped, probably due to an interaction with another galaxy. The color of the nucleus indicates it hosts intermediate age stars, without active starburst activity, surrounded by the older stars of the bulge.[7]
NGC 7412 is a member of the IC 5267 Group, also known as LGG 464. Other members of the group includeIC 5267, after which the group is named, IC 5267A, and IC 5267B.[8][9] This group, along with the groups centred aroundIC 1459 andNGC 7582, form the Grus cloud, a region of elevated galaxy density. The Grus cloud, along with the nearby Pavo-Indus cloud, lies between theLocal Supercluster andPavo–Indus Supercluster.[10]
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