NGC 7590
Galaxy in the constellation Grus
From Wikipedia, the free encyclopedia
NGC 7590 is a spiral galaxy in the constellation Grus. This galaxy is in the upper middle west part of the Virgo Supercluster.[1] Its velocity with respect to the cosmic microwave background is 1333 ± 18 km/s, which corresponds to a Hubble distance of 64.1 ± 4.6 Mly (19.66 ± 1.40 Mpc).[1] However, 12 non-redshift measurements give a distance of 84.50 ± 3.99 Mly (25.908 ± 1.222 Mpc).[2] NGC 7590 was discovered by Scottish astronomer James Dunlop on 14 July 1826.[3]
| NGC 7590 | |
|---|---|
NGC 7590 is on the right | |
| Observation data (J2000 epoch) | |
| Constellation | Grus |
| Right ascension | 23h 18m 54.827s.[1] |
| Declination | −42° 14′ 20.574″[1] |
| Redshift | 0.005255[1] |
| Heliocentric radial velocity | 1575 ± 5 km/s[1] |
| Distance | 84.5 ± 3.986 Mly (25.908 ± 1.222 Mpc)[1] |
| Group or cluster | Grus Quartet |
| Apparent magnitude (V) | 11.37[1] |
| Characteristics | |
| Type | SA(rs)bc?[1] |
| Size | ~83,700 ly (25.65 kpc) (estimated)[1] |
| Apparent size (V) | 5.0′ × 2.1′[1] |
| Other designations | |
| ESO 347- G 033, IRAS 23161-4230, 2MASX J23185483-4214206, MCG -07-47-030, PGC 71031[1] | |
The SIMBAD database lists NGC 7590 as a Seyfert I Galaxy, i.e. it has a quasar-like nucleus with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, the host galaxy is clearly detectable.[4] While the neighboring NGC 7599 is marginally brighter, NGC 7590 is easier to identify due to its bright Seyfert core and an adjacent star of 13th magnitude.[5]
Galaxy groups
According to A. M. Garcia, NGC 7590 is a member of the NGC 7582 group (also known as LGG 472). This group of galaxies contains at least 9 members. The other galaxies are NGC 7496, NGC 7531, NGC 7552, NGC 7582, NGC 7599, NGC 7632, IC 5325, and ESO 291-24.[6]
NGC 7590 also belongs a group known as the Grus quartet. Other members of the group include the spiral galaxies NGC 7552, NGC 7582, and NGC 7599.[7] A large tidal extension of HI reaches from NGC 7582 to NGC 7552, which is indicative of interactions between the group members,[7] yet NGC 7552 does not have highly disturbed morphology.[8]
