Astronomy:NGC 7590
| 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] |
| Helio 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, MCG-07-47-030, PGC 71031[1] | |
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]
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]
See also
References
- ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 "NASA/IPAC Extragalactic Database". Results for NGC 7590. https://ned.ipac.caltech.edu/byname?objname=NGC+7590.
- ↑ "Distance Results for NGC 7590". NASA. https://ned.ipac.caltech.edu/cgi-bin/nDistance?name=NGC+7590.
- ↑ "Celestial Atlas Table of Contents, NGC 7550 - 7599" (in en). http://cseligman.com/text/atlas/ngc75a.htm#7590..
- ↑ "NGC 7590". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=NGC+7590.
- ↑ O'Meara 2013, p. 428.
- ↑ Garcia, A. M. (1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series 100: 47. Bibcode: 1993A&AS..100...47G.
- ↑ 7.0 7.1 Freeland, E.; Stilp, A.; Wilcots, E. (1 July 2009). "H I Observations of Five Groups of Galaxies". The Astronomical Journal 138 (1): 295–304. doi:10.1088/0004-6256/138/1/295. Bibcode: 2009AJ....138..295F.
- ↑ Wood, Corey M.; Tremonti, Christy A.; Calzetti, Daniela; Leitherer, Claus; Chisholm, John; Gallagher, John S. (25 July 2015). "Supernova-driven outflows in NGC 7552: a comparison of H α and UV tracers". Monthly Notices of the Royal Astronomical Society 452 (3): 2712–2730. doi:10.1093/mnras/stv1471. Bibcode: 2015MNRAS.452.2712W.
Sources
- O'Meara, S.J. (2013). Deep-Sky Companions: Southern Gems. Cambridge University Press. ISBN 978-1-107-01501-2. https://books.google.com/books?id=S5QIEKns33sC&pg=PA428. Retrieved 2024-11-17.
External links
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