5h14m6.7s, −40° 2′48″| NGC 1792 | |
|---|---|
NGC 1792 with the legacy surveys
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| Observation data (J2000 epoch) | |
| Constellation | Columba |
| Right ascension | 05h05m 14.454s[1] |
| Declination | −37° 58′ 50.70″[1] |
| Redshift | 0.004059[2] |
| Heliocentric radial velocity | 1,208[3] |
| Distance | 36.4 Mly (11.17 Mpc)[3] |
| Grouporcluster | NGC 1808[4] |
| Apparent magnitude (V) | 10.18[2] |
| Apparent magnitude (B) | 10.68[2] |
| Characteristics | |
| Type | SA(rs)bc[5] |
| Mass | 0.54×1011[6] M☉ |
| Mass/Light ratio | 3.4[6] M☉/L☉ |
| Other designations | |
| IRAS 05035-3802, NGC 1792, PGC 16709, MCG -6-12-004, ESO 305-6, ESO LV3050060[2] | |
NGC 1792 is a spiral galaxy located in the southern Columba constellation. It was discovered by Scottish astronomer James Dunlop on October 4, 1826. This galaxy is located at a distance of about 36.4 million light-years and is receding from the Milky Way with a heliocentric radial velocity of 1,208 km/s.[3] NGC 1792 is a member of the NGC 1808 cluster of galaxies.[4]
The morphological classification of this galaxy in the de Vaucouleurs system is SA(rs)bc,[5] indicating a spiral galaxy with no central bar (SA), moderately wound arms (bc), and an incomplete ring structure.[5] However, the HyperLEDA classification of SBbc suggests it does have a bar. It has a flocculent appearance with no central bulge.[7] In the B-band, the angular extend of the galaxy spans 7′.5 × 3′.1. The plane of the galaxy is inclined at an angle of 66° to the line of sight from the Earth, with the major axis being aligned along a position angle of 317°.[4]
There is a high level of star formation along the spiral arms at distances of more than 3 kpc from the galactic core, which have led to a number of prominent H II regions. A comparable high level of star formation in the nearby NGC 1808 galaxy may indicate a recent, distant tidal interaction between the two.[8] Radio emission from the neutral hydrogen in the NGC 1792 galaxy shows a pronounced asymmetry, most likely as a result of this interaction. As the galaxy appears only slightly disturbed, this interaction mainly impacted the outer parts of the galaxy.[4]
The star formation rate in NGC 1792 is estimated to be 11.0 M☉·yr−1.[6] Soft x-ray emission has been detected, the majority of which may be coming from X-ray binaries.[9]
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http://www.skyfactory.org/deepskycatalogue/db_list.asp?q=(Name~contains~NGC1792)
