NGC 1792

NGC 1792
NGC 1792
	NGC 1792 with the legacy surveys
Observation data (J2000 epoch)
Constellation	Columba
Right ascension	05h 05m 14.454s
Declination	−37° 58′ 50.70″
Redshift	0.004059
Heliocentric radial velocity	1,208
Distance	36.4 Mly (11.17 Mpc)
Group or cluster	NGC 1808
Apparent magnitude (V)	10.18
Apparent magnitude (B)	10.68
Characteristics
Type	SA(rs)bc
Mass	0.54×1011 M☉
Mass/Light ratio	3.4 M☉/L☉
Other designations
	IRAS 05035-3802, NGC 1792, PGC 16709, MCG -6-12-004, ESO 305-6, ESO LV3050060

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]

References

^ ^a ^b Skrutskie, Michael F.; et al. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi:10.1086/498708. ISSN 0004-6256. S2CID 18913331.
^ ^a ^b ^c ^d "NGC 1792". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-12.
^ ^a ^b ^c Tully, R. Brent; et al. (2016). "Cosmicflows-3". The Astronomical Journal. 152 (2): 21. arXiv:1605.01765. Bibcode:2016AJ....152...50T. doi:10.3847/0004-6256/152/2/50. S2CID 250737862. 50.
^ ^a ^b ^c ^d Dahlem, M. (October 1992). "NGC 1792 : surprising radio properties". Astronomy and Astrophysics. 264: 483–488. Bibcode:1992A&A...264..483D.
^ ^a ^b ^c de Vaucouleurs, G.; et al. (1991). "Third reference catalogue of bright galaxies". 9. New York: Springer-Verlag. {{cite journal}}: Cite journal requires |journal= (help)
^ ^a ^b ^c Dahlem, M.; et al. (July 2001). "A search for intergalactic H I gas in the NGC 1808 group of galaxies". Astronomy and Astrophysics. 373 (2): 485–493. arXiv:astro-ph/0106050. Bibcode:2001A&A...373..485D. doi:10.1051/0004-6361:20010614. S2CID 15512721.
^ Marino, A.; et al. (February 2010). "Galaxy evolution in Local Group analogs. I. A GALEX study of nearby groups dominated by late-type galaxies". Astronomy and Astrophysics. 511: 18. arXiv:0912.4266. Bibcode:2010A&A...511A..29M. doi:10.1051/0004-6361/200913216. S2CID 119113397. A29.
^ Dahlem, M.; et al. (July 2001). "A search for intergalactic H I gas in the NGC 1808 group of galaxies". Astronomy and Astrophysics. 373 (2): 485–493. arXiv:astro-ph/0106050. Bibcode:2001A&A...373..485D. doi:10.1051/0004-6361:20010614. S2CID 15512721.
^ Dahlem, Michael; et al. (September 1994). "Soft X-Ray Observations of the Interacting Galaxies NGC 1808 and NGC 1792". Astrophysical Journal. 432: 598. Bibcode:1994ApJ...432..598D. doi:10.1086/174598.