NGC 1792
NGC 1792 with the legacy surveys
Observation data (J2000 epoch)
ConstellationColumba
Right ascension05h 05m 14.454s[1]
Declination−37° 58′ 50.70″[1]
Redshift0.004059[2]
Heliocentric radial velocity1,208[3]
Distance36.4 Mly (11.17 Mpc)[3]
Group or clusterNGC 1808[4]
Apparent magnitude (V)10.18[2]
Apparent magnitude (B)10.68[2]
Characteristics
TypeSA(rs)bc[5]
Mass0.54×1011[6] M☉
Mass/Light ratio3.4[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]

Hubble Space Telescope image of NGC 1792 with the blue regions indicating younger stars

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

  1. 1 2 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.
  2. 1 2 3 4 "NGC 1792". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-12.
  3. 1 2 3 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.
  4. 1 2 3 4 Dahlem, M. (October 1992). "NGC 1792 : surprising radio properties". Astronomy and Astrophysics. 264: 483–488. Bibcode:1992A&A...264..483D.
  5. 1 2 3 de Vaucouleurs, G.; et al. (1991). "Third reference catalogue of bright galaxies". 9. New York: Springer-Verlag. {{cite journal}}: Cite journal requires |journal= (help)CS1 maint: multiple names: authors list (link)
  6. 1 2 3 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.
  7. ↑ 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.
  8. ↑ 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.
  9. ↑ 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.
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