Astronomy:NGC 4236

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NGC 4236
File:NGC 4236 by Matt Smith.jpg
High-resolution visible-light astrophotograph
Observation data (J2000 epoch)
ConstellationDraco[1]
Right ascension 12h 16m 42.1s[2]
Declination+69° 27′ 45″[2]
Redshift0 ± 2 km/s[2]
Apparent magnitude (V)10.5[2]
Characteristics
TypeSB(s)dm[2]
Size74,000 ly (22.70 kpc)[2]
Apparent size (V)21.9′ × 7.2′[2]
Other designations
UGC 7306,[2] PGC 39346,[2] Caldwell 3

NGC 4236 (also known as Caldwell 3) is a barred Magellanic spiral galaxy located in the constellation Draco. It was discovered in April 1793 by William Herschel.[3]

The galaxy is a member of the M81 Group, a group of galaxies located at a distance of approximately 11.7 Mly (3.6 Mpc) from Earth.[4] The group also contains the spiral galaxy Messier 81 and the starburst galaxy Messier 82.[4] NGC 4236 is located away from the central part of the M81 group at a distance of 14.5 Mly (4.45 Mpc) from Earth.[5] The galaxy includes a large number of bright emission nebulae, easily visible from Earth. Star formation is occurring throughout the entire galactic disc. The core contains very little star formation, however this is offset by an active galactic halo. Despite the lack of star formation in the core, it contains three point radio signals, which are hypothesized to be remnants of supernovae.[6] An alternative theory suggests two of these sources could be from smaller-scale stellar formation and the remaining one is possibly a foreground G-type star.[7]

See also

References

  1. ↑ R. W. Sinnott, ed (1988). The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer. Sky Publishing Corporation and Cambridge University Press. ISBN 978-0-933346-51-2. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 "NASA/IPAC Extragalactic Database". Results for NGC 4236. http://nedwww.ipac.caltech.edu/. 
  3. ↑ "Caldwell 3". NASA. https://science.nasa.gov/mission/hubble/science/explore-the-night-sky/hubble-caldwell-catalog/caldwell-3/. 
  4. ↑ 4.0 4.1 I. D. Karachentsev (2005). "The Local Group and Other Neighboring Galaxy Groups". Astronomical Journal 129 (1): 178–188. doi:10.1086/426368. Bibcode: 2005AJ....129..178K. 
  5. ↑ I. D. Karachentsev; A. E. Dolphin; D. Geisler; E. K. Grebel; P. Guhathakurta; P. W. Hodge; V. E. Karachentseva; A. Sarajedini et al. (2002). "The M 81 group of galaxies: New distances, kinematics and structure". Astronomy and Astrophysics 383 (1): 125–136. doi:10.1051/0004-6361:20011741. Bibcode: 2002A&A...383..125K. 
  6. ↑ Chyzy, K.T.; Bomans, D.J.; Krause, M.; Beck, Beck; Soida, M.; Urbanik, M. (2008). "Magnetic fields and ionized gas in nearby late type galaxies". https://www.researchgate.net/figure/The-Ha-image-of-NGC-4236-with-the-optical-continuum-subtracted_fig7_1791614. 
  7. ↑ Lira, P.; Johnson, R. A.; Lawrence, A.; Cid Fernandes, R. (21 December 2007). "Multiwavelength study of the nuclei of a volume-limited sample of galaxies – II. Optical, infrared and radio observations". Monthly Notices of the Royal Astronomical Society 382 (4): 1552–1590. https://doi.org/10.1111/j.1365-2966.2007.12006.x. Retrieved May 30, 2026. 

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