Back Messier 32 Afrikaans مسييه 32 Arabic M 32 Azerbaijani M32 (аб’ект Месье) Byelorussian M32 BE-X-OLD M32 Bulgarian Messier 32 BS Messier 32 Catalan NGC 221 CE M32 Corsican

Messier 32

Messier 32
Dwarf Satellite Galaxy Messier 32
Observation data (J2000 epoch)
ConstellationAndromeda
Right ascension00h 42m 41.8s[1]
Declination+40° 51′ 55″[1]
Redshift−200 ± 6 km/s[1]
Distance2.49 ± 0.08 Mly (763 ± 24 kpc)[2][3][4][a]
Apparent magnitude (V)8.08[5][6]
Characteristics
TypecE2[1]
Apparent size (V)8′.7 × 6′.5[1]
Notable featuresSatellite galaxy of the
Andromeda Galaxy
Other designations
M 32, NGC 221,[1] UGC 452,[1] PGC 2555,[1] Arp 168,[1] LEDA 2555

Messier 32 (also known as M32 and NGC 221) is a dwarf "early-type" galaxy about 2,650,000 light-years (810,000 pc) from the Solar System, appearing in the constellation Andromeda. M32 is a satellite galaxy of the Andromeda Galaxy (M31) and was discovered by Guillaume Le Gentil in 1749.

The galaxy is a prototype of the relatively rare compact elliptical (cE) class. Half the stars concentrate within an effective radius (inner core) of 330 light-years (100 pc).[7][8] Densities in the central stellar cusp increase steeply, exceeding 3×107 (that is, 30 million) M☉ pc−3 (that is, per parsec cubed) at the smallest sub-radii resolved by HST,[9] and the half-light radius of this central star cluster is around 6 parsecs (20 ly).[10] Like more ordinary elliptical galaxies, M32 contains mostly older faint red and yellow stars with practically no dust or gas and consequently no current star formation.[11] It does, however, show hints of star formation in the relatively recent past.[12]

  1. ^ a b c d e f g h i "NASA/IPAC Extragalactic Database". Results for NGC 221. Retrieved 2006-11-29.
  2. ^ Cite error: The named reference jensenetal2003 was invoked but never defined (see the help page).
  3. ^ Cite error: The named reference karachentsevetal2004 was invoked but never defined (see the help page).
  4. ^ Cite error: The named reference Karachentsevetal2006 was invoked but never defined (see the help page).
  5. ^ "M32". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-11-29.
  6. ^ Armando, Gil de Paz; Boissier; Madore; Seibert; Boselli; et al. (2007). "The GALEX Ultraviolet Atlas of Nearby Galaxies". Astrophysical Journal Supplement. 173 (2): 185–255. arXiv:astro-ph/0606440. Bibcode:2007ApJS..173..185G. doi:10.1086/516636. S2CID 119085482.
  7. ^ Kent, S. M. (1987). "Surface photometry of six local group galaxies". Astronomical Journal. 94: 306–314. Bibcode:1987AJ.....94..306K. doi:10.1086/114472.
  8. ^ Mateo, M. L. (1998). "Dwarf Galaxies of the Local Group". Annual Review of Astronomy and Astrophysics. 36: 435–506. arXiv:astro-ph/9810070. Bibcode:1998ARA&A..36..435M. doi:10.1146/annurev.astro.36.1.435. S2CID 119333888.
  9. ^ Lauer, T. R.; Faber, S. M.; Currie, D. G.; Ewald, S. P.; Groth, E. J.; Hester, J. J.; Holtzman, J. A.; Light, R. M.; O'Neil Jr, E. J.; Shaya, E. J.; Westphal, J. A. (1992). "Planetary camera observations of the central parsec of M32" (PDF). Astronomical Journal. 104: 552–562. Bibcode:1992AJ....104..552L. doi:10.1086/116254.
  10. ^ Graham, A.W. and Spitler, L.R., Quantifying the coexistence of massive black holes and dense nuclear star clusters.
  11. ^ Kepple, George Robert; Sanner, Glen W. (1998). The Night Sky Observer's Guide. Vol. 1. Willmann-Bell. p. 17. ISBN 978-0-943396-58-3.
  12. ^ Rudenko, Pavlo; Worthey, Guy; Mateo, Mario (2009). "Intermediate age clusters in the field containing M31 and M32 stars". The Astronomical Journal. 138 (6): 1985–1989. Bibcode:2009AJ....138.1985R. doi:10.1088/0004-6256/138/6/1985.

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