Messier 32

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Messier 32

Dwarf Elliptical Galaxy M32
Observation data (J2000 epoch)
Constellation Andromeda
Right ascension 00h 42m 41.8s[1]
Declination +40° 51′ 55″[1]
Redshift -200 ± 6 km/s[1]
Distance 2.49 ± 0.08 Mly (763 ± 24 kpc)[2][3][4][a]
Type cE2[1]
Apparent dimensions (V) 8′.7 × 6′.5[1]
Apparent magnitude (V) 9.0[1]
Notable features satellite galaxy of the
Andromeda Galaxy
Other designations
M 32, NGC 221,[1] UGC 452,[1] PGC 2555,[1] Arp 168[1]
See also: Galaxy, List of galaxies
Another photo
Another photo

Messier 32 (also known as NGC 221 and Le Gentil) is a dwarf elliptical galaxy about 2.65 million light-years away in the constellation Andromeda. M32 is a satellite galaxy of the famous Andromeda Galaxy (M31) and was discovered by Le Gentil in 1749 and measures only 6.5 ± 0.2 kly[5] in diameter at the widest point. Like most elliptical galaxies, M32 contains mostly older faint red and yellow stars with practically no dust or gas and consequently no current star formation.[6] It does, however, shows hints of star formation in the relative recent past.

The structure and stellar content of M32 is difficult to explain by traditional galaxy formation models. Recent simulations suggest a new scenario in which the strong tidal field of M31 can transform a spiral galaxy into a compact elliptical. As a small spiral galaxy falls into the central parts of M31, most of the outer layers of the smaller spiral are stripped away. The central bulge of the galaxy is much less affected and retains its morphology. Tidal effects trigger a massive star burst in the core, resulting in the high density of M32 we observe today.[7]

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[edit] Distance measurements

At least two techniques have been used to measure distances to M 32. The infrared surface brightness fluctuations distance measurement technique estimates distances to spiral galaxies based on the graininess of the appearance of their bulges. The distance measured to M 32 using this technique is 2.46 ± 0.09 Mly (755 ± 28 kpc).[2] However, M 32 is close enough that the tip of the red giant branch (TRGB) method may be used to estimate its distance. The estimated distance to M 32 using this technique is 2.51 ± 0.13 Mly (770 ± 40 kpc).[3][4] Averaged together, these distance measurements give a distance estimate of 2.49 ± 0.08 Mly (763 ± 24 kpc).[a]

[edit] See also

[edit] External links

[edit] Notes

  1. ^ average(755 ± 28, 770 ± 40) = ((755 + 770) / 2) ± ((282 + 402)0.5 / 2) = 763 ± 24

[edit] References

  1. ^ a b c d e f g h i j NASA/IPAC Extragalactic Database. Results for NGC 221. Retrieved on 2006-11-29.
  2. ^ a b Jensen, Joseph B.; Tonry, John L.; Barris, Brian J.; Thompson, Rodger I.; Liu, Michael C.; Rieke, Marcia J.; Ajhar, Edward A.; Blakeslee, John P. (February 2003). "Measuring Distances and Probing the Unresolved Stellar Populations of Galaxies Using Infrared Surface Brightness Fluctuations". Astrophysical Journal 583 (2): 712-726. doi:10.1086/345430. 
  3. ^ a b I. D. Karachentsev, V. E. Karachentseva, W. K. Hutchmeier, D. I. Makarov (2004). "A Catalog of Neighboring Galaxies". Astronomical Journal 127: 2031-2068. doi:10.1086/382905. 
  4. ^ a b Karachentsev, I. D.; Kashibadze, O. G. (2006). "Masses of the local group and of the M81 group estimated from distortions in the local velocity field". Astrophysics 49 (1): 3-18. doi:10.1007/s10511-006-0002-6. 
  5. ^ Diameter = distance × sin(diameter_angle) = 6.5 ± 0.2 kly. diameter
  6. ^ Kepple, George Robert; Glen W. Sanner (1998). The Night Sky Observer's Guide, Volume 1. Willmann-Bell, Inc., 17. ISBN 0-943396-58-1. 
  7. ^ Bekki, Kenji; Couch, Warrick J.; Drinkwater, Michael J.; Gregg, Michael D. (2001). "A New Formation Model for M32: A Threshed Early-Type Spiral Galaxy?". The Astrophysical Journal 557: L39. doi:10.1086/323075. 
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