Messier 32

From Wikipedia, the free encyclopedia

Template:Short description

Page Module:Infobox/styles.css has no content.

Messier 32
Lua error in package.lua at line 80: module 'Module:InfoboxImage/data' not found.
Dwarf Satellite Galaxy Messier 32 (center)
Observation data (J2000 epoch)
ConstellationAndromeda
Right ascensionTemplate:RA[1]
DeclinationTemplate:DEC[1]
Redshift−200 ± 6 km/s[1]
Distance2.49 ± 0.08 Mly (763 ± 24 kpc)[2][3][4]
Apparent magnitude (V)8.08[5]Template:R/superscript[6]Template:R/superscript
Characteristics
TypecE2[1]Template:R/superscript
Size8,000 ly (2.46 kpc) (estimated)[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 2,490,000 light-years (760,000 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 are concentrated within the inner core, which has an effective radius of 330 light-years (100 pc).[7]Template:R/superscript[8]Template:R/superscript Densities in the central stellar cusp increase steeply, exceeding 3×107 M☉ pc−3 (30 million solar masses per cubic parsec) at the smallest sub-radii resolved by Hubble Space Telescope,[9]Template:R/superscript and the half-light radius of this central star cluster is around 6 pc (20 light-years).[10] Like more ordinary elliptical galaxies, M32 contains mostly old faint red and yellow stars with practically no dust or gas and consequently no current star formation.[11]Template:R/superscript It does, however, show hints of star formation in the relatively recent past.[12]Template:R/superscript

Origins

File:M31 09-01-2011.jpg
In this image of the Andromeda Galaxy, Messier 32 is to the left of the center.

The structure and stellar content of M32 are difficult to explain by traditional galaxy formation models. Theoretical arguments[13]Template:R/superscript and some simulations suggest a scenario in which the strong tidal field of M31 can transform a spiral galaxy or a lenticular galaxy into a compact elliptical. As a small disk galaxy falls into the central parts of M31, much of its outer layers will be stripped away. The central bulge of the small galaxy is much less affected and retains its morphology. Gravitational tidal effects may also drive gas inward and trigger a star burst in the core of the small galaxy, resulting in the high density of M32 observed today.[14]Template:R/superscript There is evidence that M32 has a faint outer disk,[15]Template:R/superscript and as such is not a typical elliptical galaxy.

Newer simulations find that an off-centre impact by M32 around 800 million years ago explains the present-day warp in M31's disk.[16]Template:R/superscript However, this feature only occurs during the first orbital passage, whereas it takes many orbits for tides to transform a normal dwarf into M32. The observed colours and stellar populations of M32's outskirts do not match the stellar halo of M31,[17]Template:R/superscript indicating that tidal losses from M32 are not their source. Taken together, these circumstances may suggest that M32 already began in its compact state, and has retained most of its own stars. At least one similar cE galaxy has been discovered in isolation, without any massive companion to thresh it.[18]Template:R/superscript

Another hypothesis is that M32 is in fact the largest remnant of a former spiral galaxy, M32p, which was then the third largest member of the Local Group.[19]Template:R/superscript According to this simulation, M31 (Andromeda) and M32p merged about two billion years ago, which could explain both the unusual makeup of the current M31 stellar halo, and the structure and content of M32.[20]Template:R/superscript

Distance measurements

At least two techniques have been used to measure distances to M32. 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 M32 using this technique is 2.46 ± 0.09 million light-years (755 ± 28 kpc).[2]Template:R/superscript However, M32 is close enough that the tip of the red giant branch (TRGB) method may be used to estimate its distance. The estimated distance to M32 using this technique is 2.51 ± 0.13 million light-years (770 ± 40 kpc).[3]Template:R/superscript[4]Template:R/superscript For several additional reasons, M32 is thought to be in the foreground of M31, rather than behind. Its stars and planetary nebulae do not appear obscured or reddened by foreground gas or dust.[21]Template:R/superscript[22]Template:R/superscript Gravitational microlensing of M31 by a star in M32 was observed at the end of November 2000 in one event (with peak on 2 December 2000).[23]Template:R/superscript

Black hole

File:Messier 32 from Hubble.jpg
Hubble image of Messier 32 showing resolved central region

M32 contains a supermassive black hole. Its mass has been estimated to lie between 1.5 and 5 million solar masses.[24]Template:R/superscript[25]Template:R/superscript[26]Template:R/superscript[27]Template:R/superscript[28]Template:R/superscript[29]Template:R/superscript A centrally located faint radio and X-ray source (now named M32* in analogy to Sgr A*) is attributed to gas accretion onto the black hole.[30]Template:R/superscript[31]Template:R/superscript

See also

References

  1. ^ a b c d e f g h i j Page Module:Citation/CS1/styles.css has no content."Results for object MESSIER 032". NASA/IPAC Extragalactic Database. Retrieved 2006-11-29.
  2. ^ a b Page Module:Citation/CS1/styles.css has no content.Jensen, Joseph B.; Tonry, John L.; Barris, Brian J.; Thompson, Rodger I.; Liu, Michael C.; Rieke, Marcia J.; Ajhar, Edward A.; Blakeslee, John P. (2003). "Measuring Distances and Probing the Unresolved Stellar Populations of Galaxies Using Infrared Surface Brightness Fluctuations". Astrophysical Journal. 583 (2): 712–726. arXiv:astro-ph/0210129. Bibcode:2003ApJ...583..712J. doi:10.1086/345430. S2CID 551714.
  3. ^ a b Page Module:Citation/CS1/styles.css has no content.Karachentsev, I. D.; Karachentseva, V. E.; Hutchmeier, W. K.; Makarov, D. I. (2004). "A Catalog of Neighboring Galaxies". Astronomical Journal. 127 (4): 2031–2068. Bibcode:2004AJ....127.2031K. doi:10.1086/382905.
  4. ^ a b Page Module:Citation/CS1/styles.css has no content.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. Bibcode:2006Ap.....49....3K. doi:10.1007/s10511-006-0002-6. S2CID 120973010.
  5. ^ Page Module:Citation/CS1/styles.css has no content."M32". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-11-29. {{cite web}}: Invalid |mode=Script error: No such module "Citation mode". (help)
  6. ^ Page Module:Citation/CS1/styles.css has no content.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. ^ Page Module:Citation/CS1/styles.css has no content.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. ^ Page Module:Citation/CS1/styles.css has no content.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. ^ Page Module:Citation/CS1/styles.css has no content.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. ^ Page Module:Citation/CS1/styles.css has no content.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. ^ Page Module:Citation/CS1/styles.css has no content.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.
  13. ^ Page Module:Citation/CS1/styles.css has no content.Faber, S. M. (1973). "Tidal Origin of Elliptical Galaxies of High Surface Brightness". Astrophysical Journal. 179: 423–426. Bibcode:1973ApJ...179..423F. doi:10.1086/151881.
  14. ^ Page Module:Citation/CS1/styles.css has no content.Bekki, Kenji; Couch, Warrick J.; Drinkwater, Michael J.; Gregg, Michael D. (2001). "A New Formation Model for M32: A Threshed Early-Type Spiral Galaxy?" (PDF). Astrophysical Journal Letters. 557 (1): L39. arXiv:astro-ph/0107117. Bibcode:2001ApJ...557L..39B. doi:10.1086/323075. S2CID 18707442.
  15. ^ Page Module:Citation/CS1/styles.css has no content.Graham, A. W. (2002). "Evidence for an Outer Disk in the Prototype Compact Elliptical Galaxy M32". Astrophysical Journal Letters. 568 (1): L13–L17. arXiv:astro-ph/0202307. Bibcode:2002ApJ...568L..13G. doi:10.1086/340274. S2CID 14891401.
  16. ^ Page Module:Citation/CS1/styles.css has no content.Dierickx, M.; Blecha, L.; Loeb, A. (2014). "Signatures of the M31–M32 Galactic Collision". Astrophysical Journal. 788 (2): L38. arXiv:1405.3990. Bibcode:2014ApJ...788L..38D. doi:10.1088/2041-8205/788/2/L38. S2CID 119111697.
  17. ^ Page Module:Citation/CS1/styles.css has no content.Choi, P. I.; Guhathakurta, P.; Johnston, K. V. (2002). "Tidal Interaction of M32 and NGC 205 with M31: Surface Photometry and Numerical Simulations". Astronomical Journal. 124 (1): 310–331. arXiv:astro-ph/0111465. Bibcode:2002AJ....124..310C. doi:10.1086/341041. S2CID 119356072.
  18. ^ Page Module:Citation/CS1/styles.css has no content.Huxor, A. P.; Phillipps, S.; Price, J. (2013). "Discovery of an isolated compact elliptical galaxy in the field". Monthly Notices of the Royal Astronomical Society. 430 (3): 1956–1960. arXiv:1302.6520. Bibcode:2013MNRAS.430.1956H. doi:10.1093/mnras/stt014. S2CID 119291374.
  19. ^ Page Module:Citation/CS1/styles.css has no content."The Milky Way's long-lost sibling finally found". University of Michigan News. 2018-07-23. Retrieved 2018-07-23.
  20. ^ Page Module:Citation/CS1/styles.css has no content.D’Souza, Richard; Bell, Eric F. (2018-07-23). "The Andromeda galaxy's most important merger about 2 billion years ago as M32's likely progenitor". Nature Astronomy. 2 (9): 737–743. arXiv:1807.08819. Bibcode:2018NatAs...2..737D. doi:10.1038/s41550-018-0533-x. ISSN 2397-3366. S2CID 119502746.
  21. ^ Page Module:Citation/CS1/styles.css has no content.Ford, H. C.; Jacoby, G. H.; Jenner, D. C. (1978). "Planetary nebulae in local group galaxies. VI – an observational determination that M32 is in front of M31". Astrophysical Journal. 223: 94–97. Bibcode:1978ApJ...223...94F. doi:10.1086/156239.
  22. ^ Page Module:Citation/CS1/styles.css has no content.van Dokkum, P. G.; Franx, M. (1995). "Dust in the Cores of Early-Type Galaxies". Astronomical Journal. 110: 2027. arXiv:astro-ph/9507101. Bibcode:1995AJ....110.2027V. doi:10.1086/117667. S2CID 118939047.
  23. ^ Page Module:Citation/CS1/styles.css has no content.Paulin-Henriksson, S.; Baillon, P.; Bouquet, A.; Carr, B. J.; Creze, M.; Evans, N. W.; Giraud-Heraud, Y.; Gould, A.; Hewett, P.; Kaplan, J.; Kerins, E.; Lastennet, E.; Le Du, Y.; Melchior, A.-L.; Smartt, S. J.; Valls-Gabaud, D.; Point-Agape Collaboration (2002). "A Candidate M31/M32 Intergalactic Microlensing Event". Astrophysical Journal Letters. 576 (2): L121–L124. arXiv:astro-ph/0206387. Bibcode:2002ApJ...576L.121P. doi:10.1086/343887. S2CID 2554622.
  24. ^ Page Module:Citation/CS1/styles.css has no content.Tonry, J. L. (1984). "Evidence for a central mass concentration in M32". Astrophysical Journal Letters. 283: L27. Bibcode:1984ApJ...283L..27T. doi:10.1086/184326.
  25. ^ Page Module:Citation/CS1/styles.css has no content.Bender, R.; Kormendy, J.; Dehnen, W. (1996). "Improved Evidence for a 3×106 M☉ Black Hole in M32: Canada–France–Hawaii Telescope Spectroscopy with FWHM = 0.47" Resolution". Astrophysical Journal Letters. 464 (2): L123–L126. Bibcode:1996ApJ...464L.123B. doi:10.1086/310098.
  26. ^ Page Module:Citation/CS1/styles.css has no content.Joseph, C. L.; Merritt, D.; Olling, R.; Valluri, M.; Bender, R.; Bower, G.; Danks, A.; Gull, T.; Hutchings, J.; Kaiser, M. E.; Maran, S.; Weistrop, D.; Woodgate, B.; Malumuth, E.; Nelson, C.; Plait, P.; Lindler, D. (2001). "The Nuclear Dynamics of M32. I. Data and Stellar Kinematics". Astrophysical Journal. 550 (2): 668–690. arXiv:astro-ph/0005530. Bibcode:2001ApJ...550..668J. doi:10.1086/319781. S2CID 999283.
  27. ^ Page Module:Citation/CS1/styles.css has no content.Verolme, E. K.; Cappellari, M.; Copin, Y.; van der Marel, R. P.; Bacon, R.; Bureau, M.; Davies, R. L.; Miller, B. M.; de Zeeuw, P. T. (2002). "A SAURON study of M32: measuring the intrinsic flattening and the central black hole mass". Monthly Notices of the Royal Astronomical Society. 335 (3): 517–525. arXiv:astro-ph/0201086. Bibcode:2002MNRAS.335..517V. doi:10.1111/j.1365-2966.2009.15832.x. S2CID 119238097.
  28. ^ Page Module:Citation/CS1/styles.css has no content.Valluri, M.; Merritt, D.; Emsellem, E. (2004). "Difficulties with Recovering the Masses of Supermassive Black Holes from Stellar Kinematical Data". Astrophysical Journal. 602 (1): 66–92. arXiv:astro-ph/0210379. Bibcode:2004ApJ...602...66V. doi:10.1086/380896. S2CID 16899097.
  29. ^ Page Module:Citation/CS1/styles.css has no content.van den Bosch, R. C. E.; de Zeeuw, P. T. (2010). "Estimating black hole masses in triaxial galaxies". Monthly Notices of the Royal Astronomical Society. 401 (3): 1770–1780. arXiv:0910.0844. Bibcode:2010MNRAS.401.1770V. doi:10.1111/j.1365-2966.2009.15832.x. S2CID 119238097.
  30. ^ Page Module:Citation/CS1/styles.css has no content.Ho, Luis C.; Terashima, Yuichi; Ulvestad, James S. (2003). "Detection of the "Active" Nucleus of M32". Astrophysical Journal. 589 (2): 783–789. arXiv:astro-ph/0303060. Bibcode:2003ApJ...589..783H. doi:10.1086/374738. S2CID 10268471.
  31. ^ Page Module:Citation/CS1/styles.css has no content.Yang, Yang; Li, Zhiyuan; Sjouwerman, Loránt O.; Wang, Q. Daniel; Gu, Qiusheng; Kraft, Ralph P.; Yuan, Feng (2015). "Detection of a Compact Nuclear Radio Source in the Local Group Elliptical Galaxy M32". Astrophysical Journal Letters. 807 (1): L19. arXiv:1502.03231. Bibcode:2015ApJ...807L..19Y. doi:10.1088/2041-8205/807/1/L19. S2CID 119292353.

Page Module:Side box/styles.css has no content.Page Template:Sister project/styles.css has no content.

Page Template:Plainlist/styles.css has no content.
Script error: No such module "Sister project logo".
Wikimedia Commons has media related to Messier 32.Template:Preview warning

Lua error in package.lua at line 80: module 'Module:Navbox/configuration' not found. Template:Constellation navbox Lua error in package.lua at line 80: module 'Module:Navbox/configuration' not found. Template:Ngc5 Lua error in mw.title.lua at line 404: bad argument #2 to 'title.new' (unrecognized namespace name 'Portal').

Retrieved from "https://cosmopedia.co/index.php?title=Messier_32&oldid=570056"