Messier 110

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Messier 110[1]
NGC 0205 SDSS.jpg
SDSS image of Messier 110/NGC 205
Observation data (J2000 epoch)
ConstellationAndromeda[2]
Right ascension 00h 40m 22.05446s[3]
Declination+41° 41′ 07.4963″[3]
Redshift−0.000804±0.000010[4]
Helio radial velocity−241±3[4]
Galactocentric velocity−62±8[4]
Apparent magnitude (V)8.92[4]
Characteristics
TypeE5 pec[5]
Apparent size (V)21.9 × 11′.0[4]
Other designations
IRAS 00376+4124, LEDA 2429, M110, MCG +07-02-014, NGC 0205, PGC 002429[6]
See also: Galaxy, List of galaxies

Messier 110, or M110, also known as NGC 205, is a dwarf elliptical galaxy that is a satellite of the Andromeda Galaxy.[7] Although Charles Messier never included the galaxy in his list, it was depicted by him, together with M32, on a drawing of the Andromeda Galaxy; a label on the drawing indicates that Messier first observed NGC 205 on August 10, 1773.[8] The galaxy was independently discovered by Caroline Herschel on August 27, 1783; her brother William Herschel described her discovery in 1785.[8] The suggestion to assign the galaxy a Messier number was made by Kenneth Glyn Jones in 1967.[9]

This galaxy has a morphological classification of pec dE5, indicating a dwarf elliptical galaxy with a flattening of 50%. M110 is designated peculiar because there are patches of dust and young blue stars located near the center.[10] This is unusual for dwarf elliptical galaxies in general,[7] and the reason for this peculiarity is unclear.[10] Unlike M32, NGC 205 does not (as of 2005) show evidence for a supermassive black hole at its center.[11]

The interstellar dust in M110 has a mass of (1.1–1.8)×104 M with a temperature of 18–22 K, and the interstellar gas has (4–7)×106 M. The inner regions of M110 show a deficiency in the interstellar medium (IM) materials, which most likely were ejected by supernova explosions. Tidal interactions with M31 may have stripped away a significant fraction of the expelled gas and dust, leaving the galaxy as a whole deficient in its IM density.[12]

A few novae have been detected in this galaxy, including one discovered in 1999 by Johnson and Modjaz,[13] and another detected in 2002, by Nakano and Sumoto. The latter, designated EQ J004015.8+414420, had also been captured in images taken by the Sloan Digital Sky Survey (SDSS) in October, 2002.[14]

About half of the Andromeda's satellite galaxies are orbiting the host galaxy along a highly flattened plane, with 14 out of 16 following the same sense of rotation. One theory proposes that these objects once belonged to a subhalo surrounding NGC 205, then the group was broken up by tidal forces during a close encounter with Andromeda.[15]

Gallery[edit]

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References[edit]

  1. ^ McConnachie, A. W.; et al. (2005). "Distances and metallicities for 17 Local Group galaxies". Monthly Notices of the Royal Astronomical Society. 356 (4): 979–997. arXiv:astro-ph/0410489. Bibcode:2005MNRAS.356..979M. doi:10.1111/j.1365-2966.2004.08514.x.
  2. ^ Dreyer, J. L. E.; Sinnott, R. W. (1988). Sinnott, R. W. (ed.). NGC 2000.0: The Complete New General Catalogue and Index Catalogues of Nebulae and Star Clusters by J. L. E. Dreyer. Sky Publishing Corporation and Cambridge University Press. ISBN 978-0-933346-51-2.
  3. ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.
  4. ^ a b c d e "NASA/IPAC Extragalactic Database". Results for NGC 205. Retrieved 2006-11-29.
  5. ^ Batcheldor, D.; et al. (September 2013). "An STIS Atlas of Ca II Triplet Absorption Line Kinematics in Galactic Nuclei". The Astronomical Journal. 146 (3): 10. arXiv:1308.1983. Bibcode:2013AJ....146...67B. doi:10.1088/0004-6256/146/3/67. 67.
  6. ^ "M 110". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-12-19.
  7. ^ a b Sandage, A.; Bedke, J. (1994). Carnegie Atlas of Galaxies. Carnegie Institution of Washington. ISBN 978-0-87279-667-6.
  8. ^ a b Jones, K. G. (1991). Messier's Nebulae and Star Clusters (2nd ed.). Cambridge University Press. ISBN 978-0-521-37079-0.
  9. ^ Jones, K. G. (1967). "Some New Notes on Messier's Catalogue". Sky & Telescope. 33: 156–158. Bibcode:1967S&T....33..156J.
  10. ^ a b Ford, Holland C.; et al. (July 1973), "Planetary Nebulae in Local-Group Galaxies. I. Identifications in NGC 185, NGC 205, and NGC 221", Astrophysical Journal, 183: L73, Bibcode:1973ApJ...183L..73F, doi:10.1086/181255
  11. ^ Valluri, M.; et al. (2005). "The Low End of the Supermassive Black Hole Mass Function: Constraining the Mass of a Nuclear Black Hole in NGC 205 via Stellar Kinematics". Astrophysical Journal. 628 (1): 137–152. arXiv:astro-ph/0502493. Bibcode:2005ApJ...628..137V. doi:10.1086/430752.
  12. ^ De Looze, I.; et al. (July 2012). "Herschel and JCMT observations of the early-type dwarf galaxy NGC 205". Monthly Notices of the Royal Astronomical Society. 423 (3): 2359–2373. arXiv:1204.1264. Bibcode:2012MNRAS.423.2359D. doi:10.1111/j.1365-2966.2012.21044.x.
  13. ^ van den Bergh, S. (2000). "Updated Information on the Local Group". Publications of the Astronomical Society of the Pacific. 112 (770): 529–536. arXiv:astro-ph/0001040. Bibcode:2000PASP..112..529V. doi:10.1086/316548.
  14. ^ "Forum di Astronomia Amatoriale Italiano".
  15. ^ Angus, Garry W.; Coppin, Paul; Gentile, Gianfranco; Diaferio, Antonaldo (November 2016). "The potential role of NGC 205 in generating Andromeda's vast thin corotating plane of satellite galaxies". Monthly Notices of the Royal Astronomical Society. 462 (3): 3221–3242. arXiv:1608.03763. Bibcode:2016MNRAS.462.3221A. doi:10.1093/mnras/stw1822.

External links[edit]

Coordinates: Sky map 00h 40m 22.1s, +41° 41′ 07″