Messier 100

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Messier 100
Messier 100 -- Grand Design Splendour.jpg
Galaxy Messier 100 imaged by ESO, revealing complex spiral arm structure
Observation data (J2000 epoch)
Constellation Coma Berenices [1]
Right ascension 12h 22m 54.8616s [2]
Declination +15° 49′ 17.886″ [2]
Redshift 0.005240 [2]
Heliocentric radial velocity 1,571±1 km/s [2]
Distance 55 Mly [3]
Group or cluster Virgo Cluster
Apparent magnitude  (V)9.3 [4]
Characteristics
Type SAB(s)bc [2]
Size~166,100  ly (50.93  kpc) (estimated) [2]
Apparent size  (V)7.4′ × 6.3′ [2]
Other designations
HOLM 387A, IRAS 12204+1605, NGC 4321, UGC 7450, MCG +03-32-015, PGC 40153, CGCG 099-030

Messier 100 (also known as NGC 4321 or the Mirror Galaxy) is a grand design intermediate spiral galaxy in the southern part of the mildly northern Coma Berenices. [5] It is one of the brightest and largest galaxies in the Virgo Cluster and is approximately 55 million light-years [3] from our galaxy, about 166,000 light-years in diameter. It was discovered by Pierre Méchain in 1781 [a] and 29 days later seen again and entered by Charles Messier in his catalogue "of nebulae and star clusters". [6] [7] It was one of the first spiral galaxies to be discovered, [7] and was listed as one of fourteen spiral nebulae by Lord William Parsons of Rosse in 1850. NGC 4323 and NGC 4328 are satellite galaxies of M100; the former is connected with it by a bridge of luminous matter. [8] [9]

Contents

Early observations

This is a widefield view of the galaxy, M100, directly left of the center of the picture - captured with an amateur telescope in 2025. Widefield View of M100.png
This is a widefield view of the galaxy, M100, directly left of the center of the picture - captured with an amateur telescope in 2025.

After the discovery of M100 by Méchain, Charles Messier made observations of the galaxy depicting it as a nebula without a star. He pointed out that it was difficult [7] to recognize the nebula because of its faintness. William Herschel was able to identify a bright cluster of stars [7] within the "nebula" during his observations. His son John expanded the findings in 1833. With the advent of better telescopes, John Herschel was able to see a round, brighter galaxy; however, he also mentioned that it was barely visible through clouds. William Henry Smyth [7] extended the studies of M100, detailing it as a pearly white nebula and pointing out diffuse spots.

Star formation

Messier 100 is considered a starburst galaxy [10] with the strongest star formation activity concentrated in its center, within a ring – actually two tightly wound spiral arms attached to a small nuclear bar of radius: one thousand parsecs [11] – where star formation has been taking place for at least 500 million years in separate bursts. [12]

As usual on spiral galaxies of the Virgo Cluster, in the rest of the disk both star formation [13] and neutral hydrogen, of which M100 is deficient compared to isolated spiral galaxies of similar Hubble type, [14] are truncated within the galaxy's disk, which is caused by interactions with the intracluster medium of Virgo.

Supernovae

Supernova SN 2019ehk in M100 (Hubble) Noirlab2019b.jpg
Supernova SN 2019ehk in M100 (Hubble)

Seven supernovae have been identified in M100: [5]

See also

References and footnotes

  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/Cambridge University Press. ISBN   978-0-933346-51-2.
  2. 1 2 3 4 5 6 7 "Results for object MESSIER 100". NASA/IPAC Extragalactic Database. NASA and Caltech . Retrieved 2006-08-31.
  3. 1 2 "Messier 100". Hearst Observatory . Retrieved 2010-02-23.
  4. ↑ "Messier 100". SEDS Messier Catalog. Retrieved 30 April 2022.
  5. 1 2 3 4 5 6 7 8 "Messier 100". SEDS: Spiral Galaxy M100 (NGC 4321), type Sc, in Coma Berenices. Retrieved 2010-02-23.
  6. ↑ "Catalog of Nebulae and Star Clusters". SEDS . Retrieved 2010-02-23.
  7. 1 2 3 4 5 "Messier 100". SEDS: Observations and Descriptions. Retrieved 2010-02-23.
  8. ↑ S. di Serego Alighieri; et al. (2007). "The HI content of Early-Type Galaxies from the ALFALFA survey I. Catalogued HI sources in the Virgo cluster". Astronomy and Astrophysics . 474 (3): 851–855. arXiv: 0709.2096 . Bibcode:2007A&A...474..851D. doi:10.1051/0004-6361:20078205. S2CID   5332365.
  9. ↑ "NGC 4323". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2010-02-23.
  10. ↑ Wozniak, H.; Friedli, D.; Martinet, L.; Pfenniger, D. (1999). "Double-barred starburst galaxies viewed by ISOCAM". The Universe as Seen by ISO. 427: 989. Bibcode:1999ESASP.427..989W.
  11. ↑ Sakamoto, Kazushi; Okumura, Sachiko; Minezaki, Takeo; Kobayashi, Yukiyasu; et al. (1995). "Bar-Driven Gas Structure and Star Formation in the Center of M100". The Astronomical Journal. 110 (3): 2075. Bibcode:1995AJ....110.2075S. doi:10.1086/117670.
  12. ↑ Allard, E. L.; Knapen, J. H.; Peletier, R. F.; Sarzi, M. (2006). "The star formation history and evolution of the circumnuclear region of M100". Monthly Notices of the Royal Astronomical Society . 371 (3): 1087–1105. arXiv: astro-ph/0606490 . Bibcode:2006MNRAS.371.1087A. doi: 10.1111/j.1365-2966.2006.10751.x . S2CID   119370091.
  13. ↑ R. A. Koopmann; J. D. P. Kenney (2004). "Hα Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies". Astrophysical Journal . 613 (2): 866–885. arXiv: astro-ph/0406243 . Bibcode:2004ApJ...613..866K. doi:10.1086/423191. S2CID   17519217.
  14. ↑ Chung, A.; Van Gorkom, J.H.; Kenney, J.F.P.; Crowl, Hugh; et al. (2009). "VLA Imaging of Virgo Spirals in Atomic Gas (VIVA). I. The Atlas and the H I Properties". The Astronomical Journal. 138 (6): 1741–1816. Bibcode:2009AJ....138.1741C. doi: 10.1088/0004-6256/138/6/1741 .
  15. 1 2 Pickering, E. C. (1917). "Ritchie's Nova". Harvard College Observatory Bulletin. 642: 1. Bibcode:1917BHarO.642....1P.
  16. ↑ "SN 1901B". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2010-02-23.
  17. 1 2 Curtis, Heber Doust (1917). "Three novae in spiral nebulae". Lick Observatory Bulletin. 300: 108. Bibcode:1917LicOB...9..108C. doi:10.5479/ADS/bib/1917LicOB.9.108C.
  18. ↑ "SN 1914A". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2010-02-23.
  19. ↑ "SN 1959E". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2010-02-23.
  20. ↑ Humason, M. L.; Gomes, Alercio M.; Kearns, C. E. (1961). "The 1960 Palomar Supernova Search". Publications of the Astronomical Society of the Pacific. 73 (432): 175. Bibcode:1961PASP...73..175H. doi: 10.1086/127650 .{{cite journal}}: CS1 maint: multiple names: authors list (link)
  21. ↑ "SN 1979C". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2010-02-23.
  22. ↑ International Astronomical Union (1979). "IAU Circular 3348". International Astronomical Union Circulars. 3348 (3348): 1. Bibcode:1979IAUC.3348....1M . Retrieved 2024-11-25.
  23. ↑ "SN 2006X". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2010-02-23.
  24. ↑ Ponticello, N. J.; Burket, J.; Li, W.; Chen, Y. -T.; Yang, M.; Lin, C. -S.; Soma, M.; Migliardi, M.; Dimai, A. (2006). "Supernovae 2006U, 2006V, 2006W, 2006X. (Lick Observatory Supernova Search)". International Astronomical Union Circular (8667): 1. Bibcode:2006IAUC.8667....1P.
  25. ↑ "SN 2006X". Transient Name Server. IAU . Retrieved 1 January 2025.
  26. ↑ "SN 2019ehk". Transient Name Server. IAU . Retrieved 25 November 2024.
  27. ↑ "SN 2020oi". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2010-02-23.
  28. ↑ "SN 2020oi". Transient Name Server. IAU . Retrieved 1 January 2025.
  1. ↑ On March 15
  2. ↑ February 21 to June 17
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