Wikipedia

Messier 100

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, its diameter being 107,000 light years, and being about 60% as large. 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]

Messier 100
Galaxy Messier 100 by ESO revealing complex spiral arm structure
Observation data (J2000 epoch)
ConstellationComa Berenices[1]
Right ascension12h 22m 54.9s[2]
Declination+15° 49′ 21″[2]
Redshift1571 ± 1 km/s[2]
Distance55 Mly[3]
Group or clusterVirgo Cluster
Apparent magnitude (V)9.3[4]
Characteristics
TypeSAB(s)bc[2]
Size107,000 ly (diameter)
Apparent size (V)7′.4 × 6′.3[2]
Other designations
NGC 4321

Early observations

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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

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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

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Supernova SN 2019ehk in M100 (Hubble)

Seven supernovae have been identified in M100.[5]

  • On 17 March 1901 Heber Curtis discovered SN 1901B,[5][15] a type I supernova with a magnitude of 15.6, at 110"W and 4"N from the galaxy's nucleus.[16]
  • Heber Curtis discovered SN 1914A[5][17] on 2 March 1914; its type was undeterminable but was found with a magnitude of 15.7 at 24"E and 111"S from the galaxy's nucleus.[16]
  • Milton Humason, with observations from early to mid 1960,[b] discovered SN 1959E (type I, mag. 17.5),[5][18] located 58"E and 21"S from the galaxy's nucleus.[19]
  • On April 15, 1979, amateur astronomer Gus Johnson discovered SN 1979C, the first type II supernova found in the M100 galaxy; however the star faded quickly; later observations from x-ray to radio wavelengths revealed its remnant.[5][20][21]
  • SN 2006X was discovered 7 February 2006 with a magnitude of 15.3, two weeks before fading to magnitude 17.[5][22]
  • Jaroslaw Grzegorzek discovered SN 2019ehk (type Ib, mag. 16.5) on 29 April 2019. The supernova reached a peak magnitude of approximately 15.8.[23]
  • The seventh supernova, SN 2020oi, was discovered on January 7, 2020. It was a type Ic supernova, which reached a peak magnitude of 17.7.[5][24]

See also

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References and footnotes

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  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. ^ a b c d e "NASA/IPAC Extragalactic Database". Results for NGC 4321. Retrieved 2006-08-31.
  3. ^ a b "Messier 100". Hearst Observatory. Retrieved 2010-02-23.
  4. ^ "Messier 100". SEDS Messier Catalog. Retrieved 30 April 2022.
  5. ^ a b c d e f g h "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. ^ a b c d e "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. ^ "SN 1901B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-02-23.
  16. ^ a b 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.
  17. ^ "SN 1914A". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-02-23.
  18. ^ "SN 1959E". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-02-23.
  19. ^ 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. doi:10.1086/127650.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  20. ^ "SN 1979C". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-02-23.
  21. ^ International Astronomical Union (1979). "IAU Circular 3348". International Astronomical Union Circulars (3348). Bibcode:1979IAUC.3348....1M. Retrieved 2024-11-25.
  22. ^ "SN 2006X". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-02-23.
  23. ^ "SN 2019ehk". Transient Name Server. IAU. Retrieved 25 November 2024.
  24. ^ "SN 2020oi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-02-23.
  1. ^ On March 15
  2. ^ February 21 to June 17
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