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M51 Group

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(Redirected from LGG 347) Galaxy cluster in constellation Canes Venatici
M51 Group
The Whirlpool Galaxy (M51A), the brightest member of the M51 Group, and M51B, the companion to the Whirlpool Galaxy.
Observation data (Epoch J2000)
Constellation(s)Canes Venatici
Right ascension13 24
Declination46° 13′
Brightest memberWhirlpool Galaxy (M51A)
Number of galaxies7-17
Other designations
NGC 5194 Group, LGG 347, NOGG H 712,
NOGG P1 723, NOGG P2 739

The M51 Group is a group of galaxies located in Canes Venatici. The group is named after the brightest galaxy in the group, the Whirlpool Galaxy (M51A). Other notable members include the companion galaxy to the Whirlpool Galaxy (M51B) and the Sunflower Galaxy (M63).

Members

The table below lists galaxies that have been consistently identified as group members in the Nearby Galaxies Catalog, the survey of Fouque et al., the Lyons Groups of Galaxies (LGG) Catalog, and the three group lists created from the Nearby Optical Galaxy sample of Giuricin et al.

Members of the M51 Group
Name Type R.A. (J2000) Dec. (J2000) Redshift (km/s) Apparent Magnitude
Whirlpool Galaxy (M51A) SA(s)bc pec 13 29 52.7 +47° 11′ 43″ 463 ± 3 9.0
M51B (NGC 5195) SB0 pec 13 29 59.6 +47° 15′ 58″ 465 ± 10 10.5
NGC 5023 Scd 13 12 12.6 +44° 02′ 28″ 407 ± 1 12.9
NGC 5229 SB(s)d 13 34 02.8 +47° 54′ 56″ 364 ± 8 14.3
Sunflower Galaxy (M63) SA(rs)bc 13 15 49.3 +42° 01′ 45″ 504 ± 4 9.3
UGC 8313 SB(s)c 13 13 53.9 +42° 12′ 31″ 593 ± 4 14.4
UGC 8331 IAm 13 15 30.3 +47° 29′ 56″ 260 ± 5 14.6

Other probable members (galaxies listed in two or more of the lists from the above references) include IC 4263 and UGC 8320. The exact membership is somewhat uncertain.

Nearby Groups

The M51 Group is located to the southeast of the M101 Group and the NGC 5866 Group. The distances to these three groups (as determined from the distances to the individual member galaxies) are similar, which suggests that the M51 Group, the M101 Group, and the NGC 5866 Group are actually part of a large, loose, elongated structure. However, most group identification methods (including those used by the references cited above) identify these three groups as separate entities.

See also

References

  1. ^ A. Garcia (1993). "General study of group membership. II - Determination of nearby groups". Astronomy and Astrophysics Supplement. 100: 47–90. Bibcode:1993A&AS..100...47G.
  2. ^ G. Giuricin; C. Marinoni; L. Ceriani; A. Pisani (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups". Astrophysical Journal. 543 (1): 178–194. arXiv:astro-ph/0001140. Bibcode:2000ApJ...543..178G. doi:10.1086/317070. S2CID 9618325.
  3. ^ P. Fouque, E. Gourgoulhon, P. Chamaraux, G. Paturel; Gourgoulhon; Chamaraux; Paturel (1992). "Groups of galaxies within 80 Mpc. II - The catalogue of groups and group members". Astronomy and Astrophysics Supplement. 93: 211–233. Bibcode:1992A&AS...93..211F.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  4. ^ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge: Cambridge University Press. ISBN 0-521-35299-1.
  5. ^ "NASA/IPAC Extragalactic Database". Results for various galaxies. Retrieved 2006-10-19.
  6. ^ L. Ferrarese, H. C. Ford, J. Huchra, R. C. Kennicutt Jr., J. R. Mould, S. Sakai, W. L. Freedman, P. B. Stetson, B. F. Madore, B. K. Gibson, J. A. Graham, S. M. Hughes, G. D. Illingworth, D. D. Kelson, L. Macri, K. Sebo, N. A. Silbermann (2000). "A Database of Cepheid Distance Moduli and Tip of the Red Giant Branch, Globular Cluster Luminosity Function, Planetary Nebula Luminosity Function, and Surface Brightness Fluctuation Data Useful for Distance Determinations". Astrophysical Journal Supplement. 128 (2): 431–459. arXiv:astro-ph/9910501. Bibcode:2000ApJS..128..431F. doi:10.1086/313391. S2CID 121612286.{{cite journal}}: CS1 maint: multiple names: authors list (link)

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