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Messier Index/M94

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Messier 94 (also known as NGC 4736) is a spiral galaxy in the constellation Canes Venatici. It was discovered by Pierre Méchain in 1781,[6] and catalogued by Charles Messier two days later. Although some references describe M94 as a barred spiral galaxy, the "bar" structure appears to be more oval-shaped.[7] The galaxy is also notable in that it has two ring structures.[5]

Messier 94[1][2][3]
M94: Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF
Observation data (J2000 epoch)
ConstellationCanes Venatici[4]
Right ascension12h 50m 53.1s [5]
Declination+41° 07′ 14″ [5]
Type(R)SA(r)ab[5], LINER[5]
Apparent magnitude (V)8.99 [5]
Other designations
NGC 4736, UGC 7996, PGC 43495[5]

Nucleus

M94 is classified as having a low ionization nuclear emission region (LINER) nucleus.[8] LINERs in general are characterized by optical spectra that reveal that ionized gas is present but the gas is only weakly ionized (i.e. the atoms are missing relatively few electrons).

Inner and outer rings

M94 contains both an inner ring with a diameter of 70" and an outer ring with a diameter of 600". These rings appear to form at resonance locations within the disk of the galaxy. The inner ring is the site of strong star formation activity and is sometimes referred to as a starburst ring. This star formation is fueled by gas that is dynamically driven into the ring by the inner oval-shaped bar-like structure.[9]

Pseudobulge

In a paper published in 2004, John Kormendy and Robert Kennicutt argued that M94 contains a prototypical pseudobulge.[7] A classical spiral galaxy consists of a disk of gas and young stars that intersects a large sphere (or bulge) of older stars. In contrast, a galaxy with a pseudobulge does not have a large bulge of old stars but instead contain a bright central structure with intense star formation that looks like a bulge when the galaxy is viewed face-on. In the case of M94, this pseudobulge takes the form of a ring around a central oval-shaped region.

Distance measurements

At least two techniques have been used to measure distances to M94. The 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 M94 using this technique is 17.0 ± 1.4 Mly (5.2 ± 0.4 Mpc).[1] However, M94 is close enough that the Hubble Space Telescope can be used to resolve and measure the fluxes of the brightest individual stars within the galaxy. These measured fluxes can then be compared to the measured fluxes of similar stars within the Milky Way to measure the distance. The estimated distance to M94 using this technique is 15 ± 2 Mly (4.7 ± 0.6 Mpc).[2] Averaged together, these distance measurements give a distance estimate of 16.0 ± 1.3 Mly (4.9 ± 0.4 Mpc).

Dark matter

In 2008 a study was published [10] that appeared to show that M94 had very little or no dark matter present. The study analyzed the rotation curves of the galaxy's stars and the density of hydrogen gas and found that ordinary luminous matter appeared to account for all of the galaxy's mass. This result was unusual and somewhat controversial, as current models don't indicate how a galaxy could form without a dark matter halo or how a galaxy could lose its dark matter. Other explanations for galactic rotation curves, such as MOND, also have difficulty explaining this galaxy.[11]

Galaxy group information

M94 is one of the brightest galaxies within the M94 Group, a group of galaxies that contains between 16 and 24 galaxies.[12][13][14] This group is one of many that lies within the Virgo Supercluster (i.e. the Local Supercluster).[15] Although a large number of galaxies may be associated with M94, only a few galaxies near M94 appear to form a gravitationally bound system. Most of the other nearby galaxies appear to be moving with the expansion of the universe.[2][16]

References

  1. ↑ a b J. L. Tonry, A. Dressler, J. P. Blakeslee, E. A. Ajhar, A. B. Fletcher, G. A. Luppino, M. R. Metzger, C. B. Moore (2001). "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances". Astrophysical Journal. 546 (2): 681–693. doi:10.1086/318301.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  2. ↑ a b c I. D. Karachentsev, M. E. Sharina, A. E. Dolphin, E. K. Grebel, D. Geisler, P. Guhathakurta, P. W. Hodge, V. E. Karachentseva, A. Sarajedini, P. Seitzer (2003). "Galaxy flow in the Canes Venatici I cloud". Astronomy and Astrophysics. 398: 467–477. doi:10.1051/0004-6361:20021598.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  3. ↑ average(17.0 ± 1.4, 15 ± 2) = ((17.0 + 15) / 2) ± ((1.42 + 22)0.5 / 2) = 16.0 ± 1.3
  4. ↑ R. W. Sinnott, editor (1988). The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer. Sky Publishing Corporation and Cambridge University Press. ISBN 0-933-34651-4. {{cite book}}: |author= has generic name (help)
  5. ↑ a b c d e f g "NASA/IPAC Extragalactic Database". Results for M94. Retrieved 2006-11-09.
  6. ↑ Kepple, George Robert (1998). The Night Sky Observer's Guide, Volume 2. Willmann-Bell, Inc. p. 51. ISBN 0-943396-60-3. {{cite book}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  7. ↑ a b J. Kormendy, R. C. Kennicutt, Jr. (2004). "Secular Evolution and the Formation of Pseudobulges in Disk Galaxies". Annual Reviews of Astronomy and Astrophysics. 42: 603–683. doi:10.1146/annurev.astro.42.053102.134024.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  8. ↑ L. C. Ho, A. V. Filippenko, W. L. W. Sargent (1997). "A Search for "Dwarf" Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". Astrophysical Journal Supplement. 112: 315–390. doi:10.1086/313041.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  9. ↑ C. Muñoz-Tuñón, N. Caon, J. Aguerri, L. Alfonso (2004). "The Inner Ring of NGC 4736: Star Formation on a Resonant Pattern". Astronomical Journal. 127: 58–74. doi:10.1086/380610.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  10. ↑ J. Jałocha, Ł. Bratek, and M. Kutschera (2008). "Is Dark Matter Present in NGC 4736? An Iterative Spectral Method for Finding Mass Distribution in Spiral Galaxies". The Astrophysical Journal. 679: 373–378. doi:10.1086/533511.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  11. ↑ Battersby, Stephen (06 February 2008). "Galaxy without dark matter puzzles astronomers". NewScientist.com news service. http://space.newscientist.com/article/dn13280-galaxy-without-dark-matter-puzzles-astronomers.html. 
  12. ↑ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge: Cambridge University Press. ISBN 0-521-35299-1.
  13. ↑ A. Garcia (1993). "General study of group membership. II - Determination of nearby groups". Astronomy and Astrophysics Supplement. 100: 47–90.
  14. ↑ G. Giuricin, C. Marinoni, L. Ceriani, A. Pisani (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups". Astrophysical Journal. 543: 178–194. doi:10.1086/317070.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  15. ↑ R. B. Tully (1982). "The Local Supercluster". Astrophysical Journal. 257: 389–422. doi:10.1086/159999.
  16. ↑ I. D. Karachentsev (2005). "The Local Group and Other Neighboring Galaxy Groups". Astronomical Journal. 129: 178–188. doi:10.1086/426368.
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