Messier 94

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For other uses, see M94 (disambiguation).

Messier 94[1][2][3]
Messier 94.jpg
M94 Galaxy
Observation data
Epoch J2000
Constellation Canes Venatici[4]
Right ascension 12h 50m 53.1s[5]
Declination +41° 07′ 14″[5]
Apparent dimension (V) 11.2 × 9.1 moa[5]
Apparent magnitude (V)8.99[5]
Characteristics
Type(R)SA(r)ab,[5] LINER[5]
Astrometry
Heliocentric radial velocity 308 ± 1[5] km/s
Redshift 0.001027 ± 0.000005[5]
Galactocentric velocity 360 ± 3[5] km/s
Distance 16.0 ± 1.3 Mly (4.91 ± 0.40 Mpc)
Other designations
NGC 4736, UGC 7996, PGC 43495[5]

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 has two ring structures.[5]

Nucleus[edit]

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[edit]

Detail of the central area of M94.

M94 contains both an inner ring with a diameter of 70 arcseconds and an outer ring with a diameter of 600 arcseconds. 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]

A 2009 study[10] conducted by an international team of astrophysicists revealed that the outer ring of M94 is not a closed stellar ring, as historically attributed in the literature, but a complex structure of spiral arms when viewed in mid-IR and UV. The study found that the outer disk of this galaxy is active. It contains approximately 23% of the galaxy's total stellar mass and contributes about 10% of the galaxy's new stars. In fact, the star formation rate of the outer disk is approximately two times greater than the inner disk because it is more efficient per unit of stellar mass.

There are several possible external events that could have led to the origin of M94's outer disk including the accretion of a satellite galaxy or the gravitational interaction with a nearby star system. However, further research found problems with each of these scenarios. Therefore, the report concludes that the inner disk of M94 is an oval distortion which led to the creation of this galaxy's peripheral disk.

Pseudobulge[edit]

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[edit]

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[edit]

In 2008 a study was published[11] showing 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 do not 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.[12] This result has yet to be confirmed or accepted by other research groups, however, and has not actually been tested against the predictions of standard galaxy formation models.

Galaxy group information[edit]

M94 is one of the brightest galaxies within the M94 Group, a group of galaxies that contains between 16 and 24 galaxies.[13][14][15] This group is one of many that lies within the Virgo Supercluster (i.e. the Local Supercluster).[16] 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][17]

Multi-wavelength views[edit]

M94 as seen in at various wavelengths of light

See also[edit]

  • NGC 1512, a galaxy with a similar inner ring.

References[edit]

  1. ^ a b J. L. Tonry; A. Dressler; J. P. Blakeslee; E. A. Ajhar; et al. (2001). "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances". Astrophysical Journal. 546 (2): 681–693. arXiv:astro-ph/0011223 Freely accessible. Bibcode:2001ApJ...546..681T. doi:10.1086/318301. 
  2. ^ a b c I. D. Karachentsev; M. E. Sharina; A. E. Dolphin; E. K. Grebel; et al. (2003). "Galaxy flow in the Canes Venatici I cloud". Astronomy and Astrophysics. 398 (2): 467–477. arXiv:astro-ph/0210414 Freely accessible. Bibcode:2003A&A...398..467K. doi:10.1051/0004-6361:20021598. 
  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, 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 0-933346-51-4. 
  5. ^ a b c d e f g h i j k "NASA/IPAC Extragalactic Database". Results for M94. Retrieved 2006-11-09. 
  6. ^ Kepple, George Robert; Glen W. Sanner (1998). The Night Sky Observer's Guide. Vol. 2. Willmann-Bell. p. 51. ISBN 0-943396-60-3. 
  7. ^ a b J. Kormendy; R. C. Kennicutt Jr. (2004). "Secular Evolution and the Formation of Pseudobulges in Disk Galaxies". Annual Review of Astronomy and Astrophysics. 42 (1): 603–683. arXiv:astro-ph/0407343 Freely accessible. Bibcode:2004ARA&A..42..603K. doi:10.1146/annurev.astro.42.053102.134024. 
  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 (2): 315–390. arXiv:astro-ph/9704107 Freely accessible. Bibcode:1997ApJS..112..315H. doi:10.1086/313041. 
  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 (1): 58–74. Bibcode:2004AJ....127...58M. doi:10.1086/380610. 
  10. ^ I. Trujillo; I. Martinez-Valpuesta; D. Martinez-Delgado; J. Penarrubia; et al. (2009). "Unveiling the Nature of M94's (NGC4736) Outer Region: A Panchromatic Perspective". Astrophysical Journal. 704 (1): 618–628. arXiv:0907.4884 Freely accessible. Bibcode:2009ApJ...704..618T. doi:10.1088/0004-637X/704/1/618. 
  11. ^ J. Jałocha; Ł. Bratek; M. Kutschera (2008). "Is Dark Matter Present in NGC 4736? An Iterative Spectral Method for Finding Mass Distribution in Spiral Galaxies". Astrophysical Journal. 679 (1): 373–378. arXiv:astro-ph/0611113 Freely accessible. Bibcode:2008ApJ...679..373J. doi:10.1086/533511. 
  12. ^ Battersby, Stephen (6 February 2008). "Galaxy without dark matter puzzles astronomers". New Scientist. 
  13. ^ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge University Press. ISBN 0-521-35299-1. 
  14. ^ 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. 
  15. ^ 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 Freely accessible. Bibcode:2000ApJ...543..178G. doi:10.1086/317070. 
  16. ^ R. B. Tully (1982). "The Local Supercluster". Astrophysical Journal. 257: 389–422. Bibcode:1982ApJ...257..389T. doi:10.1086/159999. 
  17. ^ I. D. Karachentsev (2005). "The Local Group and Other Neighboring Galaxy Groups". Astronomical Journal. 129 (1): 178–188. arXiv:astro-ph/0410065 Freely accessible. Bibcode:2005AJ....129..178K. doi:10.1086/426368. 

External links[edit]

Coordinates: Sky map 12h 50m 53.1s, +41° 07′ 14″

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