Messier Index/M94

Messier 94J. L. Tonry, A. Dressler, J. P. Blakeslee, E. A. Ajhar, A. B. Fletcher, G. A. Luppino, M. R. Metzger, C. B. Moore The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances Astrophysical Journal 2001 546 2 681–693 http://adsabs.harvard.edu/abs/2001ApJ...546..681T 10.1086/318301I. 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 Galaxy flow in the Canes Venatici I cloud Astronomy and Astrophysics 2003 398 467–477 http://adsabs.harvard.edu/abs/2003A&A...398..467K 10.1051/0004-6361:20021598average(17.0 ± 1.4, 15 ± 2) = ((17.0 + 15) / 2) ± ((1.42 + 22)0.5 / 2) = 16.0 ± 1.3 File:Messier object 094.jpg M94: Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF J2000 Canes VenaticiR. W. Sinnott, editor The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer 1988 Sky Publishing Corporation and Cambridge University Press 0-933-34651-4 12 50 53.1 NASA/IPAC Extragalactic Database Results for M94 http://nedwww.ipac.caltech.edu/ 2006-11-09 +41 07 14 8.99 (R)SA(r)ab, LINER NGC 4736, UGC 7996, PGC 43495 Messier 94 (also known as NGC 4736) is a spiral galaxy in the constellation Canes Venatici. It was discovered by Pierre Méchain in 1781, Kepple George Robert Glen W. Sanner The Night Sky Observer's Guide, Volume 2 Willmann-Bell, Inc. 1998 0-943396-60-3 51 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.J. Kormendy, R. C. Kennicutt, Jr. Secular Evolution and the Formation of Pseudobulges in Disk Galaxies Annual Reviews of Astronomy and Astrophysics 2004 42 603–683 http://adsabs.harvard.edu/abs/2004ARA&A..42..603K 10.1146/annurev.astro.42.053102.134024 The galaxy is also notable in that it has two ring structures. Nucleus M94 is classified as having a low ionization nuclear emission region (LINER) nucleus. L. C. Ho, A. V. Filippenko, W. L. W. Sargent A Search for "Dwarf" Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies Astrophysical Journal Supplement 1997 112 315–390 http://adsabs.harvard.edu/abs/1997ApJS..112..315H 10.1086/313041 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.C. Muñoz-Tuñón, N. Caon, J. Aguerri, L. Alfonso The Inner Ring of NGC 4736: Star Formation on a Resonant Pattern Astronomical Journal 2004 127 58–74 http://adsabs.harvard.edu/abs/2004AJ....127...58M 10.1086/380610 Pseudobulge In a paper published in 2004, John Kormendy and Robert Kennicutt argued that M94 contains a prototypical pseudobulge. 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). 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). 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 J. Jałocha, Ł. Bratek, and M. Kutschera Is Dark Matter Present in NGC 4736? An Iterative Spectral Method for Finding Mass Distribution in Spiral Galaxies The Astrophysical Journal 2008 679 373–378 http://de.arxiv.org/pdf/astro-ph/0611113v3 10.1086/533511 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.http://space.newscientist.com/article/dn13280-galaxy-without-dark-matter-puzzles-astronomers.html Galaxy without dark matter puzzles astronomers 06 February 2008 NewScientist.com news service Stephen Battersby 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.R. B. Tully 1988 Nearby Galaxies Catalog Cambridge University Press Cambridge 0-521-35299-1A. Garcia General study of group membership. II - Determination of nearby groups Astronomy and Astrophysics Supplement 1993 100 47–90 http://adsabs.harvard.edu/abs/1993A&AS..100...47GG. Giuricin, C. Marinoni, L. Ceriani, A. Pisani Nearby Optical Galaxies: Selection of the Sample and Identification of Groups Astrophysical Journal 2000 543 178–194 http://adsabs.harvard.edu/abs/2000ApJ...543..178G 10.1086/317070 This group is one of many that lies within the Virgo Supercluster (i.e. the Local Supercluster). R. B. Tully The Local Supercluster Astrophysical Journal 1982 257 389–422 http://adsabs.harvard.edu/abs/1982ApJ...257..389T 10.1086/159999 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.I. D. Karachentsev The Local Group and Other Neighboring Galaxy Groups Astronomical Journal 2005 129 178–188 http://adsabs.harvard.edu/abs/2005AJ....129..178K 10.1086/426368 External links Galaxy Messier 94 at the astro-photography site of Mr. T. Yoshida. SEDS: Spiral Galaxy M94 References