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For refcode 1988MNRAS.234..131P:
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Copyright by Royal Astronomical Society. 1988MNRAS.234..131P Dark and visible matter in spiral galaxies M. Persic and P. Salucci Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Osservatorio Astronomico, via G. B. Tiepola 11, I-34131 Trieste, Italy SISSA, Strada Costiera 11, I-34014 Trieste, Italy Physics Deparment, Durham University, Durham DH1 3LE Accepted 1988 February 19. Received 1988 February 19; in original form 1987 March 25 Summary. Exploiting relevant information from the profiles of rotation curves, we calculate the dark-to-luminous mass ratio within the disc size for a sample of 43 spiral galaxies. The values we find, while proving the ubiquitous presence of dark matter, vary with luminosity. Faint and bright galaxies are found to be respectively halo- and disc-dominated in the disc regions. The luminosity sequence turns out to be a dark-to-luminous sequence. The Tully-Fisher correlation is justified as connected with the equilibrium condition of a thin disc embedded in a spherical halo. The dynamical effect of dark matter does not disrupt such a centrifugal equilibrium, because the dark-matter mass fraction is a smooth function of luminosity. By removing the dark-matter contribution from the velocity at the disc edge, the dispersion affecting the luminosity-kinematics relation is dramatically decreased as compared with the conventional Tully-Fisher correlation ({DELTA}{delta} ~0.3 mag). Comparison with stellar evolution models shows that the dynamically computed (M/L_B_)_disc_ ratios are able to explain the colours of spiral galaxies in a scenario involving a 10-Gyr star-formation phase with H_0_=75 km s^-1^ Mpc^-1^.
Retrieve 43 NED objects in this reference.
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