We present a new technique for calculating the fraction of dark material within the optical radius of spiral galaxies. The method employs the well-established observational result that spiral galaxies have similar central surface brightnesses, as well as published stellar synthesis evolutionary models, color-magnitude relations and optical rotation curves. No assumptions about the dark matter distribution are necessary. We find that the ratio of disk-to-dynamical mass within the optical radius increases roughly as L(B)0.4. This is in good agreement with the results of Persic and Salucci which are derived from independent considerations.
|Titolo:||THE DARK MATTER CONTENT OF SPIRAL GALAXIES|
|Autori:||SALUCCI P; ASHMAN KM; PERSIC M|
|Rivista:||THE ASTROPHYSICAL JOURNAL|
|Data di pubblicazione:||1991|
|Digital Object Identifier (DOI):||10.1086/170485|
|Appare nelle tipologie:||1.1 Journal article|