Masas de la galaxias con formación estelar de la exploración UCM

Laburpena

The main purpose of this work is to find a relationship between the virial and dynamical masses and the stellar masses of the UCM galaxies exploration (UCM Survey). The UCM Survey provided a representative sample of star-forming galaxies in the local universe. To carry out this project we use the long-slit spectra of the emission line H of these galaxies, obtained by ourselves, calculating the kinematic (virial) and dynamic masses (rotational curve). We have measured the velocity dispersion in each galaxy, assuming that speed dispersion originated from the gravitational well and that the effect of turbulence is negligible. With this rate of dispersion and by the virial theorem, we have calculated the virial mass. We have calculated, also, the rotational speed in each galaxy along the long slit of the spectrograph and these speed have been used for the rotational curve (inclination corrected) in galaxies with a general velocity field. With these data we calculated the dynamical mass. Stellar masses, calculated in 2003 (Pablo Perez-Gonzalez. 2003. Thesis) by stellar populations modeling techniques, have been updated by the initial mass function (IMF) Salpeter and Chabrier IMF, for this work . We compared the virial and dynamical masses with stellar masses and calculated correlations, obtaining an estimate of any of them when we have the other in different z explorations. We have conplemented the study of the properties of UCM galaxies shows addressing the study of the dynamical masses by rotational curves, and virial masses (internal kinematics). This work provides a link between virial mass and the stellar mass. We have obtained an applicable calibration for future exploration of galaxies at higher z and we can estimate the stellar mass from spectroscopic measurement of the velocity dispersion, or, virial mass from the stellar mass measurement.