RevMexAA (Serie de Conferencias), 12, 38-38 (2002)

atios obtained earlier are used in this process. To calculate the T e and N e the user has to provide a line ratio 1 Facultad de Ciencias, UABC, Ensenada, Mexico. Instituto de Astronoma, UNAM, Ensenada, Mexico. Fig. 1. Screenshot of xAbIon. (from [O III] or [N II] to calculate the temperature and [S II] for density), the energy level transitions and an initial value for the N e or the T e , respectively. After obtaining the T e and N e , the ion abundances by number for each ion can be calculated. First, the ionic abundance ratio is estimated and recognized automatically by the system. Then, the ionic abundances by number can be calculated. This process is repeated until the ionic abundances for all the ions are computed. Both the rst and second phase write the results in a L A T E X formatted le. The le written by xGalRed contains a table with the ions, their wavelength, observed and dereddened uxes and the extinction law. xAbIon write its results in the correspondin