The galaxy NGC 2442 was observed with a REOSC spectrograph, installed in th
e 2.15 m CASLEO telescope, in order to derive galactic parameters from the
observed optical lines and to compare them with the results of radioastrono
mical observations made in the continuum, at 843 MHz, with the MOST and in
the CO lines with the SEST telescope. Recent publications allowed us to ext
end the comparison to results from interferometric observations of H alpha
and HI 21 cm lines and of the continuum at 1415 MHz. The long slit observat
ions were made placing the 5'.8 slit at six different positions on the opti
cal image of the galaxy. The emission line intensity ratios at the nuclear
region indicate that NGC 2442 is a LINER. The electron temperature and volu
me density are T-e approximate to 14 000 K and N-e approximate to 530 cm(-3
), respectively. In contrast, a spectrum of a region 87 " to the NE shows t
he typical characteristics of a H II region. In this case T-e approximate t
o 6500 K and N-e approximate to 10 cm(-3). Good correlations between the di
stributions of intensities, velocity fields and rotation curves have been f
ound for the optical and radio lines. It is shown that the three intensity
peaks along the line at PA = 40 degrees were not resolved by the observatio
ns at radio frequencies. The steep central rotation curve seen in CO has be
en confirmed and improved showing the existence of a disc or a ring, with a
radius of 12 ".5, rotating at 216/sin(i) kms-l. Two velocity components in
three optical spectra obtained in the nuclear region, have been related to
two small H alpha regions close to the nucleus and to the central ring. As
ymmetries in the distributions of the emitting sources and irregularities i
n their velocity fields indicate the need of modelling the galaxy before an
y dynamical study is attempted.