Lindblad et al. 2 tion intensities and velocities over the central region of NGC 1358 along the slit as derived with the SPLOT routine. The solid line shows the velocities of the stellar component derived from all the stellar features. As zero- point of the abscissa we have chosen the position of the maximum of the continuum (cp. Fig. 5). In Fig. 3 the emission line velocities, and in particular H α and [NII], show a rapidly increasing rotation curve with a maxi- mum about 4 ′′ from the center. Dumas et al. (2007) show that this nuclear emission line disk should have a kinematic major axis directed close to PA 90 $^{◦}$, i.e. only 5 ◦ from the PA of the present slit position, but almost perpendicular to the kinematic major axis of the stellar bulge. Within 2 ′′ from the center, on the East side, we see a reversal, or a dip, in the apparent rotation curve of the emission lines. In the NaD absorption line velocities, this dip is absent. From Fig. 3 it is clear that the emission line velocity dip corresponds to an excess of the emission line intensities up to 2 ′′ from the nucleus. The NaD lines show no such asymmetry and the position of the maxi- mum absorption coincides with that of the maximum of continuum emission. Fig. 1.— NGC 1358 optical image obtained with the EFOSC2 spectrograph on the ESO 2.2 m telescope. The straight line indi- cates the position of the slit (PA 85 $^{◦}$) for the spectrum discussed in the present paper. The slit crosses the spiral arms at about 35 ′′ galactocentric distance. The simplest interpretation of the gas kinematics ob- served in Fig. 3 seems to be a central point source and a jet-like outflow that are superimposed on a gaseous disk rotating in the potential of the stellar bulge. Preliminary simulations along the scheme presented below suggested that the jet outflow line of sight velocities should be of the order of − 200 km s − $^{1}$. We have observed NGC 1358 with the EFOSC2 spec- trograph on the ESO 2.2 m telescope and obtained a long slit spectrum over the nucleus in PA 85 ◦ on December 6th 1996. With this position angle a star was brought on the slit, which gave a check on the position angle as well as the PSF. The slit cuts the main spiral arms about 35 ′′ East and West of the nucleus (Fig. 1). The spectrum covered the wavelength region 4075 – 7000 ˚ A, where the strongest spectral features are the H β λ 4861, [OIII] λ 4960, 5007, H α λ 6563, [NII] λ 6548, 6584, [SII] λ 6716, 6731 emission lines and the Mgb and NaD absorption lines (Fig. 2). In the spatial direction the pixel size corresponds to 0 . $^{′′}$26. As flux calibration star Hiltner 600 was chosen. A support for this scenario is found in the [SII] emis- sion line profiles from HST/STIS spectra published by Rice et al. (2006) reproduced in Fig. 4. One spec- trum is observed through a 1 . $^{′′}$0 aperture and another through an aperture of 0 . $^{′′}$2. The applied Gaussian fits have been constrained to enforce the relative separation between the [SII] doublets. In both spectra a strong com- ponent is seen in the two lines with very similar flux ratios in the two apertures. In the 0 . $^{′′}$2 aperture spec- trum a secondary blueshifted component is seen. We have assumed 10000 K electron temperature and used the atomic parameters of Mendoza (1983) and Osterbrock (1989) to calculate the electron density from these spec- tra. The calculated relative fluxes yield for the spatially extended and dominating component an electron density of 793 cm − $^{3}$. The central component, only appearing in the 0 . $^{′′}$2 aperture spectrum, has a density of 1749 cm− $^{3}$. This denser component is fainter and blueshifted with a velocity difference between the strong and faint compo- nents of 214 km s − $^{1}$, being the innermost part of the jet, respectively. Figure 2 shows two fully reduced and flux calibrated example spectra obtained from the long slit spectrum. To derive the distribution and kinematic parameters, we have fitted the galaxy spectrum in two different ways. Firstly, by using the standard IRAF routine SPLOT to fit Gaussians to the emission and absorption lines, and secondly, by using the simultaneous gas and absorption line fitting IDL routine developed by Sarzi et al. (2006) and Falc´ on-Barroso et al. (2006). The latter method is designed to separate the relative contributions of stellar continuum and absorption features and nebular emission in spectra of galaxies, while measuring the gas emission and kinematics. Accordingly, it uses the routine of Cap- pellari & Emsellem (2004) to find the best fitted lin- ear combination of single stellar population spectra by Vazdekis (1999) to build a stellar spectrum representa- tive of the observed galaxy spectrum for this wavelength range and with the same spectral resolution. Simulta- neously, the nebular emission lines have been fitted, and the results yield the gas and stellar kinematics. We found that both routines deliver fully comparable gas distribu- tion and kinematics, with the advantage that the IDL routine has derived a much more robust stellar kinemat- ics. Figure 3 shows the run of [NII] λ 6584, H α , [OIII] λ 5007 and H β emission as well as NaD absorp- Most remarkably the velocity dip to the East of the nucleus is larger for [OIII] than for the [NII] and H α lines and apparently still larger for H β . Outside the dip [OIII] shows smaller rotational velocities than H α and [NII]. The stellar velocities show only a very slight variation over the region in agreement with the slight positive gra- dient expected for the stellar velocity field of Dumas et al. (2007) with the present slit inclined 74 ◦ to the stellar kinematic major axis. The NaD absorption in front of the nucleus appears to have a higher redshift than the average stellar template redshift, which also is indicated by the shape of the line residuals in Fig. 2.