A comprehensive approach to analyzing the XMM-Newton data of Seyfert 1
  galaxies
  Aims. We seek a comprehensive analysis of all the information provided by the
XMM-Newton satellite of the four Seyfert 1 galaxies ESO 359-G19, HE 1143-1810,
CTS A08.12, and Mrk 110, including the UV range, to characterize the different
components that are emitting and absorbing radiation in the vicinity of the
active nucleus.
  Methods. The continuum emission was studied through the EPIC spectra by
taking advantage of the spectral range of these cameras. The high-resolution
RGS spectra were analyzed to characterize the absorbing and emission line
features that arise in the spectra of the sources. All these data, complemented
by information in the UV, are analyzed jointly in order to achieve a consistent
characterization of the observed features in each object.
  Results. The continuum emission of the sources can be characterized either by
a combination of a power law and a black body for the weakest objects or by two
power law components for the brightest ones. The continuum is not absorbed by
neutral or ionized material in the line of sight to any of these sources. In
all of them we have identified a narrow Fe-Kalpha line at 6.4 keV. In ESO
559-G19 we also find an FeXXVI line at about 7 keV. In the soft X-rays band, we
identify only one OVII line in the spectra of HE 1143-1810 and CTS A08.12, and
two OVII-He alpha triplets and a narrow OVIII-Ly alpha emission line in Mrk
110.
  Conclusions. Not detecting warm material in the line of sight to the low
state objects is due to intrinsically weaker or absent absorption in the line
of sight and not to a low signal-to-noise ratio in the data. Besides this, the
absence of clear emission lines cannot be fully attributed to dilution of those
lines by a strong continuum.
