We present and analyze ROSAT–PSPC observations of eight Seyfert 2 galaxies , two Seyfert 1/QSOs , and one IR–luminous non–Seyfert .
These targets were selected from the Extended 12 \mu m Galaxy Sample and , therefore , have different multiwavelength properties from most ( optically or X–ray selected ) Seyferts previously observed in the soft X–rays .
The targets were also selected as having atypical X–ray fluxes among their respective classes , e.g .
relatively X–ray strong Seyfert 2s and X–ray weak Seyfert 1/QSOs .

Comparing our observations with those from the ROSAT All–Sky Survey , we find variability ( of a factor of 1.5—2 in flux ) in both of the Seyfert 1/QSOs , but in none of the Seyfert 2s .
Both variable objects have steeper photon indices in the more luminous state , with the softest ( < 1.0 keV ) flux varying the most .
The timescales indicate that the variable component arises from a region less than a parsec in size .

Fitting the spectra to an absorbed power–law model , we find that both the Seyfert 2s and the Seyfert 1/QSOs are best fit with a photon index of 3.1—3.2 .
This is in agreement with the average photon index of a sample of Markarian Seyfert 2s observed by Turner , Urry , & Mushotzky ( 1993 ) , indicating that most Seyfert 2s , even those displaying a wide variety multiwavelength of characteristics , as well as some Seyfert 1/QSOs , have a photon index much steeper than the canonical ( Seyfert 1 ) value of \sim 1.7 .
One possible explanation is that these objects have a flatter continuum plus a soft ( < 1.0 keV ) excess in the form of high–EW iron and/or oxygen fluorescence lines , a black–body or even a thermal plasma .
Alternatively , the underlying continuum may indeed be steep , powered by a different physical mechanism than that which produces the flat continua in other Seyfert 1s/QSOs .

We imaged one Seyfert 2 ( NGC 5005 ) with the ROSAT HRI , finding about 13 % of the soft X–rays to come from an extended source .
This object also has the most evidence from spectral fitting for an extra contribution to the soft–X–ray flux in addition to a power–law component , indicating that different components to the soft X–ray spectrum of this object ( and likely of other X–ray–weak Seyferts ) may come from spatially distinct regions .