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(abridged)The majority of Active Galactic Nuclei (AGN) suffer fromsignificant obscuration by surrounding dust and gas. X-ray surveys in the 2-10keV band will miss the most heavily-obscured AGN in which the absorbing columndensity exceeds $\sim10^{24}$cm$^{-2}$ (the Compton-thick AGN). It is thereforevital to know the fraction of AGN that are missed in such X-rays surveys and todetermine if these AGN represent some distinct population in terms of thefundamental properties of AGN and/or their host galaxies. In this paper wepresent the analysis of \textit{XMM-Newton} X-ray data for a complete sample of17 low-redshift Type 2 Seyfert galaxies chosen from the Sloan Digital SkySurvey based solely on the high observed flux of the [OIII]$\lambda$5007emission-line. This line is formed in the Narrow Line Region hundreds ofparsecs away from the central engine. Thus, unlike the X-ray emission, it isnot affected by obscuration due to the torus surrounding the black hole. Ittherefore provides a useful isotropic indicator of the AGN luminosity. Asadditional indicators of the intrinsic AGN luminosity, we use the Spitzer SpaceTelescope to measure the luminosities of the mid-infrared continuum and the[OIV]25.89$\mu$m narrow emission-line. We then use the ratio of the 2-10 keVX-ray luminosity to the [OIII], [OIV], and mid-infrared luminosities to assessthe amount of X-ray obscuration and to distinguish between Compton-thick andCompton-thin objects. We find that the majority of the sources suffersignificant amounts of obscuration: the observed 2-10 keV emission is depressedby more than an order-of-magnitude in 11 of the 17 cases (as expected forCompton-thick sources).

XMM-Newton Observations of a Complete Sample of Optically Selected Type 2 Seyfert Galaxies