We present results of CO ( 1-0 ) spectroscopic observations of 10 SDSS type 2 quasars ( QSO2 ) at z \sim 0.2-0.3 observed with the 30m IRAM radiotelescope and the Australia Telescope Compact Array .
We report 5 new confirmed CO ( 1-0 ) detections and 1 tentative detection .
They have L ^ { \prime } _ { CO } \sim several \times 10 ^ { 9 } K km s ^ { -1 } pc ^ { 2 } , while upper limits for the non detections are L ^ { \prime } _ { CO } < 3 \sigma = several \times 10 ^ { 9 } K km s ^ { -1 } pc ^ { 2 } .

This study increases the total number of QSO2 with CO measurements at z \la 1 to 20 , with a 50 % detection rate .
The vast majority are at z \sim 0.1-0.4 .
Assuming a conversion factor \alpha =0.8 M _ { \odot } Â ( K km s ^ { -1 } Â pc ^ { 2 } ) ^ { -1 } , the implied molecular gas masses are in the range M _ { H _ { 2 } } \mathrel { \hbox { \hbox to 0.0 pt { \hbox { \lower 2.0 pt \hbox { $ \sim$ } } } \raise 2.0 pt% \hbox { $ < $ } } } 4 \times 10 ^ { 8 } to \sim 5 \times 10 ^ { 9 } M _ { \odot } .
We compare with samples of type 1 quasars ( QSO1 ) , luminous and ultraluminous infrared galaxies .
We find no difference in the molecular gas content of QSO1 and QSO2 of a given infrared luminosity , although the QSO2 sample is affected by small number statistics .
This result , if confirmed , is consistent with the unification model for quasars .

QSO2 fall on the L ^ { \prime } _ { CO } Â vs . z , L ^ { \prime } _ { CO } Â vs . L _ { FIR } Â and \eta = \frac { L _ { FIR } } { L _ { CO } } vs . L _ { FIR } Â correlations defined by quasars at different z .
The location of the QSO2 in these diagrams is discussed in comparison with samples of QSO1 , luminous and ultraluminous infrared galaxies , and high z submm sources .

CO ( 1-0 ) has FWHM \sim 180-370 km s ^ { -1 } when detected , with a variety of kinematic profiles ( single or double horned ) .
In general , the CO line is narrower than [ OIII ] \lambda 5007 , as observed in low z QSO1 , with FWHM _ { [ OIII ] } / FWHM _ { CO } \sim 1-2 ) .
This probably reveals different spatial sizes and/or geometry of the ionized and molecular phases and a higher sensitivity of the [ OIII ] emission to non gravitational motions , such as outflows .
Considering the z \sim 0.1-0.4 range , where CO measurements for both QSO1 and QSO2 exist , we find no difference in FWHM _ { CO } between them , although this result is tentative .
In the unification scenario between QSO1 and QSO2 , this suggests that the distribution of CO gas is not related to the obscuring torus .