Recent studies of luminous infrared-selected active galactic nuclei ( AGN ) suggest that the reddest , most obscured objects display a higher angular clustering amplitude , and thus reside in higher-mass dark matter halos . This is a direct contradiction to the prediction of the simplest unification-by-orientation models of AGN and quasars . However , clustering measurements depend strongly on the ‘ ‘ mask ’ ’ that removes low-quality data and describes the sky and selection function . We find that applying a robust , conservative mask to WISE -selected quasars yields a weaker but still significant difference in the bias between obscured and unobscured quasars . These findings are consistent with results from previous Spitzer surveys , and removes any scale dependence of the bias . For obscured quasars with \langle z \rangle = 0.99 we measure a bias of b _ { q } = 2.67 \pm 0.16 , corresponding to a halo mass of \log ( M _ { h } / M _ { \odot } h ^ { -1 } ) = 13.3 \pm 0.1 , while for unobscured sources with \langle z \rangle = 1.04 we find b _ { q } = 2.04 \pm 0.17 with a halo mass \log ( M _ { h } / M _ { \odot } h ^ { -1 } ) = 12.8 \pm 0.1 . This improved measurement indicates that WISE -selected obscured quasars reside in halos only a few times more massive than the halos of their unobscured counterparts , a reduction in the factor of \sim 10 larger halo mass as has been previously reported using WISE -selected samples . Additionally , an abundance matching analysis yields lifetimes for both obscured and unobscured quasar phases on the order of a few 100 Myr ( \sim 1 % of the Hubble time ) — however , the obscured phase lasts roughly twice as long , in tension with many model predictions .