Table 5: Normalized Stokes parameters q_B and u_B for different limits of integration $\theta _0$ ; at FWHM, $3^{\circ }$ and $20^{\circ }$ . These parameters represent the optical spurious polarization introduced by PLANCK telescope optics for the studied focal plane configuration (in bold) and other study cases (see text).
30 GHz Position 1 Position 4 Position 27

$\theta _0$ $0.5^{\circ}$ $3.0^{\circ}$ $20.0^{\circ}$ $0.5^{\circ}$ $3.0^{\circ}$ $20.0^{\circ}$ $\bf {0.5^{\circ}}$ $\bf {3.0^{\circ}}$ $\bf {20.0^{\circ}}$

q_B (%) -0.0391 -0.275 -0.275 1.79 3.17 3.10 -0.0057 -0.131 -0.131

u_B (%) 0.00365 0.00117 0.00110 5.2 5.1 5.0 -0.427 -0.204 -0.205

100 GHz Position 1 Position 4 Position 27

$\theta _0$ $0.2^{\circ}$ $3.0^{\circ}$ $20.0^{\circ}$ $\bf {0.2^{\circ}}$ $\bf {3.0^{\circ}}$ $\bf {20.0^{\circ}}$ $0.2^{\circ}$ $3.0^{\circ}$ $20.0^{\circ}$

q_B (%) 0.164 0.093 0.093 -0.138 -0.0398 -0.0422 1.42 2.05 2.05

u_B (%) -0.00418 0.0052 0.0052 -0.51 -0.086 -0.086 2.22 3.44 3.43

**Table 5:** Normalized Stokes parameters q_B and u_B for different limits of integration $\theta _0$ ; at FWHM, $3^{\circ }$ and $20^{\circ }$ . These parameters represent the optical spurious polarization introduced by PLANCK telescope optics for the studied focal plane configuration (in bold) and other study cases (see text).
30 GHz	Position 1	Position 4	Position 27
$\theta _0$	$0.5^{\circ}$	$3.0^{\circ}$	$20.0^{\circ}$	$0.5^{\circ}$	$3.0^{\circ}$	$20.0^{\circ}$	$\bf {0.5^{\circ}}$	$\bf {3.0^{\circ}}$	$\bf {20.0^{\circ}}$
q_B (%)	-0.0391	-0.275	-0.275	1.79	3.17	3.10	-0.0057	-0.131	-0.131
u_B (%)	0.00365	0.00117	0.00110	5.2	5.1	5.0	-0.427	-0.204	-0.205

Source LaTeX | All tables | In the text

100 GHz	Position 1			Position 4			Position 27
$\theta _0$	$0.2^{\circ}$	$3.0^{\circ}$	$20.0^{\circ}$	$\bf {0.2^{\circ}}$	$\bf {3.0^{\circ}}$	$\bf {20.0^{\circ}}$	$0.2^{\circ}$	$3.0^{\circ}$	$20.0^{\circ}$
q_B (%)	0.164	0.093	0.093	-0.138	-0.0398	-0.0422	1.42	2.05	2.05
u_B (%)	-0.00418	0.0052	0.0052	-0.51	-0.086	-0.086	2.22	3.44	3.43