If the gas in filaments and halos shares the same velocity field than the luminous matter , it will generate measurable temperature anisotropies due to the Kinematic Sunyaev-Zeldovich effect .
We compute the distribution function of the KSZ signal produced by a typical filament and show it is highly non-gaussian .
The combined contribution of the Thermal and Kinematic SZ effects of a filament of size L \simeq 5 Mpc and electron density n _ { e } \simeq 10 ^ { 3 } m ^ { -3 } could explain the cold spots of \delta \sim - 200 \mu K on scales of 30 ^ { \prime } found in the Corona Borealis Supercluster by the VSA experiment .
PLANCK , with its large resolution and frequency coverage , could provide the first evidence of the existence of filaments in this region .
The KSZ contribution of the network of filaments and halo structures to the radiation power spectrum peaks around l \sim 400 , a scale very different from that of clusters of galaxies , with a maximum amplitude l ( l + 1 ) C _ { l } / 2 \pi \sim 10 - 25 ( \mu K ) ^ { 2 } , depending on model parameters , i.e. , \sigma _ { 8 } and the Jeans length .
About 80 % of the signal comes from filaments with redshift z \leq 0.1 .
Adding this component to the intrinsic Cosmic Microwave Background temperature anisotropies of the concordance model improves the fit to WMAP 3yr data by \Delta \chi ^ { 2 } \simeq 1 .
The improvement is not statistically significant but a more systematic study could demonstrate that gas could significantly contribute to the anisotropies measured by WMAP .