2009 Fermi Symposium, Washington, D.C., Nov. 2-5 5 FIG. 5: Positional circumstance of QSO B0133+476. Left: the VHE photon error circle is shown at α ∼ 23 $^{◦}$, δ ∼ 48 . 6 $^{◦}$, with the almost concentric WMAP and Fermi circles in the middle. Right: a zoom panel showing the 4 ′ WMAP circle contained in the 7 ′ Fermi position. QSOB0133+476 is indicated by the open hexagon and an asterix. FIG. 3: Joint CANICA - Fermi light curve of PKS 0454– 234. T he discontinuous horizontal line marks the 2MASS flux. T he dotted vertical lines indicate the change of year. FIG. 6: CANICA light curve of QSO B0133+47. The flaring at the end of 2008 is clearly visible, at a factor of 10 above the 2MASS flux levels indicated by the dashed horizontal line. FIG. 4: CANICA - Fermi light curve of PKS 1510–089. The discontinuous horizontal line marks the 2MASS flux. The dotted vertical lines indicate the change of year. emission activity. Our report of near infrared flaring from data taken between JD 2454788 and 2454795 [12] was followed by the Fermi detection report, at a flux level above the EGRET limiting sensitivity [13]. The infrared light curve is shown in figure 6. The ob- ject was caught undergoing a rapid flare which has declined relatively slowly during 2009, but always at levels above 2MASS. $^{being its marginal closeness to a 85(}$±38)GeV photon. The unprovable association of this single photon with QSO B0133+476 is of interest as its energy is close to the pair absorption EBL limit for the redshift of the object, z = 0 . 859. If true, this association would in- dicate the potential of this source for testing the EBL horizon using Fermi , specially under phases of high eConf C091122