2009 Fermi Symposium, Washington, D.C., Nov. 2-5 4 FIG. 2: Joint CANICA - Fermi light curve of PKS 0235+164. CANICA is given by the (black) points while Fermi fluxes form the (red) histogram with error bars. The discontinuous horizontal line marks the 2MASS flux. The dotted vertical lines indicate the change of year. FIG. 1: CANICA photometric measurements of mm- wave/ γ -ray sources. We show only detections. color behavior of our sample during flares and con- straining possible delays in the timing of near infrared flares relative to the γ -ray ones. Our current results on 3C 454.3 are presented in [9]. relative quiescence since (fig. 3). PKS 1510–89 is the high confidence counter- part of 3EG J1512–0849, WMAP J1512–0904 and 0FGL J1512.7–0905, with an excellent positional match between all data. We started monitoring PKS 1510–89 in early 2008, a few months prior to the Fermi launch, when the flux fluctuated around the 2MASS reference value. We caught a simultaneous infrared - γ -ray flare on JD 2454924 and the subsequent decay a month later. PKS 0235+164 is positionally coincident with WMAP J0238+1637, mm-wave source coincident with 3EG J0237+1635 = 0FGL J0238.6+1636. The WMAP source is labelled as probable variable. Fig- ure 2 shows the joint H band and 1-300 GeV fluxes scaled. The near infrared flux at the end of 2008 and beginning of 2009 matched the 2MASS values. On JD2454715 we found PKS 0235+164 almost three magnitudes brighter, prior to peaking 25 days later - in coincidence with the Fermi flare. C. PKS 1510–089 A. PKS 0235+164 V. SOURCE IDENTIFICATIONS A. The identification of QSO B0133+476 B. PKS 0454–234 QSO B0133+476 is a rather active quasar first catalogued originally as DA55 in the Dominion DA 1420 MHz survey [10]. Also known as Mis V1436, archival optical data exists since at least 1953, when it was around magnitude R=18.7. This object has been monitored by other groups since 2007, when it was found to be 4.5 magnitudes brighter. Its optical variability is well documented in [11]. The WMAP and Fermi error circles in this region of the sky intersect close to the center of the 3EG J0456– 2338 error box. PKS 0454–234 is within the intersec- tion, in a neat positional match. We started monitor- ing on JD 2454748, when the near infrared flux was 0.85 magnitudes above the 2MASS reference value. The source flared by a factor of nearly 3 in the next 50 days to drop to a half 18 days later. The near in- frared peak seems delayed by about a week relative to the 1-300 GeV maximum. The AGN has been in This object has no EGRET counterpart, the only evidence for γ -ray emission prior to the Fermi launch eConf C091122