6 2009 Fermi Symposium, Washington, D.C., Nov. 2-5 B1641.6+3949, QSO B1640+398, QSO B1641.8+3956, QSO B1641+3958, QSO B1640.5+3944, QSO B1640+396, three more QSOs, FIG. 8: Left: position of 0FGL J1641.4+3939 (larger circle) and WMAP J1642+3948 (smaller circle) with a few potential counterparts (AGN class - open hexagons). Right: CANICA H band light curve of 3C345 compared with the (1-300 GeV) fluxes from 0FGL J1641.4+3939 by Fermi . The discontinuous horizontal lines mark the 2MASS flux and error. The dotted vertical line indicates the change of year. FIG. 7: CANICA - Fermi QSO J0808–0751 light curve. The dots indicate the H band fluxes in mJy, while the histogram and upper limit arrows indicate the 1-300 GeV fluxes and limits in scaled units. The discontinuous hor- izontal line marks the 2MASS flux. The dotted vertical lines indicate the change of year. a Seyfert 1 and a radiogalaxy from SDSS. - potential counterparts for WMAP J1642+3948 are GB6 J1642+3948 = 3C 345, FIRST J164304.3+394836, QSO B1641+3949, ... 3C 345 has a lower χ 2 relative to the combined WMAP and Fermi positions (fig. 8), being the best candidate under the assumption of a common association. Even though more data are desirable, the simultaneous flux changes measured provide evidence for the physical association between 0FGL 1641.4+3939 and 3C345. The EGRET source 3EG J0812–0646 was not in the high priority GLAST/Fermi list, with the association with QSO J0808–0751 been only tentative ( D = 2). WMAP J0808–0750 is somewhat displaced from the 3EG location, but contains this z = 1 . 84 QSO. The rapid flare observed simultaneously in the near in- frared and by Fermi of this source, not in the 0FGL, confirms the identity of the QSO as the γ -ray source. We missed a second flare occurring while the source was on the daylight. The flux increase in the near infrared reached a factor of ten within 50 days. We have selected a sample of mm-wave/ γ -ray bright blazars from the WMAP , 3EG catalogs and 0FGL list. We have monitored these in the near infrared finding correlated variability, which has also allowed the iden- tification or confirmation of some of these objects. The angular distance between WMAP J1642+3948 and 0FGL J1641.4+3939 is 19 . 2 ′ = 1 . 9 σ times the combined positional uncertainty, the association between both objects being tentative only. This is a rather populated region of the sky, where several potential counterparts can be found for each object: - candidate counertparts of 0FGL J1641.4+3939 include 3C 345, QSO B1641.5+3956, QSO We acknowledge the use of 2MASS, WMAP, Fermi, SIMBAD, Vizier and POSS databases. We appreciate the support of the technical staff at the Observatorio Astrof´ısico Guillermo Haro. Acknowledgments C. The identification of 0FGL J1641.4+3939 with 3C 345 VI. SUMMARY B. QSO J0808–0751 eConf C091122