content_image/402765.jpg content_image/402766.jpg
<img src='content_image/402765.jpg'>

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. 

## C. The identification of 0FGL J1641.4+3939 with 3C 345 

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 

## B. QSO J0808–0751 

B1641.6+3949, QSO B1640+398, QSO B1641.8+3956, QSO B1641+3958, QSO B1640.5+3944, QSO B1640+396, three more QSOs, 

<img src='content_image/402766.jpg'>

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, ... 2 

3C 345 has a lower χ 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. 

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. 

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. 

## VI. SUMMARY 

## Acknowledgments 

