2009 Fermi Symposium, Washington, D.C., Nov. 2-5 3 B. Matching the WMAP catalog with the Fermi bright source list C. Sample overview III. NEAR INFRARED MONITORING IV. CORRELATED INFRARED/ γ -RAY ACTIVITY eConf C091122 The sample is presented in tables II and III. The D column expresses the distance between the WMAP and the γ -ray event in terms of the integer part of the combined positional accuracy; associations with [0] have intersecting error countours and are more likely to be real than those with [2], separated by ≥ 2 σ . Most of the sources have a suitable radio, opti- cal and/or X-ray counterpart, often in the intersection of the WMAP / γ -ray error boxes. In a few cases the candidate counterpart is not unique and the one dis- played is a subjective election. Counterparts in paren- thesis are tentative. We note the following: On August 2007, we started a dedicated monitoring program with up to 60 nights per semester awarded on the 2.1m telescope of the Observatorio Astrof´ısico Guillermo Haro (OAGH), in Cananea, Sonora, Mexico (lat=+31 . $^{05, long=}$−110 . 38). The program consists of optical photometry (BRVI), low resolution spec- troscopy (4000 - 7500 ˚ A) and near infrared JHKs imaging of the sample above, with the addition of high priority GLAST/Fermi sources and targets notified via the multi-wavelength Fermi group. The current study is to lead to programs of follow-up and identi- fication of γ -ray sources using near infrared, optical and mm-wave facilities. Particularly successful has been the JHKs photo- metric survey using the CAnanea Near Infrared CAm- era (CANICA). CANICA is equiped with a Rockwell $^{1024}$× 1024 pixel Hawaii infrared detector working at 75.4 K with standard near infrared filters. The scale plate is 0.32 $^{′′}$/pixel. Observations are usually carried out in series of dithered frames in each filter. Datasets are coadded after correcting for bias and flat-fielding using IRAF based macros. Figure 1 shows the pho- tometric magnitudes measured with CANICA, with detection thresholds around magnitudes 19, 18 and 17 for J, H and Ks respectively, i.e. about two mag- nitudes fainter than 2MASS. We have found correlated infrared and γ -ray cor- relations with little or no evidence for time delays in our sample. We show here joint CANICA H band (1.6 µ m ⇒ 0 . 76eV) and Fermi (1 − 300 GeV) light curves, normalizing the maximum γ -ray flux to the maximum H-band flux and setting both zeros at the same level. We are currently studying the infrared • WMAP J0051–0927 :: 0FGL J0050.5–0928 has a preferred association with the Bl Lac object PKS 0048–071 = PHL 856; the radiogalaxy FIRST J005051.9–092529 is an alternative. • WMAP J0237+2848 :: 0FGL J0238.4+2855 :: 3EG J0239+2815. This is listed as a low confi- dence Fermi association with 4C +28.07 in [2]. The WMAP and Fermi boxes match, both con- taining 4C +28.07. All are somewhat outside the EGRET box. • WMAP J0319+4131 :: 0FGL J0320.0+4131 is identified with the radiogalaxy NGC 1275. We note that the radiogalaxy Cen A is excluded of this study by the WMAP Galactic mask. • WMAP J0423–0120 :: 0FGL J0423.1–0112 :: 3EG J0422–0102. This is a low confidence Fermi association with PKS 0420–014, which is at the center of the WMAP circle. • WMAP J0909+0119 :: 0FGL J0909.7+0145. The 0FGL error radius is 17 $^{′}$, the WMAP and 0FGL positions differing by 25 $^{′}$. PKS 0907+022 is a low confidence Fermi association not compatible with WMAP . 4C+01.24 (PKS = QSO B0906+015) is inside the WMAP box and marginally compatible with the Fermi source. The Fermi bright source list (0FGL), made public in February 2009, consists of 205 bright γ -ray sources detected with significance √$_{T S >}$ 10 in the first three months of observations [2]. Of these, 121 are of the AGN class, mostly blazars [3]. The 0FGL list has 122 objects outside the WMAP Galactic mask, which we compared with the respective WMAP and Fermi positions. The improved positional accuracy of Fermi , in the 4 ′ − 10 ′ range, results in only 0.82 spurious coincidences expected. We found 54 matches between WMAP and the 0FGL, 25 of which are common with EGRET sources and 29 are independent. • WMAP J1517–2421 has two possible EGRET counterparts but only one (3EG J1517–2538) is compatible with the 0FGL source. • WMAP J1642+3948 is 19 ′ away from 0FGL J1641.4+3939, which has an posi- tional error of 9 . 5 $^{′}$, making the association tentative. There are suitable candidates for both sources, with 3C345 being positionally the best common counterpart, as discussed in § V C. While there is no 3EG source associa- tion, we note the revised EGRET counterpart EGR J1642+3940 [8].