## B. Matching the WMAP catalog with the Fermi bright source list 

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. 

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: 

• 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 = 

## C. Sample overview 

QSO B0906+015) is inside the WMAP box and marginally compatible with the Fermi source. 

• 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]. 

## III. NEAR INFRARED MONITORING 

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. 

## IV. CORRELATED INFRARED/ γ -RAY ACTIVITY 

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 

