2009 Fermi Symposium, Washington, D.C., Nov. 2-5 3 Table I VERITAS AGN Detections. The only non-blazar object is the radio galaxy M 87. The blazars discovered at VHE by VERITAS are marked with a dagger. ( z = 0 . 341) detected in the VHE band. In addition, VER J0521+211, likely associated with the radio-loud AGN RGB J0521.8+2112, was detected by VERTAS in ∼ 4 h of observations in October 2009 [23]. These observations were motivated by its identification as a > 30 GeV γ -ray source in the public Fermi-LAT data. Its VHE flux is 5% of the Crab Nebula flux, placing it among the brightest VHE blazars detected in recent years. VERITAS later observed even brighter VHE flaring from VER J0521+211 in November 2009 [24], leading to deeper VHE observations. ( ∼ 5.5 σ ; 3% Crab flux above 300 GeV; Γ VHE ∼ 2 . 7) during VERITAS observations from December 2008 to March 2009. The initial announcement of the VHE discovery [19] led to its discovery above 1 GeV in the Fermi-LAT data using a special analysis. RBS 0413, a relatively distant HBL (z=0.19), was observed for 16 h good-quality live time in 2008-09 $^{2}$. These data resulted in the discovery of VHE gamma-rays ( > 270 γ , ∼ 6 σ ) at a flux ( > 200 GeV) of ∼ 2% of the Crab Neb- ula flux. The discovery [20] was announced simultane- ously with the LAT MeV-GeV detection. The VHE and other MWL observations, including Fermi-LAT data, for each of these three sources will be the sub- ject of a joint publication involving both the VERI- TAS and LAT collaborations. The successful VHE discovery observations by VERITAS of three blazars was motivated primarily by results from the first year of LAT data taking. In particular, the VHE detections of PKS 1424+240 [21] and 1ES 0502+675 [22] were the result of VERITAS observations triggered by the inclusion of these objects in the Fermi-LAT Bright AGN List [13]. The former is only the third IBL known to emit VHE gamma- rays, and the latter is the most distant BL Lac object During the first three seasons of VERITAS obser- vations, pre-planned extensive MWL campaigns were organized for three blazars 1ES 2344+514 (2007-08), 1ES 1218+304 (2008-09) and 1ES 0229+200 (2009- 10 - ongoing). In addition, numerous ToO MWL- observation campaigns were performed. These include campaigns for every blazar/AGN discovered by VER- ITAS, and all include Swift (XRT and UVOT) data. All MWL campaigns on the VHE blazars discovered More than 50 VHE blazar candidates were observed by VERITAS between September 2007 and June 2009. The total exposure on the 49 non-detected candi- dates is ∼ 305 h live time (average of 6.2 h per can- didate). Approximately 55% of the total exposure is split amongst the 27 observed HBL. The remainder is divided amongst the 8 IBL (26%), 5 LBL (6%), and 9 FSRQ (13%). There are no clear indications of signifi- cant VHE γ -ray emission from any of these 49 blazars [25]. However, the observed significance distribution is clearly skewed towards positive values (see Figure 1). A stacking analysis performed on the entire data sam- ple shows an overall excess of 430 γ -rays, correspond- ing to a statistical significance of 4.8 σ , observed from the directions of the candidate blazars. The IBL and HBL targets make up 96% of the observed excess. Ob- servations of these objects also comprise ∼ 80% of the total exposure. An identical stacked analysis of all the extragalactic non-blazar targets observed, but not clearly detected ( > 5 σ ), by VERITAS does not show a significant excess ( ∼ 120 h exposure). The stacked excess persists using alternate methods for estimating the background at each blazar location, and with dif- ferent event selection criteria (e.g. soft cuts optimized for sources with Γ VHE > 4). The distribution of VHE flux upper limits is shown in Figure 1. These 49 VHE flux upper limits are generally the most-constraining ever reported for these objects. 6. Blazars Upper Limits 7. Multi-wavelength Studies of VHE Blazars 5.2. Discoveries Motivated by Fermi-LAT eConf C091122 $^{2}$RBS 0413 was observed further by VERITAS in Fall 2009. Object Class Redshift M 87 FR I 0.004 Mkn 421 HBL 0.030 Mkn 501 HBL 0.034 1ES 2344+514 HBL 0.044 1ES 1959+650 HBL 0.047 WComae † IBL 0.102 RGB J0710+591 † HBL 0.125 H 1426+428 HBL 0.129 1ES 0806+524 † HBL 0.138 1ES 0229+200 HBL 0.139 1ES 1218+304 HBL 0.182 RBS 0413 † HBL 0.190 1ES 0502+675 † HBL 0.341 3C 66A † IBL 0.444? PKS 1424+240 † IBL ? VER J0521+211 † ? ?