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J.P. Halpern, N. Mirabal (Columbia U.), M. Eracleous (Penn State), R.H. Becker (UC Davis)
Most of the EGRET high-energy \gamma-ray sources remain unidentified. It is highly likely that many of these are fainter blazars or pulsars, but there may also be new types of sources to be discovered. We have focussed our search for novel \gamma-ray sources on 3EG~1835+5918, which is the brightest and most accurately positioned of the unidentified EGRET sources at high Galactic latitude (\ell,b=89\circ,25\circ). In this talk, we will summarize the results of X-ray, radio, and optical surveys of this location. In particular, we have made complete optical identifications of all of the ROSAT and ASCA sources in this region to a flux limit of approximately 1 \times 10-13~ergs~cm-2~s-1. All of the X-ray sources within the EGRET error circle are radio-quiet quasars or coronally emitting stars. Previous radio pulsar searches have been unsuccessful. We set an upper limit of 3.8~mJy (at 1.4~GHz) on any possible radio counterpart to 3EG~1835+5918. We also find several quasars and white dwarfs using optical color selection, and we have monitored the entire field for variable optical objects on short and long time scales. Since no blazar-like or pulsar-like candidate has been found as a result of these searches, we assert that 3EG~1835+5918 must be lacking in one or more of the physically essential attributes of those classes of \gamma-ray emitters. In particular, its radio flux is at least two orders of magnitude fainter than any of the securely identified EGRET blazars, and its soft X-ray flux is at least 30 times fainter than that of Geminga and other EGRET pulsars. If it is an AGN it lacks the beamed radio emission of blazars. If it is an isolated neutron star, it lacks both the thermal X-rays from a cooling surface and the magnetospheric non-thermal X-ray emission that is characteristic of all EGRET pulsars. As such, it is more problematic physically than Geminga, which is an ordinary pulsar that only lacks radio emission. As a pulsar, 3EG~1835+5918 would have to be either older or more distant than Geminga, and probably an even more efficient \gamma-ray engine.