background due to new physics. In some cases, astronomers can help with the understanding of the astrophysical background, such as using supernovae as standard candles to measure dark energy. However, high-energy physicists will have to detect and explain high energy astrophysical phenomena in order to derive the fundamental physics. The HAWC deep survey of the TeV gamma-ray sky will provide an unbiased picture necessary to characterize the properties of the astrophysical sources in order to search for new fundamental physics effects. Examples of HAWC investigations include: Constraining the existence of nearby dark matter. HAWC's unbiased survey of 2π sr of the TeV sky allows searches known and unknown dwarf spheroidal satellites of our galaxy. The number of satellites increases with decreasing mass so there could be very nearby clumps of dark matter, which would therefore have higher gamma-ray fluxes, but might not have optical counterparts. The known dwarf spheroidal galaxies have extents of up to ~1 degree which is well matched to HAWC's angular resolution of <0.5o. A stacked analysis of these satellites would improve the limit because all will have the same gamma-ray spectra. Testing Lorentz invariance with transient gamma-ray observations. Many quantum gravity theories predict that the speed of light depends upon the energy of the photon as: Δc/c = -(E/MQGn)n where n=1 or 2. While MQG may be the Planck mass (2.4x1018 GeV), some theories predict much smaller mass scales. For theories where n=1, the Fermi-LAT collaboration has set limits above the Planck mass, and HAWC will have similar sensitivity if a GRB is detected. For theories where n=2, the higher energy sensitivity of HAWC will lead to limits roughly an order of magnitude higher mass scale than is possible with Fermi-LAT. Measuring the attenuation of astrophysical sources due to interactions with the extragalactic background light (EBL). HAWC will enable multiple sources to be observed in various flaring states to understand the intrinsic TeV spectrum. Current constraints on the EBL make a conservative assumption of a very hard intrinsic spectrum and are very close to the maximum allowed from galaxy counts. These observations have led to postulations of the existence of axions in order to reduce the attenuation of TeV emission from EBL. Searching for exotic signals such as massive relic particles, e.g. supersymmetry Q-balls, and tau neutrinos. Special triggers will be developed, allowing HAWC to search for the slow moving and high dE/dx Q-balls and the