According to the standard model of cosmology, the energy density of the observable Universe consists primarily of cold dark matter, baryonic matter, and 'dark energy,’ the last of which is responsible for the late time acceleration of the Universe. Dark energy can be explained by a slowly rolling scalar field or by various modifications of general relativity on large scales. There are also phenomenological models for dark energy which posit some parametrisation of the equation of state of the dark energy component. These models can be put to the test using a compilation of data from various cosmological surveys such as Planck (cosmic microwave background), Joint Light-Curve Analysis (Type Ia supernovae), and galaxy surveys (length scale of baryon acoustic oscillations), as well as measurements of the Hubble parameter at various redshifts. I will discuss various models of dark energy and their status compared to the standard model in light of current observational data.