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We present here our observations and analysis of the dayside emissionspectrum of the hot Jupiter WASP-103b. We observed WASP-103b during secondaryeclipse using two visits of the Hubble Space Telescope with the G141 grism onWide Field Camera 3 in spatial scan mode. We generated secondary eclipse lightcurves of the planet in both blended white-light and spectrally binnedwavechannels from 1.1-1.7 micron and corrected the light curves for fluxcontamination from a nearby companion star. We modeled the detector systematicsand secondary eclipse spectrum using Gaussian process regression and found thatthe near-IR emission spectrum of WASP-103b is featureless across the observednear-IR region to down to a sensitivity of 175 ppm, and shows a shallow slopetowards the red. The atmosphere has a single brightness temperature of T_B =2890 K across this wavelength range. This region of the spectrum isindistinguishable from isothermal, but may not manifest from a physicallyisothermal system, i.e. pseudo-isothermal. A Solar-metallicity profile with athermal inversion layer at 10^-2 bar fits WASP-103b's spectrum with highconfidence, as do an isothermal profile with Solar metallicity and amonotonically decreasing atmosphere with C/O>1. The data rule out amonotonically decreasing atmospheric profile with Solar composition, and werule out a low-metallicity decreasing profile as non-physical for this system.The pseudo-isothermal profile could be explained by a thermal inversion layerjust above the layer probed by our observations, or by clouds or haze in theupper atmosphere. Transmission spectra at optical wavelengths would allow us tobetter differentiate between potential atmospheric models.

Near-Infrared Emission Spectrum of WASP-103b using Hubble Space Telescope/Wide Field Camera 3