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We present H band spectroscopic and Halpha photometric observations of HD100546 obtained with GPI and MagAO. We detect H band emission at the locationof the protoplanet HD 100546b, but show that choice of data processingparameters strongly affects the morphology of this source. It appearspoint-like in some aggressive reductions, but rejoins an extended diskstructure in the majority of the others. Furthermore, we demonstrate that thisemission appears stationary on a timescale of 4.6 yrs, inconsistent at the2sigma level with a Keplerian clockwise orbit at 59 au in the disk plane. The Hband spectrum of the emission is inconsistent with any type of low effectivetemperature object or accreting protoplanetary disk. It strongly suggests ascattered light origin, as it is consistent with the spectrum of the star andthe spectra extracted at other locations in the disk. A non detection at the5sigma level of HD 100546b in differential Halpha imaging places an upperlimit, assuming the protoplanet lies in a gap free of extinction, on theaccretion luminosity and accretion rate of 1.7E-4 Lsun andMMdot<6.4E-7Mjup^2/yr for 1Rjup. These limits are comparable to the accretionluminosity and rate of TTauri-stars or LkCa 15b. Taken together, these lines ofevidence suggest that the H band source at the location of HD 100546b is notemitted by a planetary photosphere or an accreting circumplanetary disk but isa disk feature enhanced by the PSF subtraction process. This non-detection isconsistent with the non-detection in the K band reported in an earlier studybut does not exclude the possibility that HD 100546b is deeply embedded.

An Optical/near-infrared investigation of HD 100546 b with the Gemini Planet Imager and MagAO