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The peculiar emission properties of the $z \sim 6.6$ Ly$\alpha$ emitter CR7have been initially interpreted with the presence of either a direct collapseblack hole (DCBH) or a substantial mass of Pop III stars. Instead, updatedphotometric observations by Bowler et al. (2016) seem to suggest that CR7 is amore standard system. Here we confirm that the original DCBH hypothesis isconsistent also with the new data. Using radiation-hydrodynamic simulations, wereproduce the new IR photometry with two models involving a Compton-thick DCBHof mass $\approx 7 \times 10^6 \, \mathrm{M_{\odot}}$ accreting (a) metal-free($Z=0$) gas with column density $N_H = 8 \times 10^{25} \, \mathrm{cm^{-2}}$,or (b) low-metallicity gas ($Z = 5 \times 10^{-3} \, \mathrm{Z_{\odot}}$) with$N_H = 3 \times 10^{24} \, \mathrm{cm^{-2}}$. The best fit model reproduces thephotometric data to within $1 \sigma$. Such metals can be produced by weakstar-forming activity occurring after the formation of the DCBH. The maincontribution to the Spitzer/IRAC $3.6 \, \mathrm{\mu m}$ photometric band inboth models is due to HeI/HeII $\lambda 4714, 4687$ emission lines, while thecontribution of [OIII] $\lambda 4959, 5007$ emission lines, if present, issub-dominant. Spectroscopic observations with JWST will be required toultimately clarify the nature of CR7.

The nature of the Lyman Alpha Emitter CR7: a persisting puzzle