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- W2590123418 abstract "The peculiar emission properties of the $z sim 6.6$ Ly$alpha$ emitter CR7 have been initially interpreted with the presence of either a direct collapse black hole (DCBH) or a substantial mass of Pop III stars. Instead, updated photometric observations by Bowler et al. (2016) seem to suggest that CR7 is a more standard system. Here we confirm that the original DCBH hypothesis is consistent also with the new data. Using radiation-hydrodynamic simulations, we reproduce the new IR photometry with two models involving a Compton-thick DCBH of 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 the photometric data to within $1 sigma$. Such metals can be produced by weak star-forming activity occurring after the formation of the DCBH. The main contribution to the Spitzer/IRAC $3.6 , mathrm{mu m}$ photometric band in both models is due to HeI/HeII $lambda 4714, 4687$ emission lines, while the contribution of [OIII] $lambda 4959, 5007$ emission lines, if present, is sub-dominant. Spectroscopic observations with JWST will be required to ultimately clarify the nature of CR7." @default.
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- W2590123418 date "2017-02-20" @default.
- W2590123418 modified "2023-10-01" @default.
- W2590123418 title "The nature of the Lyman α emitter CR7: a persisting puzzle" @default.
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- W2590123418 doi "https://doi.org/10.1093/mnrasl/slx029" @default.
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