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Non-linear structure formation for fermionic dark matter particles leads todark matter density profiles with a degenerate compact core surrounded by adiluted halo. For a given fermion mass, the core has a critical mass thatcollapses into a supermassive black hole (SMBH). Galactic dynamics constraintssuggest a $\sim 100$ keV/$c^2$ fermion, which leads to $\sim 10^7 M_\odot$critical core mass. Here, we show that baryonic (ordinary) matter accretiondrives an initially stable dark matter core to SMBH formation and determine theaccreted mass threshold that induces it. Baryonic gas density $\rho_b$ andvelocity $v_b$ inferred from cosmological hydro-simulations and observationsproduce sub-Eddington accretion rates triggering the baryon-induced collapse inless than a Gyr. This process produces active galactic nuclei in galaxy mergersand the high-redshift Universe. For TXS 2116-077, merging with a nearby galaxy,the observed $3\times 10^7 M_\odot$ SMBH, for $Q_b = \rho_b/v_b^3 = 0.125M_\odot/(100 \text{km/s pc})^3$, forms in $\approx 0.6$ Gyr, consistent withthe $0.5$-$2$ Gyr merger timescale and younger jet. For the farthest centralSMBH detected by the \textit{Chandra} X-ray satellite in the $z=10.3$ UHZ1galaxy observed by the James Webb Space Telescope (\textit{JWST}), themechanism leads to a $4\times 10^7 M_\odot$ SMBH in $87$-$187$ Myr, startingthe accretion at $z=12$-$15$. The baryon-induced collapse can also explain the$\approx 10^7$-$10^8 M_\odot$ SMBHs revealed by the JWST at $z\approx 4$-$6$.After its formation, the SMBH can grow to a few $10^9 M_\odot$ in timescalesshorter than a Gyr via sub-Eddington baryonic mass accretion.

Baryon-induced collapse of dark matter cores into supermassive black holes