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Scalar Field Dark Matter (SFDM) comprised of ultralight bosons has attractedgreat interest as an alternative to standard, collisionless Cold Dark Matter(CDM) because of its novel structure-formation dynamics, described by thecoupled Schr\"odinger-Poisson equations. In the free-field ("fuzzy") limit ofSFDM (FDM), structure is inhibited below the de Broglie wavelength, butresembles CDM on larger scales. Virialized haloes have "solitonic" cores ofradius $\sim\lambda_\text{deB}$, surrounded by CDM-like envelopes. When astrong enough repulsive self-interaction (SI) is also present, structure can beinhibited below a second length scale, $\lambda_\text{SI}$, with$\lambda_\text{SI}> \lambda_\text{deB}$ -- called the Thomas-Fermi (TF) regime.FDM dynamics differs from CDM because of quantum pressure, and SFDM-TF differsfurther by adding SI pressure. In the small-$\lambda_\text{deB}$ limit,however, we can model all three by fluid conservation equations for acompressible, $\gamma=5/3$ ideal gas, with ideal gas pressure sourced byinternal velocity dispersion and, for the TF regime, an added SI pressure,$P_\text{SI}\propto \rho^2$. We use these fluid equations to simulate haloformation from gravitational collapse in 1D, spherical symmetry, demonstratingfor the first time that SFDM-TF haloes form with cores the size of$R_\text{TF}$, the radius of an SI-pressure-supported $(n=1)$-polytrope,surrounded by CDM-like envelopes. In comparison with rotation curves of dwarfgalaxies in the local Universe, SFDM-TF haloes pass the ["too-big-to-fail" +"cusp-core"]-test if $R_\text{TF}\gtrsim 1$ kpc.

Core-Envelope Haloes in Scalar Field Dark Matter with Repulsive Self-Interaction: Fluid Dynamics Beyond the de Broglie Wavelength