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We assemble a database of 12 dwarf galaxies, for which optical (R-band) andnear-infrared ($3.6\mu m$) surface brightness density together withspectroscopic rotation curve data are available, in order to test the slowlyrotating Bose-Einstein Condensate (srBEC) dark matter model. We aim toestablish the angular velocity range compatible with observations, bounded fromabove by the requirement of finite size halos, to check the modelfits with thedataset, and the universality of the BEC halo parameter $\mathcal{R}$. Weconstruct the spatial luminosity density of the stellar component of the dwarfgalaxies based on their $3.6\mu m$ and R-band surface brightness profiles,assuming an axisymmetric baryonic mass distribution. We build up the gaseouscomponent by employing a truncated disk model. We fit a baryonic plus darkmatter combined model, parametrized by the M/L ratios of the baryoniccomponents and parameters of the srBEC (the central density $\rho_c$, size ofthe static BEC halo $\mathcal{R}$, angular velocity $\omega$) to the rotationcurves. The $3.6\mu m$ surface brightness of 6 galaxies indicates the presenceof a bulge and a disk component. The shape of the $3.6\mu m$ and R-band spatialmass density profiles being similar is consistent with the stellar mass of thegalaxies emerging wavelength-independent. The srBEC model fits the rotationcurve of 11 galaxies out of 12 within $1\sigma$ significance level, with theaverage of $\mathcal{R}$ as 7.51 kpc and standard deviation of 2.96 kpc. Thisrepresents an improvement over the static BEC modelfit. For the well-fitting 11galaxies the angular velocities allowing for a finite size srBEC halo are$<2.2\times 10^{-16}$ 1/s. For a scattering length of the BEC particle of$a\approx 10^6$ fm, the mass of the BEC particle is slightly better constrainedthan in the static case as $m\in[1.26\times10^{-17}\div3.08\times10^{-17}]$eV/c$^2$.

Slowly rotating Bose-Einstein Condensate confronted with the rotation curves of 12 dwarf galaxies