缓慢旋转的玻色-爱因斯坦凝聚体与12个矮星系的自转曲线
Slowly rotating Bose-Einstein Condensate confronted with the rotation curves of 12 dwarf galaxies
摘要：
我们收集了一个数据库的12个矮星系，光学（R-波段）和近红外（$3.6μm$）的表面亮度密度连同光谱旋转曲线数据，以测试缓慢旋转的玻色-爱因斯坦凝聚体（srBEC）暗物质模型。我们的目标是建立与观测兼容的角速度范围，从上面的有限大小的晕的要求为界，检查与数据集的模型拟合，以及BEC晕参数$\mathcal{R}$的普遍性。我们根据矮星系的$3.6μm$和R-波段表面亮度轮廓，假设其重子质量分布为轴对称分布，构造了矮星系恒星成分的空间光度密度。我们建立的气体成分，采用截断盘模型。我们拟合了一个重子加暗物质的组合模型，参数化的重子组件的M/L比和参数的srBEC（中心密度$ρ_c$，静态BEC晕$\mathcal{R}$的大小，角速度$ω$）的旋转曲线。6个星系的$3.6μm$表面亮度表明存在一个凸起和一个盘组件。$3.6μm$和R-波段空间质量密度剖面的形状相似，这与新兴星系的恒星质量与波长无关是一致的。srBEC模型拟合了12个星系中11个星系的自转曲线，其平均值为$1σ$ 7.51 kpc，标准差为2.96 kpc。这代表了对静态BEC模型拟合的改进。对于拟合良好的11个星系，允许有限大小的srBEC晕的角速度是$<2.2\times 10^{-16}$ 1/s。对于BEC颗粒的散射长度为$a\approx 10^6$ fm，BEC颗粒的质量比静态情况下稍微更好地约束为$m\in[1.26\times10^{-17}\div3.08\times10^{-17}]$ eV/c $^2$。
英文摘要：
We assemble a database of 12 dwarf galaxies, for which optical (R-band) and near-infrared ($3.6μm$) surface brightness density together with spectroscopic rotation curve data are available, in order to test the slowly rotating Bose-Einstein Condensate (srBEC) dark matter model. We aim to establish the angular velocity range compatible with observations, bounded from above by the requirement of finite size halos, to check the modelfits with the dataset, and the universality of the BEC halo parameter $\mathcal{R}$. We construct the spatial luminosity density of the stellar component of the dwarf galaxies based on their $3.6μm$ and R-band surface brightness profiles, assuming an axisymmetric baryonic mass distribution. We build up the gaseous component by employing a truncated disk model. We fit a baryonic plus dark matter combined model, parametrized by the M/L ratios of the baryonic components and parameters of the srBEC (the central density $ρ_c$, size of the static BEC halo $\mathcal{R}$, angular velocity $ω$) to the rotation curves. The $3.6μm$ surface brightness of 6 galaxies indicates the presence of a bulge and a disk component. The shape of the $3.6μm$ and R-band spatial mass density profiles being similar is consistent with the stellar mass of the galaxies emerging wavelength-independent. The srBEC model fits the rotation curve of 11 galaxies out of 12 within $1σ$ significance level, with the average of $\mathcal{R}$ as 7.51 kpc and standard deviation of 2.96 kpc. This represents an improvement over the static BEC modelfit. For the well-fitting 11 galaxies 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 constrained than in the static case as $m\in[1.26\times10^{-17}\div3.08\times10^{-17}]$ eV/c$^2$.
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