富含气体的超漫射星系：用超锥修正引力缓解MOND张力
Gas-rich ultra-diffuse galaxies: alleviating the MOND tension with hyperconical modified gravity
AI总结：
本文利用超锥修正引力（HMG）模型分析六个富含气体的超漫射星系（UDGs）的旋转速度，发现HMG在缓解MOND与观测的张力方面优于MOND，但仍有部分星系存在偏差。
摘要：
富含气体的超漫射星系（UDGs）是对与重子Tully-Fisher关系相关的引力模型的一个异常尖锐的检验，因为几个系统似乎旋转得太慢，与其重子质量不符。本研究重新审视了Mancera Piña等人分析的六个孤立富气UDGs，使用超锥修正引力（HMG）的当前外半径处方，采用了已发表的外半径处的重子质量和圆周速度。对邻域尺度参数的扫描将模型推向HMG的渐近分支。在该极限下，对于六个星系中的四个，HMG速度仍然系统性地偏高。相对于观测值，固定渐近分支对六个天体给出$χ^2\simeq18.1$，而单独牛顿重子给出$χ^2\simeq9.7$，但MOND插值更差（$χ^2\simeq 615.7$）。使用组合不确定度，每个星系的HMG张力范围从$0.2σ$到$2.1σ$，与牛顿重子得到的$0.1σ$到$1.7σ$非常相似，远小于MOND得到的$3.7σ$到$5.9σ$。我们得出结论，当前外半径HMG实现缓解了MOND的困难，但仍不足以解释UDG样本已发表的中心值。因此，富气UDGs提供了MOND和HMG之间的有用判别。
英文摘要：
Gas-rich ultra-diffuse galaxies (UDGs) are an unusually sharp test for gravity models tied to the baryonic Tully--Fisher relation because several systems appear to rotate too slowly for their baryonic masses. This study revisits the six isolated gas-rich UDGs analysed by Mancera Piña et al. with the current outer-radius prescription of hyperconical modified gravity (HMG), using the published baryonic masses and circular velocities at the outer radii. The scan over the neighbourhood-scale parameter drives the model towards the asymptotic branch of HMG. For that limit, the HMG velocities are still systematically high for four of the six galaxies. Relative to the observed values, the fixed asymptotic branch gives $χ^2\simeq18.1$ for six objects, whereas Newtonian baryons alone give $χ^2\simeq9.7$, but MOND interpolation is much worse ($χ^2\simeq 615.7$). Using combined uncertainties, the per-galaxy HMG tension ranges from $0.2σ$ to $2.1σ$, very similar to the $0.1σ$ to $1.7σ$ found for Newtonian baryons, and much smaller than the $3.7σ$ to $5.9σ$ obtained for MOND. We conclude that the present outer-radius HMG implementation alleviates the difficulties of MOND, but is still not sufficient to account for the published central values of the UDG sample. Gas-rich UDGs therefore provide a useful discriminant between MOND and HMG.
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