The Link between the Baryonic Mass Distribution and the Rotation Curve Shape
The Link between the Baryonic Mass Distribution and the Rotation Curve Shape
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重子质量分布与旋转曲线形状之间的联系
DOI：
10.1111/j.1365-2966.2012.21599.x
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发表时间：
2012
影响因子：
4.8
通讯作者：
T. S. Albada
中科院分区：
文献类型：
--
作者：
R. Swaters;R. Sancisi;J. Hulst;T. S. Albada
观测到的盘状星系的旋转曲线，从晚型矮星系到早型螺旋星系，只需放大恒星盘和 H I 盘的贡献就可以很好地拟合。这种“重子标度模型”只需两个自由参数就可以解释所观察到的旋转曲线的全部范围。对于一小部分星系，特别是早期类型的螺旋星系，HI 标度似乎在外部部分失败，可能是由于观测效应或 H I 的电离。重子标度模型的总体成功表明，星系的重子质量与其旋转速度之间众所周知的全局耦合（称为重子塔利-费舍尔关系）也适用于更局部的水平，并且似乎暗示了重子质量分布和总质量（包括暗物质）的分布。
The observed rotation curves of disc galaxies, ranging from late-type dwarf galaxies to early-type spirals, can be fit remarkably well simply by scal ing up the contributions of the stellar and H I discs. This ‘baryonic scaling model’ can explain the full br eadth of observed rotation curves with only two free parameters. For a small fr action of galaxies, in particular early-type spiral galaxies, HI scaling appears to fail in th e outer parts, possibly due to observational effects or ionization of the H I. The overall success of the baryonic scaling model suggests that the well-known global coupling between the baryonic mass of a galaxy and its rotation velocity (known as the baryonic Tully-Fisher rela tion), applies at a more local level as well, and it seems to imply a link between the baryonic mass distribution and the distribution of total mass (including dark matter).