The Tully-Fisher relation for low surface brightness galaxies: implications for galaxy evolution
The Tully-Fisher relation for low surface brightness galaxies: implications for galaxy evolution
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DOI：
10.1093/mnras/273.1.l35
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发表时间：
1995-01
影响因子：
4.8
通讯作者：
M. Zwaan;J. Hulst;W. D. Blok;S. McGaugh
中科院分区：
文献类型：
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作者：
M. Zwaan;J. Hulst;W. D. Blok;S. McGaugh
给出了低表面亮度星系B波段Tully-Fisher关系。这些LSB星系遵循与正常螺旋星系相同的塔利-费舍尔关系。这意味着LSB星系的质光比（M/L）通常比具有相同总光度和形态类型的正常星系大2倍。由于星系的动力学质量与自转速度和标度长度通过M与V（2）h成正比关系，因此在固定线宽下LSB星系必须是正常星系的两倍大。这是通过检查LSB和正常星系的标度长度和线宽之间的关系得到证实。Tully-Fisher关系的普遍性质可以理解，如果LSB星系是具有低质量表面密度的星系，sigma（$）超过bar。质量面密度显然控制着星系的光度演化，使得M/L的乘积σ（$）保持不变。
We present the B-band Tully-Fisher relation for low surface brightness (LSB) galaxies. These LSB galaxies follow the same Tully-Fisher relation as normal spiral galaxies. This implies that the mass-to-light ratio (M/L) of LSB galaxies is typically a factor of 2 larger than that of normal galaxies of the same total luminosity and morphological type. Since the dynamical mass of a galaxy is related to the rotational velocity and scalelength via M proportional to V(2)h, at fixed linewidth LSB galaxies must be twice as large as normal galaxies. This is confirmed by examining the relation between scalelength and linewidth for LSB and normal galaxies. The universal nature of the Tully-Fisher relation can be understood if LSB galaxies are galaxies with low mass surface density, sigma ($) over bar. The mass surface density apparently controls the luminosity evolution of a galaxy in such a way as to keep the product sigma ($) over bar M/L constant.