THE INFRARED TULLY-FISHER RELATION IN THE URSA MAJOR CLUSTER
THE INFRARED TULLY-FISHER RELATION IN THE URSA MAJOR CLUSTER
复制标题
大熊座星团中的红外塔利-费舍尔关系
DOI：
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发表时间：
1993
期刊：
影响因子：
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通讯作者：
S. Willner
中科院分区：
文献类型：
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作者：
R. Peletier;S. Willner
我们给出了从1.65微米图像中获得的新的星等，这些图像来自于大熊座星系团中的23个星系。现在，除了一个符合我们的星系团成员标准、HI速度宽度大于187公里、S-1和倾角大于45度的螺旋外，所有的螺旋都存在震级。这些螺旋线符合Tully-Fisher关系，本征星等色散(剔除已知观测不确定性和星团深度的影响后)为0.36，斜率为10.2+/-0.6。震级差异比室女座星系团的发现要小，但仍然比一些作者所说的要大得多。我们发现了一个迹象，即塔利-费舍尔关系可能会在光明的一端发生逆转。将圆盘的中心表面亮度作为第三个参数添加会使Tully-Fisher关系的斜率变平，并且可能会给出一个距离估计，离散度稍微小一些，但降低的重要性必须在独立的样本上进行测试。
We present new magnitudes derived from 1.65 mum images for 23 galaxies in the Ursa Major cluster. Magnitudes now exist for all but one spiral meeting our criteria for cluster membership and having H I velocity width greater than 187 km s-1 and inclination greater than 45-degrees. These spirals fit a Tully-Fisher relation with dispersion in intrinsic magnitudes (after known observational uncertainties and the effect of cluster depth are removed) of 0.36 and a slope of 10.2 +/- 0.6. The magnitude dispersion is smaller than found in the Virgo cluster but still significantly larger than claimed by some authors. We find a hint that the Tully-Fisher relation may turn over at the bright end. Adding the central surface brightness of the disk as a third parameter flattens the slope of the Tully-Fisher relation and may give a distance estimate with slightly less dispersion, but the significance of the decrease must be tested on an independent sample.