arXiv 1301.48332013-01-21astro-ph.CO

中红外Tully-Fisher关系的标定

Calibration of the Mid-Infrared Tully-Fisher Relation

Jenny G. Sorce, Helene M. Courtois, R. Brent Tully, Mark Seibert, Victoria Scowcroft, Wendy L. Freedman, Barry F. Madore, S. Eric Persson, Andy Monson, Jane Rigby

备注：: Accepted for publication in The Astrophysical Journal, 14 pages, 11 figures, 4 tables
DOI：: 10.1088/0004-637X/765/2/94

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摘要：

为了解决哈勃常数和偏离平均宇宙流的突出宇宙学问题，需要对天空进行相干尺度上的距离测量。星系光度和自转速率之间的相关性可以用来确定在可能达到200 Mpc的广泛环境中数千个星系的距离。斯皮策太空望远镜的中红外（3.6微米）测光作为光度的来源特别有价值，因为它提供了整个天空质量均匀的产品。站在大气层上方，几分钟的曝光就可以记录下目标的总大小。消光是最小的，通量主要是来自老恒星的光，预计与目标的质量相关。尽管优越的测光，中红外光度和旋转速率之间的相关性提取的中性氢配置文件略有退化的相关性发现与I带光度。颜色校正恢复相关性，其提供与I波段处可用的相关性相当的准确性（在单个距离中约20%1西格玛），同时保留上述优点。在没有颜色校正的情况下，线宽和[3.6]幅度之间的关系为M^{b，i，k，a}_{[3.6]} = -20.34-9.74（log W_{mx} ^{i} -2.5）。这个描述是在定义斜率的13个星系团中的213个星系和定义零点的造父变星或红巨星分支距离尖端的26个星系的样本中发现的。构造具有减少的散射的颜色校正参数M_{ C_{[3.6]} }：M_{ C_{[3.6]} } = -20.34-9.13（log W_{mx} ^{i} -2.5）。考虑到在50 Mpc以上的7个校准星团，在明显的特殊速度范围之外，提供了一个初步的哈勃常数估计值H_0=74+/-5 km/s/Mpc。

英文摘要：

Distance measures on a coherent scale around the sky are required to address the outstanding cosmological problems of the Hubble Constant and of departures from the mean cosmic flow. The correlation between galaxy luminosities and rotation rates can be used to determine distances to many thousands of galaxies in a wide range of environments potentially out to 200 Mpc. Mid-infrared (3.6 microns) photometry with the Spitzer Space Telescope is particularly valuable as the source of the luminosities because it provides products of uniform quality across the sky. From a perch above the atmosphere, essentially the total magnitude of targets can be registered in exposures of a few minutes. Extinction is minimal and the flux is dominated by the light from old stars which is expected to correlate with the mass of the targets. In spite of the superior photometry, the correlation between mid-infrared luminosities and rotation rates extracted from neutral hydrogen profiles is slightly degraded from the correlation found with I band luminosities. A color correction recovers a correlation that provides comparable accuracy to that available at I band (~20% 1sigma in an individual distance) while retaining the advantages identified above. Without the color correction the relation between linewidth and [3.6] magnitudes is M^{b,i,k,a}_{[3.6]} = -20.34 - 9.74 (log W_{mx}^{i} -2.5). This description is found with a sample of 213 galaxies in 13 clusters that define the slope and 26 galaxies with Cepheid or tip of the red giant branch distances that define the zero point. A color corrected parameter M_{C_{[3.6]}} is constructed that has reduced scatter: M_{C_{[3.6]}} = -20.34 - 9.13 (log W_{mx}^{i} -2.5). Consideration of the 7 calibration clusters beyond 50 Mpc, outside the domain of obvious peculiar velocities, provides a preliminary Hubble Constant estimate of H_0=74+/-5 km/s/Mpc.

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