标题： II型超新星膨胀光球和河外距离尺度 显示英文标题

标题： Expanding Photospheres of Type II Supernovae and the Extragalactic Distance Scale

摘要： 我们使用膨胀光球法来确定10个II型超新星的距离。我们探讨了不对称性、消光和流量稀释的影响。利用实证证据和时不变的球形模型，这些模型以非局部热平衡处理H和He，我们展示了对于红外II型超新星以及光学中色温低于6000 K的超新星，由于流量稀释引起的黑体校正很小。II-P型超新星的消光可以从其光曲线估计出来：由于消光引入到距离测量中的不确定性通常小于10%。 通过修正消光和流量稀释，我们得出了10个超新星的距离：SN 1968L, SN 1969L, SN 1970G, SN 1973R, SN 1979C, SN 1980K, SN 1987A, SN 1988A, SN 1990E和SN 1990ae。这些距离测量范围很广，从50千秒差距到120兆秒差距，这在建立星系际距离标度的方法中是独一无二的。M101中的SN 1970G和LMC中的SN 1987A的距离与由造父变星确定的距离非常一致。我们测得的室女座星团的距离为22 ± 3兆秒差距，比最近使用表面亮度波动、行星状星云亮度函数和Tully-Fisher方法得到的距离估计值要大。 利用这些II型超新星确定的距离，我们得出一个值为$H_0 = 60 \pm 10$ 公里/秒$^{-1}$兆秒差距$^{-1}$。这个值受到哈勃流局部偏差导致误差的影响，但很快会通过将膨胀光球法应用于几个遥远的II型超新星而得到改进。 显示英文摘要

摘要： We use the Expanding Photosphere Method to determine distances to 10 type II supernovae. The effects of asymmetries, extinction, and flux dilution are explored. Using empirical evidence and time-independent, spherical models which treat H and He in non-LTE, we show that blackbody corrections caused by flux dilution are small for type II supernovae in the infrared, and in the optical when their color temperatures are less than 6000~K. The extinction to a type II-P supernova can be estimated from its light curve: the uncertainty introduced into a distance measurement due to extinction is usually less than 10\%. Correcting for extinction and flux dilution we derive distances to 10 supernovae: SN 1968L, SN 1969L, SN 1970G, SN 1973R, SN 1979C, SN 1980K, SN 1987A, SN 1988A, SN 1990E, and SN 1990ae. The distance measurements span a wide range, 50 kpc to 120 Mpc, which is unique among the methods for establishing the extragalactic distance scale. The distances measured to SN 1970G in M101 and SN 1987A in the LMC are in good agreement with distances determined from Cepheid variable stars. Our distance to the Virgo Cluster, 22 +- 3 Mpc, is larger than recent distances estimates made using surface brightness fluctuations, planetary nebula luminosity functions, and the Tully-Fisher method. Using the distances determined from these type II supernovae we derive a value of $H_0 = 60 \pm 10$ km sec$^{-1}$Mpc$^{-1}$. This value is subject to errors caused by local deviations in the Hubble flow, but will soon be improved by applying the Expanding Photosphere Method to several distant type II supernovae.