类星体之路
The Road to Quasars
摘要：
虽然早在1960年，约翰·博尔顿和其他人就讨论了3C 48和其他类恒星射电源的河外性质，但这在很大程度上被拒绝了，因为他们先入为主地认为这似乎是不切实际的高射电和光学光度。直到1962年在帕克斯观测到的强射电源3C 273的掩星，使得马丁·施密特将3C 273与一个红移为0.16的明显恒星物体联系在一起，人们才真正理解了3C 273的本质。连续的无线电和光学测量很快导致了其他类星体的识别，这些类星体的红移越来越大，并且普遍接受类星体作为星系的非常明亮的核，尽管几十年来没有普遍接受。奇怪的是，3C 273是天空中最强的河外源之一，它于1959年首次被编目，而13等的光学对应物至少早在1887年就被观测到了。自1960年以来，更微弱的光学对应物通常使用精确的无线电干涉仪位置来识别，这些位置主要在加州理工学院欧文斯谷射电天文台测量。然而，3C 273在西里尔·哈泽德（Cyril Hazard）领导的一系列月球掩星观测之前一直没有被确认。虽然之前已经用OVRO干涉仪获得了精确的射电位置，但令人费解的是，3C 273最初被错误地认为是一个距离真正的类星体位置大约一弧分的微弱星系。
英文摘要：
Although the extragalactic nature of 3C 48 and other quasi stellar radio sources was discussed as early as 1960 by John Bolton and others, it was rejected largely because of preconceived ideas about what appeared to be unrealistically high radio and optical luminosities. Not until the 1962 occultations of the strong radio source 3C 273 at Parkes, which led Maarten Schmidt to identify 3C 273 with an apparent stellar object at a redshift of 0.16, was the true nature understood. Successive radio and optical measurements quickly led to the identification of other quasars with increasingly large redshifts and the general, although for some decades not universal, acceptance of quasars as the very luminous nuclei of galaxies. Curiously, 3C 273, which is one of the strongest extragalactic sources in the sky, was first cataloged in 1959 and the magnitude 13 optical counterpart was observed at least as early as 1887. Since 1960, much fainter optical counterparts were being routinely identified using accurate radio interferometer positions which were measured primarily at the Caltech Owens Valley Radio Observatory. However, 3C 273 eluded identification until the series of lunar occultation observations led by Cyril Hazard. Although an accurate radio position had been obtained earlier with the OVRO interferometer, inexplicably 3C 273 was initially misidentified with a faint galaxy located about an arc minute away from the true quasar position.
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