标题： SNR RX J0852.0-4622（Vela Jr）的射电波段内部结构 显示英文标题

标题： The interior of the SNR RX J0852.0-4622 (Vela Jr) at radio wavelengths

摘要： 目的：我们观测了超新星遗迹Vela Jr的中心在射电连续谱中的表现，以寻找与紧凑中心X射线源CXOU J085201.4-461753相对应的天体，该源可能是中子星候选体，且可能是超新星爆炸的遗迹。 方法：利用澳大利亚望远镜紧凑阵列，在13厘米和20厘米波长进行了观测。通过数据的空间滤波以获得相同的u-v覆盖范围，并使用这些数据的流量密度相关性来获取光谱指数。进行了多波段搜索以寻找与紧凑中心X射线源相对应的天体。 结果：我们编制了一个包含31个小型直径射电源的新目录，其中包括已知的PMN J0853-4620源，列出20厘米波长的积分流量密度以及一半源的13厘米波长的流量密度及其对应的光谱指数。所有源在当前角分辨率下均未解析，但源18明显拉长且非常靠近CXOU J085201.4-461753。 我们的观测没有发现与点状X射线源相关的脉冲星风驱动星云存在的证据。此外，源18具有热谱，指数为+0.8±0.4，并似乎与光学源Wray 16-30相对应。尽管文献中报告缺乏OIII发射线，但我们发现此对象可以解释为属于“蝴蝶”形态类别的低发射行星状星云。 结论：我们认为，如果射电源18实际上是行星状星云，则CXOU J085201.4-461753更可能与其有关，而不是与Vela Jr有关。 显示英文摘要

摘要： Aim: We observed the center of the supernova remnant Vela Jr in radio continuum in order to search for a counterpart to the compact central X-ray source CXOU J085201.4-461753, possibly a neutron star candidate which could be the remnant of the supernova explosion. Method: Observations were made with the Australia Telescope Compact Array at 13 and 20 cm. Spectral indices were obtained using flux density correlations of the data which were spatially filtered to have the same u-v coverage. A multiwavelength search for counterparts to the compact central X-ray source was made. Results: We compiled a new catalogue of 31 small diameter radio sources, including the previously known source PMN J0853-4620, listing the integrated flux densities at 20 cm and, for half of the sources, the flux densities at 13 cm with the corresponding spectral indices. All sources are unresolved at the present angular resolution except for Source 18, which is clearly elongated and lies strikingly close to CXOU J085201.4-461753. Our observations show no evidence for the existence of a pulsar wind driven nebula associated with the point X-ray source. Furthermore, Source 18 has a thermal spectrum with index +0.8 +/- 0.4, and appears to be the counterpart of the optical source Wray 16-30. In spite of the absence of OIII emission lines as reported in the literature, we find that this object could be explained as a low emission planetary nebula belonging to the ``butterfly'' morphological class. Conclusions: We conclude that if the radio source 18 is actually a planetary nebula, then CXOU J085201.4-461753 is more likely to be related to it rather than to Vela Jr.