标题： 编号NGC 6240的超亮远红外星系的射电辐射 显示英文标题

标题： The Radio Emission from the Ultra-Luminous Far-Infrared Galaxy NGC 6240

摘要： 我们展示了对“典型”的超亮远红外星系NGC 6240的新射电观测，使用VLA在'B'构型下20 cm波长和'A'构型下3.6 cm波长获得这些数据，连同来自四次之前VLA观测的数据一起，用于对NGC 6240的射电辐射进行全面研究。 大约70%（约3×10$^{23}$ W~Hz$^{-1}$）的总射电功率来自核区（<~1.5千秒差距），其中一半由两个无法解析的源发出（$R <~ 36 pc) cores and half by a diffuse component. The radio spectrum of the nuclear emission is relatively flat ($\alpha $ =~ 0.6; $ S_{\nu } \propto \nu ^{-\alpha }$). The supernova rate required to power the diffuse component is consistent with that predicted by the stellar evolution models of Rieke \etal (1985). If the radio emission from the two compact cores is powered by supernova remnants, then either the remnants overlap and form hot bubbles in the cores, or they are very young ( <~ 100 yr). Nearly all of the other 30\% of the total radio power comes from an ``arm-like'' region extending westward from the nuclear region. The western arm emission has a steep spectrum ($\alpha $ =~ 1.0), suggestive of aging effects from synchrotron or inverse-Compton losses, and is not correlated with starlight; we suggest that it is synchrotron emission from a shell of material driven by a galactic superwind. Inverse-Compton scattering of far-infrared photons in the radio sources is expected to produce an X-ray flux of ~2-6 x 10$ ^{-14}\$ erg/s/cm2 在2-10 keV带宽内）。 未检测到来自或靠近布兰德-霍索恩、威尔逊与图利（1991）假设的可能超大质量“暗核”的显著无线电辐射。 显示英文摘要

摘要： We present new radio observations of the ``prototypical'' ultra-luminous far- infrared galaxy NGC~6240, obtained using the VLA at 20~cm in `B' configuration and at 3.6~cm in `A' configuration. These data, along with those from four previous VLA observations, are used to perform a comprehensive study of the radio emission from NGC~6240. Approximately 70\% (~3 x 10$^{23}$ W~Hz$^{-1}$) of the total radio power at 20 cm originates from the nuclear region ( <~ 1.5 kpc), of which half is emitted by two unresolved ($R <~ 36 pc) cores and half by a diffuse component. The radio spectrum of the nuclear emission is relatively flat ($\alpha$ =~ 0.6; $S_{\nu} \propto \nu^{-\alpha}$). The supernova rate required to power the diffuse component is consistent with that predicted by the stellar evolution models of Rieke \etal (1985). If the radio emission from the two compact cores is powered by supernova remnants, then either the remnants overlap and form hot bubbles in the cores, or they are very young ( <~ 100 yr). Nearly all of the other 30\% of the total radio power comes from an ``arm-like'' region extending westward from the nuclear region. The western arm emission has a steep spectrum ($\alpha$ =~ 1.0), suggestive of aging effects from synchrotron or inverse-Compton losses, and is not correlated with starlight; we suggest that it is synchrotron emission from a shell of material driven by a galactic superwind. Inverse-Compton scattering of far-infrared photons in the radio sources is expected to produce an X-ray flux of ~2-6 x 10$^{-14}$ erg/s/cm2 in the 2-10 keV band. No significant radio emission is detected from or near the possible ultra-massive ``dark core'' hypothesized by Bland-Hawthorn, Wilson \& Tully (1991).