论文标题
OH Megamaser Galaxy IIZW 096的无线电属性
Radio properties of the OH megamaser galaxy IIZw 096
论文作者
论文摘要
基于IIZW 096的OH线观测值的两个时期EVN档案数据，我们确认该来源的高分辨率OH发射主要来自该合并系统的COMP D1的两个斑点（OH1和OH2）。我们发现OH线发射没有显着变化。通过组合两个时期EVN观测值，OH1区域的OH 1665 MHz线排放在OH1区域的水平约为6 $σ。我们发现Comp D1显示了最明亮的CO，HCO+线发射以及多波段无线电连续体发射。 D1周围的环境没有与圆形运动相关的明显速度结构，这使其与文献中的大多数其他欧姆不同，这可能是在合并阶段的效果引起的。同时，我们发现CO发射显示了D1周围的三个速度结构，包括中央宽FWHM区域，CO线谱显示两个分离的峰以及高速云的区域，其中CO线在高速度上峰值（$ \ sim $ \ sim $ 11000 \ kms）。 \ HI在吸收中还显示了D1区域周围的高速云，这可能是由于两个或多个星系组件的合并引起的流入所致。根据无线电连续发射的高分辨率K波段VLA和L波段VLBA观察结果，我们在$ 10^{5} $ k的范围内得出了亮度温度，至$ 10^{6} $ k，这与文学文献中其他的其他Starburst Ohm ohm separt ohm sarte sar n sarburst Ohm e ohm一致。多波段VLA观察结果表明，除了同步加速器发射外，Comp D的无线电连续发射也可能具有自由发射的贡献。作为企图，这些结果支持了欧姆的星爆，而没有AGN的存在。
Based on the two epochs EVN archive data from OH line observations of IIZw 096, we confirm that the high-resolution OH emission in this source mainly comes from two spots (OH1 and OH2) of comp D1 of this merging system. We found no significant variations in the OH line emission. The OH 1665 MHz line emission is detected at about 6 $σ$ level in the OH1 region by combining two epoch EVN observations. We found that the comp D1 shows the brightest CO, HCO+ line emission, as well as multi-band radio continuum emission. The environment around D1 shows no clear velocity structure associated with circular motions, making it different from most other OHMs in the literature, which might have been caused by an effect during the merger stage. Meanwhile, we found that the CO emission shows three velocity structures around D1, including the central broad FWHM region, the double peak region where the CO line profile shows two separated peaks, and the region of the high-velocity clouds where the CO line peaks at a high velocity ($\sim$ 11000 \kms). \HI in absorption also show high-velocity clouds around the D1 region, which might be due to inflows caused by the merging of two or more galaxy components. Based on the high-resolution K-band VLA and L-band VLBA observations of the radio continuum emission, we derived the brightness temperature in the range $10^{5}$ K to $10^{6}$ K, which is consistent with other starburst dominant OHM sources in the literature. The multi-band VLA observations show that the radio continuum emission of comp D might also have contributions from free-free emission, besides synchrotron emission. As a concenquence, these results support a starburst origin for the OHMs, without the presence of an AGN.
