Diffuse radio recombination line emission on the Galactic plane between l= 36 ° and 44 °
Diffuse radio recombination line emission on the Galactic plane between l= 36 ° and 44 °
复制标题
银河平面上 l= 36 ° 和 44 ° 之间的漫射射电重组线发射
DOI：
10.1111/j.1365-2966.2010.16595.x
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发表时间：
2010
影响因子：
4.8
通讯作者：
Alves M
中科院分区：
文献类型：
--
作者：
Alves M
无线电重组线（RRLs）可以用来确定沿银道平面的发射量。我们使用了深（2100秒/波束）的hi Parkes避让区（ZOA）调查，其中包括三个rrl （H166α， H167α和H168α）在其带宽内。选择的区域是：l = 36°到44°，b=−4°到+ 4°，包括来自本星、人马座和盾座臂的辐射。以(r, b)=（40°，0°）为中心构建了一个8°× 8°数据立方体，其速度和空间分辨率分别为27 km s−1和15.5 arcmin。已知的H ii区域以及银河系平面上的漫射RRL发射被识别出来。整体RRL发射横跨银道平面的星系纬度剖面描绘了亮度温度（tb）分布，其纬度为。通过与威尔金森微波各向异性探针（WMAP）自由-自由最大熵法的比较，得到了电子温度T≃8000 K的值。将现有RRL数据的T - b分布与WMAP 5年数据相结合，得出了银河系脊上残余“异常”发射的纬度分布。在本文中，我们证明了利用ZOA巡天的RRLs可以恢复银河系脊上的漫射电离辐射。因此，这种方法能够补充银河系低纬度的Hα数据，从而能够推导出全天自由-自由模板。
Radio recombination lines (RRLs) can be used to determine the emission measure unambiguously along the Galactic plane. We use the deep (2100 s per beam) H i Parkes Zone of Avoidance (ZOA) survey which includes three RRLs (H166α, H167α and H168α) within its bandwidth. The region ℓ= 36° to 44°, b=− 4° to+ 4° is chosen to include emission from the Local, Sagittarius and Scutum arms. An 8°× 8° data cube centred at (ℓ, b)=(40°, 0°) is constructed of RRL spectra with velocity and spatial resolution of 27 km s− 1 and 15.5 arcmin, respectively. Well-known H ii regions are identified as well as the diffuse RRL emission on the Galactic plane. A Galactic latitude section of the integrated RRL emission across the Galactic plane delineates the brightness temperature (T b) distribution which has a half-power width in latitude of. A value of the electron temperature T e≃ 8000 K is derived from a comparison with the Wilkinson Microwave Anisotropy Probe (WMAP) free–free maximum entropy method. The T b distribution from the present RRL data is combined with the WMAP 5-yr data to derive the latitude distribution of the residual ‘anomalous’ emission on the Galactic ridge. In this paper, we demonstrate that diffuse ionized emission on the Galactic ridge can be recovered using RRLs from the ZOA survey. This method is therefore able to complement the Hα data at low Galactic latitudes, to enable an all-sky free–free template to be derived.