论文标题
分子云中的巨大恒星富含高能源：G332.809-0.132和CS 78 NGC 6334中的桥梁
Massive Stars in Molecular Clouds Rich in High-energy Sources: The Bridge of G332.809-0.132 and CS 78 in NGC 6334
论文作者
论文摘要
这里介绍了NGC 6334和G332.809-0.132在H II区域CS 78方向上的大型恒星的检测。 G332.809-0.132复合物所覆盖的区域与RCW 103恒星协会一致。在其核心（半径为40'）中，使用2Mass，denis和limpse数据鉴定了大约110个OB候选星（KS <10 mag和0.4 <aks <1.6 mag）。该数量的OB恒星占该区域观察到的Lyman连续光子数量的50％以上。获得了七种早期类型的中分辨率K波段，其中包括1颗WN 8星和一个OfPE/WN 9星；后者位于RCW 103残留物附近，其发光度与约3 kpc的距离一致。该区域分析的区域包含了先前在RCW 103中已知的34个OB恒星中的9个，以及IRAS 16115-5044，我们将其重新分类为候选发光蓝色变量。视线特别有趣，越过三个螺旋臂。检测到-50的分子云（在Scutum -Crux臂中有RCW 103），另一个分子云检测到-90 km S -1（在Norma臂中），既有巨大的恒星和超新星残余物。我们还报告了B Supergiant的检测是CS 78，2MASS J17213513-3532415的主要电离源。中分辨率H和K带光谱显示H I和HE I线以及Fe II线。通过假设距离为1.35 kpc，我们估计辐射幅度为-6.16，这是超级巨人的典型特征。
Detections of massive stars in the direction of the H II region CS 78 in NGC 6334 and of G332.809-0.132 are here presented. The region covered by the G332.809-0.132 complex coincides with the RCW 103 stellar association. In its core (40' in radius), approximately 110 OB candidate stars (Ks < 10 mag and 0.4 < AKs < 1.6 mag) were identified using 2MASS, DENIS, and GLIMPSE data. This number of OB stars accounts for more than 50% of the observed number of Lyman continuum photons from this region. Medium-resolution K-band spectra were obtained for seven early types, including one WN 8 star and one Ofpe/WN 9 star; the latter is located near the RCW 103 remnant and its luminosity is consistent with a distance of about 3 kpc. The area analyzed encloses 9 of the 34 OB stars previously known in RCW 103, as well as IRAS 16115-5044, which we reclassify as a candidate luminous blue variable. The line of sight is particularly interesting, crossing three spiral arms; a molecular cloud at -50 (with RCW 103 in the Scutum-Crux arm) and another at -90 km s-1 (in the Norma arm) are detected, both rich in massive stars and supernova remnants. We also report the detection of a B supergiant as the main ionizing source of CS 78, 2MASS J17213513-3532415. Medium-resolution H and K band spectra display H I and He I lines, as well as Fe II lines. By assuming a distance of 1.35 kpc, we estimate a bolometric magnitude of -6.16, which is typical of supergiants.
