A distance-limited sample of massive star-forming cores from the RMS survey
A distance-limited sample of massive star-forming cores from the RMS survey
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DOI：
10.1093/mnras/stv1334
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发表时间：
2015-09
影响因子：
4.8
通讯作者：
L. Maud;S. Lumsden;T. Moore;J. Mottram;J. Urquhart;A. Cicchini
中科院分区：
文献类型：
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作者：
L. Maud;S. Lumsden;T. Moore;J. Mottram;J. Urquhart;A. Cicchini
我们分析了C18 O（J = 3-2）的数据，从99个红外（IR）明亮的大质量年轻恒星天体（MYSO）和紧凑的H II区域，被确定为潜在的分子外流源在红色MSX源调查。我们提取的距离有限（D < 6千秒差距）的样本是代表星星形成覆盖源类型之间的过渡。在空间分辨率探测，拉尔森样的关系，发现这些核心，虽然另一种解释，拉尔森的关系出现在表面密度有限的样品被认为是，也与我们的数据一致。MYSO和H II区域的源属性之间没有显着差异，这表明核心属性是在大质量恒星形成之前建立的，随后在后来的演化阶段几乎没有影响。尘埃连续体和C18 O气体质量之间有很强的相关性，支持这两种物质在这些红外亮源中追踪相同物质的解释。在独立建立的核心质量和光度之间可以看到一个清晰的线性关系。MYSO和紧凑的H II地区的质量-光度平面中的位置是一致的光度预期从最大的原星星在集群中使用的星星的形成效率为40%时，表明它们是在一个类似的演化阶段，吸积阶段的结束附近。
We analyse C18O (J = 3-2) data from a sample of 99 infrared (IR)-bright massive young stellar objects (MYSOs) and compact H II regions that were identified as potential molecular-outflow sources in the Red MSX Source survey. We extract a distance-limited (D < 6 kpc) sample shown to be representative of star formation covering the transition between the source types. At the spatial resolution probed, Larson-like relationships are found for these cores, though the alternative explanation, that Larson's relations arise where surface-density-limited samples are considered, is also consistent with our data. There are no significant differences found between source properties for the MYSOs and H II regions, suggesting that the core properties are established prior to the formation of massive stars, which subsequently have little impact at the later evolutionary stages investigated. There is a strong correlation between dust-continuum and C18O-gas masses, supporting the interpretation that both trace the same material in these IR-bright sources. A clear linear relationship is seen between the independently established core masses and luminosities. The position of MYSOs and compact H II regions in the mass-luminosity plane is consistent with the luminosity expected from the most massive protostar in the cluster when using an ˜40 per cent star formation efficiency and indicates that they are at a similar evolutionary stage, near the end of the accretion phase.