乙二醇对W51/e2和G34的试验性检测.3+0.2
Tentative detection of ethylene glycol toward W51/e2 and G34.3+0.2
摘要：
复杂的有机分子和潜在的生命起源分子是如何在低质量和高质量恒星形成的区域形成的，这仍然是天体化学的一个中心问题。特别是，由于只有少数来源进行了详细研究，目前还不清楚环境在复杂分子形成中起着什么作用。在这种情况下，比较不同来源之间相关物种的相对丰度可能有助于解释观察到的差异。我们试图测量三个重要的复杂的有机分子，乙二醇（（CH $_2$ OH）$_2$），乙醇醛（CH $_2$ OHCHO）和甲酸甲酯（HCOOCH $_3$）之间的相对丰度，对高质量的原恒星，从而提供额外的限制，其形成途径。我们使用IRAM 30米单碟观测的三个物种对两个高质量的恒星形成区域- W51/e2和G34.3+0.2 -和报告的（CH 2 OH）2的试探性检测对这两个来源。假设（CH $_2$ OH）$_2$、CH $_2$ OHCHO和HCOOCH $_3$空间共存，则G34.3+0.2和W51/e2的相对丰度比HCOOCH $_3$ /（CH $_2$ OH）$_2$分别为31和35。未检出CH $_2$ OHCHO，但数据提供了HCOOCH $_3$ /CH $_2$ OHCHO丰度比的下限，G34.3+0.2为$\ge$ 193，W51/e2为$\ge$ 550。将这些结果与文献中各种来源的测量结果进行比较，表明源光度可能与HCOOCH $_3$ /（CH $_2$ OH）$_2$和HCOOCH $_3$ /CH $_2$ OHCHO比值相关。这种明显的相关性可能是每个源在不同温度范围内演化的相对时间尺度的结果。此外，我们获得了G34.3+0.2（$\ge$ 6）和W51/e2（$\ge$ 16）的（CH $_2$ OH）$_2$ /CH 2 OHCHO比值的下限。这一结果证实了高（CH $_2$ OH）$_2$ /CH $_2$ OHCHO丰度比不是彗星的特有性质，正如先前推测的那样。
英文摘要：
How complex organic - and potentially prebiotic - molecules are formed in regions of low- and high-mass star-formation remains a central question in astrochemistry. In particular, with just a few sources studied in detail, it is unclear what role environment plays in complex molecule formation. In this light, a comparison of relative abundances of related species between sources might be useful to explain observed differences. We seek to measure the relative abundance between three important complex organic molecules, ethylene glycol ((CH$_2$OH)$_2$), glycolaldehyde (CH$_2$OHCHO) and methyl formate (HCOOCH$_3$), toward high-mass protostars and thereby provide additional constraints on their formation pathways. We use IRAM 30-m single dish observations of the three species toward two high-mass star-forming regions - W51/e2 and G34.3+0.2 - and report a tentative detection of (CH2OH)2 toward both sources. Assuming that (CH$_2$OH)$_2$, CH$_2$OHCHO and HCOOCH$_3$ spatially coexist, relative abundance ratios, HCOOCH$_3$/(CH$_2$OH)$_2$, of 31 and 35 are derived for G34.3+0.2 and W51/e2, respectively. CH$_2$OHCHO is not detected, but the data provide lower limits to the HCOOCH$_3$/CH$_2$OHCHO abundance ratios of $\ge$193 for G34.3+0.2 and $\ge$550 for W51/e2. A comparison of these results to measurements from various sources in the literature indicates that the source luminosities may be correlated with the HCOOCH$_3$/(CH$_2$OH)$_2$ and HCOOCH$_3$/CH$_2$OHCHO ratios. This apparent correlation may be a consequence of the relative timescales each source spend at different temperatures-ranges in their evolution. Furthermore, we obtain lower limits to the ratio of (CH$_2$OH)$_2$/CH2OHCHO for G34.3+0.2 ($\ge$6) and W51/e2 ($\ge$16). This result confirms that a high (CH$_2$OH)$_2$/CH$_2$OHCHO abundance ratio is not a specific property of comets, as previously speculated.
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