含硫物质显示的SVS13-A I类化学复杂性。SOLIS XIII
The SVS13-A Class I chemical complexity as revealed by S-bearing species. SOLIS XIII
摘要：
目的：目标是使用干涉测量图像对SVS 13-A进行含硫物种普查，SVS 13-A是一个I类天体，与富含星际复杂有机分子的热科里诺有关。方法：我们使用的数据在3 mm和1.4mm的IRAM-NOEMA在大型程序的框架SOLIS。结果：我们成像了32 SO、34 SO、C32 S、C34 S、C33 S、OCS、H2 C32 S、H2 C34 S和NS的线发射的空间分布。低激发（9 K）~（32）SO谱线跟踪的是由附近的SVS 13-B驱动的快速准直喷流。相反，其余的线被限制在内部SVS 13-A区域，在那里复杂的有机物已经预先成像。SO、SO2和H2 CS的非LTE LVG分析表明热科里诺起源（60-120 au）。温度在50 K到300 K之间，体积密度大于10^5 cm-3。丰度范围如下：0.3-6 × 10^-6（CS）、7 × 10^-9} - 1 × 10^-7（SO）、1-10 × 10^-7（SO2）、少量10^-10（H2 CS和OCS）和10^{-10} - 10^{-9}（NS）。N（NS）/N（NS^+）比值大于10，支持NS^+离子主要在扩展包层中形成。结论：[H2 CS]/[H2 CO]比值随时间增加（从0类到II类物体）超过一个数量级。这表明[S]/[O]在类似太阳的恒星形成过程中会发生变化。SVS 13-A中的[S]/[H]预算估计值为太阳系值（1.8 × 10^-5）的2%-17%，与之前对0类天体测量的值（1%-8%）一致。这支持了相对于暗云的硫化物种的富集在低质量恒星形成的0级到I级阶段保持恒定。目前的发现强调了使用大型观测调查以及太阳系尺度上的采样区域来调查恒星形成区域的化学的重要性。
英文摘要：
Aims: The goal is to obtain a census of S-bearing species using interferometric images, towards SVS13-A, a Class I object associated with a hot corino rich in interstellar complex organic molecules. Methods: We used data at 3mm and 1.4mm obtained with IRAM-NOEMA in the framework of the Large Program SOLIS. Results: We imaged the spatial distribution of the line emission of 32SO, 34SO, C32}S, C34S, C33S, OCS, H2C32S, H2C34S, and NS. The low excitation (9 K) 32SO line is tracing the fast collimated jet driven by the nearby SVS13-B. Conversely, the rest of the lines are confined in the inner SVS13-A region, where complex organics have been previously imaged. The non-LTE LVG analysis of SO, SO2, and H2CS indicates a hot corino origin (60-120 au). Temperatures between 50 K and 300 K, and volume densities larger than 10^5 cm-3 have been derived. The abundances are in the following ranges: 0.3-6 10^-6 (CS), 7 10^-9} - 1 10^-7 (SO), 1-10 10^-7 (SO2), a few 10^-10 (H2CS and OCS), and 10^{-10} - 10^{-9}(NS). The N(NS)/N(NS^+) ratio is larger than 10, supporting that the NS^+ ion is mainly formed in the extended envelope. Conclusions: The [H2CS]/[H2CO] ratio increases with time (from Class 0 to Class II objects) by more than one order of magnitude. This suggests that [S]/[O] changes along the Sun-like star forming process. The estimate of the [S]/[H] budget in SVS13-A is 2%-17% of the Solar System value (1.8 10^-5), being consistent with what was previously measured towards Class 0 objects (1%-8%). This supports that the enrichment of the sulphuretted species with respect to dark clouds keeps constant from the Class 0 to the Class I stages of low-mass star formation. The present findings stress the importance of investigating the chemistry of star forming regions using large observational surveys as well as sampling regions on a Solar System scale.
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