论文标题
来自0类Protostars的JET的Calypso IRAM-PDBI调查。喷气机在年轻的星星中无处不在吗？
The CALYPSO IRAM-PdBI survey of jets from Class 0 protostars. Are jets ubiquitous in young stars ?
论文作者
论文摘要
作为Calypso大程序的一部分，我们将原始喷气机的性质和流出的性质限制在21类0类Protostars的样本中，其内部发光度（lint）从0.035到47 lsun。我们分析了CO（2-1）中的高角度分辨率（〜0.5“ -1”）IRAM PDBI观察，SO（$ 5_6-4_5 $）和SIO（5-4）。在所有来源中检测到探测流出气体的CO（2-1）（在SERPS-MM22和SERPS-MM18B中首次检测到。在67％的来源中检测到SIO（5-4）中的准直射流（这是IRAS4B2，IRAS4B1，L1448-NB，SERPS-MM18A）的首次，其中77％也显示出$ 5_6-4_5 $）。在5个来源（占样本的24％）中，因此（$ 5_6-4_5 $）探测内部信封和/或磁盘。 CALYPSO的调查表明，流出现象无处不在，高速射流的检测率随着原恒星增生的形式增加，至少80％的源含量> 1 lsun驾驶喷气机。原始流量表现出类似洋葱的结构，其中SIO喷气机（开头〜10 $^o $）嵌套在更宽的角度，因此（〜15 $^o $）和CO（〜25 $^o $）流出。在尺度上> 300 au，Sio喷气机的准确性少于II类来源的原子喷气机（〜3 $^o $）。在三分之一的来源中检测到两个喷气叶之间的速度不对称性，类似于II类原子喷气机，这表明相同的发射机制在起作用。大多数喷气机的SIO富含SIO（从> 2.4e-7到> 5E-6），这表明从灰尘过热半径内发射的无尘风中有效释放了> 1％-10％的硅在气相中。质量损失率（从〜7E-8到〜3E-6 MSUN/YR）大于II类喷气机测量的质量率。与II级来源类似，质量损失率约为质量积聚率的〜1％-50％，表明年轻恒星的射血和增生之间的相关性从1E4年达到1％，达到了一些MYR。
As a part of the CALYPSO large programme, we constrain the properties of protostellar jets and outflows in a sample of 21 Class 0 protostars with internal luminosities, Lint, from 0.035 to 47 Lsun. We analyse high angular resolution (~0.5"-1") IRAM PdBI observations in CO (2-1), SO ($5_6-4_5$), and SiO (5-4). CO (2-1), which probes outflowing gas, is detected in all the sources (for the first time in SerpS-MM22 and SerpS-MM18b). Collimated high-velocity jets in SiO (5-4) are detected in 67% of the sources (for the first time in IRAS4B2, IRAS4B1, L1448-NB, SerpS-MM18a), and 77% of these also show jet/outflow emission in SO ($5_6-4_5$). In 5 sources (24% of the sample) SO ($5_6-4_5$) probes the inner envelope and/or the disk. The CALYPSO survey shows that the outflow phenomenon is ubiquitous and that the detection rate of high-velocity jets increases with protostellar accretion, with at least 80% of the sources with Lint>1 Lsun driving a jet. The protostellar flows exhibit an onion-like structure, where the SiO jet (opening angle ~10$^o$) is nested into a wider angle SO (~15$^o$) and CO (~25$^o$) outflow. On scales >300 au the SiO jets are less collimated than atomic jets from Class II sources (~3$^o$). Velocity asymmetry between the two jet lobes are detected in one third of the sources, similarly to Class II atomic jets, suggesting that the same launching mechanism is at work. Most of the jets are SiO rich (SiO/H2 from >2.4e-7 to >5e-6), which indicates efficient release of >1%-10% of silicon in gas phase likely in dust-free winds, launched from inside the dust sublimation radius. The mass-loss rates (from ~7e-8 to ~3e-6 Msun/yr) are larger than what was measured for Class II jets. Similarly to Class II sources, the mass-loss rates are ~1%-50% of the mass accretion rates suggesting that the correlation between ejection and accretion in young stars holds from 1e4 yr up to a few Myr.
