论文标题
来自Herschel Gould Belt调查
The census of dense cores in the Serpens region from the Herschel Gould Belt Survey
论文作者
论文摘要
Herschel Gould Belt调查绘制了附近的（D <500 PC）星形区域，以更好地了解Prestell阶段如何影响恒星形成过程。在这里，我们报告了位于D = 420 PC和484 PC之间的15 deg2区域的密集核心的完整人口普查。 PAC和尖峰摄像机从70米到500米的云成像。使用多波长的源提取算法获取，我们提取833个来源，其中709个是无星核，而124个是候选原始核心核心。我们获得所有样品的温度和质量，对604个Prestellar核心和105个未结合核心的无星核进行了分类。对于大于0.8 msun的群众，我们的源头普查为80％。我们产生核心质量函数（CMF），并将其与初始质量函数（IMF）进行比较。 PRESTELLAR CMF与高达2 MSUN的对数正态趋势一致，之后它跟随斜率为-2.05 +/- 0.34的势力。其CMF的尾巴更陡峭，但仍与我们在这项工作中研究的地区的IMF兼容。我们还提取了Serpens区域的细丝网络，发现81％的Prestellar核心位于丝状结构上。核心与丝状结构之间的空间关联支持范式，由其他塞列列列术提出，这些范式主要是在丝状上形成的。蛇被证实是一个年轻的低质量和活跃的恒星形成区域。
The Herschel Gould Belt survey mapped the nearby (d < 500 pc) star-forming regions to understand better how the prestellar phase influences the star formation process. Here we report a complete census of dense cores in a 15 deg2 area of the Serpens star-forming region located between d=420 pc and 484 pc. The PACS and SPIRE cameras imaged this cloud from 70micron to 500micron. With the multi-wavelength source extraction algorithm getsources, we extract 833 sources, of which 709 are starless cores and 124 are candidate proto-stellar cores. We obtain temperatures and masses for all the sample, classifying the starless cores in 604 prestellar cores and 105 unbound cores. Our census of sources is 80% complete for masses larger than 0.8 Msun overall. We produce the core mass function (CMF) and compare it with the initial mass function (IMF). The prestellar CMF is consistent with log-normal trend up to 2 Msun, after which it follows a power-law with slope of -2.05+/-0.34. The tail of its CMF is steeper but still compatible with the IMF for the region we studied in this work. We also extract the filaments network of the Serpens region, finding that 81% of prestellar cores lie on filamentary structures. The spatial association between cores and filamentary structure supports the paradigm, suggested by otherHerschelobservations, that prestellar cores mostly form on filaments. Serpens is confirmed to be a young, low-mass and active star-forming region.
