The Herschel first look at protostars in the Aquila Rift
S. Bontemps, Ph. Andre, V. Konyves, A. Men'shchikov, N. Schneider, A. Maury, N. Peretto, D. Arzoumanian, M. Attard, F. Motte, V. Minier, P. Didelon, P. Saraceno… 展开作者
S. Bontemps, Ph. Andre, V. Konyves, A. Men'shchikov, N. Schneider, A. Maury, N. Peretto, D. Arzoumanian, M. Attard, F. Motte, V. Minier, P. Didelon, P. Saraceno, A. Abergel, J. -P. Baluteau, J. -Ph. Bernard, L. Cambresy, P. Cox, J. Di Francesco, A. M. Di Giorgo, M. Griffin, P. Hargrave, M. Huang, J. Kirk, J. Li, P. Martin, B. Merin, S. Molinari, G. Olofsson, S. Pezzuto, T. Prusti, H. Roussel, D. Russeil, M. Sauvage, B. Sibthorpe, L. Spinoglio, L. Testi, R. Vavrek, D. Ward-Thompson, G. White, C. Wilson, A. Woodcraft, A. Zavagno
As part of the science demonstration phase of the Herschel mission of the Gould Belt Key Program, the Aquila Rift molecular complex has been observed. The complete ~ 3.3deg x 3.3deg imaging with SPIRE 250/350/500 micron and PACS 70/160 micron allows a deep investigation of embedded protostellar phases, probing of the dust emission from warm inner regions at 70 and 160 micron to the bulk of the cold envelopes between 250 and 500 micron. We used a systematic detection technique operating simultaneously on all Herschel bands to build a sample of protostars. Spectral energy distributions are derived to measure luminosities and envelope masses, and to place the protostars in an M_env - L_bol evolutionary diagram. The spatial distribution of protostars indicates three star-forming sites in Aquila, with W40/Sh2-64 HII region by far the richest. Most of the detected protostars are newly discovered. For a reduced area around the Serpens South cluster, we could compare the Herschel census of protostars with Spitzer results. The Herschel protostars are younger than in Spitzer with 7 Class 0 YSOs newly revealed by Herschel. For the entire Aquila field, we find a total of ~ 45-60 Class 0 YSOs discovered by Herschel. This confirms the global statistics of several hundred Class~0 YSOs that should be found in the whole Gould Belt survey.
Mapping Active Star-Formation in Serpens and the Aquila Rift
University of Alaska Anchorage（阿拉斯加安克雷奇大学）；Dunlap Institute for Astronomy & Astrophysics, University of Toronto（多伦多大学邓普天文学与天体物理研究所）；Northern Arizona University（北亚利桑那大学）；Space Science Institute（空间科学研究所）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；University of Toronto Mississauga（多伦多大学密西沙加分校）
Wide-Field $^{12}$CO ($J=2-1$) and $^{13}$CO ($J=2-1$) Observations toward the Aquila Rift and Serpens Molecular Cloud Complexes. I. Molecular Clouds and Their Physical Properties
我们提出了宽场$^{12}$ CO（$J = 2 - 1$）和$^{13}$ CO（$J = 2 - 1$）对天鹰座裂谷和巨蛇座分子云复合体的观测（25 $^\circ < l < 33^\circ$和$1^\circ < b < 6^\circ$），角分辨率为3 $'$. 4（$\approx$ 0.25个）速度分辨率为0.079 km s $^{-1}$，速度覆盖范围为$-5$ km s $^{-1} < V_{\rm LSR} <$ 35 km s $^{-1}$。我们发现，$^{13}$ CO排放更好地跟踪消光图中看到的结构，并推导出该地区的$X_{\rm ^{13}CO}$因子。应用\texttt{SCIMES}的$^{13}$ CO数据立方体，我们确定了61云，并推导出它们的质量，半径和线宽。谱线-宽度-半径的关系基本上遵循附近的分子云。大多数已识别的云接近维里平衡，虽然分散大。通过用眼睛检查$^{12}$ CO通道图，我们发现了几个在空间上延伸到0.2 $-$ 3度长度的弧。在$^{12}$ CO的速度图中，我们还发现了两个空间延伸的分量，它们似乎向巨蛇座南部和W 40区域会聚。两个不同速度和弧线的分量的存在表明，大规模的膨胀气泡和/或流动在巨蛇座南云和W 40云的形成和演化中发挥了作用。
