The JCMT Gould Belt Survey: constraints on prestellar core properties in Orion A North
The JCMT Gould Belt Survey: constraints on prestellar core properties in Orion A North
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DOI：
10.1093/mnras/stu2297
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发表时间：
2015-05
影响因子：
4.8
通讯作者：
C. Salji;J. Richer;J. Buckle;J. Hatchell;H. Kirk;S. Beaulieu;D. Berry;H. Broekhoven-Fiene;M. Currie;M. Fich;T. Jenness;D. Johnstone;J. Mottram;D. Nutter;K. Pattle;J. Pineda;C. Quinn;S. Tisi;S. Walker-Smith;J. Francesco;M. Hogerheijde;D. Ward-Thompson;P. Bastien;H. Butner;M. C. Chen;A. Chrysostomou;S. Coudé;C. Davis;E. Drabek-Maunder;A. Duarte-Cabral;J. Fiege;P. Friberg;R. Friesen;G. Fuller;S. Graves;J. Greaves;J. Gregson;W. Holland;G. Joncas;J. Kirk;L. Knee;S. Mairs;K. Marsh;B. Matthews;G. Moriarty-Schieven;J. Rawlings;D. Robertson;E. Rosolowsky;D. Rumble;S. Sadavoy;H. Thomas;N. Tothill;S. Viti;G. White;C. Wilson;J. Wouterloot;J. Yates;M. Zhu
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作者：
C. Salji;J. Richer;J. Buckle;J. Hatchell;H. Kirk;S. Beaulieu;D. Berry;H. Broekhoven-Fiene;M. Currie;M. Fich;T. Jenness;D. Johnstone;J. Mottram;D. Nutter;K. Pattle;J. Pineda;C. Quinn;S. Tisi;S. Walker-Smith;J. Francesco;M. Hogerheijde;D. Ward-Thompson;P. Bastien;H. Butner;M. C. Chen;A. Chrysostomou;S. Coudé;C. Davis;E. Drabek-Maunder;A. Duarte-Cabral;J. Fiege;P. Friberg;R. Friesen;G. Fuller;S. Graves;J. Greaves;J. Gregson;W. Holland;G. Joncas;J. Kirk;L. Knee;S. Mairs;K. Marsh;B. Matthews;G. Moriarty-Schieven;J. Rawlings;D. Robertson;E. Rosolowsky;D. Rumble;S. Sadavoy;H. Thomas;N. Tothill;S. Viti;G. White;C. Wilson;J. Wouterloot;J. Yates;M. Zhu
我们使用Scuba-2(亚毫米通用测辐射热计阵列2)对猎户座A北分子云的观测来得出柱密度和温度图。我们应用了一种新的、基于黑森的结构识别算法来检测这些数据的前恒星核，从而允许自动生成前恒星质量函数。由此产生的质量函数在1.39+0.18−0.19M⊙处达到峰值，与猎户座星云星团初始质量函数峰值相比，恒星形成效率下限为∼14%。此外，观测到的恒星前质量函数以高质量幂指数α=2.53+0.16−0.14衰减，这表明与Salpeter IMF的功能相似(α=2.35)。这一结果与以前的研究结果相结合，表明恒星形成效率具有区域相关性。
We employ SCUBA-2 (Submillimetre Common-User Bolometer Array 2) observations of the Orion A North molecular cloud to derive column density and temperature maps. We apply a novel, Hessian-based structural identification algorithm for detection of prestellar cores to these data, allowing for automated generation of the prestellar mass function. The resulting mass function is observed to peak at 1.39+0.18−0.19 M⊙, indicating a star-forming efficiency lower limit of ∼14 per cent when compared with the Orion nebula Cluster initial mass function (IMF) peak. Additionally, the prestellar mass function is observed to decay with a high-mass power-law exponent α=2.53+0.16−0.14, indicating approximate functional similarity with the Salpeter IMF (α = 2.35). This result, when combined with the results of previous investigations suggests a regional dependence of the star-forming efficiency.