The JCMT Gould Belt Survey: SCUBA-2 observations of circumstellar discs in L 1495
The JCMT Gould Belt Survey: SCUBA-2 observations of circumstellar discs in L 1495
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DOI：
10.1093/mnras/stv438
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发表时间：
2015-02
影响因子：
4.8
通讯作者：
J. Buckle;E. Drabek-Maunder;J. Greaves;J. Richer;B. Matthews;D. Johnstone;H. Kirk;S. Beaulieu;D. Berry;H. Broekhoven-Fiene;M. Currie;M. Fich;J. Hatchell;T. Jenness;J. Mottram;D. Nutter;K. Pattle;J. E. Pineda;J. E. Pineda;C. Salji;S. Tisi;J. Francesco;M. Hogerheijde;D. Ward-Thompson;P. Bastien;H. Butner;M. C. Chen;A. Chrysostomou;S. Coudé;C. Davis;A. Duarte-Cabral;P. Friberg;R. Friesen;G. Fuller;S. Graves;J. Gregson;J. Gregson;W. Holland;W. Holland;G. Joncas;J. Kirk;L. Knee;S. Mairs;K. Marsh;G. Moriarty-Schieven;J. Rawlings;E. Rosolowsky;D. Rumble;S. Sadavoy;H. Thomas;N. Tothill;S. Viti;G. White;G. White;C. Wilson;J. Wouterloot;J. Yates;M. Zhu
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文献类型：
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作者：
J. Buckle;E. Drabek-Maunder;J. Greaves;J. Richer;B. Matthews;D. Johnstone;H. Kirk;S. Beaulieu;D. Berry;H. Broekhoven-Fiene;M. Currie;M. Fich;J. Hatchell;T. Jenness;J. Mottram;D. Nutter;K. Pattle;J. E. Pineda;J. E. Pineda;C. Salji;S. Tisi;J. Francesco;M. Hogerheijde;D. Ward-Thompson;P. Bastien;H. Butner;M. C. Chen;A. Chrysostomou;S. Coudé;C. Davis;A. Duarte-Cabral;P. Friberg;R. Friesen;G. Fuller;S. Graves;J. Gregson;J. Gregson;W. Holland;W. Holland;G. Joncas;J. Kirk;L. Knee;S. Mairs;K. Marsh;G. Moriarty-Schieven;J. Rawlings;E. Rosolowsky;D. Rumble;S. Sadavoy;H. Thomas;N. Tothill;S. Viti;G. White;G. White;C. Wilson;J. Wouterloot;J. Yates;M. Zhu
本文介绍了利用SCUBA-2获得的JCMT古尔德带调查的850 μ m和450 μ m数据，并对L1495中I类、II类和III类盘状源的尘埃属性进行了分析。我们在两个波长下检测到23%的样品，检测率从I-III类下降。中间盘掩模为1.6 × 10 − 3 M，只有7%的II类源的盘质量大于20个木星质量。我们检测到更高比例的磁盘对源与恒星主机的光谱类型K比光谱类型M。光谱类型为K的单恒星宿主的II类盘的质量比光谱类型为M的高，这支持了高质量恒星有更多质量盘的假设。在两个波长处计算的星盘质量的变化表明，具有K光谱类型的星盘与具有M光谱类型的星盘之间的尘埃不透明度和/或尘埃温度可能存在差异。
We present 850μm and 450μm data from the JCMT Gould Belt Survey obtained with SCUBA-2 and characterise the dust attributes of Class I, Class II and Class III disk sources in L1495. We detect 23% of the sample at both wavelengths, with the detection rate decreasing through the Classes from I--III. The median disk mask is 1.6×10−3M⊙, and only 7% of Class II sources have disk masses larger than 20 Jupiter masses. We detect a higher proportion of disks towards sources with stellar hosts of spectral type K than spectral type M. Class II disks with single stellar hosts of spectral type K have higher masses than those of spectral type M, supporting the hypothesis that higher mass stars have more massive disks. Variations in disk masses calculated at the two wavelengths suggests there may be differences in dust opacity and/or dust temperature between disks with hosts of spectral types K to those with spectral type M.