THE JCMT GOULD BELT SURVEY: EVIDENCE FOR DUST GRAIN EVOLUTION IN PERSEUS STAR-FORMING CLUMPS
THE JCMT GOULD BELT SURVEY: EVIDENCE FOR DUST GRAIN EVOLUTION IN PERSEUS STAR-FORMING CLUMPS
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DOI：
10.3847/0004-637x/826/1/95
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发表时间：
2016-05
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通讯作者：
M. C. Chen;J. Francesco;D. Johnstone;S. Sadavoy;J. Hatchell;J. Mottram;H. Kirk;J. Buckle;D. Berry;H. Broekhoven-Fiene;M. J. Currie;M. Fich;T. Jenness;D. Nutter;K. Pattle;J. E. Pineda;J. E. Pineda;J. E. Pineda;C. Quinn;C. Salji;S. Tisi;M. Hogerheijde;D. Ward-Thompson;P. Bastien;D. Bresnahan;H. Butner;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;J. Gregson;W. Holland;W. Holland;G. Joncas;J. Kirk;L. Knee;S. Mairs;K. Marsh;B. Matthews;G. Moriarty-Schieven;C. Mowat;S. Pezzuto;J. Rawlings;J. Richer;D. Robertson;E. Rosolowsky;D. Rumble;N. Schneider-Bontemps;N. Schneider-Bontemps;H. Thomas;N. Tothill;S. Viti;G. White;G. White;J. Wouterloot;J. Yates;M. Zhu
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作者：
M. C. Chen;J. Francesco;D. Johnstone;S. Sadavoy;J. Hatchell;J. Mottram;H. Kirk;J. Buckle;D. Berry;H. Broekhoven-Fiene;M. J. Currie;M. Fich;T. Jenness;D. Nutter;K. Pattle;J. E. Pineda;J. E. Pineda;J. E. Pineda;C. Quinn;C. Salji;S. Tisi;M. Hogerheijde;D. Ward-Thompson;P. Bastien;D. Bresnahan;H. Butner;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;J. Gregson;W. Holland;W. Holland;G. Joncas;J. Kirk;L. Knee;S. Mairs;K. Marsh;B. Matthews;G. Moriarty-Schieven;C. Mowat;S. Pezzuto;J. Rawlings;J. Richer;D. Robertson;E. Rosolowsky;D. Rumble;N. Schneider-Bontemps;N. Schneider-Bontemps;H. Thomas;N. Tothill;S. Viti;G. White;G. White;J. Wouterloot;J. Yates;M. Zhu
尘埃辐射率光谱指数β是一个关键参数，可以用来推导恒星形成结构的质量和温度，以及它们的引力稳定性。β值取决于各种尘埃颗粒的性质，如大小、孔隙度和表面成分，预计会随着尘埃颗粒的演变而变化。在这里，我们提供了英仙座分子云中恒星形成团块的β，尘埃温度和光学深度图，这些图是通过将光谱能量分布与赫歇尔和JCMT在160，250，350，500和850 μm波段的观测结果相结合来确定的。大多数导出的β和尘埃温度值分别落在1.0-2.7和8-20 K的范围内。在英仙座，我们发现β分布显着不同的丛，晶粒生长的指示。此外，我们还看到单个团块内的显著局部β变化，并发现低β区域与局部温度峰值相关，暗示了低β颗粒的可能起源。在英仙座各处，我们还看到了来自B星和嵌入的原恒星的加热迹象，以及外流塑造当地景观的证据。
The dust emissivity spectral index, β, is a critical parameter for deriving the mass and temperature of star-forming structures and, consequently, their gravitational stability. The β value is dependent on various dust grain properties, such as size, porosity, and surface composition, and is expected to vary as dust grains evolve. Here we present β, dust temperature, and optical depth maps of the star-forming clumps in the Perseus Molecular Cloud determined from fitting spectral energy distributions to combined Herschel and JCMT observations in the 160, 250, 350, 500, and 850 μm bands. Most of the derived β and dust temperature values fall within the ranges of 1.0–2.7 and 8–20 K, respectively. In Perseus, we find the β distribution differs significantly from clump to clump, indicative of grain growth. Furthermore, we also see significant localized β variations within individual clumps and find low-β regions correlate with local temperature peaks, hinting at the possible origins of low-β grains. Throughout Perseus, we also see indications of heating from B stars and embedded protostars, as well evidence of outflows shaping the local landscape.