THE HERSCHEL AND JCMT GOULD BELT SURVEYS: CONSTRAINING DUST PROPERTIES IN THE PERSEUS B1 CLUMP WITH PACS, SPIRE, AND SCUBA-2
THE HERSCHEL AND JCMT GOULD BELT SURVEYS: CONSTRAINING DUST PROPERTIES IN THE PERSEUS B1 CLUMP WITH PACS, SPIRE, AND SCUBA-2
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DOI：
10.1088/0004-637x/767/2/126
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发表时间：
2013-03
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通讯作者：
S. Sadavoy;S. Sadavoy;J. D. Francesco;J. D. Francesco;D. Johnstone;D. Johnstone;M. Currie;E. D
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作者：
S. Sadavoy;S. Sadavoy;J. D. Francesco;J. D. Francesco;D. Johnstone;D. Johnstone;M. Currie;E. D
我们介绍了赫歇尔观测从赫歇尔古尔德带调查和SCUBA-2科学验证观测从JCMT古尔德带调查的B1块在英仙座分子云。利用联合收割机将Herschel PACS+SPIRE的160-500 μm波段数据与SCUBA-2的450 μm和850 μm波段数据相结合，采用4种不同的方法测定了沙尘的发射率指数。在我们的四种技术中，我们发现最稳健的方法是过滤掉赫歇尔波段中的大尺度发射，以匹配SCUBA-2还原管道恢复的空间尺度。使用这种方法，我们发现在暗条区和中等密度物质中β值为2，而在致密的原恒星核心中β值较低（β = 1.6），这可能是由于尘埃颗粒的生长。我们发现，β和温度是更强大的包括SCUBA-2的数据，提高估计从赫歇尔数据单独的因子为β的10.2倍，温度的10.40%。此外，我们发现核心质量的差异为10.30%相比，赫歇尔只有估计采用β = 2，突出了长波长亚毫米数据的必要性，以获得准确的质量的星前和原恒星的核心。
We present Herschel observations from the Herschel Gould Belt Survey and SCUBA-2 science verification observations from the JCMT Gould Belt Survey of the B1 clump in the Perseus molecular cloud. We determined the dust emissivity index using four different techniques to combine the Herschel PACS+SPIRE data at 160–500 μm with the SCUBA-2 data at 450 μm and 850 μm. Of our four techniques, we found that the most robust method was filtering out the large-scale emission in the Herschel bands to match the spatial scales recovered by the SCUBA-2 reduction pipeline. Using this method, we find β ≈ 2 toward the filament region and moderately dense material and lower β values (β ≳ 1.6) toward the dense protostellar cores, possibly due to dust grain growth. We find that β and temperature are more robust with the inclusion of the SCUBA-2 data, improving estimates from Herschel data alone by factors of ∼2 for β and by ∼40% for temperature. Furthermore, we find core mass differences of ≲ 30% compared to Herschel-only estimates with an adopted β = 2, highlighting the necessity of long-wavelength submillimeter data for deriving accurate masses of prestellar and protostellar cores.