The dust mass in Cassiopeia A from infrared and optical line flux differences
The dust mass in Cassiopeia A from infrared and optical line flux differences
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DOI：
10.1093/mnras/stab932
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发表时间：
2021-03
影响因子：
4.8
通讯作者：
M. Niculescu-Duvaz;M. Barlow;A. Bevan;D. Milisavljevic;I. D. Looze
中科院分区：
文献类型：
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作者：
M. Niculescu-Duvaz;M. Barlow;A. Bevan;D. Milisavljevic;I. D. Looze
在一些高红移星系中发现了大量的尘埃，这使得人们认为核心塌缩超新星(CCSNe)是其尘埃的主要来源，并推动了对当地CCSNe形成的尘埃质量的测量。对于IIb型CCSN的富氧残骸仙后座A(CaS A)，已经通过两种不同的方法确定了0.6-1.1M⊙的尘埃质量，即(A)根据其远红外光谱能量分布和(B)根据其积分光谱中红蓝发射线的不对称性分析。我们提出了第三种独立的方法来确定CaA内的尘埃质量。该方法比较了在类似口径中从远红外和可见光发射线测量的相对通量，考虑了前景尘埃的消光，以确定内部尘埃光学深度，由此可以获得相应的尘埃质量。使用这种方法，我们确定了CaS A中的尘埃质量至少为0.99$^+0.10}_-0.09}$M⊙。
The large quantities of dust that have been found in a number of high-redshift galaxies have led to suggestions that core-collapse supernovae (CCSNe) are the main sources of their dust and have motivated the measurement of the dust masses formed by local CCSNe. For Cassiopeia A (Cas A), an oxygen-rich remnant of a Type IIb CCSN, a dust mass of 0.6–1.1 M⊙ has already been determined by two different methods, namely (a) from its far-infrared spectral energy distribution and (b) from analysis of the red–blue emission line asymmetries in its integrated optical spectrum. We present a third, independent, method for determining the mass of dust contained within Cas A. This compares the relative fluxes measured in similar apertures from [O iii] far-infrared and visual-region emission lines, taking into account foreground dust extinction, in order to determine internal dust optical depths, from which corresponding dust masses can be obtained. Using this method, we determine a dust mass within Cas A of at least 0.99$^{+0.10}_{-0.09}$ M⊙.