A complete catalogue of dusty supernova remnants in the Galactic plane
A complete catalogue of dusty supernova remnants in the Galactic plane
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DOI：
10.1093/mnras/staa221
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发表时间：
2020-01
影响因子：
4.8
通讯作者：
H. Chawner;H. Gomez;M. Matsuura;Matthew W. L. Smith;A. Papageorgiou;Jeonghee Rho;A. Noriega-Crespo;I. D. Looze;M. Barlow;P. Cigan;L. Dunne;Ken Marsh
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文献类型：
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作者：
H. Chawner;H. Gomez;M. Matsuura;Matthew W. L. Smith;A. Papageorgiou;Jeonghee Rho;A. Noriega-Crespo;I. D. Looze;M. Barlow;P. Cigan;L. Dunne;Ken Marsh
我们用赫歇尔望远镜在70-500 μm的银面（经度360°，$b = \pm \, 1^{\circ}$）上寻找已知超新星遗迹（SNRs）的远红外（FIR）对应体。我们在190个信噪比中检测到39个的尘埃特征，其中包括13个核心坍缩超新星（CCSNe），包括4个脉冲星风星云（PWNe）和2个Ia型SNe。另外24个FIR检测到的信噪比类型未知。我们确认了在G350.1 - 0.3范围内对喷射粉尘的FIR检测，并添加到含有喷射粉尘的已知样品中~ 10个信噪比。我们在G351.2+0.1中心的射电核心位置发现了尘埃特征，表明FIR发射与可能的蟹状致密天体一致，尘埃温度和质量为Td = 45.8 K, Md = 0.18 M⊙，与PWN G54.1+0.3相似。我们发现年轻信噪比的检出率更高。我们制作了11个信噪比的尘埃温度图和距离估计的尘埃质量图，发现温度为$15\,\lesssim \, T_d\, \lesssim \, 40$ k的尘埃。如果尘埃被激波相互作用加热，激波气体必须相对较冷和/或具有低密度，以解释观察到的低颗粒温度。
We search for far-infrared (FIR) counterparts of known supernova remnants (SNRs) in the Galactic plane (360° in longitude and $b = \pm \, 1^{\circ }$) at 70–500 μm with Herschel. We detect dust signatures in 39 SNRs out of 190, made up of 13 core-collapse supernovae (CCSNe), including 4 Pulsar Wind Nebulae (PWNe), and 2 Type Ia SNe. A further 24 FIR detected SNRs have unknown types. We confirm the FIR detection of ejecta dust within G350.1−0.3, adding to the known sample of ∼ 10 SNRs containing ejecta dust. We discover dust features at the location of a radio core at the centre of G351.2+0.1, indicating FIR emission coincident with a possible Crab-like compact object, with dust temperature and mass of Td = 45.8 K and Md = 0.18 M⊙, similar to the PWN G54.1+0.3. We show that the detection rate is higher among young SNRs. We produce dust temperature maps of 11 SNRs and mass maps of those with distance estimates, finding dust at temperatures $15\, \lesssim \, T_d\, \lesssim \, 40$ K. If the dust is heated by shock interactions the shocked gas must be relatively cool and/or have a low density to explain the observed low grain temperatures.