论文标题
SNR 0540-69.3
Atacama Compact Array Observations of the Pulsar-Wind Nebula of SNR 0540-69.3
论文作者
论文摘要
我们介绍了SNR 0540-69.3的脉冲星云（PWN）区域的观察结果。观察结果是用4和6带的Atacama紧凑型阵列（ACA）进行的。我们还以3厘米的速度添加了澳大利亚紧凑型阵列（ATCA）的无线电观测值。对于1.449-233.50 GHz，我们获得了一个同步子频谱$f_ν\ propto c n { - α_ν} $，带有频谱索引$α_ν= 0.17 \ pm {0.02} $。为了得出结论，该结论如何在较高频率下加入同步子频谱，我们包括迄今未发表的Akari中红外数据，并评估紫外线（UV），光学和红外（IR）中已发布的数据。特别是，由于光谱线排放受污染，光学中的某些宽带滤波器数据必须从我们的分析中丢弃。对于同步子频谱的UV/IR部分，我们以$α_ν= 0.87^{+0.08} _ { - 0.10} $到达。如果同步器频谱中有双重断裂，则有$ 2.5 \ times10^{ - 3} $带有温度$ \ sim 55 $ k的灰尘的太阳块，一个大约$ \ sim 9 \ sim 9 \ times10^{10} $ hz，而另一个则为$ \ sim 2 \ sim 2 \ sim 2 \\ times10^{13^{13} $ hz。然后，频谱索引从$ \ sim 9 \ sim 9 \ sim 10^{10} $ hz从收音机中的$α_ν= 0.14 \ pm0.07 $变为$α_ν= 0.35^{ - 0.35^{ - 0.07} _ {+0.05} $，以毫米至远-IR范围内。 ACA频段6数据略有解析PWN。特别是，在其他波长下可见的脉冲星西南1.5“ 1.5”，并在3厘米的数据中以0.8英寸的空间分辨率解决，在毫米范围内也很强。 ACA数据清楚地揭示了Pulsar西部的超新星残余壳20-35 Arcsec，对于壳，我们得出$ 8.6-145 $ 〜GHz的$α_ν= 0.64 \ pm {0.05} $。
We present observations of the pulsar-wind nebula (PWN) region ofSNR 0540-69.3. The observations were made with the Atacama Compact Array (ACA) in Bands 4 and 6. We also add radio observations from the Australia Compact Array (ATCA) at 3 cm. For 1.449 - 233.50 GHz we obtain a synchrotron spectrum $F_ν \propto ν^{-α_ν}$, with the spectral index $α_ν = 0.17\pm{0.02}$. To conclude how this joins the synchrotron spectrum at higher frequencies we include hitherto unpublished AKARI mid-infrared data, and evaluate published data in the ultraviolet (UV), optical and infrared (IR). In particular, some broad-band filter data in the optical must be discarded from our analysis due to contamination by spectral line emission. For the UV/IR part of the synchrotron spectrum, we arrive at $α_ν = 0.87^{+0.08}_{-0.10}$. There is room for $2.5\times10^{-3}$ solar masses of dust with temperature $\sim 55$ K if there are dual breaks in the synchrotron spectrum, one around $\sim 9\times10^{10}$ Hz, and another at $\sim 2\times10^{13}$ Hz. The spectral index then changes at $\sim 9\times10^{10}$ Hz from $α_ν = 0.14\pm0.07$ in the radio, to $α_ν = 0.35^{-0.07}_{+0.05}$ in the millimetre to far-IR range. The ACA Band 6 data marginally resolves the PWN. In particular, the strong emission 1.5" south-west of the pulsar, seen at other wavelengths, and resolved in the 3-cm data with its 0.8" spatial resolution, is also strong in the millimeter range. The ACA data clearly reveal the supernova remnant shell 20-35 arcsec west of the pulsar, and for the shell we derive $α_ν = 0.64\pm{0.05}$ for the range $8.6-145$~GHz.
