Optical Structure and Proper-Motion Age of the Oxygen-rich Supernova Remnant 1E 0102–7219 in the Small Magellanic Cloud
Optical Structure and Proper-Motion Age of the Oxygen-rich Supernova Remnant 1E 0102–7219 in the Small Magellanic Cloud
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小麦哲伦云中富氧超新星遗迹 1E 0102–7219 的光学结构和自行年龄
DOI：
10.1086/500570
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发表时间：
2006
期刊：
影响因子：
--
通讯作者：
A. Stern
中科院分区：
文献类型：
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作者：
S. Finkelstein;Jon A. Morse;James C. Green;J. Linsky;J. Shull;T. Snow;J. Stocke;K. Brownsberger;D. Ebbets;E. Wilkinson;Sara R. Heap;C. Leitherer;B. Savage;Oswald H. Siegmund;A. Stern
我们提出了新的光学发射线图像的年轻的SNR 1 E 0102-7219在SMC上获得的ACS HST。这个天体是富氧类SNRs的成员，在其光学和X射线光谱中显示出强烈的氧，氖和其他金属线发射，并且不存在氢和氦。1 E 0102-7219的前身可能是一颗沃尔夫-拉叶星星，在爆炸成为Ib/c或IIL/B型超新星之前，它经历了相当大的质量损失。该SNR中的喷出物通常快速移动（V > 1000 km s-1），并在反向冲击中被压缩和加热时发射。在2003年，我们获得了光学[O III]，Hα，和连续图像与ACS宽视场相机。通过F475 W滤波器的[O III]图像捕获了喷出物的全速度范围，并显示了投射在SNR中间的相当多的高速发射，该发射被多普勒频移出了之前WFPC 2图像的窄F502 N带通。1995年。使用这两个时期分开约8.5年，我们测量的横向膨胀的喷出物周围的外缘在这个SNR的第一次在可见光波长。从自行测量的12个喷出物细丝，我们估计的平均膨胀速度为2000公里s-1的明亮的喷出物和推断的运动学年龄的SNR为2050 ± 600年。我们从HST数据中推断的年龄大约是Hughes等人从X射线数据中推断的年龄的两倍，尽管我们的1 σ误差线重叠。我们的自行年龄与Eriksen等人在2003年使用空间分辨[O III]径向速度数据得出的独立光学运动学年龄一致。我们得到一个膨胀中心，位于非常接近明显的X射线和无线电热点，这可能表明存在一个紧凑的残余（中子星星或黑洞）。
We present new optical emission-line images of the young SNR 1E 0102-7219 in the SMC obtained with the ACS on HST. This object is a member of the oxygen-rich class of SNRs showing strong oxygen, neon, and other metal-line emissions in its optical and X-ray spectra, and an absence of hydrogen and helium. The progenitor of 1E 0102-7219 may have been a Wolf-Rayet star that underwent considerable mass loss prior to exploding as a Type Ib/c or IIL/b supernova. The ejecta in this SNR are generally fast-moving (V > 1000 km s-1) and emit as they are compressed and heated in the reverse shock. In 2003 we obtained optical [O III], Hα, and continuum images with the ACS Wide Field Camera. The [O III] image through the F475W filter captures the full velocity range of the ejecta and shows considerable high-velocity emission projected in the middle of the SNR that was Doppler-shifted out of the narrow F502N bandpass of a previous WFPC2 image from 1995. Using these two epochs separated by ~8.5 yr, we measure the transverse expansion of the ejecta around the outer rim in this SNR for the first time at visible wavelengths. From proper-motion measurements of 12 ejecta filaments, we estimate a mean expansion velocity for the bright ejecta of ~2000 km s-1 and an inferred kinematic age for the SNR of ~2050 ± 600 yr. The age we derive from HST data is about twice that inferred by Hughes et al. from X-ray data, although our 1 σ error bars overlap. Our proper-motion age is consistent with an independent optical kinematic age derived by Eriksen et al. in 2003 using spatially resolved [O III] radial-velocity data. We derive an expansion center that lies very close to conspicuous X-ray and radio hot spots, which could indicate the presence of a compact remnant (neutron star or black hole).