Chandra ACIS Survey of M33 (ChASeM33): X-Ray Imaging Spectroscopy of M33SNR 21, the Brightest X-Ray Supernova Remnant in M33
Chandra ACIS Survey of M33 (ChASeM33): X-Ray Imaging Spectroscopy of M33SNR 21, the Brightest X-Ray Supernova Remnant in M33
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M33 的钱德拉 ACIS 巡天 (ChASeM33)：M33SNR 21（M33 中最亮的 X 射线超新星遗迹）的 X 射线成像光谱
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发表时间：
2006
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通讯作者：
D. Breitschwerdt
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作者：
T. Gaetz;W. Blair;J. Hughes;P. Winkler;K. Long;T. Pannuti;B. Williams;R. Edgar;P. Ghavamian;P. Plucinsky;M. Sasaki;R. Kirshner;M. Avillez;D. Breitschwerdt
我们提出并解释了新的X射线数据M33 SNR 21，最明亮的X射线超新星遗迹（SNR）在M33。SNR是相对于明亮的H II区域NGC 592的可见投影（并且似乎与其相互作用）。该源的数据是作为钱德拉ACIS M33（ChASeM 33）超大型项目调查的一部分获得的。接近同轴的钱德拉数据将SNR分解为直径约为5'（在我们假设的M33距离为817 ± 58 kpc时为20 pc）的略椭圆壳。壳层在东部更亮，这表明它在那个方向遇到了密度更高的物质。光辐射与北部的X射线壳层同延，但在西南部远远超出X射线边缘。用吸收的Sedov模型模拟X射线光谱，得到的冲击温度为0.46 keV，电离时标为净= 2.1 × 1012 cm-3 s，丰度为半个太阳（0.45）。假设Sedov动力学给出的平均震前H密度为1.7 ± 0.3 cm-3。动力学年龄估计值为6500 ± 600年，而最佳拟合净值和推导出的ne为8200 ± 1700年;年龄估计值的加权平均值为6700 ± 600年。我们估计了X射线光度（0.25-4.5 keV）为（1.2 ± 0.2）× 1037 ergs-1（吸收）和（1.7 ± 0.3）× 1037 ergs-1（未吸收），与最近的XMM-Newton测定结果吻合得很好。没有检测到显著的过量硬发射;对于任何硬点源，亮度都在1.2 × 1035尔格·s-1（2-8 keV）。
We present and interpret new X-ray data for M33SNR 21, the brightest X-ray supernova remnant (SNR) in M33. The SNR is in seen projection against (and appears to be interacting with) the bright H II region NGC 592. Data for this source were obtained as part of the Chandra ACIS Survey of M33 (ChASeM33) Very Large Project. The nearly on-axis Chandra data resolve the SNR into a ~5' diameter (20 pc at our assumed M33 distance of 817 ± 58 kpc) slightly elliptical shell. The shell is brighter in the east, which suggests that it is encountering higher density material in that direction. The optical emission is coextensive with the X-ray shell in the north, but extends well beyond the X-ray rim in the southwest. Modeling the X-ray spectrum with an absorbed sedov model yields a shock temperature of 0.46 keV, with an ionization timescale of net = 2.1 × 1012 cm-3 s and half-solar abundances (0.45). Assuming Sedov dynamics gives an average preshock H density of 1.7 ± 0.3 cm-3. The dynamical age estimate is 6500 ± 600 yr, while the best-fit net value and derived ne gives 8200 ± 1700 yr; the weighted mean of the age estimates is 6700 ± 600 yr. We estimate an X-ray luminosity (0.25-4.5 keV) of (1.2 ± 0.2) × 1037 ergs s-1 (absorbed), and (1.7 ± 0.3) × 1037 ergs s-1 (unabsorbed), in good agreement with the recent XMM-Newton determination. No significant excess hard emission was detected; the luminosity ≲1.2 × 1035 ergs s-1 (2-8 keV) for any hard point source.