The nature of the infrared counterpart and of the optical nebula associated with the Central Compact Object in Vela Jr.
The nature of the infrared counterpart and of the optical nebula associated with the Central Compact Object in Vela Jr.
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红外对应物和与 Vela Jr. 中心致密天体相关的光学星云的性质。
DOI：
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发表时间：
2019
影响因子：
4.8
通讯作者：
A. Pellizzoni
中科院分区：
文献类型：
--
作者：
R. Mignani;A. Luca;S. Zharikov;W. Hummel;W. Becker;A. Pellizzoni
X射线源CXO，J085201.4$-$461753在几个kyr-old Vela Jr.超新星遗迹（G266.2-1.2）属于被称为“中央致密天体”（CCOs）的特殊孤立中子星类别。与仅在X射线中检测到的其他CCO不同，cxo也可能在其他波长处被检测到。特别是，甚大望远镜（VLT）除了在H$alpha$中探测到一个6arcsec宽的星云外，还探测到一个候选的近红外对应物（H = 21.6 $pm $0.1），解释为速度驱动的弓形激波。在这里，我们提出了新的近红外和光学VLT观测的候选对应cxo及其星云，以确认拟议的协会。此外，我们使用档案钱德拉观测测量的第一次CXO，J085201.4$-$461753自行。两组近红外VLT图像（相隔10.56年）之间的比较没有显示出CXO候选对应物J085201.4$-461753自行的证据，预计从SNR几何中心的4弧分偏移量，3sigma $上限为$sim 10$ mas $^{-1}$。这比预期的自行50 - 100 mas yr ^{-1}$要小得多，而后者又低于我们用Chandra得到的3sigma $上限300 mas yr ^{-1}$。与此同时，VLT光谱学解决了星云的光学发射，这是占主导地位的NII双峰在6548和6584 A，而不是由H$α $。总而言之，我们的结论是，我们提出的近红外对应物可能与cxo无关，而且星云不是一个速度驱动的弓形激波。
The X-ray source CXO, J085201.4$-$461753in the few kyr-old Vela Jr. supernova remnant (G266.2-1.2) belongs to the peculiar class of isolated neutron stars dubbed "Central Compact Objects" (CCOs). At variance with the other CCOs, which are only detected in the X-rays, cxo has been possibly detected also at other wavelengths. In particular, a candidate near-infrared counterpart (H = 21.6 $pm$0.1) was detected by the Very Large Telescope (VLT) in addition to a 6arcsec-wide nebula detected in H$alpha$, interpreted as a velocity-driven bow-shock. Here, we present new near-infrared and optical VLT observations of the candidate counterpart to cxo and its nebula to confirm the proposed associations. Moreover, we used archival Chandra observations to measure for the first time the CXO, J085201.4$-$461753 proper motion. The comparison between the two sets of near-infrared VLT images, taken 10.56 year apart, do not show evidence of proper motion for the candidate counterpart to CXO, J085201.4$-$461753, expected from its 4arcmin offset from the SNR geometrical centre, with a $3sigma$ upper limit of $sim 10$ mas yr$^{-1}$. This is much smaller than the expected proper motion of $sim$50--100 mas yr$^{-1}$, which, in turn, is below the $3sigma$ upper limit of $sim$ 300 mas yr$^{-1}$ that we obtained with Chandra. At the same time, VLT spectroscopy resolved the nebula optical emission, which is dominated by the NII doublet at 6548 and 6584 A and not by H$alpha$. To summarise, we conclude that the proposed near-infrared counterpart is likely unassociated with cxo and that the nebula is not a velocity-driven bow-shock.
超新星遗迹 Puppis A 中中央致密天体 RX J0822-4300 的固有运动，重新审视
DOI：
10.3847/1538-4357/aba121
发表时间：
2020
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Mayer, Martin;Becker, Werner;Patnaude, Daniel;Winkler, P. Frank;Kraft, Ralph
通讯作者：
Kraft, Ralph