A New Microquasar Candidate in M83
A New Microquasar Candidate in M83
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DOI：
10.3847/1538-4357/ab5b0c
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发表时间：
2019-11
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影响因子：
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通讯作者：
R. Soria;W. Blair;K. Long;T. Russell;P. Winkler
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作者：
R. Soria;W. Blair;K. Long;T. Russell;P. Winkler
微类星体是带有喷流的中子星或黑洞 X 射线双星。这些喷流可以产生电离的热等离子体冲击气泡，这些气泡可以在河外勘测中伪装成特殊的超新星遗迹（SNR）。为了了解在经过充分研究的螺旋星系 M83 中是否存在这种情况，其中已经识别出一个微类星体候选者 (M83-MQ1)，我们研究了九个 SNR 候选者的特性，这些候选者是因为它们的细长或不规则形态而从该星系中先前识别的 SNR 集中选择的。使用来自钱德拉、哈勃太空望远镜、双子座和澳大利亚望远镜紧凑阵列的多波长数据，我们发现九个源中至少有六个最能解释为信噪比。对于一个来源，我们没有足够的观测数据来解释其线性形态。另一个来源显示了由 O 星光电离主导的星云光谱，但其过量的 [Fe ii] 和射电光度表明可能存在隐藏的 SNR。最后，一个源 (S2) 显示了电离气体的细长结构，沿该线有两个无线电源，以及它们之间的吸积动力 X 射线源（钱德拉源 L14-139）。虽然 S2 可能是多个 SNR 和一个 X 射线双星的偶然排列，但它似乎更有可能是由吸积致密天体喷流驱动的单一物理结构。在后一种情况下，S2 的大小和光度表明其动能约为 1040 erg s−1，与本地宇宙中最强大的微类星体属于同一级别（例如，NGC 7793 中的 S26 和我们银河系中的 SS 433）。
Microquasars are neutron star or black hole X-ray binaries with jets. These jets can create bubbles of hot plasma shock ionized that can masquerade as peculiar supernova remnants (SNRs) in extragalactic surveys. To see if this is the case in the well-studied spiral galaxy M83, where one microquasar candidate (M83-MQ1) has already been identified, we studied the properties of nine SNR candidates, selected because of their elongated or irregular morphology, from the set of previously identified SNRs in that galaxy. Using multiwavelength data from Chandra, the Hubble Space Telescope, Gemini, and the Australia Telescope Compact Array, we found that at least six of our nine sources are best interpreted as SNRs. For one source, we do not have enough observational data to explain its linear morphology. Another source shows a nebular optical spectrum dominated by photoionization by O stars, but its excess [Fe ii] and radio luminosity suggest a possible hidden SNR. Finally, one source (S2) shows an elongated structure of ionized gas, two radio sources along that line, and an accretion-powered X-ray source in between them (the Chandra source L14-139). While S2 could be a chance alignment of multiple SNRs and one X-ray binary, it seems more likely that it is a single physical structure powered by the jet from the accreting compact object. In the latter case, the size and luminosity of S2 suggest a kinetic power of ∼1040 erg s−1, in the same class as the most powerful microquasars in the local universe (e.g., S26 in NGC 7793 and SS 433 in our own Galaxy).