臺灣博碩士論文加值系統

儘管對極亮 X 射線源的研究已歷時 30 年，然而像是射線源的本質，例如中子 星、恆星質量黑洞或是中間質量黑洞，亦或是其中的吸積機制至今尚未有定論。為 了知曉其中奧秘，增加更多對極亮 X 射線源的分析是有明確助益的。對此，我們使 用於 2016 年由錢卓拉望遠鏡觀測棒旋星系 NGC 1559 的數據來調查該星系之 X 射 線源分佈，特別是極亮 X 射線源。整組數據歷時 45 仟秒，我們以 2.′7 的等光強線 半徑作為此星系之範圍，於內發現了 33 個 X 射線源。其中，滿足極亮 X 射線源光 度標準 Lx > 1039 erg s−1 (0.3–7 keV) 的光源有 8 個。我們檢查了所有 X 射線源的光 變曲線與光譜。除了一些低光子數的光譜無法給出明確的結果之外，所有 X 射線源 基本上都屬於硬 X 射線光譜，因此極有可能是非熱輻射源。由於觀測時間較短，大 多數 X 射線源皆沒有明確的變化性，但我們仍發現一個值得留意的極亮 X 射線源， 代號 X-24，表現出約 7500 秒的週期性，探測顯著性有 2.7σ。我們推測此週期為一 個雙星系統的軌道週期。洛希瓣溢流與洛希極限能夠與我們的推測一致。因此，我 們認為 X-24 可能是是一個罕見的緻密雙星極亮 X 射線源，同時也是恆星質量黑洞 的績優候選者。

Despite the 30-year history of ultra-luminous X-ray sources (ULXs) studies, issues like the majority of their physical natures (i.e., neutron stars, stellar-mass black holes, or intermediate black holes) as well as the accretion mechanisms are still under debate. Expanding the ULX sample size in the literature is clearly a way to help. To this end, we investigated the X-ray source population, ULXs in particular, in the barred spiral galaxy NGC 1559 using a Chandra observation made in 2016. In this 45-ks exposure, 33 X-ray point sources were detected within the 2.′7 isophotal radius of the galaxy. Among them, 8 ULXs were identified with the criterion of the X-ray luminosity Lx > 1039 erg s−1(0.3–7 keV). Both X-ray light curves and spectra of all the sources were examined. Except for some low-count spectra that only provide ambiguous spectral fitting results, all the X-ray sources were basically spectrally hard and therefore likely have non-thermal origins. While no strong X-ray variability was present in most of the sources owing to the relatively short exposure of the observation, we found an intriguing ULX, named X-24, exhibiting a periodicity of ∼7500 s with a detection significance of 2.7σ. We speculate that it is the orbital period of the system. Roche-lobe over flow and Roche limit are consistent with the speculation. Thus, we suggest that X-24 may be the one of the rare compact binary ULXs, and hence, a good candidate as a stellar-mass black hole.

中文摘要 ....................................... i
Abstract........................................ ii
Acknowledgements .................................. iv
Contents........................................ v
ListofTables..................................... vii
ListofFigures .................................... viii
1 Introduction.................................... 1
2 NGC1559..................................... 6
3 X-rayObservations ................................ 8
3.1 ChandraX-rayObservatory ........................ 8
3.2 XMM-NewtonandSwift .......................... 11
4 DataReduction.................................. 12
4.1 Sourcedetection............................... 12
4.2 Spectralanalysis .............................. 13
4.3 Hardnessratios ............................... 15
4.4 Lightcurvesandsearchforperiodicities . . . . . . . . . . . . . . . . . 16
5 Results....................................... 18
5.1 Sourcedetection............................... 18
5.2 X-rayspectraandluminosities....................... 21
5.3 Timinganalysis............................... 25
5.4 TheobservationsofXMM-Newton andSwift . . . . . . . . . . . . . . . 26
6 Discussions .................................... 41
6.1 NGC1559asaULXfactory........................ 41
6.2 X-24..................................... 43
7 Conclusions .................................... 47
References....................................... 48

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