研究射电探测的宽谱线和窄谱线 Seyfert 1 星系的 X 射线发射
Investigating X-ray Emission from Radio-detected Broad- and Narrow-line Seyfert 1 Galaxies
- Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）
- Instituto de Estudios Astrofisicos Facultad de Ingenieria y Ciencias Universidad Diego Portales（迭戈帕托利亚斯大学工程与科学学院天体物理研究所）
- College of Mathematics and Physics, Handan University（邯郸学院数理学院）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究通过拟合 XMM-Newton 光谱并结合多波段数据，比较了射电探测的 NLS1s 和 BLS1s 的 X 射线发射，发现 NLS1s 具有更陡的光子指数和更弱的 X 射线发射，差异源于其更早的演化阶段，并支持喷流相关的多波段辐射联系。
AI中文摘要：
背景：本文对一组射电探测（RD-）宽谱线和窄谱线 Seyfert 1 星系（NLS1s 和 BLS1s）样本的 X 射线发射进行了研究。目的：探究 NLS1s 中早期吸积活动或早期喷流的 X 射线发射特性。方法：通过拟合 XMM-Newton X 射线光谱，并结合 SDSS 和 FIRST 的多波段数据，我们对 NLS1s 和 BLS1s 的 X 射线发射及多波段相关性进行了统计比较研究。结果：NLS1s 和 BLS1s 在软 X 射线黑体温度上没有显著差异，但 NLS1s 表现出更陡的硬 X 射线光子指数和光学到 X 射线斜率（$\alpha_{\rm ox}$）。此外，各种参数的相关性分析揭示了两个样本在 X 射线发射上的内在差异。例如，在相当的光学光度下，NLS1s 表现出更高的 $\alpha_{\rm ox}$（即更弱的 X 射线发射），在基本平面中射电光度与黑洞质量之间的依赖性略有不同，以及 $\alpha_{\rm ox}$ 与射电 loudness 之间的不同相关性。基于 RQ-AGN 中 UV 光度与 $\alpha_{\rm ox}$ 的关系，两个样本中估计的 X 射线过剩（$\Delta \alpha_{\rm ox}$）与射电 loudness 正相关。RQ-BLS1s 通常表现出 X 射线过剩，而 RQ-NLS1s 倾向于表现出 X 射线不足。由 X 射线光度推导的 RQ-NLS1s 的爱丁顿比率低于由光学光度推断的值，进一步支持了它们本质上较弱的 X 射线发射。结论：NLS1s 和 BLS1s 之间 X 射线发射的这些差异可能最终源于 NLS1s 更早的演化阶段。对 NLS1s 和 BLS1s 的射电光度、X 射线光度和射电 loudness 进行的多元线性拟合支持了与喷流相关的多波段辐射联系。
英文摘要：
Context: This paper presents a study of the X-ray emission for a sample of radio-detected (RD-) broad- and narrow-line Seyfert 1 galaxies (NLS1s and BLS1s). Aims: To investigate the X-ray emission properties of early-stage accretion activity or early jets in NLS1s. Methods: By fitting XMM-Newton X-ray spectra and combining with multi-band data from SDSS and FIRST, we conducted a statistical comparative study on the X-ray emission and multi-band correlations of NLS1s and BLS1s. Results: NLS1s and BLS1s show no significant difference in their soft X-ray blackbody temperatures, but NLS1s exhibit steeper hard X-ray photon indices and optical-to-X-ray slopes ($α_{\rm ox}$). Moreover, correlation analyses of various parameters reveal intrinsic differences in the X-ray emission between the two samples. For instance, at comparable optical luminosities, NLS1s exhibit a higher $ α_{\rm ox} $ (i.e., weaker X-ray emission), marginally distinct dependencies between radio luminosity and black hole mass in the fundamental plane, and different correlations between $α_{\rm ox} $ and radio loudness. Based on the relationship between UV luminosity and $α_{\rm ox} $ in RQ-AGN, the estimated X-ray excess ($Δα_{\rm ox} $) in both samples is positively correlated with radio loudness. RQ-BLS1s generally display the X-ray excess, whereas RQ-NLS1s tend to show an X-ray deficiency. The Eddington ratio of RQ-NLS1s derived from X-ray luminosity is lower than that inferred from optical luminosity, further supporting their intrinsically weaker X-ray emission. Conclusions: These differences in X-ray emission between NLS1s and BLS1s may ultimately stem from the earlier evolutionary stage of NLS1s. Multivariate linear fits among radio luminosity, X-ray luminosity, and radio loudness for NLS1s and BLS1s support a multi-wavelength radiative connection associated with jets.
