We present the results of the long-term multiwavelength observations of the TeV-detected blazar PKS 2005$-$489. During the 15-yr period of the monitoring with X-ray Telescope (XRT) onboard Neil Gehrels Swift Observatory, the most extreme flaring event was recorded in 2009 June when the 2–10 keV flux boosted by a factor of $\sim$50 compared to the previous observation with the same instrument and was comparable to that observed during the exceptional flare in 1998. However, strong flaring epochs were followed by much longer periods with significantly lower X-ray states and lesser activity, as revealed during the monitoring with different X-ray instruments and possibly related to the rare emergence of strong shock waves in the jet. Moreover, the target was passive on intraday timescales: only one 0.3–10 keV IDV was shown during 60 XRT observations, incorporating very fast brightness increase by 70% within 160 s which was superimposed on the significantly slower variability over the 82-ks time interval. Generally, the XRT-band spectra are well-fit with a simple powerlaw model, yielding a very broad range of the 0.3–10 keV photon index $\Gamma$=1.95(0.04)–3.25(0.09). The source showed a wide range of the synchrotron peak position in the UV–soft X-ray range (with $E_{\mathrm{p}}^{max}\sim$1.5 keV), thus confirming its previous classification as a high-energy-peaking BL Lac source. PKS 2005$-$489 did not show a clear “harder-when-brighter” spectral trend that could be related to very different physical conditions in the jet emission zone in diverse epochs. The source exhibited moderate and strong flaring activities in the MeV–GeV and UV–optical–IR energy ranges, respectively, which were weakly correlated with the X-ray variability and demonstrated a need of more complex emission scenarios than one-zone synchrotron self-Compton model. The lognormal function is well-fit with the distributions of the X-ray and MeV–GeV fluxes, thus hinting at the possible imprint of the accretion disc’s variability onto the jet.

我们展示了 TeV 检测到的耀变体 PKS  2005的长期多波长观测结果$-$489. 在 Neil Gehrels Swift 天文台 X 射线望远镜 (XRT) 监测的 15 年期间，最极端的燃烧事件记录在 2009 年 6 月，当时 2-10  keV 通量增加了$～$50 与之前使用相同仪器的观测结果相比，与 1998 年异常耀斑期间观测到的结果相当。 然而，正如监测期间所揭示的那样，强烈的耀斑时期之后的时间要长得多，X 射线状态显着降低，活动更小使用不同的 X 射线仪器，可能与喷流中罕见的强烈冲击波有关。此外，该目标在日内时间尺度上是被动的： 在 60 次 XRT 观测期间仅显示一个 0.3-10 keV 的 IDV，在 160 秒内亮度增加了 70%，这叠加在 82 ks 时间间隔内显着较慢的可变性上. 通常，XRT 波段光谱非常适合简单的幂律模型，产生 0.3-10 keV 光子指数 $\Gamma$=1.95(0.04)–3.25(0.09)。源显示出在紫外软 X 射线范围内的同步加速器峰值位置范围很宽（与${乙}_{\mathrm{磷}}^{米\mathrm{一种}X}～$1.5 千电子伏），从而证实其先前分类为一个高能量峰化BL紫胶源。PKS  2005$-$489 没有显示出明显的“更硬时更亮”的光谱趋势，这可能与不同时期喷流发射区非常不同的物理条件有关。该源分别在 MeV-GeV 和 UV-optical-IR 能量范围内表现出中等和强烈的燃烧活动，这与 X 射线变异性弱相关，并表明需要比单区同步加速器更复杂的发射场景。康普顿模型。对数正态函数与 X 射线和 MeV-GeV 通量的分布非常吻合，因此暗示了吸积盘的可变性可能会在射流上留下印记。