We present a multiwavelength analysis of the cluster A1668, performed by means of new EVLA and Chandra observations and archival Hα data. The radio images exhibit a small central source (∼14 kpc at 1.4 GHz) with L _1.4GHz ∼ 6 10²³ W Hz⁻¹. The mean spectral index between 1.4 GHz and 5 GHz is ∼−1, consistent with the usual indices found in BCGs. The cooling region extends for 40 kpc, with bolometric X-ray luminosity L _cool = 1.9 0.1 10⁴³ erg s⁻¹. We detect an offset of ∼6 kpc between the cluster BCG and the X-ray peak, and another offset of ∼7.6 kpc between the Hα and the X-ray peaks. We discuss possible causes for these offsets, which suggest that the coolest gas is not condensing directly from the lowest-entropy gas. In particular, we argue that the cool ICM was drawn out from the core by sloshing, whereas the Hα filaments were pushed aside from the expanding radio galaxy lobes. We detect two putative X-ray cavities, spatially associated with the west radio lobe (cavity A) and the east radio lobe (cavity B). The cavity power and age of the system are P _cav ∼ 9 10⁴² erg s⁻¹ and t _age ∼ 5.2 Myr, respectively. Evaluating the position of A1668 in the cooling luminosity–cavity power parameter space, we find that the AGN energy injection is currently consistent within the scatter of the relationship, suggesting that offset cooling is likely not breaking the AGN feedback cycle.

我们通过新的 EVLA 和 Chandra 观测以及档案 H α数据对 A1668 星团进行了多波长分析。无线电图像显示了一个小的中心源（1.4 GHz 时的 ∼14 kpc），L _1.4GHz ∼ 6 10 ²³ W Hz ^-1。1.4 GHz 和 5 GHz 之间的平均光谱指数为 ~-1，与 BCG 中发现的通常指数一致。冷却区域延伸 40 kpc，热辐射 X 射线光度L _cool = 1.9 0.1 10 ⁴³ erg s ^-1。我们检测到簇 BCG 和 X 射线峰值之间的~6 kpc 偏移，以及 H α之间的~7.6 kpc 的另一个偏移和 X 射线峰值。我们讨论了这些偏移的可能原因，这表明最冷的气体不是直接从最低熵气体冷凝的。特别是，我们认为凉爽的 ICM 是通过晃动从核心中拉出来的，而 H α细丝被推到了膨胀的射电星系瓣之外。我们检测到两个假定的 X 射线腔，它们在空间上与西射波瓣（腔 A）和东射瓣（腔 B）相关。系统的腔功率和年龄分别为P _cav ∼ 9 10 ⁴² erg s ^-1和t _age分别约为 5.2 Myr。评估 A1668 在冷却光度-腔功率参数空间中的位置，我们发现 AGN 能量注入目前在关系的分散范围内是一致的，这表明偏移冷却可能不会破坏 AGN 反馈循环。