We present early results from the Epoch of Giant Planet Migration program, a precise radial velocity (RV) survey of more than 100 intermediate-age (∼20–200 Myr) G and K dwarfs with the Habitable Zone Planet Finder spectrograph (HPF) at McDonald Observatory’s Hobby–Eberly Telescope. The goals of this program are to determine the timescale and dominant physical mechanism of giant planet migration interior to the water ice line of Sun-like stars. Here, we summarize results from the first 14 months of this program, with a focus on our custom RV pipeline for HPF, a measurement of the intrinsic near-infrared RV activity of young Solar analogs, and modeling the underlying population-level distribution of stellar jitter. We demonstrate on-sky stability at the sub-2 m s⁻¹ level for the K2 standard HD 3765 using a least-squares matching method to extract precise RVs. Based on a subsample of 29 stars with at least three RV measurements from our program, we find a median rms level of 34 m s⁻¹. This is nearly a factor of 2 lower than the median rms level in the optical of 60 m s⁻¹ for a comparison sample with similar ages and spectral types as our targets. The observed near-infrared jitter measurements for this subsample are well reproduced with a log-normal parent distribution with μ = 4.15 and σ = 1.02. Finally, by compiling rms values from previous planet search programs, we show that near-infrared jitter for G and K dwarfs generally decays with age in a similar fashion to optical wavelengths, albeit with a shallower slope and lower overall values for ages ≲1 Gyr.

我们提供了“大行星迁移纪元”计划的早期结果，该计划是利用位于“可居住区的行星搜寻器”（HPF）对100多个中年（〜20–200 Myr）G和K小矮星进行的精确径向速度（RV）调查。麦当劳天文台的爱好-艾伯里望远镜。该计划的目标是确定巨型行星向太阳样恒星水冰线内部迁移的时间尺度和主导的物理机制。在这里，我们总结了该计划前14个月的结果，重点是为HPF定制的RV管道，对年轻Solar类似物的固有近红外RV活动的测量，并为恒星的潜在种群水平分布建模抖动。我们展示了在2 ms ^-1以下的空中稳定性使用最小二乘匹配方法提取K2标准HD 3765的水平，以提取精确的RV。根据我们程序中至少有3个RV测量值的29个恒星的子样本，我们发现中值均方根值为34 ms ^-1。对于年龄和光谱类型与我们的目标相似的比较样本，这比光学60 ms ^-1的均方根值低2倍。用对数正态母分布（μ = 4.15和σ）很好地再现了该子样本的观察到的近红外抖动测量值= 1.02。最后，通过汇总先前行星搜索程序的均方根值，我们发现G和K矮星的近红外抖动通常会随着年龄的增长而以与光波长相似的方式衰减，尽管斜率较浅且1 Gyr年龄的总体值较低。