We combine orbital information from N-body simulations with an analytic model for star formation quenching and SDSS observations of galaxy positions, redshifts, and colours to infer the differential effect of the group/cluster environment on star formation in satellite galaxies. We repeat a similar exercise with a similar model for gas stripping and supplement the same input catalogue with HI fluxes from the ALFALFA survey. The statistical models are motivated by and tested on the Hydrangea cosmological hydrodynamical simulation suite. Our models recover the typical time when galaxies in the satellite population are stripped and quenched: stripping in massive ($M_{\rm vir}\sim 10^{14.5}\,{\rm M}_\odot$) clusters typically occurs at or just before the first pericentric passage, and up to $\sim 4\,{\rm Gyr}$ later in low mass ($\sim 10^{12.5}\,{\rm M}_\odot$) groups. Quenching occurs later: Balmer emission lines typically fade $\sim 4\,{\rm Gyr}$ ($6.5\,{\rm Gyr}$) after first pericentre in clusters (groups), followed a few hundred ${\rm Myr}$ later by reddening in $(g-r)$ colour. These 'delay timescales' are remarkably constant across the entire satellite stellar mass range probed ($\sim 10^{9.5}$--$10^{11}\,{\rm M}_\odot$); this feature is closely tied to our treatment of 'group pre-processing'. While our measurements are qualitatively consistent with the `delayed-then-rapid' quenching scenario advocated for by several other studies, we find significantly longer delay times. The origin of this apparent discrepancy is difficult to pinpoint. However, our unique use of a homogeneous analysis and input catalogues yields new insight into the sequence of events leading to quenching across wide intervals in host and satellite mass.

中文翻译：

---

在群和星团的卫星星系中气体剥离开始和恒星形成淬灭之间的延迟的均匀测量

我们将来自 N 体模拟的轨道信息与恒星形成淬灭的分析模型和对星系位置、红移和颜色的 SDSS 观测相结合，以推断群/星团环境对卫星星系中恒星形成的不同影响。我们使用类似的气提模型重复类似的练习，并用来自 ALFALFA 调查的 HI 通量补充相同的输入目录。统计模型由绣球花宇宙学流体动力学模拟套件驱动并在其上进行测试。我们的模型恢复了卫星群中星系被剥离和淬灭的典型时间：通常会发生大规模 ($M_{\rm vir}\sim 10^{14.5}\,{\rm M}_\odot$) 星团的剥离在或就在第一个近心通道之前，直到 $\sim 4\,{\rm Gyr}$ 之后的低质量 ($\sim 10^{12.5}\, {\rm M}_\odot$) 组。淬灭发生较晚：巴尔默发射线通常在簇（组）中的第一个中心点之后衰减 $\sim 4\,{\rm Gyr}$ ($6.5\,{\rm Gyr}$)，然后是几百 ${\rm Myr }$ 之后用 $(gr)$ 颜色变红。这些“延迟时间尺度”在探测到的整个卫星恒星质量范围内都非常稳定（$\sim 10^{9.5}$--$10^{11}\,{\rm M}_\odot$）；此功能与我们对“组预处理”的处理密切相关。虽然我们的测量在质量上与其他几项研究提倡的“延迟然后快速”淬火方案一致，但我们发现延迟时间明显更长。这种明显差异的起源很难确定。然而，