骚扰对坠落的晚型侏儒有多大效果？
How effective is harassment on infalling late-type dwarfs?
摘要：
提出了一个新的骚扰模型，模拟复杂的，动态的室女座似星系团的潮汐场。该模型适用于小，晚型矮盘星系（大大低于在以前的骚扰模拟质量），因为他们从外围落入集群。这些矮星系只受到高速潮汐的轻微影响，几乎没有或根本没有可观测到的后果;典型的恒星损失是$<10\%$，产生非常低的表面亮度流（$μ_B > 31$ mag arcsec $^{-2}$），以及动力学质光比下降两倍。最后恒星盘仍然是盘状的，并由旋转为主，但往往与潮汐诱导的螺旋结构。通过蒙特卡罗模拟，确定了扰动对下落矮星系的统计可能影响。骚扰的影响被发现是高度依赖于星系团内的星系轨道，这样新吸积的矮星系通常只受到轻微的骚扰。对于$Λ$ CDM星系团质量晕中的子结构轨道，在矮星系坍缩的$<15 \%$中很少发生能将盘状结构转变为球状结构的强潮汐相遇。对于小的远心距离（$<$ 250 kpc）的轨道，骚扰明显更强，导致完全破坏或严重的质量损失（$>90 \%$暗物质和$> 50 \%$恒星），然而，由于星系团的深势阱，这种轨道预计是非常不可能的。
英文摘要：
A new harassment model is presented that models the complex, and dynamical tidal field of a Virgo like galaxy cluster. The model is applied to small, late-type dwarf disc galaxies (of substantially lower mass than in previous harassment simulations) as they infall into the cluster from the outskirts. These dwarf galaxies are only mildly affected by high speed tidal encounters with little or no observable consequences; typical stellar losses are $<10\%$, producing very low surface brightness streams ($μ_B > 31$ mag arcsec$^{-2}$), and a factor of two drop in dynamical mass-to-light ratio. Final stellar discs remain disc-like, and dominated by rotation although often with tidally induced spiral structure. By means of Monte-Carlo simulations, the statistically likely influences of harassment on infalling dwarf galaxies are determined. The effects of harassment are found to be highly dependent on the orbit of the galaxy within the cluster, such that newly accreted dwarf galaxies typically suffer only mild harassment. Strong tidal encounters, that can morphologically transform discs into spheroidals, are rare occurring in $<15 \%$ of dwarf galaxy infalls for typical orbits of sub-structure within $Λ$CDM cluster mass halos. For orbits with small apocentric distances ($<$250 kpc), harassment is significantly stronger resulting in complete disruption or heavy mass loss ($>90 \%$ dark matter and $> 50 \%$ stellar), however, such orbits are expected to be highly improbable for newly infalling galaxies due to the deep potential well of the cluster.
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