Juana Rapoport
Secondary Biases and Their Dependence on Omega Matter
Cosmological simulations show that, for dark matter halos of equal mass, the level of clustering with neighboring structures increases or decreases when a secondary property is considered. This effect is known as “secondary bias.” Since halos correspond to peaks in a density field that evolves according to a cosmological model, the existence of secondary biases implies that mass alone is insufficient to characterize the evolution of this field. In this study, we explore the relationship between cosmology and the observed distribution of halos with equal mass but differing secondary properties (spin, shape, alignment, and concentration). To this end, we present preliminary results on the measurement of secondary biases in 17 cosmological simulations with a variable ΩM.
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Secondary Biases and Their Dependence on Omega Matter