Research
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2024.11.29
Investigating the Squeezed Limit of Primordial Non-Gaussianity: New Constraints from CMB Anisotropies [EN]
The Primordial non-Gaussianity provides fundamental insights into the early Universe and constitutes a crucial area of research in contemporary cosmology. Recently, we extended the cosmological analysis presented in Ibitoye2024 beyond the intergalactic medium (IGM) to investigate the primordial non-Gaussianity parameter (f^0_NL) in the squeezed limit, using the auto- and cross-power spectra of ...
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2024.11.25
The research of dark matter halos with galaxy-galaxy lensing method
In the standard LambdaCDM cosmological framework, cosmic structures grow through a hierarchical process. As fundamental building blocks of the dark matter universe, halos are believed to follow a self-similar structure distribution. Thus, we could stacking the weak lensing signal of multiple halos with the galaxy-galaxy lensing (gglens) method, and obtain the average profile of halos. (A.) With...
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2024.11.18
On the Role of Structural Bimodality on Galaxy Quenching in Local Universe [EN]
Observations have shown that the termination of the star-forming activity in galaxies (quenching of star formation) is closely related to the structure of the galaxies, in the sense that passive galaxies tend to possess more compact structure. The surface mass density in the core region effectively describes the compactness of galaxies, and therefore have served to be one of the most sensitive ...
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2024.11.11
Halo Responses to Baryonic Mechanisms at Small Scale [EN]
The Voids-within-Voids-within-Voids (VVV) project developed a series of extremely high-resolution N-body simulations to study haloes over the entire range of ΛCDM halo masses, from Earth mass to the largest clusters. In this talk, I will present our latest results about how baryons could modify these results for haloes with masses between 10^4 and 10^7 M_sun, below the threshold for galaxy for...
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2024.11.04
A study on Kinematical Small-scale Fluctuations Vary with Galaxy Surface Density
Massive galaxies usually observed as symmetric stellar motions and can be fitted well by the commonly used symmetric dynamical models. However, the stellar kinematics of many low-mass galaxies typically contain lots of small patches, causing the stellar second moment of velocity distribution to be non-smooth in small-scales and far from symmetry, we call these patches kinematical small-scale fl...
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