Research
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2024.06.18
The strong-lensing revolution in the JWST-Rubin-Roman era: from resolving the Hubble tension to constraining baryonic feedback
Despite the remarkable success of the Lambda Cold Dark Matter (LCDM) cosmological model, several challenges have recently emerged. One of the most prominent is the “Hubble tension”: the Hubble expansion rate (H_0) measured using the Cepheid-calibrated distance ladder of type Ia supernovae and the value extrapolated from the cosmic microwave background using LCDM disagree by 5 standard deviati...
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2024.06.14
Heating the Super-hot Corona in Solar Active Regions: Insights from RMHD Simulations
What physical mechanisms heat the outer solar or stellar atmosphere to million-kelvin temperatures is a fundamental but long-standing open question. In particular, the solar corona in active-region cores contains an even hotter component reaching 10 MK, manifesting as persistent coronal loops in extreme ultraviolet and soft X-ray images, which imposes a stringent energy budget. Here, we present...
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2024.06.13
Weak lensing cosmology beyond two-point shear correlations
With the fast development of high-precision large photometric surveys, weak lensing (WL) effects have become one of the major probes in cosmology. While the two-point shear correlations are the most extensively employed analyses, other statistics beyond that are desired because of the non-Gaussian nature of cosmic structures. In this presentation, I will discuss the cosmological application of ...
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2024.06.11
Perturbative Modeling of Galaxy Large-scale Structure
Current and future galaxy surveys such as HETDEX, DESI, Euclid, PFS, and SPHEREx aim to address fundamental questions in cosmology. For all these galaxy surveys, galaxy clustering is the primary observable, so modeling the nonlinearities in galaxy clustering is essential to decipher the survey data. Perturbative modeling offers an efficient, flexible, and robust method to achieve this.In this t...
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2024.06.07
Glitching pulsars as sources of transient gravitational waves
The spin of neutron stars can be timed with exquisite precision and are seen observationally as pulsars. They are observed to spin-down steadily over long periods but once in a while, they can undergo a rapid and sudden increase in their spin, which is known as a glitch. For some cases, the glitch is followed by a post-glitch recovery. There are several models that predict the emission of conti...
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