科学研究
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2025.08.21
What drove the lunar dynamo?
Although the Moon today has no global magnetic field, paleomagnetic measurements of Apollo samples indicate the existence of an ancient field from at least 4.25 to 1.92 billion years ago. It has been proposed that the paleofield was generated by a core dynamo. However, the paleofield’s apparent high intensity and longevity are major challenges to current theory. Three key difficulties have bee...
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2025.08.20
NEXUS: A Spectroscopic Census of Broad-line AGNs and Little Red Dots at 3≲z≲6
In this talk, I will present analysis of a spectroscopic sample of 23 broad-line AGNs (BLAGNs) at 3≲z≲6 selected using F322W2+F444W NIRCam/WFSS grism spectroscopy of the central 100 arcmin2 area of the NEXUS survey. Among these BLAGNs, 15 are classified as Little Red Dots (LRDs) based on their rest-frame UV-optical spectral slopes and compact morphology. The number density of LRDs is ∼1e-5 c...
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2025.08.18
Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations using Lyman alpha forests from DESI and CSST
The Baryon Acoustic Oscillations (BAO) is a powerful large-scale structure probe that is used to constrain dark energy models, and is the main goal of the latest large cosmology survey, eBOSS and Dark Energy Spectroscopic Instrument (DESI). I will present DESI second Data Release (DR2) cosmological results with a particular focus on the measurement of BAO from Lyman-α forest. We measure the is...
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2025.08.15
DESI DR1 Full-Shape analysis: constraining cosmology and mitigating projection effects
Full-shape clustering measurements from DESI DR1 leverage information from the linear to quasi-nonlinear scales to deliver percent-level constraints on cosmological parameters. However, FS analyses relying on broad priors frequently suffer from projection effects, where marginalization over poorly constrained nuisance parameters can bias the inferred posteriors. To address this, we introduce ph...
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2025.07.09
The Population of LISA MBHBs: What we have learned from simulations
Massive black holes (MBHs) are found in the centres of most massive galaxies. When two galaxies merge, their respective MBHs are brought together, some of them will eventually coalesce and become powerful sources of gravitational waves (GWs). The detection of GWs from stellar-mass black hole binaries by the Laser Interferometer Gravitational-Wave Observatory (LIGO) marked the dawn of the GW ast...
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