Seunghwan Lim

An extended Zel'dovich model for the halo mass function

A new way to construct a fitting formula for the halo mass function is presented. Our formula is expressed as a solution to the modified Jedamzik matrix equation that automatically satisfies the normalization constraint. The characteristic parameters expressed in terms of the linear shear eigenvalues are empirically determined by fitting the analytic formula to the numerical results from the high-resolution N-body simulation and found to be independent of scale, redshift and background cosmology. Our fitting formula with the best-fit parameters is shown to work excellently in the wide mass-range at various redshifts: The ratio of the analytic formula to the N-body results departs from unity by up to 10% and 5% over 1011 ≤ M/(h−1M⊙) ≤ 5 × 1015 at z = 0,0.5 and 1 for the FoF-halo and SO-halo cases, respectively.

Constraining the H i-Halo Mass Relation from Galaxy Clustering

We study the dependence of galaxy clustering on atomic gas mass using a sample of

An observational proxy of halo assembly time and its correlation with galaxy properties

\sim

Galaxy groups in the low-redshift Universe

16,000 galaxies with redshift in the range of

ELUCID. V. Lighting Dark Matter Halos with Galaxies

0.0025 10^8M_{\odot}

Testing galaxy formation models with galaxy stellar mass functions

, drawn from the 70% complete sample of the Arecibo Legacy Fast ALFA survey. We construct subsamples of galaxies with

Full-sky Ray-tracing Simulation of Weak Lensing Using ELUCID Simulations: Exploring Galaxy Intrinsic Alignment and Cosmic Shear Correlations

M_{\rm HI}

The Dearth of Difference between Central and Satellite Galaxies. I. Perspectives on Star Formation Quenching and AGN Activities

above different thresholds, and make volume-limited clustering measurements in terms of three statistics: the projected two-point correlation function, the projected cross-correlation function with respect to a reference sample selected from the Sloan Digital Sky Survey, and the redshift-space monopole moment. In contrast to previous studies, which found no/weak HI-mass dependence, we find both the clustering amplitude on scales above a few Mpc and the bias factors to increase significantly with increasing HI mass for subsamples with HI mass thresholds above

The Dearth of Differences between Central and Satellite Galaxies. II. Comparison of Observations with L-GALAXIES and EAGLE in Star Formation Quenching

10^9M_{\odot}

GALAXY GROUPS IN THE 2MASS REDSHIFT SURVEY

. For HI mass thresholds below