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researcher

Kohei Hayashi

4 papers hereh-index 211 citations8 works total

Matching runs newest-first, so older work may not be attached to this profile yet.

author position
  • first author1
  • middle author3

Across the 4 of 4 papers where every author was matched, so the position is known.

fields
  • astro-ph.GA3
  • cs.CL1
same name
  • Kohei Hayashi — 8 papers, h 6
  • Kohei Hayashi — 5 papers, h 5
  • Kohei Hayashi — 4 papers, h 2
  • Kohei Hayashi — 3 papers, h 1
  • Kohei Hayashi — 1 paper, h 20

Either other researchers who publish under this name, or the same person where the external sources have not merged their records.

identity via Semantic Scholar / OpenAlex

collaborators

4 papers

astro-ph.GA2026

Cusp-to-Core Transition of Dark Matter Halos across Galaxy Mass Scales

Kohei Hayashi, Yuka Kaneda, Masao Mori +1

We investigate the diversity of dark matter (DM) density profiles in a large sample of late-type galaxies from the SPARC database, with the goal of testing whether a cusp-to-core t…

astro-ph.GA2025

Chemodynamics of BoötesI with S5: Revised Velocity Gradient, Dark Matter Density, and Galactic Chemical Evolution Constraints

Nathan R. Sandford, Ting S. Li, Sergey E. Koposov +14

We combine new spectroscopic observations of the ultra faint dwarf galaxy (UFD) Boötes I (Boo I) from the Southern Stellar Stream Spectroscopic Survey (S5) with ∼15 year…

cs.CL2025

When Does Metadata Conditioning (NOT) Work for Language Model Pre-Training? A Study with Context-Free Grammars

Rei Higuchi, Ryotaro Kawata, Naoki Nishikawa +7

The ability to acquire latent semantics is one of the key properties that determines the performance of language models. One convenient approach to invoke this ability is to prepen…

astro-ph.GA2025

JFlow: Model-Independent Spherical Jeans Analysis using Equivariant Continuous Normalizing Flows

Sung Hak Lim, Kohei Hayashi, Shun'ichi Horigome +2

The kinematics of stars in dwarf spheroidal galaxies have been studied to understand the structure of dark matter halos. However, the kinematic information of these stars is often…

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