Scholarlink

<p>The initial gravitational collapse of dark matter and gas formed a universal filamentary network where the first galaxies formed, with shapes and sizes that depended on the type of dark matter. Claims from deep-space imaging surveys that elongated galaxies predominate at <i>z</i> &gt; 3 are examined here by comparison with detailed hydrodynamical simulations of cold dark matter (CDM), warm dark matter (WDM) and wave/fuzzy dark matter (<i>ψ</i>DM). For CDM and WDM, we have sufficient volume, 10<sup>3</sup> Mpc/<i>h</i><sup>3</sup>, to generate galaxies with stellar masses &gt;10<sup>9</sup> <i>M</i><sub>⊙</sub> at <i>z</i> &gt; 2, which allows a comparison with the CEERS and CANDELS surveys. Here we find that the observed tendency towards elongated, prolate-shaped young galaxies is well matched by WDM based on material accreted along smooth filaments during the first ~500 Myr, with little dependence on stellar mass. This contrasts with CDM, where the stellar morphology is mainly spheroidal and formed from the merging of fragmented filaments. For CDM, several subhaloes are predicted to be visible, whereas for WDM and <i>ψ</i>DM, early merging is rare. Our findings show how the shapes and sizes of early galaxies are sensitive to the smoothness of the underlying filament network, which provides a new constraint on the nature of dark matter.</p>

错误：搜索内容不能为空，请输入英文关键词
错误：关键词超出字数限制，请精简
高级检索

A smooth filament origin for distant prolate galaxies seen by JWST and HST

  • 期刊论文

  • 发表日期：

    2025年12月8日

查看全文
  • Alvaro Pozo,
  • Tom Broadhurst,
  • Razieh Emami,
  • Philip Mocz,
  • Mark Vogelsberger,
  • Lars Hernquist,
  • Christopher J. Conselice,
  • Hoang Nhan Luu,
  • George F. Smoot,
  • Rogier Windhorst

摘要

The initial gravitational collapse of dark matter and gas formed a universal filamentary network where the first galaxies formed, with shapes and sizes that depended on the type of dark matter. Claims from deep-space imaging surveys that elongated galaxies predominate at z > 3 are examined here by comparison with detailed hydrodynamical simulations of cold dark matter (CDM), warm dark matter (WDM) and wave/fuzzy dark matter (ψDM). For CDM and WDM, we have sufficient volume, 103 Mpc/h3, to generate galaxies with stellar masses >109 M⊙ at z > 2, which allows a comparison with the CEERS and CANDELS surveys. Here we find that the observed tendency towards elongated, prolate-shaped young galaxies is well matched by WDM based on material accreted along smooth filaments during the first ~500 Myr, with little dependence on stellar mass. This contrasts with CDM, where the stellar morphology is mainly spheroidal and formed from the merging of fragmented filaments. For CDM, several subhaloes are predicted to be visible, whereas for WDM and ψDM, early merging is rare. Our findings show how the shapes and sizes of early galaxies are sensitive to the smoothness of the underlying filament network, which provides a new constraint on the nature of dark matter.