How do galaxies build up their spin in the cosmic web?

被引：0

作者：

Welker, Charlotte ^{[1
,2
]}

Dubois, Yohan ^{[1
,2
]}

Pichon, Christophe ^{[1
]}

Devriendt, Julien ^{[2
]}

Peirani, Sebastien ^{[1
]}

机构：

[1] Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France

[2] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England

来源：

ZELDOVICH UNIVERSE: GENESIS AND GROWTH OF THE COSMIC WEB | 2016年 / 11卷 / S308期

关键词：

large-scale structure; galaxy formation; galaxy evolution; merger;

D O I：

10.1017/S1743921316010310

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using the Horizon-AGN simulation we find a mass dependent spin orientation trend for galaxies: the spin of low-mass, rotation-dominated, blue, star-forming galaxies are preferentially aligned with their closest filament, whereas high-mass, velocity dispersion- supported, red quiescent galaxies tend to possess a spin perpendicular to these filaments. We explore the physical mechanisms driving galactic spin swings and quantify how much mergers and smooth accretion re-orient them relative to their host filaments.

引用

页码：433 / 436

页数：4

共 6 条

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[2]

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[5]

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Welker, C. ;

Devriendt, J. ;

Dubois, Y. ;

Pichon, C. ;

Peirani, S. .

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2014, 445 (01) :L46-L50

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