은하 형성

논문 5편

은하는 어떻게 질량을 모을까요? 은하는 우주 거대구조 속에서 어떻게 진화할까요?

다중 줌(multi-zoom) 우주론 유체역학 시뮬레이션을 이용해 병합과 매끄러운 가스 강착이 각각 은하 질량에 얼마나 기여하는지 정량화했습니다 (L'Huillier, Combes & Semelin 2012).

유체역학 시뮬레이션 속 은하단 확대 영상. L'Huillier, Combes & Semelin (2012), A&A.

Horizon Run 4 시뮬레이션(Kim et al. 2015)을 이용해 헤일로의 상호작용 빈도(병합과 근접 통과, L'Huillier, Park & Kim 2015)와 정렬(L'Huillier, Park & Kim 2017)을 환경(질량과 대규모 밀도)에 따라 정량화했습니다.

David Fernández Gil이 주도하고 Nature Astronomy에 발표한 연구에서, 초장기선 간섭계(VLBI)로 관측한 AGN 제트의 중심부와 여러 탐사에서 얻은 모은하의 광학적 모양 사이에 약하지만 유의한 정렬이 있음을 발견했습니다 (Fernández Gil et al. 2025, Nat. Astron.).

How the jet–host angle is measured: VLBI jet position angle (a) against the minor axis of the optical host in DES, DESI LS, SDSS and SkyMapper (b–e).

블랙홀 제트는 모은하를 ‘알고’ 있다

2025 · Nature Astronomy 9 (2025) 302

Detection of an orthogonal alignment between parsec-scale AGN jets and their host galaxies

Fernández Gil, D.†, Hodgson, J. A., L'Huillier, B., Asorey, J., Saulder, C., Finner, K., et al.

Comparing VLBI jet directions with optical host-galaxy shapes for about 6,000 AGN, we detect a weak but significant alignment between the parsec-scale jet and the minor axis of its host galaxy: a link between the black hole and its host across three orders of magnitude in scale.

DOI · arXiv:2411.09099

주요 논문 활동은하핵과 제트 은하 형성 VLBI 지도 학생과 함께

How the jet–host angle is measured: VLBI jet position angle (a) against the minor axis of the optical host in DES, DESI LS, SDSS and SkyMapper (b–e). (Figure from the 2025 follow-up paper.)

2023 · arXiv 프리프린트

Exploring connections between the VLBI and optical morphology of AGNs and their host galaxies

Fernández Gil, D.†, Hodgson, J. A., L'Huillier, B.

Matching over 9,000 VLBI sources from the Astrogeo catalogue to their optical host galaxies and fitting the hosts' shapes, this first study finds no clear correlation between host morphology and jet direction.

arXiv:2305.06713

활동은하핵과 제트 은하 형성 VLBI 지도 학생과 함께

Evolution of the alignment between the spins of interacting haloes, by environment (columns) and mass (rows).

2017 · MNRAS 466 (2017) 4875

Ecology of dark matter haloes – II. Effects of interactions on the alignment of halo pairs

L'Huillier, B., Park, C., Kim, J.

In Horizon Run 4, interacting haloes have lower spin and are more spherical than typical haloes. Pairs start with antiparallel spins that gradually become parallel, interactions are mostly radial, and alignments are strongest for massive, close pairs and persist up to $z = 4$ .

DOI · arXiv:1701.04417

은하 형성 암흑물질 헤일로 시뮬레이션 제1저자

Haloes in the cosmic web at z = 0 (top) and z = 1 (bottom): the densest environments (red) sit in the nodes, intermediate ones (cyan) in filaments. — Haloes in the cosmic web at $z = 0$ (top) and $z = 1$ (bottom): the densest environments (red) sit in the nodes, intermediate ones (cyan) in filaments.

2015 · MNRAS 451 (2015) 527

The ecology of dark matter haloes – I. The rates and types of halo interactions

L'Huillier, B., Park, C., Kim, J.

Using Horizon Run 4, we measure how often haloes interact as a function of environment, separation, mass ratio, mass and redshift. Most interactions happen at density contrast $\delta \approx 20$ , while the interacting fraction peaks at $\delta \approx 1000$ ; we provide a fitting formula and identify two interaction modes.

DOI · arXiv:1505.00788

은하 형성 암흑물질 헤일로 시뮬레이션 제1저자

Fraction of stellar mass gained through smooth accretion rather than mergers, versus galaxy mass. The mean is 77%.

2012 · A&A 544 (2012) A68

Mass assembly of galaxies: smooth accretion versus mergers

L'Huillier, B., Combes, F., Semelin, B.

Multi-zoom cosmological simulations show that galaxies grow mostly by smooth accretion, which brings on average 77% of their mass, while mergers bring 23%. Only the most massive galaxies grow significantly through mergers.

DOI · arXiv:1108.4247

주요 논문 은하 형성 시뮬레이션 제1저자

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