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Summary (English):
In this review we focus on the physical properties – phase space properties, metallicity and age distribution – of the ICL and IGL components of groups and clusters in the local universe within 100 Mpc distance.
Kinematic information on these very low surface brightness structures mostly comes from discrete tracers such as planetary nebulae and globular clusters, showing highly unrelaxed velocity distributions.
Cosmological hydrodynamical simulations provide key predictions for the dynamical state of IGL and ICL components in galaxies, finding that most IC stars are dissolved from galaxies that subsequently merge with the central galaxy.
The increase of measured velocity dispersion with radius in outer halos of bright galaxies is a physical feature that makes it possible to identify IGL and ICL components.
In local groups and clusters within 100 Mpc distance, IGL and ICL are located in dense regions of these structures, where their light fractions relative to the total luminosity of satellite galaxies in a given group or cluster range between a few percent to ten percent, significantly lower than average values found in more evolved, distant clusters.
The kinematics of stellar components such as outer halos of galaxies, IGL and ICL have been challenging due to absorption line spectroscopy confined within two effective radii (Re) for early-type galaxies (ETGs).
Kinematic measurements of the stellar motions in extended structures like groups and clusters date back to Dressler’s work on IC1101, where he measured broadening functions from absorption lines obtained around ETGs.
Today we associate such diffuse light around central bright galaxies with intracluster light (ICL), defined as a stellar component at the centers of galaxy groups not bound to individual galaxies.
Kinematic measurements of stellar motions in extended structures such as outer halos, IGL and ICL are challenging due to absorption line spectroscopy confined within two effective radii for ETGs.
Discrete tracers like planetary nebulae and globular clusters provide kinematic information on these very low surface brightness structures mostly come from cosmological hydrodynamical simulations, predicting the dynamical state of IGL and ICL components in galaxies within 100 Mpc distance.
Cosmological hydrodynamical simulations find that most IC stars are dissolved from galaxies that subsequently merge with central galaxy.
Kinematic measurements of stellar motions in extended structures such as outer halos, IGL and ICL have been challenging due to absorption line spectroscopy confined within two effective radii for ETGs.
Kinematic measurements of stellar motions in extended structures such as outer halos, ICL and IGL have been challenging due to absorption line spectroscopy confined within two effective radii for ETGs.
Kinematic measurements of stellar motions in extended structures

Kinematics of the diffuse intragroup and intracluster light in groups and clusters of galaxies in the Local Universe within 100 Mpc distance Magda Arnaboldi1*, Ortwin E. Gerhard2 1European Southern Observatory (ESO), Garching, Germany 2Max-Planck-Institute für extraterrestrische Physik, Garching, Germany * Correspondence: Corresponding Author: marnabol@eso.org Keywords: galaxies: halos, evolution. Galaxies: clusters: diffuse component, interactions. planetary nebulae: general Abstract Nearly all intragroup (IGL) and intracluster light (ICL) comes from stars that are not bound to any single galaxy but were formed in galaxies and later unbound from them. In this review we focus on the physical properties – phase space properties, metallicity and age distribution – of the ICL and IGL components of the groups and clusters in the local universe, within 100 Mpc distance. Kinematic – information on these very low surface brightness structures mostly comes from discrete tracers such as planetary nebulae and globular clusters, showing highly unrelaxed velocity distributions. Cosmological hydrodynamical simulations provide key predictions for the dynamical state of IGL and ICL and find that most IC stars are dissolved from galaxies that subsequently merge with the central galaxy. The increase of the measured velocity dispersion with radius in the outer halos of bright galaxies is a physical feature that makes it possible to identify IGL and ICL components. In the local groups and clusters, IGL and ICL are located in the dense regions of these structures. Their light fractions relative to the total luminosity of the satellite galaxies in a given group or cluster are between a few to ten percent, significantly lower than the average values in more evolved, more distant clusters. IGL and ICL in the Leo I and M49 groups, and the Virgo cluster core around M87, has been found to arise from mostly old (≥10 Gyr) metal-poor ([Fe/H] < -1.0) stars of low-mass progenitor galaxies. New imaging facilities such as LSST, Euclid, and the ``big eyes’’ on the sky - ELT and JWST with their advanced instrumentation - promise to greatly increase our knowledge of the progenitors of the IGL and ICL stars, their ages, metal content, masses and evolution, thereby increasing our understanding of this enigmatic component. 1. Introduction The motivation to learn about the physics of extended stellar halos in galaxies and the diffuse light in larger structures is synthesized by the statement of Eggen, Lynden-Bell and Sandage in their 1962 seminal paper (Eggen, Lynden-Bell & Sandage 1962), that is “ the time required for stars in the galactic system to exchange their energies and momenta is very long compared with the age of the galaxy. Hence the knowledge of the present energies and momenta of individual objects tells us something of the initial dynamic conditions under which they were formed”. This statement from sixty years ago is still very relevant today: we study the dynamics and chemical composition of stars in the diffuse outer Arnaboldi and Gerhard Kinematics of IGL and ICL 2 Review published on 15 Dec. 2022, doi: https://doi.org/10.3389/fspas.2022.872283 halos of galaxies and in the intracluster and intragroup...

Kinematics of the diffuse intragroup and intracluster light in groups and clusters of galaxies in the Local Universe within 100 Mpc distance Magda Arnaboldi1*, Ortwin E.
Gerhard2 1European Southern Observatory (ESO), Garching, Germany 2Max-Planck-Institute für extraterrestrische Physik, Garching, Germany * Correspondence: Corresponding Author: marnabol@eso.org 키워드 : 은하 : 후광, 진화.
은하 : 클러스터 : 확산 성분, 상호 작용.
행성 성운 : 일반적인 초록 거의 모든 그룹 인트라 드 (IGL)와 클러스터 내 빛 (ICL)은 단일 은하에 묶여 있지 않지만 은하에서 형성되어 나중에 그들로부터 바지를 입지 않은 별에서 비롯됩니다.
이 검토에서 우리는 100 MPC 거리 내에 로컬 우주의 그룹 및 클러스터의 ICL 및 IGL 구성 요소의 물리적 특성 (위상 공간 특성, 금속성 및 연령 분포)에 중점을 둡니다.
Kinematic- 이러한 매우 낮은 표면 밝기 구조에 대한 정보는 주로 행성 성운 및 구형 클러스터와 같은 개별 추적자에서 비롯되며, 고도로 삭감되지 않은 속도 분포를 보여줍니다.
우주적 유체 역학적 시뮬레이션은 IGL 및 ICL의 동적 상태에 대한 주요 예측을 제공하고 대부분의 IC 별은 그 이후 중앙 은하와 합병되는 은하에서 용해된다는 것을 발견합니다.
밝은 은하의 외부 후광에서 반경으로 측정 된 속도 분산의 증가는 IGL 및 ICL 구성 요소를 식별 할 수있는 물리적 특징입니다.
로컬 그룹 및 클러스터에서 IGL 및 ICL은 이러한 구조의 조밀 한 영역에 있습니다.
주어진 그룹 또는 클러스터에서 위성 은하의 총 광도에 대한 광 분획은 몇 ~ 10 %이며, 더 진화 된 더 먼 클러스터의 평균값보다 상당히 낮습니다.
LEO I 및 M49 그룹의 IGL 및 ICL 및 M87 주변의 처녀 자리 클러스터 코어는 저 질병 전조 은하의 대부분의 오래된 (≥10 gyr) Metal-Poor ([Fe/H] <-1.0) 별에서 발생하는 것으로 밝혀졌습니다.
LSST, 유클리드 및“큰 눈 ”과 같은 새로운 이미징 시설은 하늘과 ELT 및 JWST의 고급 계측을 통해 IGL 및 ICL 스타, 연령, 금속 함량, 질량 및 진화에 대한 지식을 크게 높이겠다고 약속합니다.
1.
소개 은하에서 확장 된 스텔라 후광의 물리학에 대해 배우는 동기와 더 큰 구조물의 확산광은 1962 년 정액 용지 (Eggen, Lynden-Bell & Sandage 1962)에서 Eggen, Lynden-Bell 및 Sandage의 진술에 의해 합성됩니다.“은하계에서 별을 교환하는 데 필요한 시간은 오랫동안, 순간과 비교할 때, 그에 따른 순간과 비교됩니다.
개별 물체의 현재 에너지와 순간은 우리에게 형성된 초기 동적 조건을 알려줍니다.” 60 년 전의이 진술은 오늘날에도 여전히 매우 관련이 있습니다.
우리는 2022 년 12 월 15 일에 출판 된 IGL 및 ICL 2 리뷰의 확산 외부 Arnaboldi 및 Gerhard Kinematics에서 별의 역학과 화학적 구성을 연구합니다.
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