On the Origin and Evolution of the Intra-Cluster Light: A Brief Review of the Most Recent Developments

Contini, E.

doi:10.3390/galaxies9030060

Cited by 47 publications

(38 citation statements)

References 136 publications

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“…For further details about the profiles, and in particular about the free parameter γ, we refer the reader to Contini & Gu (2020, 2021. We just stress here that, being the following analysis focused at the present time, the value of γ used is 3, which means that the ICL is more concentrated than the DM halo in which it resides.…”

Section: Bcg and Icl Profilesmentioning

confidence: 99%

“…Generally known as Intra-Cluster Light (ICL), or Diffuse Stellar Component (DSC), it is made of stars that are not gravitationally bound to any cluster galaxy and feels only the potential well of the dark matter (DM) halo. Although the ICL is spread along the whole group/cluster, most of it is usually associated with the Brightest Cluster Galaxy (BCG), which is the galaxy residing at the centre of the DM halo, but considerable amounts of ICL are predicted (e.g., Contini et al 2014Contini et al , 2018 and found (e.g., Gonzalez et al 2013;Presotto et al 2014) to be concentrated around intermediate and massive galaxies (for an introductory review on the ICL see Montes 2019or Contini 2021.…”

Section: Introductionmentioning

confidence: 99%

“…At this point, the only contribution supposedly not ICL should be provided by the BCG. The final separation between the BCG and the ICL is still a challeging task (e.g., Gonzalez et al 2013;Kravtsov et al 2018;Montes & Trujillo 2018;Gonzalez et al 2021;Contini & Gu 2021;Contini 2021). There are several techniques to do that, both theoretical and observational, and all of them with pros and cons.…”

Section: Introductionmentioning

confidence: 99%

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The Transition Region between Brightest Cluster Galaxies and Intra-Cluster Light in Galaxy Groups and Clusters

Contini,

Chen,

2022

Preprint

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We take advantage of a state-of-art semi analytic model of galaxy formation, and the model presented in Contini & Gu (2021), to investigate the mass distribution of Brightest Cluster Galaxies (BCGs) and Intra-Cluster Light (ICL) by addressing two points: (1) the region of transition between a BCG dominated distribution and an ICL dominated one, and; (2) the relation between the total BCG+ICL mass and the ICL one alone. We find the transition radius to be independent of both BCG+ICL and halo masses, with an average of 60±40 kpc, in good agreement with previous observational measurements, but given the large scatter, it can be considered as a sort of physical separation between the two components only on cluster scale. From the analysis of M ICL − M BCG+ICL relation, we build a method able to extract the ICL mass directly from the knowledge of the BCG+ICL one. Given the large scatter on low mass systems, such method under/overpredicts the true value of the ICL in a significant way, up to a factor of three in the worst cases. On the other hand, for log M BCG+ICL > 12 or log M Halo > 14, the difference between the true value and the one extracted from the M ICL − M BCG+ICL relation ranges between ±30%. We therefore suggest this relation as a reliable test for observational works aiming to isolate the ICL from the BCG, for systems hosted by haloes on cluster scale.

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Section: Bcg and Icl Profilesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Transition Region between Brightest Cluster Galaxies and Intra-Cluster Light in Galaxy Groups and Clusters

Contini,

Chen,

2022

Preprint

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“…almost exclusively composed of old, red, low-mass stars. Whereas these cluster galaxies often exhibit super-solar abundance ratios of their stars 16 (Fig. 6), their stellar populations have mostly low masses (< 8 M ) and long lifetimes, implying that they should in principle explode as SNIa and inject large amounts of Fe-peak elements in the ICM over cosmic time.…”

Section: Chemical Composition Of the Icmmentioning

confidence: 99%

Chemical enrichment in groups and clusters

Mernier¹,

Biffi²

2022

Preprint

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As building blocks of dust, rocky planets, and even complex life, the chemical elements heavier than hydrogen (H) and helium (He) -called "metals" in astronomy -play an essential role in our Universe and its evolution. Up to Fe and Ni, these metals are known to be created by stars and stellar remnants via nuclear fusion and to be ejected into their immediate surroundings to enrich new stellar generations. A spectacular finding, however, is that these processed elements are found even outside stellar systems, in particular in the hot, X-ray atmospheres surrounding early-type galaxies and pervading galaxy clusters and groups. These large-scales structures are thus a remarkable fossil record of the integrated history of the enrichment of our Universe. In this Chapter, we briefly discuss the chemical properties of this intracluster -or intragroup -medium (ICM). After introducing the concept of chemical abundances, and recalling which stellar sources produce which elements, we review the method to derive abundance measurements from observations of the ICM and detail some chemical models implemented in numerical hydrodynamical simulations of cosmic structures. In particular, we explore how synergies between X-ray observations and numerical simulations help us to understand (i) the cosmic epoch at which the bulk of the enrichment occurred, (ii) the physics of these stellar sources responsible for this enrichment, and (iii) the main mechanisms responsible for metal diffusion and mixing outside galaxies.

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“…amount, color) are fundamental to set constrains for numerical simulations [32,33,11,15,34], and to reduce the discrepancy between observations and cosmological simulations on the baryon component of the universe [35]. An aspect that is still much debated in literature, both from a theoretical and observational side, regards how the ICL fraction relates to the virial mass (M vir ) of the host environment [36,37]. From a theoretical point of view, Lin and Mohr [38], Murante et al [25], Purcell et al [26] and Henden et al [39] found a slight increase in the ICL fraction in systems with higher M vir .…”

Section: Introductionmentioning

confidence: 99%

The intra-group baryons in the LEO I pair from the VST Early-type GAlaxy Survey

Ragusa¹,

Mirabile²,

Spavone³

et al. 2022

Preprint

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In this paper we present the deep, wide-field and multi-band imaging of the LEO I pair NGC 3379-NGC 3384, from the VST Early-type GAlaxy Survey (VEGAS). The main goal of this study is to map the intra-group baryons in the pair, in the form of diffuse light and globular clusters (GCs). Taking advantage from the large covered area, which extends for ∼ 3.9 square degrees around the pair, and the long integration time, we can map the light distribution out to ∼ 63 kpc and down to ∼ 30 mag/arcsec 2 in the g band and ∼ 29 mag/arcsec 2 in the r band, deeper than previous data available for this target. The map of the intragroup light (IGL) presents two very faint (µ g ∼ 28-29 mag/arcsec 2 ) streams protruding from the brightest group member NGC 3379 and elongated toward North-West and South. We estimate that the fraction of the stellar halo around NGC 3379 plus the IGL is ∼ 17 ± 2% in both g and r bands, with an average color g-r= 0.75 ± 0.04 mag. The color distribution of the GCs appears multi-modal, with two dominant peaks at (u-r) = 1.8 mag and (u-r) = 2.1 mag, respectively. The GC population stretches from North-East to South-West and from North-West to South of the pair, in the last case overlapping with the streams of IGL, as well as the PNe distribution found by Hartke et al. [1] and Hartke et al. [2]. Since these structures are elongated in the direction of the two nearby galaxies M96 and NGC 3338, they could be the remnant of a past gravitational interactions with the pair.

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On the Origin and Evolution of the Intra-Cluster Light: A Brief Review of the Most Recent Developments

Cited by 47 publications

References 136 publications

The Transition Region between Brightest Cluster Galaxies and Intra-Cluster Light in Galaxy Groups and Clusters

The Transition Region between Brightest Cluster Galaxies and Intra-Cluster Light in Galaxy Groups and Clusters

Chemical enrichment in groups and clusters

The intra-group baryons in the LEO I pair from the VST Early-type GAlaxy Survey

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