Intragroup and Intracluster Light

Mihos, J. Christopher

doi:10.1017/s1743921315006857

Cited by 24 publications

(19 citation statements)

References 54 publications

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“…Krick & Bernstein 2007) have shown that the ICL is more centrally concentrated than the galaxies of the cluster implying that this light is formed via the mergers that build up the BCG. Consequently, there is no clear differentiation between the outskirts of the BCG and the extended ICL (see Mihos 2016). Therefore, we did not attempt to separate both components.…”

Section: Hst Near-ir Data To Characterize the Iclmentioning

confidence: 99%

“…In the current cosmological paradigm (ΛCDM), clusters of galaxies are assembled hierarchically by the accretion of galaxies or small galaxy groups. Observationally, one of the most revealing signatures of this assembly is the ICL (see Mihos 2016 for a review). This diffuse light is composed of a substantial fraction of stars, between 5 − 20% of the total amount of stars in the cluster, (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Intracluster light: a luminous tracer for dark matter in clusters of galaxies

Montes

Trujillo

2018

Monthly Notices of the Royal Astronomical Society

120

113

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The bulk of stars in galaxy clusters are confined within their constituent galaxies. Those stars do not trace the extended distribution of dark matter well as they are located in the central regions of the cluster's dark matter sub-halos. A small fraction of stars is expected, however, to follow the global dark matter shape of the cluster. These are the stars whose extended spatial distribution results from the merging activity of galaxies and form the intracluster light (ICL). In this work, we compare the bi-dimensional distribution of dark matter in massive galaxy clusters (as traced by gravitational lensing models) with the distribution of the ICL. To do that, we use the superb data from the Hubble Frontier Fields Initiative. Using the Modified Hausdorff distance (MHD) as a way of quantifying the similarities between the mass and ICL distributions, we find an excellent agreement (MHD∼25 kpc) between the two components. This result shows that the ICL exquisitely follows the global dark matter distribution, providing an accurate luminous tracer of dark matter. This finding opens up the possibility of exploring the distribution of dark matter in galaxy clusters in detail using only deep imaging observations.

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Section: Hst Near-ir Data To Characterize the Iclmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Intracluster light: a luminous tracer for dark matter in clusters of galaxies

Montes

Trujillo

2018

Monthly Notices of the Royal Astronomical Society

120

113

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“…This "missing light" is termed the intrahalo light (IHL) which would permeate the Universe. IHL is to be distinguished from "intracluster light" (ICL; Mihos, 2016;Mihos et al, 2005), associated with clusters of galaxies, which in turn are removed/isolated in CIB fluctuations studies; much of the ICL is further linked to extended halos of brightest cluster galaxies. The mean luminosity of an IHL contributing halo of mass M is assumed to be modeled at rest λ as l λ (M, z) = f IHL (M )[F λ L 2.2µm (M )](1 + z) α with F λ being the SED of the IHL component, normalized to unity at 2.2 µm and assumed to be the same as that of old red stellar populations of elliptical galaxies.…”

Section: E New Diffuse Sources At Intermediate and Low Zmentioning

confidence: 99%

Looking at cosmic near-infrared background radiation anisotropies

et al. 2018

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The cosmic infrared background (CIB) contains emissions accumulated over the entire history of the Universe, including from objects inaccessible to individual telescopic studies. The near-IR (∼ 1 − 10 µm) part of the CIB, and its fluctuations, reflects emissions from nucleosynthetic sources and gravitationally accreting black holes (BHs). If known galaxies are removed to sufficient depths the source-subtracted CIB fluctuations at near-IR can reveal sources present in the first-stars-era and possibly new stellar populations at more recent times. This review discusses the recent progress in this newly emerging field which identified, with new data and methodology, significant source-subtracted CIB fluctuations substantially in excess of what can be produced by remaining known galaxies. The CIB fluctuations further appear coherent with unresolved cosmic X-ray background (CXB) indicating a very high fraction of BHs among the new sources producing the CIB fluctuations. These observations have led to intensive theoretical efforts to explain the measurements and their properties. While current experimental configurations have limitations in decisively probing these theories, their potentially remarkable implications will be tested in the upcoming CIB measurements with the ESA's Euclid dark energy mission. We describe the goals and methodologies of LIBRAE (Looking at Infrared Background Radiation with Euclid), a NASA-selected project for CIB science with Euclid, which has the potential for transforming the field into a new area of precision cosmology. * Alexander. Kashlinsky@nasa.gov; Code 665, Observational Cosmology Lab, E. Probing IGM at pre-reionization: CMB-CIB crosspower 48 F. History of emissions from Lyman tomography 49 G. Probing BAOs and dark energy at 10 < z < 16 50 H. LIBRAE summary 51 VIII. Other forthcoming experimental configurations 52 IX. Outlook for the future 53 X. Appendix: acronyms and abbreviations 54 XI. Acknowledgments 54 References 55 4π c I ν /h Planck = 0.63 Iν MJy/sr cm −3 . For comparison the CMB photons are orders-of-magnitude more abundant with n CMB = 413 cm −3 .CMB observations established the flat geometry of the Universe. We will thus adopt the Friedman-Robertson-Walker flat metric for the Universe with the interval given by dsω are the redshift, comoving coordinate distance, cosmic time, and solid angle. Photons move along null geodesics, ds 2 = 0. The Friedman equations with the matter, dark energy (Λ), radiation/relativistic component and curvature density parameters Ω m , Ω Λ , Ω γ , Ω K lead to c(1 + z)dt/dz = R H /E(z), where E(z) ≡ [Ω γ (1 + z) 4 + Ω m (1 + z) 3 + Ω K (1 + z) 2 + Ω Λ f (z)] 1/2 with f (z) describing the evolution of DE and R H ≡ cH −1 0 . The Hubble constant is H(z) = H 0 E(z) and the distance measures become: the coordinate distance x(z) = c (1 + z)dt = R H z 0 dz/E(z), the comoving angular di-Advanced CCD Imaging Spectrometer -imaging arrays AEGIS XD All-wavelength Extended Groth strip International Survey -X-ray, deep AGB Asymptotic giant branch AKARI A Japane...

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“…Throughout this cluster assembly, individual galaxies interact with one other. During these interactions, matter can be stripped from galaxies and form tidal tails, shells, bridges, and liberating stars from their host galaxies, which contribute to formation of a very faint component of diffuse intacluster light (ICL) (Mihos 2015).…”

Section: Introductionmentioning

confidence: 99%

VEGAS: A VST Early-type Galaxy Survey. III. Mapping the Galaxy Structure, Interactions, and Intragroup Light in the NGC 5018 Group

Spavone

Iodice

Capaccioli

et al. 2018

ApJ

106

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Most of the galaxies in the Universe at present day are in groups, which are key to understanding the galaxy evolution. In this work we present a new deep mosaic of 1.2 × 1.0 square degrees of the group of galaxies centered on NGC 5018, acquired at the ESO VLT Survey Telescope. We use u, g, r images to analyse the structure of the group members and to estimate the intra-group light. Taking advantage of the deep and multiband photometry and of the large field of view of the VST telescope, we studied the structure of the galaxy members and the faint features into the intra-group space and we give an estimate of the intragroup diffuse light in the NGC 5018 group of galaxies. We found that ∼ 41% of the total g-band luminosity of the group is in the form of intragroup light (IGL). The IGL has a (g -r) color consistent with those of other galaxies in the group, indicating that the stripping Corresponding author: Marilena Spavone marilena.spavone@oacn.inaf.it arXiv:1807.11204v1 [astro-ph.GA] 30 Jul 2018 2 Spavone et al.leading to the formation of IGL is ongoing. From the study of this group we can infer that there are at least two different interactions involving the group members: one between NGC 5018 and NGC 5022, which generates the tails and ring-like structures detected in the light, and another between NGC 5022 and MCG-03-34-013 that have produced the HI tail. A minor merging event also happened in the formation history of NGC 5018 that have perturbed the inner structure of this galaxy.

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Intragroup and Intracluster Light

Cited by 24 publications

References 54 publications

Intracluster light: a luminous tracer for dark matter in clusters of galaxies

Intracluster light: a luminous tracer for dark matter in clusters of galaxies

Looking at cosmic near-infrared background radiation anisotropies

VEGAS: A VST Early-type Galaxy Survey. III. Mapping the Galaxy Structure, Interactions, and Intragroup Light in the NGC 5018 Group

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