Intracluster light properties in a fossil cluster at <i>z</i> = 0.47

Yoo, Jaewon; Ko, Jongwan; Kim, Jae-Woo; Kim, Hyo-Won

doi:10.1093/mnras/stab2707

Cited by 19 publications

(24 citation statements)

References 104 publications

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“…One of the most promising routes to understanding how a cluster assembles is to observe cluster quantities that are sensitive to the evolutionary state of the cluster. Recent deep observations of nearby clusters show distinct diffuse intracluster light (ICL), which is the light from stars that are not gravitationally bound to any individual cluster galaxy (Feldmeier et al 2002;Lin & Mohr 2004;Gonzalez et al 2005;Mihos et al 2005;Zibetti et al 2005;Mihos et al 2017;DeMaio et al 2018;Ko & Jee 2018;Jiménez-Teja et al 2019;Kluge et al 2020;Furnell et al 2021;Yoo et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Comparison of Spatial Distributions of Intracluster Light and Dark Matter

Yoo

Sabiu

et al. 2022

ApJS

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In a galaxy cluster, the relative spatial distributions of dark matter, member galaxies, gas, and intracluster light (ICL) may connote their mutual interactions over the cluster’s evolution. However, it is a challenging problem to provide a quantitative measure for matching the shapes between two multidimensional scalar distributions. We present a novel methodology, named the weighted overlap coefficient (WOC), to quantify the similarity of two-dimensional spatial distributions. We compare the WOC with a standard method known as the modified Hausdorff distance (MHD) method. We find that our method is robust, and performs well even with the existence of multiple substructures. We apply our methodology to search for a visible component whose spatial distribution resembles that of dark matter. If such a component could be found to trace the dark-matter distribution with high fidelity for more relaxed galaxy clusters, then the similarity of the distributions could also be used as a dynamical stage estimator of the cluster. We apply the method to six galaxy clusters at different dynamical stages, simulated within a GRT simulation, which is an N-body simulation using the galaxy replacement technique. Among the various components (stellar particles, galaxies, ICL), the ICL+brightest cluster galaxy (BCG) component most faithfully traced the dark-matter distribution. Among the sample galaxy clusters, the relaxed clusters show stronger similarity in the spatial distribution of the dark matter and ICL+BCG than the dynamically young clusters, while the results of the MHD method show a weaker trend with the dynamical stages.

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Section: Introductionmentioning

confidence: 99%

Comparison of Spatial Distributions of Intracluster Light and Dark Matter

Yoo

Sabiu

et al. 2022

ApJS

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“…In fact, the validity of the results presented in this work depends on the accuracy of our semi-analytic model in predicting the right amounts of the BCG and ICL masses. Starting from the latter, it has been shown in several works, theoretical (e.g., Contini et al 2014;Tang et al 2018;Henden et al 2020;Cañas et al 2020;Alonso Asensio et al 2020) but most importantly observational (e.g., Montes & Trujillo 2014;Edwards et al 2016;Harris et al 2017;Alamo-Martínez & Blakeslee 2017;Montes & Trujillo 2018;DeMaio et al 2018;Edwards et al 2020;DeMaio et al 2020;Spavone et al 2020;Raj et al 2020;Ragusa et al 2021;Furnell et al 2021;Chen et al 2021;Yoo et al 2021), that our semi-analytic model provides a good description of the formation and evolution of the ICL. Not just its mass at different redshifts, or the fraction as a function of halo mass, but several other properties that have been confirmed by observational studies.…”

Section: Separation Of the Bcg And Icl Massesmentioning

confidence: 87%

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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“…30 It should be noted that this value is more than twice the time needed to the late-A and early-F stars injected in the ICL during a merger to evolve away and erase the BIE feature, given the average half-life of ∼2 Gyr for a mainsequence F2 star. In principle, the BIE lifespan could give a rough timescale corresponding to the lower limit for the last ) and a candidate fossil cluster RX J105452.03+552112.5 in green (Yoo et al 2021). We show the transmission curves of the HST filters used to determine the ICL in RXJ1007 in the bottom.…”

Section: Discussionmentioning

confidence: 99%

“…In Figure 5, in addition to all ICLHST clusters, we also included a recently measured merging system, WHL J013719.8-08284 at z = 0.566 (Jiménez-Teja et al 2021a), two Frontier Fields clusters with ICL analyzed very recently, A370 (z = 0.375) and S1063 (z = 0.348) (de Oliveira et al 2022) and a potential "fossil system," where a somewhat similar ICL analysis has been performed (Yoo et al 2021), RX J105453.3+552102 at z ∼ 0.47. Compared to the systems that we analyzed in the abovementioned previous works, in Figure 5 it can be seen that RXJ1007 behaves in a different way from all clusters: it does not show either a constant ICLf or the previously described BIE.…”

Section: Iclmentioning

confidence: 99%

“…Black lines indicate the error weighted mean of each main-sequence spectral-type subsample and colored shadowed areas, the mean of the errors. We also plot the values for a candidate fossil cluster RX JJ105452.03+552112.5 in green (Yoo et al 2021). Gray vertical lines at the top of the figure split the wavelength range expected for the peak emission for an average main-sequence star, labeled with gray letters.…”

Section: Spectral Analysismentioning

confidence: 99%

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Independent Evidence for Earlier Formation Epochs of Fossil Groups of Galaxies through the Intracluster Light: The Case for RX J100742.53+380046.6

Dupke

Jiménez-Teja

et al. 2022

ApJ

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Fossil groups (FG) of galaxies still present a puzzle to theories of structure formation. Despite the low number of bright galaxies, they have relatively high velocity dispersions and ICM temperatures often corresponding to cluster-like potential wells. Their measured concentrations are typically high, indicating early formation epochs as expected from the originally proposed scenario for their origin as being older undisturbed systems. This is, however, in contradiction with the typical lack of expected well developed cool cores. Here, we apply a cluster dynamical indicator recently discovered in the intracluster light fraction (ICLf) to a classic FG, RX J1000742.53+380046.6, to assess its dynamical state. We also refine that indicator to use as an independent age estimator. We find negative radial temperature and metal abundance gradients, the abundance achieving supersolar values at the hot core. The X-ray flux concentration is consistent with that of cool core systems. The ICLf analysis provides an independent probe of the system’s dynamical state and shows that the system is very relaxed, more than all clusters, where the same analysis has been performed. The specific ICLf is about 6 times higher, than any of the clusters previously analyzed, which is consistent with an older noninteractive galaxy system that had its last merging event within the last ∼5 Gyr. The specific ICLf is predicted to be an important new tool to identify fossil systems and to constrain the relative age of clusters.

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Intracluster light properties in a fossil cluster at z = 0.47

Cited by 19 publications

References 104 publications

Comparison of Spatial Distributions of Intracluster Light and Dark Matter

Comparison of Spatial Distributions of Intracluster Light and Dark Matter

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

Independent Evidence for Earlier Formation Epochs of Fossil Groups of Galaxies through the Intracluster Light: The Case for RX J100742.53+380046.6

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