Diffuse intracluster light at intermediate redshifts: intracluster light observations in an X-ray cluster at z= 0.29★

Toledo, I.; Melnick, J.; Selman, F.; Quintana, H.; Giraud, E.; Zelaya, P.

doi:10.1111/j.1365-2966.2011.18423.x

Cited by 43 publications

(47 citation statements)

References 28 publications

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“…On the other hand, other studies report super-solar metallicities in the diffuse light in Abell 3888 (1.0 Z < Z < 2.5 Z , Krick et al 2006) that are interpreted as ICL formed early with the collapse of the main cluster, unrelated to the BCG halos. From a kinematic point of view, the line-of-sight velocity distribution of intra-cluster planetary nebulae in one Coma cluster core field is consistent with the ICL being formed from stars stripped from the halos of the two brightest galaxy in the cluster while they orbit each other , while recent studies of absorption line spectra in the RX J0054.0-2823 cluster are consistent with the ICL being the remnant of tidally destroyed galaxies and streaming in the central regions of the cluster, in which the three central giant ellipticals act as "grinding machines" (Toledo et al 2011). The origin of the ICL and its connection with the BCG halos is thus not fully understood, and it is likely that several mechanisms are acting in its formation.…”

Section: Introductionmentioning

confidence: 58%

Stellar population and the origin of intra-cluster stars around brightest cluster galaxies: the case of NGC 3311

Coccato

Gerhard

Arnaboldi

et al. 2011

A&A

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Context. We investigate the stellar population and the origin of diffuse light around brightest cluster galaxies. Aims. We study the stellar population of the dynamically hot stellar halo of NGC 3311, the brightest galaxy in the Hydra I cluster, and that of photometric substructures in the diffuse light to constrain the origin of these components. Methods. We analyze absorption lines in medium-resolution, long-slit spectra in the wavelength range 4800-5800 Å obtained with FORS2 at the Very Large Telescope. We measure the equivalent width of Lick indices out to 20 kpc from the center of NGC 3311 and fit them with stellar population models that account for the [α/Fe] overabundance. Results. Stars in the dynamically hot halo of NGC 3311 are old (age > 13 Gyr), metal-poor ([Z/H] ∼ −0.35), and alpha-enhanced ([α/Fe] ∼ 0.48). Together with the high velocity dispersion, these measurements indicate that the stars in the halo were accreted from the outskirts of other early-type galaxies, with a possible contribution from dwarf galaxies. We identify a region in the halo of NGC 3311 associated with a photometric substructure where the stellar population is even more metal-poor ([Z/H] ∼ −0.73). In this region, our measurements are consistent with a composite stellar population superposed along the line of sight, consisting of stars from the dynamically hot halo of NGC 3311 and stars stripped from dwarf galaxies. The latter component contributes ≤28% to the local surface brightness. Conclusions. The build-up of diffuse light around NGC 3311 is on-going. Based on the observed stellar population properties, the dominant part of these stars may have come from the outskirts of bright early-type galaxies, while stars from stripped dwarf galaxies are presently being added.

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Section: Introductionmentioning

confidence: 58%

Stellar population and the origin of intra-cluster stars around brightest cluster galaxies: the case of NGC 3311

Coccato

Gerhard

Arnaboldi

et al. 2011

A&A

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“…Similarly, using various samples, Feldmeier et al (), Zibetti et al () and Krick et al () conclude between them that contamination by non‐cluster galaxies is not significant out to z ≃ 0.3. A more robust approach is taken by Toledo et al (), who account for non‐member contamination by calculating the luminosity function of the cluster from spectroscopically confirmed members and then integrating the fitted luminosity function out to faint magnitudes to find the total luminosity of the cluster.…”

Section: Resultsmentioning

confidence: 99%

“…For example, as mentioned in Section , Gonzalez et al (, ) fit the surface brightness profile of the BCG using two DeVaucouleurs profiles. A similar method was followed by Toledo et al (), where all the galaxies in the cluster were masked out except for the BCG, and the surface brightness profile of the extended BCG component was measured. This kind of measurement naturally provides estimates of the fraction of cluster light which is contained in the BCG+ICL.…”

Section: Measuring the Iclmentioning

confidence: 99%

“…The estimates of the fraction of cluster light contained in the ICL in nearby clusters range from 10 to 50 per cent, with the upper end set by the observations in the core of Coma (Bernstein et al ). With the growing realization of the ICL's potential importance there have been concerted efforts on both the observational and theoretical front; new deep observations of ICL have been made in clusters now covering a range of redshifts out to z = 0.8 (Gonzalez, Zabludoff & Zaritsky ; Krick, Bernstein & Pimbblet ; Rudick, Mihos & McBride ; Gonzalez, Zaritsky & Zabludoff ; Krick & Bernstein ; Toledo et al ; Guennou et al ). In addition, recent simulations of the ICL cluster evolution (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Measurement of the intracluster light at z∼1

Burke

Collins

Stott³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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A significant fraction of the total photospheric light in nearby galaxy clusters is thought to be contained within the diffuse intracluster light (ICL), which extends hundreds of kpc from cluster cores. The study of the ICL can reveal details of the evolutionary histories and processes occurring within galaxy clusters; however, since it has a very low surface brightness, it is often difficult to detect. We present here the first measurements of the ICL as a fraction of the total cluster light at z ∼ 1 using deep J‐band (1.2 μm) imaging from a high‐acuity wide‐field K‐band imager on the Very Large Telescope. We investigate the ICL in six X‐ray selected galaxy clusters at 0.8 ≤ z ≤ 1.2 and find that the ICL below isophotes μJ = 22 mag arcsec−2 constitutes 1–4 per cent of the total cluster light within a radius R500. This is broadly consistent with simulations of the ICL at a similar redshift and when compared to nearby observations suggests that the fraction of the total cluster light that is in the ICL has increased by a factor of 2–4 since z ∼ 1. We also find the fraction of the total cluster light contained within the brightest cluster galaxy (BCG) to be 2.0–6.3 per cent at these redshifts, which in five out of six cases is larger than the fraction of the ICL component, in contrast to the results from nearby clusters. This suggests that the evolution in cluster cores involves substantial stripping activity at late times, in addition to the early build‐up of the BCG stellar mass through merging. The presence of significant amount of stellar light at large radii from these BCGs may help towards solving the recent disagreement between the semi‐analytic model predictions of BCG mass growth and the observed large masses and scale sizes reported for BCGs at high redshift.

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“…As discussed in Section 7, Gonzalez et al (2007) posit that the relevant quantity is f IHL+BHG , because it can be difficult to disentangle the stellar mass associated with the central galaxy from the diffuse IHL component. It has been found that f IHL+BHG ∼ 30% on average on cluster scales (Zibetti et al 2005;Gonzalez et al 2007;Pierini et al 2008;Toledo et al 2011).…”

Section: Summary and Discussionmentioning

confidence: 99%

Constraining Satellite Galaxy Stellar Mass Loss and Predicting Intrahalo Light. I. Framework and Results at Low Redshift

Watson¹,

Berlind²,

Zentner³

2012

ApJ

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We introduce a new technique that uses galaxy clustering to constrain how satellite galaxies lose stellar mass and contribute to the diffuse "intrahalo light" (IHL). We implement two models that relate satellite galaxy stellar mass loss to the detailed knowledge of subhalo dark matter mass loss. Model 1 assumes that the fractional stellar mass loss of a galaxy, from the time of merging into a larger halo until the final redshift, is proportional to the fractional amount of dark matter mass loss of the subhalo it lives in. Model 2 accounts for a delay in the time that stellar mass is lost due to the fact that the galaxy resides deep in the potential well of the subhalo and the subhalo may experience dark matter mass loss for some time before the galaxy is affected. We use these models to predict the stellar masses of a population of galaxies and we use abundance matching to predict the clustering of several r-band luminosity threshold samples from the Sloan Digital Sky Survey. Abundance matching assuming no stellar mass loss (akin to abundance matching at the time of subhalo infall) overestimates the correlation function on small scales ( 1 Mpc), while allowing too much stellar mass loss leads to an underestimate of small-scale clustering. For each luminosity threshold sample, we are thus able to constrain the amount of stellar mass loss required to match the observed clustering. We find that satellite galaxy stellar mass loss is strongly luminosity dependent, with less luminous satellite galaxies experiencing substantially more efficient stellar mass loss than luminous satellites. With constrained stellar mass loss models, we can infer the amount of stellar mass that is deposited into the IHL. We find that both of our model predictions for the mean amount of IHL as a function of halo mass are consistent with current observational measurements. However, our two models predict a different amount of scatter in the IHL from halo to halo, with Model 2 being favored by observations. This demonstrates that a comparison to IHL measurements provides independent verification of our stellar mass loss models, as well as additional constraining power.

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Diffuse intracluster light at intermediate redshifts: intracluster light observations in an X-ray cluster at z= 0.29★

Cited by 43 publications

References 28 publications

Stellar population and the origin of intra-cluster stars around brightest cluster galaxies: the case of NGC 3311

Stellar population and the origin of intra-cluster stars around brightest cluster galaxies: the case of NGC 3311

Measurement of the intracluster light at z∼1

Constraining Satellite Galaxy Stellar Mass Loss and Predicting Intrahalo Light. I. Framework and Results at Low Redshift

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