Intragroup diffuse light in compact groups of galaxies: HCG 79, 88 and 95

Rocha, C. Da; Oliveira, C. Mendes de

doi:10.1111/j.1365-2966.2005.09641.x

Cited by 88 publications

(81 citation statements)

References 72 publications

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“…X-ray emission (Ponman et al 1996) and intra-group diffuse light (e.g. Nishiura et al 2000;White et al 2003;Da Rocha & Mendes de Oliveira 2005;Da Rocha et al 2008;Hess et al 2017) have been detected in these objects, confirming their spatial association and intense dynamic activity. We assume a spatial scale of 0.288 kpc arcsec −1 for HCG07, 0.429 kpc arcsec −1 for HCG25 and 0.535 kpc arcsec −1 for HCG98.…”

Section: Datamentioning

confidence: 65%

Ultra-diffuse galaxies outside clusters: clues to their formation and evolution

Román

Trujillo

2017

Monthly Notices of the Royal Astronomical Society

204

242

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We identify six ultra-diffuse galaxies (UDGs) outside clusters in three nearby isolated groups (0.014 < z < 0.026) using very deep imaging in three different Sloan Digital Sky Survey filters (g, r and i bands) from the IAC Stripe82 Legacy Project. By comparing with the abundance of UDGs in rich galaxy clusters, we find that the density of UDGs (i.e. their number per unit mass of the host structure where they are located) decreases towards the most massive systems. This is compatible with a scenario where UDGs are formed preferentially outside clusters. In the periphery (D > 250 kpc) of our three groups, we identify a population of potential UDG progenitors (two of them confirmed spectroscopically). These progenitors have similar masses, shapes and sizes but are bluer, g − i ∼ 0.45 (and for this reason brighter, µ g (0) < 24 mag arcsec −2 ) than traditional UDGs (g − i ∼ 0.76). Passive evolution of these progenitors will transform them into regular (i.e. µ g (0) > 24 mag arcsec −2 ) UDGs after ∼6 Gyr. If confirmed, our observations support a scenario where UDGs are old, extended, low surface brightness dwarf galaxies (M ∼ 10 8 M ) born in the field, are later processed in groups and, ultimately, infall into galaxy clusters by group accretion.

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Section: Datamentioning

confidence: 65%

Ultra-diffuse galaxies outside clusters: clues to their formation and evolution

Román

Trujillo

2017

Monthly Notices of the Royal Astronomical Society

204

242

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“…Some works found that ICL colors are consistent with those of the BCG (e.g., Zibetti et al 2005;Krick & Bernstein 2007;Pierini et al 2008;Rudick et al 2010), suggesting that the ICL has been triggered by ongoing interactions among cluster members and the BCG. The merging cluster in the sample of Pierini et al (2008) and some compact groups (Da Rocha & Mendes de Oliveira 2005) represent an exception showing bluer colors for the ICL, hinting at either in-situ star formation or blue dwarf disruption after interaction.…”

Section: Introductionmentioning

confidence: 92%

“…Observational studies show fractions of ICL ranging from a few percent of the total light up to half of it (Feldmeier et al 2004;Da Rocha & Mendes de Oliveira 2005;Zibetti et al 2005;Krick & Bernstein 2007;Gonzalez et al 2007;Da Rocha et al 2008;Guennou et al 2012;Burke et al 2012;Adami et al 2012), depending on enclosing radius and cluster mass. On top of this, there is no common definition of ICL among both observational works and simulations.…”

Section: Introductionmentioning

confidence: 99%

“…However, both choosing the separation between the BCG and the ICL and determining the best fit model of member galaxies is a difficult task. As a consequence some studies prefer to focus on a BCG+ICL map and mask other members (Gonzalez et al 2005(Gonzalez et al , 2007, while other authors chose to mask all galaxies down to different arbitrary surface brightness levels (Zibetti et al 2005;Krick & Bernstein 2007;Burke et al 2012), and finally Da Rocha & Mendes de Oliveira (2005) and Guennou et al (2012) remove all the galaxy contribution via a wavelet technique. Different ICL detection methods can suffer from different systematics or bias thus providing discordant ICL fractions as shown for simulations (Cui et al 2014).…”

Section: Introductionmentioning

confidence: 99%

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Intracluster light properties in the CLASH-VLT cluster MACS J1206.2-0847

Presotto

Girardi

Nonino

et al. 2014

A&A

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Aims. We aim constrain the assembly history of clusters by studying the intracluster light (ICL) properties, estimating its contribution to the fraction of baryons in stars, f * , and understanding possible systematics or bias using different ICL detection techniques. Methods. We developed an automated method, GALtoICL, based on the software GALAPAGOS, to obtain a refined version of typical BCG+ICL maps. We applied this method to our test case MACS J1206.2-0847, a massive cluster located at z ∼ 0.44, which is part of the CLASH sample. Using deep multiband Subaru images, we extracted the surface brightness (SB) profile of the BCG+ICL and studied the ICL morphology, color, and contribution to f * out to R 500 . We repeated the same analysis using a different definition of the ICL, SBlimit method, i.e., a SB cut-off level, to compare the results. Results. The most peculiar feature of the ICL in MACS1206 is its asymmetric radial distribution, with an excess in the SE direction and extending toward the second brightest cluster galaxy, which is a post starburst galaxy. This suggests an interaction between the BCG and this galaxy that dates back to τ ≤ 1.5 Gyr. The BCG+ICL stellar content is ∼8% of M * , 500 , and the (de-) projected baryon fraction in stars is f * = 0.0177(0.0116), in excellent agreement with recent results. The SBlimit method provides systematically higher ICL fractions and this effect is stronger at lower SB limits. This is due to the light from the outer envelopes of member galaxies that contaminate the ICL. Though more time consuming, the GALtoICL method provides safer ICL detections that are almost free of this contamination. This is one of the few ICL study at redshift z > 0.3. At completion, the CLASH/VLT program will allow us to extend this analysis to a statistically significant cluster sample spanning a wide redshift range: 0.2 z 0.6.

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“…The amount of pre-processing will depend on the characteristics of the infalling group, such as density and dynamical evolution stage (Da Rocha & Mendes de Oliveira 2005;Da Rocha et al 2005, 2008. Guennou et al (2012) used deep HST ACS data to detect diffuse light for ten clusters between z = 0.4 and 0.8 and did not detect any significant variation in the cluster diffuse light content with redshift.…”

Section: ) Is In Good Agreementmentioning

confidence: 99%

Diffuse light in the young cluster of galaxies CL J1449+0856 atz= 2.07

Adami

Durret

Guennou

et al. 2013

A&A

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Context. Cluster properties do not seem to be changing significantly during their mature evolution phase; for example, they do not seem to show any strong dynamical evolution at least up to z ∼ 0.5, their galaxy red sequence is already in place at least up to z ∼ 1.2, and their diffuse light content remains stable up to z ∼ 0.8. The question is now to know if cluster properties can evolve more significantly at redshifts that are notably higher than 1. Aims. We propose here to see how the properties of the intracluster light (ICL) evolve with redshift by detecting and analysing the ICL in the X-ray cluster CL J1449+0856 at z = 2.07, based on deep HST NICMOS H band exposures. Methods. We used the same wavelet-based method as one applied to 10 clusters between z = 0.4 and 0.8. Results. We detect three diffuse light sources with total magnitudes of H = 24.8, 25.5, and 25.9, plus a more compact object with a magnitude H = 25.3. We discuss the significance of our detections and show that they are robust. Conclusions. The three sources of diffuse light indicate an elongation along a north-east south-west axis, similar to that of the distribution of the central galaxies and to the X-ray elongation. This strongly suggests a history of merging events in this direction. While we found a roughly constant amount of diffuse light for clusters between z ∼ 0 and 0.8, we prove at least a 1.5 mag increase between z ∼ 0.8 and 2. If we assume that the amount of diffuse light is directly linked to the infall activity on the cluster, this implies that CL J1449+0856 is still undergoing strong merging events.

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Intragroup diffuse light in compact groups of galaxies: HCG 79, 88 and 95

Cited by 88 publications

References 72 publications

Ultra-diffuse galaxies outside clusters: clues to their formation and evolution

Ultra-diffuse galaxies outside clusters: clues to their formation and evolution

Intracluster light properties in the CLASH-VLT cluster MACS J1206.2-0847

Diffuse light in the young cluster of galaxies CL J1449+0856 atz= 2.07

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