The complex case of MACS J0717.5+3745 and its extended filament: intra-cluster light, galaxy luminosity function, and galaxy orientations

Ellien, A.; Durret, F.; Adami, C.; Martinet, N.; Lobo, C.; Jauzac, Mathilde

doi:10.1051/0004-6361/201935673

Cited by 26 publications

(19 citation statements)

References 118 publications

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“…Only one point presents a big difference between the two values (PA red -PA blue > 120 • ). We found that the ICL associated with this BCG is more extended in the reddest filter; Ellien et al (2019), also show that the ICL tends to be more extended in redder filters. The other BCGs with a significant difference between the values measured in the two different filters are circular in shape (b/a > 0.80), so the PAs are ill-defined, which also explains the huge error bars.…”

Section: Bcgs Observed In Too Blue Filterssupporting

confidence: 68%

“…During this verification, we found that our detection differs from that of Durret et al (2019) and Bai et al (2014) for the BCGs in MACS-J0717.5+3745 and SpARCS-J0224, respectively. MACS-J0717.5+3745 presents a very complex structure because is it undergoing multiple mergers (see Limousin et al 2016;Ellien et al 2019, and references therein). Durret et al (2019) define the BCG as the one in the southern structure; instead, we detected a brighter galaxy in the northern structure, which we define as the BCG.…”

Section: Results For Detected Red Bcgsmentioning

confidence: 99%

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Physical properties of brightest cluster galaxies up to redshift 1.80 based on HST data

Chu

Durret

Márquez

2021

A&A

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Context. Brightest cluster galaxies (BCGs) grow by accreting numerous smaller galaxies, and can be used as tracers of cluster formation and evolution in the cosmic web. However, there is still controversy regarding the main epoch of formation of BCGs; some authors believe they already formed before redshift z = 2, while others find that they are still evolving at more recent epochs. Aims. We study the physical properties of a large sample of BCGs covering a wide redshift range up to z = 1.8 and analyzed in a homogeneous way, to see if their characteristics vary with redshift. As a first step we also present a new tool to determine for each cluster which galaxy is the BCG. Methods. For a sample of 137 clusters with HST images in the optical and/or infrared, we analyzed the BCG properties by applying GALFIT with one or two Sérsic components. For each BCG we thus computed the Sérsic index, effective radius, major axis position angle, and surface brightness. We then searched for correlations of these quantities with redshift. Results. We find that the BCGs follow the Kormendy relation (between the effective radius and the mean surface brightness), with a slope that remains constant with redshift, but with a variation with redshift of the ordinate at the origin. Although the trends are faint, we find that the absolute magnitudes and the effective radii tend to become respectively brighter and bigger with decreasing redshift. On the other hand, we find no significant correlation of the mean surface brightnesses or Sérsic indices with redshift. The major axes of the cluster elongations and of the BCGs agree within 30° for 73% of our clusters at redshift z ≤ 0.9. Conclusions. Our results agree with the BCGs being mainly formed before redshift z = 2. The alignment of the major axes of BCGs with their clusters agree with the general idea that BCGs form at the same time as clusters by accreting matter along the filaments of the cosmic web.

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Section: Bcgs Observed In Too Blue Filterssupporting

confidence: 68%

Section: Results For Detected Red Bcgsmentioning

confidence: 99%

Physical properties of brightest cluster galaxies up to redshift 1.80 based on HST data

Chu

Durret

Márquez

2021

A&A

Self Cite

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“…Interestingly enough, Ellien et al (2019) analysed the distribution of intra-cluster light (ICL) in this system and detected a large amount of it in the cluster core but no such light in the cosmic filament. As ICL is thought to be made up of disrupted galactic material, the findings of Ellien et al (2019) corroborate the existence of a harsh environment in the core, contrasting with softer conditions along the filament. This is expected and the distribution of jellyfish galaxy candidates found in this work may reflect that, quite probably, transient phenomena such as A63, page 16 of 38 jellyfish features cannot survive for long in the tumultuous core of MACS0717.…”

Section: Discussionmentioning

confidence: 99%

Jellyfish galaxy candidates in MACS J0717.5+3745 and 39 other clusters of the DAFT/FADA and CLASH surveys

Durret

Chiche

Lobo

et al. 2021

A&A

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Context. Galaxies in clusters undergo several phenomena, such as RPS and tidal interactions, that can trigger or quench their star formation and, in some cases, lead to galaxies acquiring unusual shapes and long tails – some become jellyfish. Aims. We searched for jellyfish galaxy candidates in a sample of 40 clusters from the DAFT/FADA and CLASH surveys covering the redshift range 0.2 < z < 0.9. In MACS J0717.5+3745 (MACS0717), our large spatial coverage and abundant sampling of spectroscopic redshifts allowed us to pursue a detailed analysis of jellyfish galaxy candidates in this cluster and its extended filament. Methods. We retrieved galaxy spectroscopic redshifts in the NASA Extragalactic Database for galaxies in all the clusters of our sample (except for MACS0717 for which we had an extensive catalogue), looked at the Hubble Space Telescope ACS images of these objects (mainly the F606W and F814W bands), and classified them as a function of their likeliness to be jellyfish galaxies. We give catalogues of jellyfish galaxy candidates with positions, redshifts, magnitudes, and projected distance to their respective cluster centre. For MACS0717, an eight-magnitude optical and infrared catalogue covering the entire region allowed us to compute the best stellar population fits with LePhare through the GAZPAR interface. For the 31 jellyfish candidates in the other clusters belonging to the CLASH survey, we extracted up to 17 magnitudes available in the CLASH catalogues to fit their spectral energy distribution in the same way. Results. We found 81 jellyfish galaxy candidates in the extended region around MACS0717 as well as 97 in 22 other clusters. Jellyfish galaxy candidates in MACS0717 tend to avoid the densest regions of the cluster, while this does not appear to be the case in the other clusters. The best fit templates found by LePhare show that star formation is occurring. Stellar masses are in the range 109 − 1011 M⊙, and the star formation rates (SFRs) are in the 10−1 − 60 M⊙ yr−1 range for MACS0717 and in the 10−1 − 10 M⊙ yr−1 range for the other sample. Specific star formation rates (sSFRs) are notably higher in MACS0717, with more than half of the sample having values larger than 10−9 yr−1, while in the other clusters, most galaxies have sSFR < 10−10 yr−1. Stellar populations appear younger in MACS0717 (more than half have an age smaller than 1.5 × 109 yrs), and, following mid-infrared criteria, two galaxies may contain an active galactic nucleus. In a SFR versus stellar mass diagram, jellyfish galaxy candidates appear to have somewhat larger SFRs than “non-jellyfish star-forming” galaxies. For MACS0717, the mean sSFR of the 79 jellyfish galaxy candidates is 3.2 times larger than that of star-forming non-jellyfish galaxies (selected with log(sSFR) ≥ − 11). Conclusions. Our jellyfish galaxy candidates are star-forming objects, with young ages and blue colours. Based on several arguments, the jellyfish candidates identified in MACS0717 seem to have fallen rather recently into the cluster. A very rough estimate of the proportions of jellyfish galaxies in the studied clusters is about 10%; this number does not seem to vary strongly with the cluster relaxation state, though this result must be confirmed with more data. Our sample of 97 galaxies in 22 clusters represents the basis of future works.

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“…It is worth mentioning another approach for detecting the ICL that has recently been having some success, a method that makes use of multiscale, wavelet-based algorithms. There are several examples of this approach that have been used in recent years (e.g., [105][106][107][108][109]). One of the latest, just to quote an example, is the code called DAWIS ( [109] and references therein).…”

Section: Observational Methodsmentioning

confidence: 99%

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

Contini

2021

Galaxies

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Not all the light in galaxy groups and clusters comes from stars that are bound to galaxies. A significant fraction of it constitutes the so-called intracluster or diffuse light (ICL), a low surface brightness component of groups/clusters generally found in the surroundings of the brightest cluster galaxies and intermediate/massive satellites. In this review, I will describe the mechanisms responsible for its formation and evolution, considering the large contribution given to the topic in the last decades by both the theoretical and observational sides. Starting from the methods that are commonly used to isolate the ICL, I will address the remarkable problem given by its own definition, which still makes the comparisons among different studies not trivial, to conclude by giving an overview of the most recent works that take advantage of the ICL as a luminous tracer of the dark matter distribution in galaxy groups and clusters.

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The complex case of MACS J0717.5+3745 and its extended filament: intra-cluster light, galaxy luminosity function, and galaxy orientations

Cited by 26 publications

References 118 publications

Physical properties of brightest cluster galaxies up to redshift 1.80 based on HST data

Physical properties of brightest cluster galaxies up to redshift 1.80 based on HST data

Jellyfish galaxy candidates in MACS J0717.5+3745 and 39 other clusters of the DAFT/FADA and CLASH surveys

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

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