The Fornax Deep Survey with VST

Spavone, M.; Iodice, E.; Ven, Glenn van de; Falcón-Barroso, J.; Raj, M. A.; Hilker, M.; Peletier, Reynier F.; Capaccioli, M.; Mieske, S.; Venhola, Aku; Napolitano, N. R.; Cantiello, M.; Paolillo, M.; Schipani, P.

doi:10.1051/0004-6361/202038015

Cited by 68 publications

(105 citation statements)

References 92 publications

(182 reference statements)

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“…There is no general agreement of a possible dependence of f ICL on cluster mass among different studies, both observational and theoretical ( [4,10,14,16,17,24,31,33,49,53,54,60,78,96,97,109,110,[128][129][130][131] just to quote some theoretical and the most recent observational studies). Some theoretical works (e.g., [49,55,130,132]) find an increasing f ICL with cluster mass, others (e.g., [4,18,20]) no relation, and others (e.g., [14]) a slight decreasing f ICL with increasing cluster mass.…”

Section: Icl Fractionmentioning

confidence: 99%

“…By looking at these two properties, it is possible to discern which, among the above quoted mechanisms, is the main responsible mechanism for the formation of the ICL. In the last few years, many authors focused on the age, color and metallicity gradients of BCG + ICL systems [10,16,23,59,62,63,[70][71][72][73][74][75][76][77][78][79][80] and in particular on their shape. It is reasonable to argue that, if mergers are the main responsible mechanisms, we would expect a flat gradient, i.e., no gradient, simply because mergers would tend to mix up the two components (see discussion in [6,77]).…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Icl Fractionmentioning

confidence: 99%

Section: Introductionmentioning

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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“…C.1. We also briefly describe the 1D multicomponent fitting method we adopt, published by Spavone et al (2017Spavone et al ( , 2020. This is done to determine the starting point of the disc regions for the break-radius algorithm (described in Sect.…”

Section: Appendix A: Bright Ltgs In the Fornax A Subgroupmentioning

confidence: 99%

The Fornax Deep Survey with VST

Raj

Iodice

Napolitano

et al. 2020

A&A

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Context. We present the study of the south-west group in the Fornax cluster centred on the brightest group galaxy (BGG) Fornax A, which was observed as part of the Fornax Deep Survey (FDS). This includes the analysis of the bright group members (mB < 16 mag) and the intra-group light (IGL). Aims. The main objective of this work is to investigate the assembly history of the Fornax A group and to compare its physical quantities as a function of the environment to that of the Fornax cluster core. Methods. For all galaxies, we extracted the azimuthally averaged surface brightness profiles in three optical bands (g, r, i) by modelling the galaxy’s isophotes. We derived their colour (g − i) profiles, total magnitude, effective radius in all respective bands, stellar mass, and the break radius in the r-band. The long integration time and large covered area of the FDS allowed us to also estimate the amount of IGL. Results. The majority of galaxies in the Fornax A group are late-type galaxies (LTGs), spanning a range of stellar mass of 8 < log(M* M⊙) < 10.5. Six out of nine LTGs show a Type III (up-bending) break in their light profiles, which is either suggestive of strangulation halting star formation in their outskirts or their H I-richness causing enhanced star formation in their outer-discs. Overall, we do not find any correlations between their physical properties and their group-centric distance. The estimated luminosity of the IGL is 6 ± 2 × 1010 L⊙ in the g-band, which corresponds to about 16% of the total light in the group. Conclusions. The Fornax A group appears to be in an early-stage of assembly with respect to the cluster core. The environment of the Fornax A group is not as dense as that of the cluster core, with all galaxies except the BGG showing similar morphology, comparable colours and stellar masses, and Type III disc-breaks, without any clear trend in these properties with group-centric distances. The low amount of IGL is also consistent with this picture, since there were no significant gravitational interactions between galaxies that modified the galaxies’ structure and contributed to the build-up of the IGL. The main contribution to the IGL is from the minor merging in the outskirts of the BGG NGC 1316 and, probably, the disrupted dwarf galaxies close to the group centre.

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“…The FDS provides two photometric galaxy catalogs of dwarfs and separate measurements for the giant galaxies , Spavone et al 2020, Raj et al 2019, and Raj et al 2020. The FDSDC, which contains all the dwarf galaxies with semimajor axis a > 2 arcsec in the whole FDS, was generated by V18.…”

Section: The Fornax Deep Survey Datamentioning

confidence: 99%

The Fornax Deep Survey (FDS) with VST XII: Low surface brightness dwarf galaxies in the Fornax cluster

Venhola¹,

Peletier²,

Salo³

et al. 2021

Preprint

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Context. Low surface brightness (LSB) dwarf galaxies in galaxy clusters are an interesting group of objects as their contribution to the galaxy luminosity function and their evolutionary paths are not yet clear. Increasing the completeness of our galaxy catalogs is crucial for understanding these galaxies, which have effective surface brightnesses below 23 mag arcsec −2 (in optical). Progress is continuously being made via the performance of deep observations, but detection depth and the quantification of the completeness can also be improved via the application of novel approaches in object detection. For example, the Fornax Deep Survey (FDS) has revealed many faint galaxies that can be visually detected from the images down to a surface brightness level of 27 mag arcsec −2 , whereas traditional detection methods, such as using Source Extractor (SE), fail to find them. Aims. In this work we use a max-tree based object detection algorithm (Max-Tree Objects, MTO) on the FDS data in order to detect previously undetected LSB galaxies. After extending the existing Fornax dwarf galaxy catalogs with this sample, our goal is to understand the evolution of LSB dwarfs in the cluster. We also study the contribution of the newly detected galaxies to the faint end of the luminosity function. Methods. We test the detection completeness and parameter extraction accuracy of MTO using simulated and real images. We then apply MTO to the FDS images to identify LSB candidates. The identified objects are fitted with 2D Sérsic models using GALFIT and classified as imaging artifacts, likely cluster members, or background galaxies based on their morphological appearance, colors, and structure.Results. With MTO, we are able to increase the completeness of our earlier FDS dwarf catalog (FDSDC) 0.5-1 mag deeper in terms of total magnitude and surface brightness. Due to the increased accuracy in measuring sizes of the detected objects, we also add many small galaxies to the catalog that were previously excluded as their outer parts had been missed in detection. We detect 265 new LSB dwarf galaxies in the Fornax cluster, which increases the total number of known dwarfs in Fornax to 821. Using the whole cluster dwarf galaxy population, we show that the luminosity function has a faint-end slope of α=-1.38±0.02. We compare the obtained luminosity function with different environments studied earlier using deep data but do not find any significant differences. On the other hand, the Fornax-like simulated clusters in the IllustrisTNG cosmological simulation have shallower slopes than found in the observational data. We also find several trends in the galaxy colors, structure, and morphology that support the idea that the number of LSB galaxies is higher in the cluster center due to tidal forces and the age dimming of the stellar populations. The same result also holds for the subgroup of large LSB galaxies, so-called ultra-diffuse galaxies.

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The Fornax Deep Survey with VST

Cited by 68 publications

References 92 publications

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

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

The Fornax Deep Survey with VST

The Fornax Deep Survey (FDS) with VST XII: Low surface brightness dwarf galaxies in the Fornax cluster

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