Characterization of Omega-WINGS galaxy clusters

Chiosi

Sciarratta

et al. 2020

A&A

Self Cite

Context. This is the second work dedicated to the observed parallelism between galaxy clusters (GCs) and early-type galaxies (ETGs). The focus is on the distribution of these systems in the scaling relations (SRs) observed when effective radii, effective surface brightness, total luminosities, and velocity dispersions are mutually correlated. Aims. Using the data of the Illustris simulation we speculate on the origin of the observed SRs. Methods. We compare the observational SRs extracted from the database of the WIde-field Nearby Galaxy-cluster Survey with the relevant parameters coming from the Illustris simulations. Then we use the simulated data at different redshift to infer the evolution of the SRs. Results. The comparison demonstrate that GCs at z ∼ 0 follow the same log(L)−log(σ) relation of ETGs and that both in the log(⟨I⟩e)−log(Re) and log(Re)−log(M*) planes the distribution of GCs is along the sequence defined by the brightest and massive early-type galaxies (BCGs). The Illustris simulation reproduces the tails of the massive galaxies visible both in the log(⟨I⟩e)−log(Re) and log(Re)−log(M*) planes, but fails to give the correct estimate of the effective radii of the dwarf galaxies that appear too large and those of GCs that are too small. The evolution of the SRs up to z = 4 permits to reveal the complex evolutionary paths of galaxies in the SRs and indicate that the line marking the zone of exclusion, visible in the log(⟨I⟩e)−log(Re) and the log(Re)−log(M*) planes, is the trend followed by virialized and passively evolving systems. Conclusions. We speculate that the observed SRs originate from the intersection of the virial theorem and a relation L = L0′σβ where the luminosities depend on the star formation history.

Section: Samplementioning

confidence: 99%

“…The corresponding parameters for the galaxy clusters are those measured by Biviano et al (2017) and Cariddi et al (2018).…”

Section: Samplementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The parallelism between galaxy clusters and early-type galaxies

Chiosi

Sciarratta

et al. 2020

A&A

Self Cite

“…The color-magnitude diagram (CMD) is one of the main diagnostic tools used to understand the physical properties of stars and galaxies, and, in recent years, also of clusters of galaxies (Cariddi et al 2018). Color-magnitude diagrams have allowed researchers to infer the past history of galaxies and clusters and have been considered to be key cosmological probes for a long time now (Tully et al 1982;Bower et al 1992).…”

Section: The U-v Color Of Cluster Galaxiesmentioning

confidence: 99%

The second u-band extension of the WINGS cluster survey

Grado

Bettoni

et al. 2020

A&A

Self Cite

Context. This is the second u-band extension of the WIde-field Nearby Galaxy-cluster Survey (WINGS) whereby 39 clusters were imaged with the ESO-VLT survey telescope. This follows the first part of the survey which was performed with several telescopes of the northern hemisphere in the U Cousin–Bessel filter band covering 17 clusters. Aims. The u-band data, in combination with those already collected by the WINGS survey, permit a detailed multi-wavelength investigation of the properties of the member galaxies from the cluster center out to the periphery. Methods. We used SExtractor to derive the main properties of the galaxies in the observed fields and measure the u − V colors on circular apertures of increasing radius. The photometric accuracy of the magnitudes was calibrated with the standard stars and was tested by means of comparisons with the u-band data of the Sloan Digital Sky Survey (SDSS). Results. We present the catalogs of the photometric analysis performed by SExtractor. We also provide a brief analysis of the u − V versus V color–magnitude diagram of our clusters, the plots of the color as a function of the cluster-centric distance (for cluster members only), the mass–color relation and the correlation of the current star formation rate (SFR) with the absolute V and u magnitudes for the galaxies in the observed fields.

“…8 shows the distribution of our systems in the log(R e ) − log(n) plane. The values of n used here are those derived by D' Onofrio et al (2014) with GASPHOT for the singles ETGs and those of Cariddi et al (2018) for clusters. Note the solid line which represents the best fit of the whole distribution of ETGs (BCGs+II-BCGs+random ETGs).…”

Section: Non Homologymentioning

confidence: 99%

The Parallelism between Galaxy Clusters and Early-type Galaxies. I. The Light and Mass Profiles

Sciarratta

Cariddi

et al. 2019

ApJ

Self Cite

We have analyzed the parallelism between the properties of galaxy clusters and early-type galaxies (ETGs) by looking at the similarity between their light profiles. We find that the equivalent luminosity profiles of all these systems in the V band, once normalized to the effective radius R e and shifted in surface brightness, can be fitted by the Sérsic's law r 1/n and superposed with a small scatter (≤ 0.3 mag). By grouping objects in different classes of luminosity, the average profile of each class slightly deviates from the other only in the inner and outer regions (outside 0.1 ≤ r/R e ≤ 3), but the range of values of n remains ample for the members of each class, indicating that objects with similar luminosity have quite different shapes.The "Illustris" simulation reproduces quite well the luminosity profiles of ETGs, with the exception of in the inner and outer regions where feedback from supernovae and active galactic nuclei, wet and dry mergers, are at work. The total mass and luminosity of galaxy clusters as well as their light profiles are not well reproduced.By exploiting simulations we have followed the variation of the effective half-light and half-mass radius of ETGs up to z = 0.8, noting that progenitors are not necessarily smaller in size than current objects. We have also analyzed the projected dark+baryonic and dark-only mass profiles discovering that after a normalization to the half-mass radius, they can be well superposed and fitted by the Sérsic's law.