Florian Sarron
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View article: Euclid preparation. Establishing the quality of the 2D reconstruction of the filaments of the cosmic web with DisPerSE using Euclid photometric redshifts
Euclid preparation. Establishing the quality of the 2D reconstruction of the filaments of the cosmic web with DisPerSE using Euclid photometric redshifts Open
Cosmic filaments are prominent structures of the matter distribution of the Universe. Modern detection algorithms are an efficient way to identify filaments in large-scale observational surveys of galaxies. Many of these methods were origi…
View article: Euclid Quick Data Release (Q1). Galaxy shapes and alignments in the cosmic web
Euclid Quick Data Release (Q1). Galaxy shapes and alignments in the cosmic web Open
Galaxy morphologies and shape orientations are expected to correlate with their large-scale environments, since they grow by accreting matter from the cosmic web and are subject to interactions with other galaxies. We extracted cosmic fila…
View article: Distinct origins of environmentally quenched galaxies in the core and outer virialized regions of massive clusters at 0.8 &lt; <i>z</i> &lt; 1.5
Distinct origins of environmentally quenched galaxies in the core and outer virialized regions of massive clusters at 0.8 < <i>z</i> < 1.5 Open
High-redshift ($z\sim 1$) galaxy clusters are the domain where environmental quenching mechanisms are expected to emerge as important factors in the evolution of the quiescent galaxy population. Uncovering these initially subtle effects re…
View article: Distinct origins of environmentally quenched galaxies in the core and outer virialised regions of massive clusters at $0.8
Distinct origins of environmentally quenched galaxies in the core and outer virialised regions of massive clusters at $0.8 Open
High-redshift ($z\sim1$) galaxy clusters are the domain where environmental quenching mechanisms are expected to emerge as important factors in the evolution of the quiescent galaxy population. Uncovering these initially subtle effects req…
View article: EPOCHS paper – X. Environmental effects on Galaxy formation and protocluster Galaxy candidates at 4.5 &lt; <i>z</i> &lt; 10 from JWST observations
EPOCHS paper – X. Environmental effects on Galaxy formation and protocluster Galaxy candidates at 4.5 < <i>z</i> < 10 from JWST observations Open
In this paper, we describe our search for galaxy protocluster candidates at $4.5{4.5$ galaxy candidates within an area of 185.4 arcmin$^2$. We determine nearest neighbour statistics and galaxy environments. We find that high-z galaxies in …
View article: Euclid Quick Data Release (Q1). The Euclid view on Planck galaxy protocluster candidates: towards a probe of the highest sites of star formation at cosmic noon
Euclid Quick Data Release (Q1). The Euclid view on Planck galaxy protocluster candidates: towards a probe of the highest sites of star formation at cosmic noon Open
We search for galaxy protoclusters at redshifts $z > 1.5$ in the first data release (Q1) of the $\textit{Euclid}$ survey. We make use of the catalogues delivered by the $\textit{Euclid}$ Science Ground Segment (SGS). After a galaxy selecti…
View article: Euclid Quick Data Release (Q1). The role of cosmic connectivity in shaping galaxy clusters
Euclid Quick Data Release (Q1). The role of cosmic connectivity in shaping galaxy clusters Open
The matter distribution around galaxy clusters is distributed over several filaments, reflecting their positions as nodes in the large-scale cosmic web. The number of filaments connected to a cluster, namely its connectivity, is expected t…
View article: EPOCHS Paper X: Environmental effects on Galaxy Formation and Protocluster Galaxy candidates at $4.5
EPOCHS Paper X: Environmental effects on Galaxy Formation and Protocluster Galaxy candidates at $4.5 Open
In this paper we describe our search for galaxy protocluster candidates at $4.54.5$ candidates within an area of 185.4 arcmin$^2$. We determine nearest neighbour statistics and galaxy environments. We find that high-$z$ galaxies in overden…
When the well runs dry: modelling environmental quenching of high-mass satellites in massive clusters at <i>z</i> ≳ 1 Open
We explore models of massive (>1010 M⊙) satellite quenching in massive clusters at z ≳ 1 using an MCMC framework, focusing on two primary parameters: Rquench (the host-centric radius at which quenching begins) and τquench (the time-scale u…
When the Well Runs Dry: Modeling Environmental Quenching of High-mass Satellites in Massive Clusters at \boldmath$z \gtrsim 1$ Open
We explore models of massive ($\gt 10^{10}~{\rm M}_{\odot}$) satellite quenching in massive clusters at $z\gtrsim1$ using an MCMC framework, focusing on two primary parameters: $R_{\rm quench}$ (the host-centric radius at which quenching b…
Mechano-biochemical marine stimulation of inversion, gastrulation, and endomesoderm specification in multicellular Eukaryota Open
The evolutionary emergence of the primitive gut in Metazoa is one of the decisive events that conditioned the major evolutionary transition, leading to the origin of animal development. It is thought to have been induced by the specificati…
GOGREEN: A critical assessment of environmental trends in cosmological hydrodynamical simulations at <i>z</i> ≈ 1 Open
Recent observations have shown that the environmental quenching of galaxies at z ∼ 1 is qualitatively different to that in the local Universe. However, the physical origin of these differences has not yet been elucidated. In addition, whil…
GOGREEN: a critical assessment of environmental trends in cosmological hydrodynamical simulations at z ~ 1 Open
Recent observations have shown that the environmental quenching of galaxies at z ~ 1 is qualitatively different to that in the local Universe. However, the physical origin of these differences has not yet been elucidated. In addition, whil…
The GOGREEN survey: constraining the satellite quenching time-scale in massive clusters at <i>z</i> ≳ 1 Open
We model satellite quenching at z ∼ 1 by combining 14 massive (1013.8 1010 M⊙), we find that the satellite quenching time-scale decreases with increasing satellite stellar mass from ∼1.6 Gyr at 1010 M⊙ to ∼0.6−1 Gyr at 1011 M⊙ and is rough…
The GOGREEN Survey: Constraining the Satellite Quenching Timescale in Massive Clusters at $\boldsymbol{z} \gtrsim 1$ Open
We model satellite quenching at $z \sim 1$ by combining $14$ massive ($10^{13.8} 10^{10}~\mathrm{M}_{\odot}$), we find that the satellite quenching timescale decreases with increasing satellite stellar mass from $\sim1.6~{\rm Gyr}$ at $10^…
DETECTIFz galaxy groups in the REFINE survey – I. Group detection and quenched fraction evolution at <i>z</i> < 2.5 Open
We use a large K-selected sample of 299 961 galaxies from the REFINE survey, consisting of a combination of data from three of the deepest near-infrared surveys, UKIDSS UDS, COSMOS/UltraVISTA, and CFHTLS-D1/VIDEO, that were homogeneously r…
Galaxy groups up to z=2.5 in deep near-infrared surveys : detection and quenched fractions Open
Obtaining large samples of galaxy groups and (proto-)cluster cores at redshift z > 1.5 is crucial to better understand cluster formation and the role environment plays in shaping galaxy properties. While dozens of these structures have now…
Evolutionary Emergence of First Animal Organisms Triggered by Environmental Mechano-Biochemical Marine Stimulation Open
The evolutionary emergence of the first animals is thought to have been intimately associated to the formation of a primitive endomesodermal gut ( i.e gastrulation) from ancestral multi-cellular spheres, blastulae, more than 700 million ye…
Candidate fossil groups in the CFHTLS: a probabilistic approach Open
\nContext. Fossil groups (FGs) have been discovered 25 years ago, and are now defined as galaxy groups with an X-ray luminosity higher than $ 10^{42}\\,h_{50}^{-2} $ erg s−1 and a brightest group galaxy brighter than the other group member…
Mapping and characterization of cosmic filaments in galaxy cluster outskirts: strategies and forecasts for observations from simulations Open
Upcoming wide-field surveys are well suited to studying the growth of galaxy clusters by tracing galaxy and gas accretion along cosmic filaments. We use hydrodynamic simulations of volumes surrounding 324 clusters from The ThreeHundred pro…
Group connectivity in COSMOS: a tracer of mass assembly history Open
Cosmic filaments are the channel through which galaxy groups assemble their mass. Cosmic connectivity, namely the number of filaments connected to a given group, is therefore expected to be an important ingredient in shaping group properti…
View article: Euclid preparation. III. Galaxy cluster detection in the wide photometric survey, performance and algorithm selection
Euclid preparation. III. Galaxy cluster detection in the wide photometric survey, performance and algorithm selection Open
Galaxy cluster counts in bins of mass and redshift have been shown to be a competitive probe to test cosmological models. This method requires an efficient blind detection of clusters from surveys with a well-known selection function and r…
Evolution of the cluster optical galaxy luminosity function in the CFHTLS: breaking the degeneracy between mass and redshift Open
Obtaining large samples of galaxy clusters is important for cosmology: cluster counts as a function of redshift and mass can constrain the parameters of our Universe. They are also useful in order to understand the formation and evolution …
Evolution Of The Cluster Optical Galaxy Luminosity Function In The Cfhtls Open
Poster presented at the conference Galaxy evolution Across Time, 12-16 June, Paris, France There is some disagreement in the literature concerning the evolution with redshift of the galaxy luminosity function (GLF) in galaxy clusters. Inde…
Weak lensing study of 16 DAFT/FADA clusters: Substructures and filaments Open
\n While our current cosmological model places galaxy clusters at the nodes of a filament network (the cosmic web), we still struggle to detect these filaments at high redshifts. We perform a weak lensing study for a sample of 16 massive, …