activity
20242026
collaborators

66 papers

astro-ph.CO2026

Euclid Quick Data Release (Q1). The role of cosmic connectivity in shaping galaxy clusters

Euclid Collaboration, C. Gouin, C. Laigle +337

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 con…

astro-ph.GA2026

COSMOS-Web galaxy groups: Evolution of red sequence and quiescent galaxy fraction

Greta Toni, Matteo Maturi, Gianluca Castignani +33

We investigate the redshift and group richness dependence of the quiescent fraction and red-sequence (RS) parameters in COSMOS galaxy groups from z=0 to z=3.7. We analyzed the deep…

astro-ph.GA2026

Euclid Quick Data Release (Q1): The evolution of the passive-density and morphology-density relations between and

Euclid Collaboration, C. Cleland, S. Mei +320

The extent to which the environment affects galaxy evolution has been under scrutiny by researchers for decades. With the first data from Euclid, we can begin to systematically stu…

astro-ph.CO2026

Euclid preparation. LXXXIX. Accurate and precise data-driven angular power spectrum covariances

Euclid Collaboration, K. Naidoo, J. Ruiz-Zapatero +280

We develop techniques for generating accurate and precise internal covariances for measurements of clustering and weak-lensing angular power spectra. These methods have been design…

astro-ph.CO2026

Euclid Quick Data Release (Q1). The first Euclid view of Planck galaxy protocluster candidates at cosmic noon

Euclid Collaboration, T. Dusserre, H. Dole +339

[ABRIGED ABSTRACT] A large catalogue of candidate galaxy protoclusters with high star-formation rates was produced by the Planck collaboration. We search, in the first data release…

astro-ph.CO2026

Euclid preparation. The impact of redshift interlopers on the two-point correlation function analysis

Euclid Collaboration, I. Risso, A. Veropalumbo +317

The Euclid survey aims to measure the spectroscopic redshift of emission-line galaxies by identifying the H line in their slitless spectra. This method is sensitive to the si…