Euclid preparation. The shape of halo profiles in ΛCDM and non-standard cosmologies

@misc{pizzuti2026euclid,
  title = {{Euclid preparation. The shape of halo profiles in $Λ$CDM and non-standard cosmologies}},
  author = {L Pizzuti and G.Y Ferron and A Ragagnin and A.M.C Le Brun and P.-S Corasaniti and T Gayoux and G Rácz and E Altamura and Z Sakr and C Carbone and M Baldi and C Giocoli and T Castro and F Pace and J.E Taylor and S Borgani and O Luongo and C.T Mpetha and R.E Angulo and B Altieri and S Andreon and N Auricchio and C Baccigalupi and S Bardelli and P Battaglia and A Biviano and E Branchini and M Brescia and S Camera and V Capobianco and V.F Cardone and J Carretero and M Castellano and G Castignani and S Cavuoti and K.C Chambers and A Cimatti and C Colodro-Conde and G Congedo and L Conversi and Y Copin and F Courbin and H.M Courtois and M Cropper and H Degaudenzi and G de Lucia and H Dole and F Dubath and X Dupac and S Dusini and S Escoffier and M Farina and F Faustini and S Ferriol and F Finelli and P Fosalba and S Fotopoulou and M Frailis and E Franceschi and M Fumana},
  howpublished = {HAL},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.04192},
  eprint = {2609.04192},
  archivePrefix = {arXiv},
  url = {https://hal.science/hal-05759213v1},
  note = {CC BY 4.0},
}

TY  - UNPB
TI  - Euclid preparation. The shape of halo profiles in ΛCDM and non-standard cosmologies
AU  - L Pizzuti
AU  - G.Y Ferron
AU  - A Ragagnin
AU  - A.M.C Le Brun
AU  - P.-S Corasaniti
AU  - T Gayoux
AU  - G Rácz
AU  - E Altamura
AU  - Z Sakr
AU  - C Carbone
AU  - M Baldi
AU  - C Giocoli
AU  - T Castro
AU  - F Pace
AU  - J.E Taylor
AU  - S Borgani
AU  - O Luongo
AU  - C.T Mpetha
AU  - R.E Angulo
AU  - B Altieri
AU  - S Andreon
AU  - N Auricchio
AU  - C Baccigalupi
AU  - S Bardelli
AU  - P Battaglia
AU  - A Biviano
AU  - E Branchini
AU  - M Brescia
AU  - S Camera
AU  - V Capobianco
AU  - V.F Cardone
AU  - J Carretero
AU  - M Castellano
AU  - G Castignani
AU  - S Cavuoti
AU  - K.C Chambers
AU  - A Cimatti
AU  - C Colodro-Conde
AU  - G Congedo
AU  - L Conversi
AU  - Y Copin
AU  - F Courbin
AU  - H.M Courtois
AU  - M Cropper
AU  - H Degaudenzi
AU  - G de Lucia
AU  - H Dole
AU  - F Dubath
AU  - X Dupac
AU  - S Dusini
AU  - S Escoffier
AU  - M Farina
AU  - F Faustini
AU  - S Ferriol
AU  - F Finelli
AU  - P Fosalba
AU  - S Fotopoulou
AU  - M Frailis
AU  - E Franceschi
AU  - M Fumana
PY  - 2026
DA  - 2026/09/03
PB  - HAL
DO  - 10.48550/arxiv.2609.04192
UR  - https://hal.science/hal-05759213v1
AB  - We study the shape of three-dimensional and projected dark-matter halo profiles extracted from cosmological N-body simulations in ΛCDM and non-standard cosmologies, using the \texttt{DUSTGRAIN-PF} and \texttt{DEMNUni} suites. The models considered include massive neutrinos, f(ℛ) gravity, and dynamical dark energy. By comparing density, mass, velocity-dispersion, and excess-surface-density profiles up to 5 r_500c, we quantify the differential imprint of non-standard physics on halo structure in view of \textit{Euclid} cluster WL studies. Our main analysis is performed at z=1.1, a high-redshift regime where the weak-lensing signal-to-noise starts to degrade, providing a conservative stress test for detectability; for \texttt{DUSTGRAIN-PF} we additionally analyse z=0.5 and z=0.3 snapshots. In low-mass haloes (M_200c<7×10^13 M_⊙), f(ℛ) gravity produces deviations of order 10 % in projected and three-dimensional profiles, especially in the outskirts where screening is less efficient. Massive neutrinos partially reduce this signal, reflecting the competition between free streaming and fifth-force-enhanced growth. Dynamical dark energy and massive-neutrino cosmologies generally induce smaller, few-percent deviations, with the largest effects again found in low-mass haloes and at large radii. Under simplified assumptions for \Euclid WL, detecting such profile differences at z=1.1 requires stacks of ∼10^5 haloes, while a few thousands haloes may be sufficient at z≲0.5. This further calls for the need of integrating such precise modelling of non-standard effects -- along with other observational effects -- in any likelihood involving \textit{Euclid} WL masses to avoid non-negligible systematic biases. Concentration--mass relations show weaker cosmology dependence, typically at the ∼5 % level. [...]
ER  -