Simulations of Euclid Deep Fields show that cosmic web structures can be reconstructed from H-alpha galaxies with biases from redshift distortions and selection effects that can be partially mitigated, allowing recovery of stellar mass gradients toward filaments.
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Euclid Q1 data shows the passive-density and morphology-density relations persist from z=0.25 to z=1, with local density increasing the quenched and early-type fractions at fixed stellar mass for galaxies below 10^10.8 solar masses.
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Euclid preparation. 3D reconstruction of the cosmic web with simulated Euclid Deep spectroscopic samples
Simulations of Euclid Deep Fields show that cosmic web structures can be reconstructed from H-alpha galaxies with biases from redshift distortions and selection effects that can be partially mitigated, allowing recovery of stellar mass gradients toward filaments.
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Euclid Quick Data Release (Q1): The evolution of the passive-density and morphology-density relations between $z=0.25$ and $z=1$
Euclid Q1 data shows the passive-density and morphology-density relations persist from z=0.25 to z=1, with local density increasing the quenched and early-type fractions at fixed stellar mass for galaxies below 10^10.8 solar masses.