In Auriga Superstars simulations, old stellar morphological lopsidedness correlates strongly with HI lopsidedness at z=0, with tidal interactions inducing coherent asymmetries in both while smooth accretion primarily affects gas and young stars.
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Deep g,r,i photometry of IC 5332 shows redder color gradients in the outskirts and faint stellar streams, supporting ongoing stellar mass assembly via accretion.
At z=0.9, disk galaxies show a TFR slope of 3.82 and FR slope of 0.44 with moderate TFR and strong FR evolution from z=0, implying higher and less mass-dependent stellar-to-halo mass fractions f_M while f_j remains near 0.8.
citing papers explorer
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Coupling between stellar and HI lopsidedness in Milky Way-type galaxies from the Auriga Superstars cosmological simulations
In Auriga Superstars simulations, old stellar morphological lopsidedness correlates strongly with HI lopsidedness at z=0, with tidal interactions inducing coherent asymmetries in both while smooth accretion primarily affects gas and young stars.
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VST-SMASH: VST Survey of Mass Assembly and Structural Hierarchy I. Survey presentation and deep photometry of IC 5332: tracing the mass assembly in the challenging faintest-end regime
Deep g,r,i photometry of IC 5332 shows redder color gradients in the outskirts and faint stellar streams, supporting ongoing stellar mass assembly via accretion.
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Kinematic scaling relations of disc galaxies from ionised gas at $z\sim1$ and their connection with dark matter haloes
At z=0.9, disk galaxies show a TFR slope of 3.82 and FR slope of 0.44 with moderate TFR and strong FR evolution from z=0, implying higher and less mass-dependent stellar-to-halo mass fractions f_M while f_j remains near 0.8.