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We investigate the dependence of Lyα emitter (LAE) clustering on Lyα luminosity and connect the clustering properties of ≈L⋆ LAEs with those of much fainter ones, namely, ≈0.04L⋆. We use 1030 LAEs from the MUSE-Wide survey, 679 LAEs from MUSE-Deep, and 367 LAEs from the to-date deepest ever spectroscopic survey, the MUSE Extremely Deep Field. All objects have spectroscopic redshifts of 3 < z < 6 and cover a large dynamic range of Lyα luminosities: 40.15 < log(LLyα/erg s−1) < 43.35. We apply the Adelberger et al. K-estimator as the clustering statistic and fit the measurements with state-of-the-art halo occupation distribution (HOD) models. We find that the large-scale bias factor increases weakly with an increasing line luminosity. For the low-luminosity (log⟨LLyα/[erg s−1]⟩ = 41.22) and intermediate-luminosity (log⟨LLyα/[erg s−1]⟩ = 41.64) LAEs, we compute consistent bias factors blow = 2.43−0.15+0.15 b low = 2. 43 − 0.15 + 0.15 $ b_\mathrm{{low}}=2.43^{+0.15}_{-0.15} $ and binterm. = 2.42−0.09+0.10 b interm. = 2. 42 − 0.09 + 0.10 $ b_\mathrm{{interm.}}=2.42^{+0.10}_{-0.09} $ , whereas for the high-luminosity (log⟨LLyα/[erg s−1]⟩ = 42.34) LAEs we calculated bhigh = 2.65−0.11+0.13 b high = 2. 65 − 0.11 + 0.13 $ b_\mathrm{{high}}=2.65^{+0.13}_{-0.11} $. Consequently, high-luminosity LAEs occupy dark matter halos (DMHs) with typical masses of log(Mh/[h−1 M⊙]) = 11.09−0.09+0.10 log (M h / [ h − 1 M ⊙ ]) = 11. 09 − 0.09 + 0.10 $ \log (M_{\mathrm{h}}/[h^{-1}M_\odot])=11.09^{+0.10}_{-0.09} $ , while low-luminosity LAEs reside in halos of log(Mh/[h−1 M⊙]) = 10.77−0.15+0.13 log (M h / [ h − 1 M ⊙ ]) = 10. 77 − 0.15 + 0.13 $ \log (M_{\mathrm{h}}/[h^{-1}M_\odot])=10.77^{+0.13}_{-0.15} $. The minimum masses to host one central LAE, Mmin, and (on average) one satellite LAE, M1, also vary with Lyα luminosity, growing from log(Mmin/[h−1M⊙]) = 10.3−0.3+0.2 log (M min / [ h − 1 M ⊙ ]) = 10. 3 − 0.3 + 0.2 $ \log (M_\mathrm{{min}}/[h^{-1}M_\odot])=10.3^{+0.2}_{-0.3} $ and log(M1/[h−1 M⊙]) = 11.7−0.2+0.3 log (M 1 / [ h − 1 M ⊙ ]) = 11. 7 − 0.2 + 0.3 $ \log (M_1/[h^{-1}M_\odot])=11.7^{+0.3}_{-0.2} $ to log(Mmin/[h−1 M⊙]) = 10.7−0.3+0.2 log (M min / [ h − 1 M ⊙ ]) = 10. 7 − 0.3 + 0.2 $ \log (M_\mathrm{{min}}/[h^{-1}M_\odot])=10.7^{+0.2}_{-0.3} $ and log(M1/[h−1 M⊙]) = 12.4−0.6+0.4 log (M 1 / [ h − 1 M ⊙ ]) = 12. 4 − 0.6 + 0.4 $ \log (M_1/[h^{-1}M_\odot])=12.4^{+0.4}_{-0.6} $ from low- to high-luminosity samples, respectively. The satellite fractions are ≲10% (≲20%) at 1σ (3σ) confidence level, supporting a scenario in which DMHs typically host one single LAE. We next bisected the three main samples into disjoint subsets to thoroughly explore the dependence of the clustering properties on LLyα. We report a strong (8σ) clustering dependence on Lyα luminosity, not accounting for cosmic variance effects, where the highest luminosity LAE subsample (log(LLyα/erg s−1) ≈ 42.53) clusters more strongly (bhighest = 3.13−0.15+0.08 b highest = 3. 13 − 0.15 + 0.08 $ b_\mathrm{{highest}}=3.13^{+0.08}_{-0.15} $) and resides in more massive DMHs (log(Mh/[h−1M⊙] )= 11.43−0.10+0.04 log (M h / [ h − 1 M ⊙ ]) = 11. 43 − 0.10 + 0.04 $ \log(M_\mathrm{{h}} / [h^{-1}{M}_{\odot}])=11.43^{+0.04}_{-0.10} $) than the lowest luminosity one (log(LLyα/erg s−1) ≈ 40.97), which presents a bias of blowest = 1.79−0.06+0.08 b lowest = 1. 79 − 0.06 + 0.08 $ b_\mathrm{{lowest}}=1.79^{+0.08}_{-0.06} $ and occupies log(Mh/[h−1M⊙]) = 10.00−0.09+0.12 log (M h / [ h − 1 M ⊙ ]) = 10. 00 − 0.09 + 0.12 $ \log(M_\mathrm{{h}} / [h^{-1}{M}_{\odot}])=10.00^{+0.12}_{-0.09} $ halos. We discuss the implications of these results for evolving Lyα luminosity functions, halo mass dependent Lyα escape fractions, and incomplete reionization signatures. [ABSTRACT FROM AUTHOR]

Sérsic parameters characterizing the density profiles of remnants formed in collisionless disc galaxy mergers are obtained; no bulge is included in our simulations. The Sérsic index range for the luminous matter, , is similar to that found in early-type galaxies, for about the same luminous mass range, while the effective radius tends to be higher, . A strong correlation of n with the central projected surface density I0 is found, , which is consistent with observations. No strong positive linear correlation between the size, Re, and structure, n, of our remnants is found. The derived scaling of the index n with luminous mass, , compares favourably with its observational counterpart, . The dependence of the effective radius with luminous mass for our remnants, , compares well with that determined from early-type galaxies of the Sloan Digital Sky Survey, . The photometric plane scaling found for the luminous component, , assuming a constant stellar mass-to-light ratio, is consistent with that determined for ellipticals in the B band, , and for K-band remnants, . We find that the surface defined by Sérsic parameters in log space is not a true plane, but a pseudo-plane with a small curvature at low values of n owed to intrinsic properties of the Sérsic model. The dark haloes of our remnants have a mean 3D Sérsic index of , that is somewhat smaller than the one obtained for dark haloes in Lambda cold dark matter cosmologies, . Also, a tight dark Sérsic ‘plane’ is found to be defined by the parameters of the remnants haloes with . We conclude that collisionless merger remnants of pure disc galaxies have Sérsic properties and correlations consistent with those of observed in early-type galaxies and local remnants. [ABSTRACT FROM AUTHOR]