ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O B-Survey I-Survey I-Survey I-Survey B-Survey B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model I-Model O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: other secondary biases, since it shows that the fact that it increases with mass was an artefact of the mass scales that were being probed. Our results place updated constraints to models addressing the connection between galaxies and haloes. The wide dynamical range that we probe encompasses haloes hosting from emission-line galaxies at the low-mass end to massive quiescent galaxies and clusters at the high-mass end. In the context of the halo-galaxy connection, it has become an observational challenge to prove the existence of galaxy assembly bias , a hypothesis that states that the clustering properties of galaxies, at fixed halo mass, depend on secondary halo properties such as the accretion history (or age) of haloes (see e.g. Lin et al. 2016 ; Miyatake et al. 2016 ; Montero-Dorta et al. 2017 ; Niemiec et al. 2018 ). For luminous red galaxies (LRGs), indications of the existence of galaxy assembly bias have been reported by Montero-Dorta et al. ( 2017 ) and Niemiec et al. ( 2018 ), from a sample extracted from the Baryon Oscillation Spectroscopic Survey (BOSS; Dawson et al. 2013 ). The typical mass of the haloes inhabited by these galaxies is estimated in ∼10 12.7−13 h −1 M ⊙ (Niemiec et al. 2018 ), but a large scatter is expected, so that the most massive LRGs could inhabit haloes above ∼10 14 h −1 M ⊙ . These results are, in principle, compatible with both the halo assembly bias and the concentration bias signal reported in Fig. 4 . Our measurement of halo assembly bias at the high-mass end can be properly connected to the results presented in Montero-Dorta et al. ( 2017 ) and Niemiec et al. ( 2018 ) through the technique of ‘age matching’ (Hearin et al. 2016 ). In addition, the large scale of the spin bias signal for cluster-size haloes, of almost a factor 2 at ∼10 14.5 h −1 M ⊙ , suggests an alternative route towards an observational proof of secondary bias. Probing the effect of spin bias requires measuring rotation, or a proxy for it, in a large sample of galaxy clusters. These measurements, which are still extremely challenging, might be possible in the near future thanks to techniques such as kinetic Sunyaev–Zel’dovich effect (see e.g. Baldi et al. 2018 ). We have applied, for the first time, a fully multitracer approach to the measurement of secondary bias. Here, different subsets of haloes are viewed as different LSS tracers. We show that this method is capable of reproducing all features observed from the standard measurement. In addition, we have obtained statistical uncertainties which are comparable to other bias estimates from N -body simulations that minimize cosmic variance by relying on direct knowledge of the density field, e.g. Gao White ( 2007 ); Chue et al. ( 2018 ). However, in contrast to those methods, which in effect compute δ α /δ m at each point (in configuration or Fourier space), the technique used in this work can be applied both to simulations as well as to actual data, in real or redshift space. The