The SDSS-DR12 large-scale cross-correlation of damped Lyman alpha systems with the Lyman alpha forest

• Published in: Monthly notices of the Royal Astronomical Society 2018-01, Vol.473 (3), p.3019-3038
• Main Authors: Pérez-Ràfols, Ignasi, Font-Ribera, Andreu, Miralda-Escudé, Jordi, Blomqvist, Michael, Bird, Simeon, Busca, Nicolás, du Mas des Bourboux, Hélion, Mas-Ribas, Lluís, Noterdaeme, Pasquier, Petitjean, Patrick, Rich, James, Schneider, Donald P.
• Format: Article
• Language: English
• Subjects: Astrophysics; Physics
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stx2525

Abstract We present a measurement of the damped Ly α absorber (DLA) mean bias from the cross-correlation of DLAs and the Ly α forest, updating earlier results of Font-Ribera et al. (2012) with the final Baryon Oscillations Spectroscopic Survey data release and an improved method to address continuum fitting corrections. Our cross-correlation is well fitted by linear theory with the standard ΛCDM model, with a DLA bias of bDLA = 1.99 ± 0.11; a more conservative analysis, which removes DLA in the Ly β forest and uses only the cross-correlation at r > 10 h−1 Mpc, yields bDLA = 2.00 ± 0.19. This assumes the cosmological model from Planck Collaboration (2016) and the Ly α forest bias factors of Bautista et al. (2017) and includes only statistical errors obtained from bootstrap analysis. The main systematic errors arise from possible impurities and selection effects in the DLA catalogue and from uncertainties in the determination of the Ly α forest bias factors and a correction for effects of high column density absorbers. We find no dependence of the DLA bias on column density or redshift. The measured bias value corresponds to a host halo mass ∼4 × 1011 h−1 M⊙ if all DLAs were hosted in haloes of a similar mass. In a realistic model where host haloes over a broad mass range have a DLA cross-section $\Sigma (M_h) \propto M_h^{\alpha }$ down to Mh > Mmin = 108.5 h−1 M⊙, we find that α > 1 is required to have bDLA > 1.7, implying a steeper relation or higher value of Mmin than is generally predicted in numerical simulations of galaxy formation.