An empirical measurement of the halo mass function from the combination of GAMA DR4, SDSS DR12, and REFLEX II data. Issue 2 (6th April 2022)

• Record Type: Journal Article
• Authors: Driver, Simon P; Robotham, Aaron S G; Obreschkow, Danail; Peacock, John A; Baldry, Ivan K; Bellstedt, Sabine; Bland-Hawthorn, Joss; Brough, Sarah; Cluver, Michelle; Holwerda, Benne W; Hopkins, Andrew; Lagos, Claudia; Liske, Jochen; Loveday, Jon; Phillipps, Steven; Taylor, Edward N
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 515:Issue 2(2022)
• Page Start: 2138
• Page End: 2163
• Publication Date: 2022-04-06
• Subjects: surveys -- galaxies: groups: general -- galaxies: haloes -- cosmological parameters -- cosmology: observations -- dark matter; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac581
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We construct the halo mass function (HMF) from the GAMA (Galaxy And Mass Assembly) galaxy group catalogue over the mass range of 10 12.7 –10 15.5 M⊙, and find good agreement with the expectation from Lambda cold dark matter. In comparison to previous studies, this result extends the mass range over which the HMF has now been measured over by an order of magnitude. We combine the GAMA data release (DR) 4 HMF with similar data from the Sloan Digital Sky Survey (SDSS) DR12 and REFLEX II ( ROSAT -ESO Flux Limited X-ray Galaxy Cluster Survey) surveys, and fit a four-parameter Murray–Robotham–Power function, valid at $\tilde{z} \approx 0.1$, yielding a density normalization of log10 (ϕ* Mpc$^{3})= -3.96^{+0.55}_{-0.82}$, a high mass turnover of log10 ( M * M$_{\odot }^{-1})=14.13^{+0.43}_{-0.40}$, a low-mass power-law slope of $\alpha =-1.68^{+0.21}_{-0.24}$, and a high-mass softening parameter of $\beta =0.63^{+0.25}_{-0.11}$ . If we fold in the constraint on ΩM from the Planck 2018 cosmology, we are able to reduce these uncertainties further, but this relies on the assumption that the power-law trend can be extrapolated from 10 12.7 M⊙ to zero mass. Throughout, we highlight the effort needed to improve on our HMF measurement: improved halo mass estimates that do not rely on calibration to simulations; reduced halo mass uncertainties needed to mitigate the strong Eddington bias that arises from the steepness of the HMF low-mass slope; and deeper wider area spectroscopic surveys. To our halo mass limit of 10 12.7 M⊙, we are directly resolving ('seeing') 41 ± 5 per cent of the total mass density, i.e. ΩM, >12.7 = 0.128 ± 0.016, opening the door for the direct construction of three-dimensional dark matter mass maps at Mpc resolution.