The ALFALFA H i velocity width function. Issue 3 (1st November 2021)

• Record Type: Journal Article
• Authors: Oman, Kyle A
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 509:Issue 3(2022)
• Page Start: 3268
• Page End: 3284
• Publication Date: 2021-11-01
• Subjects: galaxies: abundances -- galaxies: luminosity function, mass function -- dark matter -- radio lines: galaxies; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab3164
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We make the most precise determination to date of the number density of extragalactic 21-cm radio sources as a function of their spectral line widths – the H i velocity width function (H i WF) – based on 21 827 sources from the final $7000\, \mathrm{deg}^2$ data release of the Arecibo Legacy Fast ALFA (ALFALFA) survey. The number density of sources as a function of their neutral hydrogen masses – the H i mass function (H i MF) – has previously been reported to have a significantly different low-mass slope and 'knee mass' in the two sky regions surveyed during ALFALFA. In contrast with this, we find that the shape of the H i WF in the same two sky regions is remarkably similar, consistent with being identical within the confidence intervals implied by the data (but the overall normalization differs). The spatial uniformity of the H i WF implies that it is likely a stable tracer of the mass function of dark matter haloes, in spite of the environmental processes to which the measured variation in the H i MF are attributed, at least for galaxies containing enough neutral hydrogen to be detected. This insensitivity of the H i WF to galaxy formation and evolution can be exploited to turn it into a powerful constraint on cosmological models as future surveys yield increasingly precise measurements. We also report on the possible influence of a previously overlooked systematic error affecting the H i WF, which may plausibly see its low-velocity slope steepen by ∼40 per cent in analyses of future, deeper surveys. Finally, we provide an updated estimate of the ALFALFA completeness limit.