… When |$\mathcal {F}(R)$| is negative (overmaximal discs), we increase its magnitude by a
factor |$f\cdot \mathcal {F}(R)$| where f is a user-… We adopt for f the conservative value of unity. …

… To implement the maximum disc method, we adopt the maximum disc values of Υ ⋆ from
Starkman et al. (2018). For consistency, we fix galaxy distances and disc inclinations to the …

… with S/N between 2.9 and 3.1. Total line fluxes are measured summing pixels with S/N > 3 in
… are estimated repeating the sum for pixels with S/N > 2 and S/N > 4. Emission-line maps are …

… 2019a,b) at z ≈ 8 (McGaugh 2024). This becomes more challenging to assess at z > 10
where much of the observed luminosity is in the ultraviolet where the short-lived nature of high …

… units and need to be scaled down to more realistic values at 3.6 μm (Lelli et al. 2016; Starkman
et al. 2018). SPARC is a large sample by the standard of H i interferometry. It includes all …

… ), and is consistent with but independent of our own estimates (McGaugh 2016a, 2019). It …
For the outer circular speed, we apply the method of Lelli et al. (2016a) to the stellar rotation …

… et al. 2016) database comes as close as has so far been achieved (McGaugh et al. 2020).
In this paper, we apply Sellwood’s compression code to a large number of SPARC galaxies. …

We present an empirical method to measure the halo mass function (HMF) of galaxies. We
determine the relation between the H i line width from single-dish observations and the dark …

… Blue points are galaxies in the SPARC database (Lelli … 2016b) and the gas rich galaxies
discussed by McGaugh (2012)… [3.6] data are used to trace the stellar mass distribution (Lelli …

We analyze the existing rotation-curve data of the Milky Way and M31 galaxies that extend
to very large distances and low accelerations. We find a systematic downward trend in the …