Law, David R.David R.LawWestfall, Kyle B.Kyle B.WestfallBershady, Matthew A.Matthew A.BershadyCappellari, MicheleMicheleCappellariYan, RenbinRenbinYanBELFIORE, FRANCESCO MICHEL CONCETTOFRANCESCO MICHEL CONCETTOBELFIOREBizyaev, DmitryDmitryBizyaevBrownstein, Joel R.Joel R.BrownsteinChen, YanpingYanpingChenCherinka, BrianBrianCherinkaDrory, NivNivDroryLazarz, DanielDanielLazarzShetty, ShravanShravanShetty2022-01-042022-01-0420210004-6256http://hdl.handle.net/20.500.12386/31301The Sloan Digital Sky Survey IV Mapping Nearby Galaxies at APO (MaNGA) program has been operating from 2014 to 2020, and has now observed a sample of 9269 galaxies in the low redshift universe (z ∼ 0.05) with integral-field spectroscopy. With rest-optical (λλ0.36-1.0 μm) spectral resolution R ∼ 2000 the instrumental spectral line-spread function (LSF) typically has 1σ width of about 70 km s−1, which poses a challenge for the study of the typically 20-30 km s−1 velocity dispersion of the ionized gas in present-day disk galaxies. In this contribution, we present a major revision of the MaNGA data pipeline architecture, focusing particularly on a variety of factors impacting the effective LSF (e.g., under-sampling, spectral rectification, and data cube construction). Through comparison with external assessments of the MaNGA data provided by substantially higher-resolution R ∼ 10,000 instruments, we demonstrate that the revised MPL-10 pipeline measures the instrumental LSF sufficiently accurately (≤0.6% systematic, 2% random around the wavelength of Hα) that it enables reliable measurements of astrophysical velocity dispersions σHα ∼ 20 km s−1 for spaxels with emission lines detected at signal-to-noise ratio > 50. Velocity dispersions derived from [O II], Hβ, [O III], [N II], and [S II] are consistent with those derived from Hα to within about 2% at σHα > 30 km s−1. Although the impact of these changes to the estimated LSF will be minimal at velocity dispersions greater than about 100 km s−1, scientific results from previous data releases that are based on dispersions far below the instrumental resolution should be reevaluated.STAMPAenArticle10.3847/1538-3881/abcaa22-s2.0-85099218361https://iopscience.iop.org/article/10.3847/1538-3881/abcaa2https://api.elsevier.com/content/abstract/scopus_id/850992183612021AJ....161...52LFIS/05 - ASTRONOMIA E ASTROFISICA