SDSS-IV MaNGA: bar pattern speed estimates with the Tremaine–Weinberg method and their error sources. Issue 3 (5th November 2019)

• Record Type: Journal Article
• Authors: Garma-Oehmichen, L; Cano-Díaz, M; Hernández-Toledo, H; Aquino-Ortíz, E; Valenzuela, O; Aguerri, J A L; Sánchez, S F; Merrifield, M
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 491:Issue 3(2020)
• Page Start: 3655
• Page End: 3671
• Publication Date: 2019-11-05
• Subjects: galaxies: evolution -- galaxies: kinematics and dynamics -- galaxies: statistics -- galaxies: structure; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz3101
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Estimating the bar pattern speed (Ωbar ) is one of the main challenges faced in understanding the role of stellar bars in galaxy dynamical evolution. This work aims to characterize different uncertainty sources affecting the Tremaine–Weinberg (TW) method to study the correlation between bar and galaxies physical parameters. We use a sample of 15 MaNGA SDSS-IV galaxies and 3 CALIFA galaxies from Aguerri et al. We studied the errors related with (i) galaxy centre determination, (ii) disc position angle (PA) emphasizing the difficulties triggered by outer non-axisymmetric structures besides the bar, (iii) the slits length, and (iv) the spatial resolution. In average, the PA uncertainties range $\sim 15 {{\ \rm per\ cent}}$, the slit length $\sim 9 {{\ \rm per\ cent}}$ and the centring error $\sim 5 {{\ \rm per\ cent}}$ . Reducing the spatial resolution increases the sensitivity to the PA error. Through Monte Carlo simulations, we estimate the probability distribution of the $\mathcal {R}$ bar speed parameter. The present sample is composed of seven slow, four fast, and seven ultrafast bars, with no trend with morphological types. Although uncertainties and low sample numbers may mask potential correlations between physical properties, we present a discussion of them: we observe an anticorrelation of Ωbar with the bar length and the stellar mass, suggesting that massive galaxies tend to host longer and slower bars. We also observe a correlation of the molecular gas fraction with $\mathcal {R}$, and a weak anticorrelation with Ωbar, suggesting that bars rotate slower in gaseous discs. Confirmation of such trends awaits future studies.