VizieR Online Data Catalog: The bTFr of MIGHTEE-H I spiral galaxies (Ponomareva+, 2021)

Exploration (MIGHTEE), one of the first deep, blind, medium-wide interferometric surveys for H I ever undertaken (Jarvis et al. 2016mks..confE...6J). It will detect more than 1000 galaxies in H I up to z = 0.6, thus allowing the systematic study of the evolution of the neutral gas content of galaxies over the past 5 billion years in different environments (Ranchod et al. 2021MNRAS.506.2753R) using direct detections and statistical stacking methods (Maddox et al. 2021A&A...646A..35M; Pan et al. 2020MNRAS.491.1227P, Pan et al. 2021, preprint arXiv:2109.04273).

In this work, we use the MIGHTEE Early Science data to perform, for the first time, a homogeneous study of the H I-based bTFr over the last billion years (0 =< z =< 0.081). Furthermore, we consider the bTFr based on two velocity measures: W₅₀ from the corrected width of the global H I profile, and V_out, the rotational velocity measured at the outermost point of the resolved H I rotation curves. This allows us to study how the statistical properties of the bTFr change with redshift and with different definitions of the rotational velocity. This is the first study which tests a completely automated version of 3D Barolo (Di Teodoro & Fraternali 2015MNRAS.451.3021D) at higher redshift, software that was developed to derive H I rotation curves for the marginally resolved galaxies.

The MIGHTEE is a survey of four well-known deep, extragalactic fields currently being observed by MeerKAT, the SKA precursor radio interferometer located in South Africa (Jonas J.L. 2009IEEEP..97.1522J). MeerKAT consists of 64 offset Gregorian dishes (13.5 m diameter main reflector and 3.8 m sub-reflector), and equipped with three receivers: UHF band (580 < ν < 1015 MHz), L band (900 < ν < 1670 MHz), and S band (1750 < ν < 3500 MHz). The MeerKAT data are collected in spectral mode, which makes MIGHTEE a spectral line, continuum, and polarization survey. The H I emission project within the MIGHTEE survey (MIGHTEE-H I). The source finding was performed visually, using the Cube Analysis and Rendering Tool for Astronomy (Comrie et al. 2020zndo...3746095C), and unguided by the deep optical information available for these well-studied fields, by the MIGHTEE-HI group. The total Early Science sample consists of 276 objects each with an identified optical counterpart (Maddox et al. 2021A&A...646A..35M).

We compute baryonic masses, inclination angles and rotational velocities with a tool for fitting 3D tilted-ring models to emission-line data cubes of 93 galaxies which is 40 per cent of the entire sample of the MIGHTEE-H I Early Science Data. Thus, we perform an assessment of the resulting models by visually inspecting the data, model and residuals, as well as the resulting rotation curves projected on the position-velocity diagrams (figs 5 and 6 in Maddox et al. 2021A&A...646A..35M).

Consequently, SNR and velocity resolution are the main reasons why 3D Barolo is not able to model the kinematics of some galaxies in our initial sample. Only 67 of 93 galaxies pass our visual assessment criteria. We regroup all useful galaxy parameters in the tablem.dat which forms the final bTFr sample that covers the 0.006 < z < 0.081 redshift range.

(1 data file).