|Abstract : ||The Baryonic Tully-Fisher relation (BTFR) is a vital relation correlating the baryonic mass and the rotation velocity of the galaxies. It has been used widely to determine the distances, estimate the Hubble constant, study local galaxy flows, test galaxy formation model in a ΛCDM cosmology, and test alternative theories like modified gravity. To date, different forms of the rotation velocity (e.g., wp20 and wm50, V_flat and V_max ) have been used to establish this relation. In most previous studies, HI spectra' widths are taken from the single-dish observation; there are key differences between spatially resolved data from interferometric HI observations and spatially unresolved data from single-dish HI observations (Lelli et al. 2019). Furthermore, inclination angles, the dominant error in BTFR (Jacoby et al. 1992; Bothun & Mould 1987), changes significantly defined from optical observation, single-dish HI maps and found from the kinematic modeling done with HI interferometric data. These all lead to different slopes, intercepts and scatters in BTFR.
By analyzing the data of 26 galaxies, 11 from GMRT archive as a part of The GMRT ARChIve Atomic gas survey (GARCIA)-I (Biswas et al., under review) and 15 observed by us with GMRT as part of the MasQue (Mass Modelling and Star-formation Quenching of Nearby Galaxies; Kalinova et al. 2021) project, we explore BTFR with spacially resolved HI interferometric data in detail. We study 3D kinematic modeling using the two pipelines: FAT and BBarolo; compare the inclination angles, rotation velocities obtained from the kinematic modeling with the single-dish and optical observations. We then use different velocities from our analysis in BTFR and compare this to the existing literature. We expand this study by doing the mass-modeling and testing different dark matter profiles through MCMC simulation adopting a constant mass-to-light ratio and using the derived baryonic mass in the BTFR.|