| Name: | Prerana Biswas |
| Affiliation: | Joint Astronomy Programme, Indian Institue of Science, Bangalore |
| Conference ID : | ASI2024_726 |
| Title : | Indication of shallower slope in Baryonic Tully-Fisher relation with 3D kinematic modelling and robust modelling of galaxies |
| Authors : | Prerana Biswas, Veselina Kalinova, Nirupam Roy, Narendra Nath Patra |
| Authors Affiliation: | Prerana Biswas (Joint Astronomy Programme, Indian Institute of Science, Bangalore 560012, India) Veselina Kalinova (Max Planck Institute for Radioastronomy, Auf dem Hügel 69, D-53121 Bonn, Germany)
Nirupam Roy (Department of Physics, Indian Institute of Science, Bangalore 560012, India)
Narendra Nath Patra (Department of Astronomy, Astrophysics and Space Engineering, Indian Institute of Technology Indore, Indore 453552, India) |
| Mode of Presentation: | Poster |
| Abstract Category : | Galaxies and Cosmology |
| Abstract : | Baryonic Tully-Fisher relation (BTFR) is a vital relation correlating baryonic mass and rotation velocity of galaxies. It has been extensively used to estimate distances, determine value of Hubble constant, examine galaxy formation models, etc. So far, different measures of rotation velocity have been used to establish this relation. These mostly include widths of HI spectra measured in single-dish observation corrected for optical or 2D-kinematic inclination, and rotation velocity measured from 2D kinematically modelled rotation curves. However, 2D modelling suffers from the problem of beam smearing and projection effect, but 3D modelling does not. Recent studies also showed that both rotation velocities and inclination can have significant differences between those found by 2D and 3D kinematic modelling. Till now, to establish BTFR, these different measures of velocity from 2D kinematic modelling or HI widths and also baryonic masses from different sources with heterogeneous data products, have been used. Here in this study, to revisit BTFR, we first derived 3D kinematic modelling of 18 nearby galaxies from GARCIA (Biswas et al. 2022) and CALIFA (S ́anchez et al. 2012) survey using uniformly analysed data products. We further build their robust mass modelling considering 3D modelled rotation curve, Multi-Gaussian Expansion method+Jeans Anisotropic Modelling to derive stellar kinematics and our own developed method that does not assume any profile on gas surface brightness beforehand to find the contribution of gas. All these have not been put together before for doing mass modelling of galaxies via MCMC optimisation method (Biswas et al. 2023). Equipped with parameters derived from 3D kinematic modelling and robust mass modelling, we revisit BTFR. In comparison to previous studies, our study shows a shallower slope in BTFR (Biswas et al. 2023), indicating a revision of this relation with 3D kinematic models and robust mass models of a larger sample of galaxies. |
