Advances in the Research of Tully-Fisher Relation and Baryonic Tully-Fisher Relation

Subjects: Astronomy submitted time 2023-12-13 Cooperative journals: 《天文学进展》

GUO Ming-yu1,2, HU Hui-jie1,2, GU Qing1,2, YANG Hang1,2, GUO Qi1,2

Abstract： This work reviews Tully-Fisher relation and baryonic Tully-Fisher relation(TFR and BTFR), which are important scaling relations connecting galaxy luminosity and baryonic mass with its rotation velocity. TFR and BTFR both serve as the standard rules in comic distance measurements and thus are crucial in determining cosmological parameters. TheTFR make use of photometries in several bands. Despite the scaling relation existing in different wavelength, the slope and scatter varies. This can be explained by the different formation histories of different main tracers, e.g. the mass-to-light ratio is lower at shorter wavelength which is contributed mainly by young stars. Among all bands, the I and R bands present the smallest scatter. In order to further reduce the scatter of TFR, the luminosity is later replaced with stellar mass. Compared to TFR, BTFR includes gas components. It has many advantages. For example, the scatter, especially the intrinsic scatter, of BTFR is even smaller than that of the (stellar mass)TFR. Such tight relation also holds at low-masses. Besides, BTFR is more compatible, as it applies not only to disky galaxies, but also for irregular galaxies. To obtain the rotation velocity of the galaxy gas component, two kinds of telescope are used, telescope arrays and single-dish telescopes. The telescope array is superior to the single-dish in providing high spatial resolution image and velocity field data. With the help of modern theories, such as the tilted-ring model, one could obtain the rotation curve. On the other hand, large single-dish telescopes like FAST have high sensitivities given their large area, which is very useful in detecting weak sources like ultra diffuse galaxies(UDGs). In this paper, we present our preliminary results on the dependence of BTFR of massive galaxies on their gas fraction. We combine ALFALFA survey data with SDSS data, finding evidence of the gas fraction dependence. While BTFR is nearly independent on gas fraction for massive galaxies, at low masses, a weak yet positive dependence on gas fraction presents itself. Further studies using upcoming large arrays like SKA could be able to provide more reliable data for the kinematical studies.

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