The morphological dependent Tully-Fisher relation of spiral galaxies

Abstract

The Tully-Fisher relation of spiral galaxies shows notable dependence on morphological types, with earlier type spirals having systematically lower luminosity at fixed maximum rotation velocity $V_{max}$. This decrement of luminosity is more significant in shorter wavelengths. By modeling the rotation curve and stellar population of different morphological type spiral galaxies in combination, we find the $V_{max}$ of spiral galaxies is weakly dependent on the morphological type, whereas the difference of the stellar population originating from the bulge disk composition effect mainly account for the morphological type dependence of the Tully-Fisher relation.

8 pages, 3 figures, ApJ accepted

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Cited by in corpus (6)

• The SAMI Galaxy Survey: Stellar and gas misalignments and the origin of gas in nearby galaxies
• The Atlas3D project - V. The CO Tully-Fisher relation of early-type galaxies
• The HI Tully-Fisher Relation of Early-Type Galaxies
• CO Tully-Fisher Relation of Star-forming Galaxies at z=0.05-0.3
• Calibration of the Tully-Fisher relation in the WISE W1 ($3.4\mu \mathrm{m}$) and W2 ($4.6\mu \mathrm{m}$) Bands
• Variation Of The Tully-Fisher Relation As A Function Of The Magnitude Interval Of A Sample Of Galaxies