Non-linearity of the Tully-Fisher relation

Tully–Fisher Relation

The Baryonic Tully-Fisher Relation.

We explore the Tully-Fisher relation over five decades in stellar mass in galaxies with circular velocities ranging over 30 less, similarVc less, similar300 km s-1. We find a clear break in the optical Tully-Fisher relation: field galaxies with Vc less, similar90 km s-1 fall below the relation defined by brighter galaxies. These faint galaxies, however, are very rich in gas; adding in the gas m...

Tully-Fisher relation

Detailed neutral hydrogen observations have been obtained of the large barred spiral galaxy NGC 3992 and its three small companion spiral galaxies, UGC 6923, UGC 6940, and UGC 6969. Contrary to the large galaxy, for the companions the H i distribution ends quite abruptly at the optical edges. Velocity fields have been constructed from which rotation curves have been derived. Assuming a reasonab...

Interpreting Offsets from the Tully-fisher Relation

We have previously demonstrated that TullyFisher (TF) residuals correlate with tracers of star formation history (color and emission line equivalent width, EW) for a broad sample of Sa–Sd spiral galaxies (Kannappan, Fabricant, & Franx 2002, KFF). Here we use these correlations to study two other classes of galaxies: (1) galaxies in close pairs, and (2) galaxies at intermediate redshift. In the ...

Maximal Disks and the Tully-Fisher Relation

We show that for luminous, non-barred, high-surface brightness (HSB) spirals the Tully-Fisher (TF) relation residuals can be used to estimate the relative mass contributions of the stellar disk and the dark halo at the peak of the disk rotation, near 2.2 exponential scale lengths. For “maximal disks”, a large fraction (0.85 ± 0.1) of the total rotational support, V2.2, at such radii should aris...