Understanding the Fundamental Plane and the 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

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...

LSB Galaxies and the Tully-Fisher Relation

We present Very Large Array (VLA) Hi imaging of four low surface brightness (LSB) galaxies ([OBC97] P01-3, [OBC97] C06-1, [OBC97] C04-1, [OBC97] C04-2)1 which were thought to strongly deviate from the Tully-Fisher (TF) relation based on Arecibo singledish observations. We do not detect three of the four targeted LSB galaxies in Hi down to a 4σ limit of 0.08Jy km s−1. We find that two of the fou...

The Tully – Fisher Relation and H ◦

The use of the Tully–Fisher (TF) relation for the determination of H◦ relies on the availability of an adequate template TF relation and of reliable primary distances. Here we use a TF template relation with the best available kinematical zero–point, obtained from a sample of 24 clusters of galaxies extending to cz ∼ 9, 000 km s , and the most recent set of Cepheid distances for galaxies fit fo...