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Abstract
Using the Very Large Telescope in Multi Object Spectroscopy mode, we have observed a sample of 113 field spiral galaxies in the FORS Deep Field (FDF) with redshifts in the range . The galaxies were selected based on apparent brightness () and encompass all late spectrophotometric types from Sa to Sdm/Im. Spatially resolved rotation curves have been extracted for 77 galaxies and fitted with synthetic velocity fields taking into account all observational effects from inclination and slit misalignment to seeing and slit width. We also compared different shapes for the intrinsic rotation curve. To obtain robust values of Vmax, our analysis is focused on galaxies with rotation curves that extend well into the region of constant rotation velocity at large radii. If the slope of the local Tully-Fisher relation (TFR) is held fixed, we find evidence for a mass-dependent luminosity evolution which is as large as up to for the lowest-mass galaxies, but is small or even negligible for the highest-mass systems in our sample. In effect, the TFR slope is shallower at in comparison to the local sample. We argue for a mass-dependent evolution of the mass-to-light ratio. An additional population of blue, low-mass spirals does not seem a very appealing explanation. The flatter tilt we find for the distant TFR is in contradiction to the predictions of recent semi-analytic simulations.
Highlights
Ever since the relation between the luminosity L and the maximum rotation velocity Vmax of spiral galaxies was first observed (Tully & Fisher 1977), the physical origin of its slope and scatter, as well as the possible evolution thereof over different cosmic epochs have been subject to debate both in theoretical and observational studies
If the slope of the local Tully-Fisher relation (TFR) is held fixed, we find evidence for a mass-dependent luminosity evolution which is as large as up to ∆MB ≈ −2m for the lowest-mass galaxies, but is small or even negligible for the highest-mass systems in our sample
Using imaging data and spectroscopy taken with the ESO Very Large Telescope, we have derived structural parameters and resolved rotation curves of a magnitude-limited sample of 77 spiral galaxies in the FORS Deep Field
Summary
Ever since the relation between the luminosity L and the maximum rotation velocity Vmax of spiral galaxies was first observed (Tully & Fisher 1977), the physical origin of its slope and scatter, as well as the possible evolution thereof over different cosmic epochs have been subject to debate both in theoretical and observational studies. Robust measurements of rotation velocities and luminosities become increasingly difficult This is partly because of the low apparent magnitudes of the galaxies, and due to the limited intrinsic spatial resolution We will describe the derivation of the maximum rotation velocities, the galaxies’ structural parameters and the luminosities in more detail and present the data table of the enlarged, full sample.
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