here - Institute for Astronomy Umleitung

Title: Science Case
Reference: MUSE-MEM-SCI-052
Issue: 1.3
Date: 04/02/2004
Page: 36/100
an emission line surface brightness through a Schmidt star-formation law, normalised to a
total flux of 10 -17 erg s -1 cm -2 . Consistent with Fig 1, the velocity field can be mapped with
MUSE to approximately two disk scale lengths. Clearly, in addition to the rotation curves for,
e.g., Tully-Fisher studies as a function of internal galactic properties, any internal kinematic
sub-structure on these scales will also be detected by MUSE, allowing for example the
investigation of environment-induced perturbations to the velocity fields, and their possible
effect on global galactic properties such as total galactic star formation rates and metal
enrichment properties.
For all galaxies with 0.25 10 -17 erg s -1
cm -2 and R,I AB < 22.5. Note that this simple calculation does not take
into account the beneficial effects of spatial inhomogeneities such as
spiral structure in tracing the emission further out, nor does it take into
account averaging over adjacent spaxels further out in the galaxy
profile.