Max Planck Institute for Astronomy - Annual Report 2007

seems consistent with the present value. Only beyond
z 1.7 are there indications that black holes were more
massive than today relative to their galaxies in the early
universe. Accordingly, the black holes would have first
grown quickly – their galaxies building their masses only
later and more slowly.
However, because of selection effects, the uncertainties
of this method are still so high that these results could
possibly be insignificant. Further, methodically independent
approaches are necessary in order to obtain a coherent
picture at these and other redshifts. To achieve this,
the MPIA astronomers have started among other things
an observing program using the VLT and Si n F o n i (the
near infrared integral field spectrograph with camera),
for which they make use of MPIAʼs guaranteed observing
time from building the pa r S e c laser guidance system
HE1104–1805 Host galaxy Einstein Ring
(after point source removal)
A
B
lensing galaxy
3
III.2 In What Type of Galaxies Do Quasars III.X Live? Titel 77
that supports Si n F o n i. The initial goal is to determine dynamic
galaxy masses for four quasars, three of which are
gravitationally lensed. Through Si n F o n i, extended line
emission in the host galaxy is measured in order to derive
the velocity field present there and thus dynamically
determine the included masses. This method differs in
principle from the above-described approach and is also
complementary to the mass determinations based on the
33 FOV
Source plane velocity field Image plane velocity field
Fig. III.2.8: The lense system HE1104-1805. Top left: the optical
image (HST), top right: the image of the host galaxy after
subtraction of the quasar core pulled apart near an Einstein
ring, right bottom: a velocity field likely observed according
to the lens model, and left bottom: the velocity field calculated
back into the source plane.
3 3
3