Max Planck Institute for Astronomy - Annual Report 2005

68 III. Scientific Work
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Fig. III.2.4: Spectral energy distributions (SEDs) of disks composed
of 1 and 40 µm grains with different grain chemical
compositions, for a model resembling the solar system (i.e., the
planets, excluding Mercury and Pluto, and the Kuiper belt as
Once interesting debris disks have been identified by
spItzEr, the next step will be to obtain high-sensitivity
and high-spatial resolution images in scattered light
and/or thermal emission (using, e.g., LBT, JWST, soFIa,
alMa, or saFIr). Of particular interest are the longer
wavelengths, at which observations can constrain the
amount of material farther away from the planet and at
which the emission of the larger dust particles, the ones
that show more prominent structure, dominate. If one
could spatially resolve the disk, the dynamical models
could allow us to locate the perturbing planet. Then we
could compare the information derived from the SED
alone with that derived from the resolved image. This is
important to understand the limitations of the characterization
of planetary architectures on the basis of spatially
unresolved debris disks only. In addition, by obtaining
resolved images in one or more wavelengths we can
break the degeneracy expected from the analysis of the
disk SED. In anticipation of these spatially resolved observations,
we have started working on the modeling of
the brightness density distributions arising from debris
disks in the presence of different planetary configurations
(see Fig III.2.6).
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the source of dust). Top left: Single grain size (40 µm) disk with
planets; Top right: Single grain size (1 µm) disk with planets;
Bottom left: Single grain size (40 µm) disk without planets;
Bottom right: Single grain size (1 µm) disk without planets.
Radiative Transfer Simulations in the Context of
MatIsse Science Case Studies
MatIssE is foreseen as a mid-infrared spectro-interferometer
combining the beams of up to four UTs/Ats of
the Very Large Telescope Interferometer (VLTI). MatIssE
will measure closure phase relations and thus offer an
efficient capability for image reconstruction. In addition
to the ability to reconstruct images with interferometric
resolution, MatIssE will open three new observing windows
at the VLTI: the L, M, and Q band which all belong
to the mid-infrared domain. Furthermore, the instrument
will offer the possibility to perform simultaneous observations
in separate bands.
MatIssE will also provide several spectroscopic
modes. In summary, MatIssE can be seen as a successor
of MIdI by providing imaging capabilities in the entire
mid-infrared accessible from the ground. The extension
of MatIssE down to 2.7 µm as well as its generalisation
of the use of closure phases make it also a successor of
aMbEr. Thus, in many respects MatIssE will combine and
extend the experience acquired with two first generation
VLTI instruments – MIdI and aMbEr.