Max Planck Institute for Astronomy - Annual Report 2005
Max Planck Institute for Astronomy - Annual Report 2005
Max Planck Institute for Astronomy - Annual Report 2005
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14 I. General<br />
Point Source sensitivity (1 h , 5s) [Jy]<br />
1<br />
0.01<br />
10 –4<br />
10 –6<br />
10 –8<br />
10 –10<br />
LAICA<br />
CHEOPS<br />
LINC-NIRVANA<br />
Ω 2000<br />
MIDI<br />
LUCIFER<br />
APRÈS–MIDI<br />
DARWIN<br />
(est.)<br />
JWST<br />
MIRI<br />
HERSCHEL– PACS<br />
1 10 100<br />
Wavelength [mm]<br />
Fig. I.7: The <strong>Institute</strong>'s major instruments. Left: sensitivity as a<br />
function of wavelength; right: spatial resolution as a function<br />
of the field of view.<br />
cision-optical hearts of miri and nirSpec the MPIA<br />
is also closely cooperating with Carl Zeiss Optronics,<br />
Oberkochen. The MPIA has been representing Germany<br />
since 1998 within the Darwin Science Advisory Team.<br />
Darwin is a space interferometer to be launched by the<br />
European Space Agency eSa not be<strong>for</strong>e 2015. In the<br />
plan it will comprise up to eight telescopes orbiting the<br />
Sun at the Lagrangian point L2, at 1.5 million kilometer<br />
distance from Earth. This observatory will be used <strong>for</strong><br />
imaging and spectroscopy of extrasolar planets in the<br />
mid-infrared range. At present, the <strong>Institute</strong> is carrying<br />
out preparatory technology studies.<br />
MPIA also contributes to eSa's Gaia project, a space<br />
observatory scheduled <strong>for</strong> launch between 2010 and 2012.<br />
Spatial Resolution [milli-arsec]<br />
1<br />
10<br />
100<br />
1000<br />
10 4<br />
10 5<br />
APRÈS–MIDI<br />
MIDI<br />
DARWIN<br />
PLANET<br />
FINDER<br />
JWST<br />
MIRI<br />
HERSCHEL<br />
PACS<br />
LINC-NIRVANA<br />
CONICA/<br />
LUCIFER<br />
Ω 2000<br />
LAICA<br />
1� 10� 100� 1000� 10000�<br />
Field of view<br />
Gaia will be the successor to the hipparcoS astrometry<br />
satellite, exceeding the latter’s sensitivity by several orders<br />
of magnitude. With this the satellite will measure<br />
positions, magnitudes and radial velocities of one billion<br />
stars plus numerous galaxies, quasars and asteroids. The<br />
telescope will provide photometric data in 15 spectral<br />
bands as well as spectra in a selected spectral range.<br />
Unlike hipparcoS, however, Gaia needs not be provided<br />
with an input catalogue, but will measure systematically<br />
all accessible objects. An automatic object classification<br />
will thus be of major importance <strong>for</strong> data analysis. At<br />
present, concepts <strong>for</strong> coping with this demanding task<br />
are being developed at the MPIA (supported by a grant<br />
from DLR).<br />
Figure I.7 gives an overview of the major instruments<br />
which are already working or are about to be put into<br />
operation. Sensitivity is shown as a function of wavelength<br />
(left), and spatial resolution as a function of the<br />
size of the field of view (right).<br />
PRIME