The DENIS instrument has been described in detail by Copet et al.
([1999]). A sketch of its main optical components is displayed in
Fig. 1. It is located at the Cassegrain focus of the ESO 1 m
telescope at La Silla Observatory (Chile). After reflection from the two
telescope mirrors, the light beam goes through a field lens at the telescope
focus, covered by a protective blade, both of CaF2 and uncoated. Then a
dichroic splits the i beam in reflection from the J/
beam in
transmission.
The i beam has two more reflections from coated mirrors before entering the objective (3 CaF2 and 2 silica coated lenses), then goes through the Gunn i filter, a shutter, the cryostat entrance window (BK7) and arrives at the Tektronix 1 K CCD detector, cooled to 180 K.
The J/
beam is reflected off a microscanning mirror (uncoated Al), then
J is reflected by a second dichroic and a coated mirror before entering
the J objective (3 CaF2 and 2 fused silica coated lenses), then the
cryostat entrance window (coated fused silica), the filter and finally the
NICMOS-3 detector, both cooled to 80 K.
The
beam is transmitted by the second dichroic, then reflects off two
more coated mirrors, passes through the
objective (4 ZnS-Cleartran and 1
fused silica coated lenses), the cryostat entrance window (coated fused
silica), the filter and the other NICMOS-3 detector.
We have tried to obtain response curves for all these elements. When this was
not possible, a reasonable estimate of the transmission was adopted. Filter
response curves as provided by Barr Associates (U.S.A.) for J and ,
at the
nominal detector temperature (77 K), and by MTO-France for the Gunn i filter
(at ambient temperature) are displayed in Fig. 2. The full
system response curves (atmosphere, optics, filter and detector) are shown in
Fig. 3.
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Figure 3: The complete DENIS system normalized response curves (atmosphere, optics, filters, detectors) |
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