Each telescope is a three-mirror anastigmat featuring a rectangular
aperture2.1of
, an inter-mirror distance of about
3 m and a focal length of 50 m.
The image scale on the focal plane is thus of about
,
while the instrument's Airy Disk is an ellipse of axes
at
and
at
.
The aperture is elongated in the scan direction, so as to provide the
narrowest PSF in the measurement direction while being compatible with the
volume of the spacecraft and the optical quality of the mirrors.
The large primary and tertiary mirrors are polished to
rms, while the smaller secondary mirrors are polished to
rms, yielding a diffraction limited performance over
the whole field of view.
The focal plane of each telescope is basically a rectangular mosaic made
of more than 300 of CCDs, giving a field of view of
.
A rectangular pixel size of
or
was chosen in order to match the Airy Disk
shape and thus providing an higher resolution in the scan direction.
The large focal length allows a proper sampling of the diffraction pattern
with about 4 pixels along scan and 3 pixels across scan covering the Airy Disk.
CCDs of two different sizes are used in order to increase redundancy in some
key areas of the focal plane such as the sky mapper and the overlapping
regions.
Smaller CCDs have a size of
,
while bigger CCDs are the same size along scan and twice as large across scan, giving a size of
.
An observed object follows a nearly horizontal line on the focal plane
with a speed given by the spinning period, and therefore successively
crosses all the columns of CCDs.
With the 3-hour spinning period provided by the scanning law the object has
an along-scan speed of
, corresponding to about
3200 pixels/s or 0.31 ms/pixel.
Due to the high speed, the charges accumulated in the CCD pixels cannot be
read out as it is done with conventional imaging telescopes, but a dedicated
integration technique must be used.
In the case of GAIA, the CCDs will be operated in Time Delay Integration
(TDI), a concept introduced for an astrometric satellite by [Høg 1993].
The idea is to let the integration process follow the image while it is
moving across the CCD. In practice, every 0.31 ms, i.e. every time the image
has moved of one pixel along scan, all charges are quickly shifted by one
pixel in the scan direction. The readout of the accumulated charges takes
place at the serial register at the ``end'' of each CCD.
The image is thus integrated over the entire crossing of each CCD,
leading to an exposure time of about 0.86 s per CCD per scan.
The main drawback of this technique is the additional smearing of the
image due to the charge shift and to the slow across-scan motion
of the objects, which together cause an appreciable but acceptable
loss of resolution.
On the other hand, the loss of resolution due to the non optimal charge
transfer efficiency is expected to be negligible.
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The focal plane layout is represented in Figure 2.7. The 25 columns of detectors covering the focal plane are functionally grouped in four parts: the Astrometric Sky Mapper (ASM, 4 columns), the Astrometric Field (AF, 16 columns), the Photometric Sky Mapper2.2(PSM, 1 column) and the Broad-Band Photometer (BBP, 4 columns). A thorough description of the functions fulfilled by the different parts of the focal plane is given in Section 5.1. In brief, the ASM is used for object detection, the AF for multiple multi-epoch astrometric measurements, the PSM to generate a 1 arcsec radius high-resolution map around each detected star and the BBP for multi-color and multi-epoch broad-band photometry.
The ASM, the AF and the PSM work without filters in a very broad band, having
a response curve defined by the telescope transmittance and the Quantum
Efficiency (QE) of the presently agreed-upon CCD, the so called CCD#1B.
The resulting response curve extends in the range of wavelengths
250-1050 nm, and the zero-point of the magnitude scale, the so called
(GAIA) magnitude, is such that for most stellar types the
magnitude
has a value which is intermediate between
and
.
The BBP columns work in four different broad bands defined by the product of
the aforementioned global response curve and the response curve of four
filters.
The photometric system ([Høg, Knude and Straizys 1999]) adopted in this study
consists of five passbands of about 100 nm width. A rectangular
response and a peak transmission of 0.90 is assumed for all filters.
Roughly speaking, the
bands closely resemble the
bands, while
the
bands together cover a waveband with the same center as the
band.
The QE curve of the is shown in Figure 2.8, in
which the normalized response curves for the Asiago Photometric System
([Munari 1999]) have been preferred for illustrative purposes to the
corresponding curves for the
system.
The specifications of the two photometric systems are given in
Table 2.1.
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Band | ![]() |
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445 | 550 | 650 | 750 | 850 |
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110 | 100 | 100 | 100 | 100 |
Asiago system | |||||
Band | ![]() |
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300 | 480 | 630 | 792 | 964 |
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141.5 | 150 | 150 | 172 | 170 |