Hubble Space Telescope Primer for Cycle 11

2.2 Telescope Design and Field of View

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The design and layout of HST are shown schematically in Figure 2.1. The telescope receives electrical power from two solar arrays, which are turned (and the spacecraft rolled about its optical axis) so that the panels face the incident sunlight. Nickel-hydrogen batteries power the telescope during orbital night. Two high-gain antennas provide communications with the ground via the Tracking and Data Relay Satellite System (TDRSS). Power, control and communications functions are carried out by the Support Systems Module (SSM) that encircles the primary mirror.

The SIs are mounted in bays behind the primary mirror. The WFPC2 occupies one of the radial bays, with an attached 45 degree pickoff mirror that allows it to receive the on-axis beam. There are three Fine Guidance Sensors (FGSs) which occupy the other radial bays and receive light 10-14 arcminutes off-axis. Since at most two FGSs are required to guide the telescope, it is possible to conduct astrometric observations with the third FGS. The remaining SIs are mounted in the axial bays and receive images several arcminutes off-axis.

When referring to the HST and its focal plane, we use a coordinate system that is fixed to the telescope and consists of three orthogonal axes: U1, U2 and U3. As shown in Figure 2.1, U1 lies along the optical axis, U2 is parallel to the solar-array rotation axis, and U3 is perpendicular to the solar-array axis. (Note: Some HST documentation uses the alternative V1, V2, V3 coordinate system for which V1=U1, V2=-U2 and V3=-U3.)

Figure 2.1: The Hubble Space Telescope. Major components are labelled, and definitions of the U1,U2,U3 spacecraft axes are indicated.
 
Figure 2.2: The HST field of view with the locations of the SIs and the FGS apertures in the (U2,U3) focal plane. The scale in arcsec is indicated.
 

Figure 2.2 shows the layout of the instrument entrance apertures in the telescope focal plane, as projected onto the sky.

Table 2.1 lists the relative effective locations of the SI apertures in the U2,U3 coordinate system; linear dimensions were converted to arcseconds using a plate scale of 3.58 arcsec/mm, which yields aperture locations accurate to about +/- 1 arcsec. The predicted aperture location for ACS, which remains to be installed in the telescope, could be in error by as much as 10". The Instrument Handbooks (see Section 1.2) should be consulted for accurate details of each instrument's aperture sizes and orientations.

Table 2.1: Nominal Effective Relative Aperture Locations

Instrument	Aperture	U2 (arcsec)	U3 (arcsec)
ACS	WFC HRC SBC	-256 -177 -177	-245 -485 -485
FGS	FGS1R	-726	0
NICMOS	NIC1 NIC2 NIC3	296 319 249	-290 -311 -235
STIS		214	225
WFPC2	PC WF2 WF3 WF4	-2 51 0 -55	30 6 -48 6