|Space Telescope Science Institute|
|STIS Data Handbook 6.0 May 2011|
References to multiple coordinate systems appear in the headers of STIS data, tied to the spacecraft frame, the user frame, and the aperture frame. We briefly explain here the relationships among these coordinate systems, and show them in Figure 2.6. These coordinate systems are discussed in detail in STIS TIR 1999-02.
• Vehicle Frame (V1, V2, V3): The right-handed coordinate system for the telescope, with V1 pointing in the direction the telescope is looking.
• User Frame (Xuser, Yuser): This is the user frame, aligned with the detector. The coordinate system in IRAF is aligned with the user frame.
• Aperture Frame (Xaperture, Yaperture): This frame is aligned with the slit. POS-TARG movements are aligned with the aperture frame.
• PA_V3: The position angle of the V3 axis; the angle from North, towards East, to V3, measured at the center of the HST focal plane (in the _spt header).
• ROLL_AVG: The average angle from North towards East to V3, measured at the position of the STIS field in the HST focal plane (in the _jit header, computed).
• PA_APER: The angle from North through East to Yaperture measured at the aperture reference (in the science header). PA_V3 - PA_APER is either 225 or -135 degrees, with small variations (a few tenths of a degree).
• ORIENTAT: The angle from North through East to Yuser measured at the aperture reference (in science header). It can differ from PA_APER by up to ~1.5 degrees (e.g., for the long slits with offset occulting bars). Note that this is not the same angle as the ORIENT specified in Phase II, which gives the position angle of the U3 axis, where U3 = -V3. For further information on slit orientation while planning STIS observations, see Figure 3.2 and “Fixing Orientation on the Sky” in Chapter 11 of the STIS Instrument Handbook.Figure 2.6: STIS Coordinate SystemsThe STIS CCD detector supports on-chip binning by factors of 2 and 4 in each dimension. This option was often used early in the operational life of the instrument to increase the signal-to-noise for faint targets, but became less favorable as the number of hot pixels increased over time. The readout of subarrays, with less than the full dimension in Y, is also supported to reduce the readout time. These modes are discussed in Section 11.1.1 of the STIS Instrument Handbook.Reference files for the CCD use unbinned full-frame coordinates (Xref, Yref) after overscan trimming. The coordinates in a trimmed science image (X, Y) are related to these reference coordinates by values given in keywords in the primary header:X=(Xref*LTM1_1)+LTV1Y=(Yref*LTM2_2)+LTV2
Table 2.9 gives examples of coordinates and conversion parameters for datasets with different binnings (BINAXIS1, BINAXIS2) and array size (NAXIS1, NAXIS2). The image coordinates of the reference pixel (CRPIX1, CRPIX2) are near the center of the image. A more detailed discussion of coordinate transformations is given in STIS TIR 1999-02.
1x1 full array:
2x1 full array:
1x1 full array:
2x1 full array: