The ACS detectors exhibit more distortion than previous HST
instruments. The principal reason for this is that the optics have been designed with a minimum number of components, consistent with correcting for the spherical aberration induced by the OTA, without introducing coma. The result is a high throughput, but with focal surfaces far from normal to the principal rays. The WFC detector is tilted at 22°
giving an elongation of 8% while the HRC and SBC have a 25°
tilt leading to an elongation of 12%. In each case, the scales in arcseconds per pixel are smaller along the radial direction of the OTA (Optical Telescope Assembly) field of view than along the tangential direction.
Accurate geometric distortion corrections for the WFC and HRC detectors by Anderson & King, Calibration Workshop 2002
, ACS ISR 2004-15
, ACS ISR 2006-01
were derived from observations of the globular cluster 47 Tuc, with multiple pointings and orientations, and through the F475W filter. The geometric distortion models for each of the WFC chips and the HRC detector are expressed in a 4th order polynomial and filter dependent look-up tables. The solution for both cameras is accurate to 0.01 pixels. The coefficients of the 4th order polynomial in the filter dependent look-up tables as well as correction images are installed in the ACS on-the-fly re-calibration (OTFR) pipeline and could be used independently in IRAF task CALACS.
The rhombus shape of the WFC is evident in Figure 7.9
. The angle between the X and Y axes is 84.9°
for WFC1 and 86.1°
for WFC2. The geometric distortion map for WFC1 and WFC2 is illustrated in Figure 10.127
. A vector diagram shows the contribution of the non-linear part of a quadratic fit only. The size of the residuals are scaled by a factor of 5 relative to the sky coordinates and could reach the residuals at about 4.1 arcseconds or 82 ACS/WFC pixels. At the center of chip WFC1, the scale in the X direction is 0.0493 arcseconds per pixel, and 0.0486 arcseconds per pixel in the Y direction. In the case of WFC2, the scale is 0.0498 arcseconds per pixel in the X direction, and 0.0503 arcseconds per pixel in the Y direction. Between the corner of WFC nearest to the V1 axis and the diagonally opposite corner, the scale increases by 10%. Therefore, WFC1 forms a slightly distorted rectangle 201 by 100 arcseconds in size, while WFC2 is 203 by 103 arcseconds. There is a 2.5 arcsecond gap between the two chips.
The skew of the distortion of the WFC has been shown to change slowly over time (ACS ISR 2007-08
). The best estimate of the time-dependence of this skew term has been incorporated into the geometric distortion coefficients used by MultiDrizzle
and its replacement software package AstroDrizzle
. This solution is well-tested in pre-SM4 data. For this time period, typical relative position errors across the entire FOV of the ACS WFC are of order 0.05 pixels, though errors up to 0.1 pixels have been observed. It was discovered that whatever caused the time dependent drift in the geometric solution skew term ceased when ACS was switched off during failure. The time dependent terms have been monitored post-SM4 and seem to follow the pre-SM4 slope when accounting for the ACS dead time. Revisions to the solution have been made to accommodate the ACS dead time.
The High Resolution Channel has its edges aligned approximately along the V2 and V3 axes. In this case, the center of the aperture lies on a line passing through the V2-V3 origin and making an angle of 22°
with the V3 axis. The diagonal of the aperture does not correspond to a radius of the HST
field of view, so the distortion has no particular symmetry with respect to the detector axes. The focal plane of HRC is also 25°
away from the plane normal to the light path, hence the scales along the axes differ by 14%. The full field of view of the HRC is less than 30 arcseconds, therefore the scale variation over the field is much less than for the WFC, about 1%. At the center, the X and Y scales are 0.0284 and 0.0248 arcseconds/pixel respectively. The average scales across the middle of the detector are 0.02842 and 0.02485 arcseconds/pixel, making the X and Y widths 29.1 and 25.4 arcseconds. The slightly non-square projected aperture shape is evident in Figure 7.8
. The angle between the X and Y axes on the sky is 84.2°
. The geometric distortion map for HRC is given in Figure 10.129
, where the residuals from the non-linearity are scaled by a factor of 10.
The map of the effective pixel areas of the SBC is shown in Figure 10.132
. Because the pixel area map is normalized to square pixels which are 0.025 arcseconds on a side rather than an area equal to that of the central SBC pixel, the pixel area map ranges from about 1.58 to 1.65. (Meurer et al. 2002
).The maximum deviation from the central value is just over 2%.