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IRAC: Dither Patterns


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Jump directly to: Dither Pattern | Dither Strategies | Dither Scales | Dither Characteristics | Dither Tables


Dither Patterns

Dithering performs a number of functions. It allows the identification and removal of small-scale detector defects such as bad pixels, it reduces noise from the effects of pixel-to-pixel errors in the flat field (in fact for large numbers of dithers a flat field can be constructed from the data themselves), and sub-pixel dithering can be used to recover some level of information which would otherwise be lost through undersampling of the array. These considerations drive the optimization of the dither patterns in different ways; there is thus no "ideal" dither pattern. For the standard IRAC dither patterns, we have chosen designs that we think should please most observers most of the time. However, the option always remains for observers to define their own dither patterns using array offsets in cluster mode.

For the full-array mode there are two types of dither patterns available. Five such patterns are fixed patterns, which are performed identically at each mapping position. The cycling pattern is a set of dither positions (also referred to as "points"), a different subset of which is performed at each map grid position.

Different patterns are available in subarray mode, as the angular scales covered by the arrays are quite different. Two fixed patterns are available for this mode. See this page for copies of the actual dither tables themselves.

Dithering Strategies

The dithering strategy adopted for a particular observation will depend on the type of object and the required depth and resolution of the final image. The Reuleaux Triangle patterns were designed with the idea of optimizing the Figure of Merit of Arendt, Fixsen, & Moseley (2000, Astrophysical Journal, 536, 500). They thus sample a wide range of spatial frequencies in a fairly uniform manner, and are well-suited to the Fixsen least-squares flat fielding technique. The 9-point and 16-point patterns were designed to be the optimum size for 1/3 and 1/4 sub-pixel dithering, respectively. The "random 9" pattern is based on a uniform random distribution. The "spiral 16" pattern was designed by R. Arendt to provide a pattern which is both compact and has a good figure of merit for self-calibration.

The cycling patterns are designed for AORs having many mapping/dithering observations, but may also be of more general use. The large and medium patterns are Gaussian distributions (with dithers >128 pixels removed). The small pattern is specifically designed for mapping, where only a few dithers are taken at each map position. It is also based on a Gaussian distribution, but the center is downweighted to decrease the fraction of small dithers in the pattern, and it is truncated at a maximum dither of 11 pixels to ensure that maps with up to 280 arcsec spacing have no holes, even if there is only one dither per map point. All the patterns are constrained to have no pair of dithers closer than three pixels in any run of four consecutive points. To use these patterns, you specify the number of dithers to perform at each map grid position and the starting point in the cycling dither table. You may specify a single dither at each map grid position. This will result in a single observation at each map grid position, but the location of that observation will be slightly shifted from the rectangular grid. Such a "fuzzy" grid should allow a better flat field determination and reduce jail-bar or other pattern noise in the resulting mosaic. The cycling dither table will wrap around once the final (311th) element is reached. For example, selecting a starting point of 310 and three dithers per map, the first grid position will use points 310, 311 and 1 from the table, the second 2, 3 and 4 and so on. This pattern has a 1/2 sub-pixel sampling pattern superposed on it, starting with point 1 and repeating continuously every four points (at point 311, the final cycle is simply truncated early, thus patterns which wrap around the table will miss a sub-pixel dither point).

The five-point Gaussian pattern is a general use pattern suitable for shallow observations where the exact sub-pixel sampling is unimportant. It has a 1/2 sub- pixel pattern, with the 5th point at sub-pixel (1/4,1/4).

The Figures below show the dither patterns at the default (large) scale and the distribution of both the dithers and of the separation between dithers for each scale.

Example of one IRAC dither pattern, at the large scale factor. Click for full-size image

IRAC Dither patterns for the 'large' scale factor.

Example of one IRAC dither pattern. Click for full-size image

Characteristics of the cycling dither patterns, in pixels.

Cosmic ray rejection is greatly facilitated by taking highly-dithered observations. The SSC mosaicking software provides good cosmic ray rejection in cases where each position on the sky is observed with several dithered frames. The SSC mosaicker works well with five or more dithered observations per position on the sky, though will manage some rejection with fewer. It has not been found necessary to take repeated, non-dithered observations at each position in a map or dither pattern to obtain good cosmic ray rejection if dithering is being carried out with sufficient redundancy.

Dither Scales

Each of the IRAC dither patterns is available in three sizes, large (default), medium, and small. For most of the patterns, the scaling of the large, medium, and small patterns is approximately in the ratio 4:2:1. Exceptions are the small cycling pattern, which is about 1/5 of the size of the large cycling pattern and has a lower-weighted inner region to reduce the numbers of small separation dithers, and the 4-point subarray pattern where the scaling is 4:3:1.5. For all the patterns, the sub-pixel dithering is maintained, independent of scale.

The dialog box in Spot for the dither patterns is shown below, which illustrates how the pattern and scale are selected.

IRAC Dither patterns dialog box.

Sub-pixel dithering, combined with the drizzle technique (Fruchter & Hook, 2002, PASP, 114, 144) to reconstruct the images, can improve the sampling of the mosaics that can be obtained from IRAC (or any other) observations. Such strategies have been used for the WFPC2 and NICMOS instruments on the HST for some time (for details see the HST Drizzle Handbook). Dithering is also needed to calibrate intra-pixel sensitivity variations, and needed for programs requiring accurate photometry and astrometry (Anderson & King, PASP, 112, 1360). To be effective, however, accurate pointing and low image distortion are required. The offsetting accuracy of Spitzer is in the range 0.1-0.4 arcsec. This, combined with the image distortion in the IRAC arrays, places a limit of about 1/4 pixel on the sub-sampling that is likely to prove useful in practice. For example, the distortion of the IRAC camera is <1%. Thus for the largest dither patterns, which typically offset up to +/-64 pixels from the starting point, the offsets will be up to +/-0.6 pixels from the nominal values. Thus only in the small scale patterns, where the offsets are less than +/-16 pixels, will the sub-pixel sampling work well, though even on the larger scales some improvement of the images will probably be noticeable.

Dither Characteristics

Dither PatternScaleMax Dither
(Pixels from (0,0))
Median Dither Separation
(pixels)
Sub-Pixel Dither Pattern
Cyclingsmall 1110.51/2 px
medium119531/2 px
large161971/2 px
5-point random
(aka 5-point Gaussian)
small26231/2 px
medium52461/2 px
large105921/2 px
9-point random small16141/3 px
medium34281/3 px
large69591/3 px
12-point Reuleaux small13151/2 px
medium27301/2 px
large55591/2 px
16-point spiral small16121/4 px
medium32231/4 px
large64451/4 px
36-point Reuleaux small17191/4 px
medium34391/4 px
large67781/4 px

Dither Tables

See this page for copies of the actual dither tables.


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This file was last modified on Tue Oct 17 14:32:19 2006.

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