E Instrument Recipe Notes

This appendix summarises the modifications of instrument-specific variants of the recipes, and the restricted availability of certain recipes by instrument.

E.1 Classic Cam

There is no recipe name in the headers, therefore recipes must be supplied on the command line or the data’s FITS headers edited. See Section 5 for instructions.

Actual testing has been performed on the core recipes JITTER_SELF_FLAT(_APHOT),
BRIGHT_POINT_SOURCE(_APHOT), REDUCE_DARK. Other near infra-red plain-imaging recipes should work provided the observation pattern matches that expected by the recipe.

Aperture photometry accesses the Persson HST lists.

E.2 INGRID

By default the infrastructure uses information in the headers to assign recipe names to REDUCE_DARK for a dark, and JITTER_SELF_FLAT for jittered target frames. Otherwise it defaults to QUICK_LOOK. Other recipes supplied on the oracdr command line should work provided the observation pattern matches that expected by the recipe.

E.3 IRCAM

ARRAY_TESTS uses eight frames and derives both the STARE and ND_STARE readout noises, which are both filed with the calibration system. The range of acceptable dark current is 0–10 electrons/sec compared with $-$1–$+$1 for UFTI, and the nominal ND_STARE readout noise is 20–50 electrons compared with 8–30 electrons for UFTI. The STARE mode readout noise should be 30–70 electrons to be nominal. The log file goes to $ORAC_DATA_OUT/ircam3_array_tests.log.

E.4 IRIS2

The four EXTENDED_$n\times$$m$ recipes cope with missing offset information and a lower completeness (0.25 from 0.4) for automatic registration, thus a smaller fraction of detected objects need match.

ARRAY_TESTS logs to a different location /inst2_soft/iris2red/logs/array_tests.log at the AAT compared with UFTI at UKIRT. References to NDSTARE are not applicable, and so are absent from the documentation. The observation mode is DRM. The upper limit on the readout noise is 20 electrons compared with 30 electrons for UFTI.

There are JITTER_SELF_FLAT variants with a higher registration completeness (0.5 from 0.4) giving purer registration but may rely on the telescope offsets more often.

For a full list of available recipes see the IRIS2 web page.

E.5 ISAAC

The observation template and sequence names are converted into matching recipes with a default of QUICK_LOOK. Available are: CHOP_SKY_JITTER, JITTER_SELF_FLAT, JITTER_SELF_FLAT_APHOT, NOD_SELF_FLAT_NO_MASK, NOD_SELF_FLAT_NO_MASK_APHOT, POL_JITTER, REDUCE_DARK, and SKY_FLAT_MASKED. Please note that at the time of writing the thermal recipes have yet to be tested with ISAAC data. Polarimetry is not available yet. Other recipes supplied on the oracdr command line should work provided the observation pattern matches that expected by the recipe.

The CHOP_SKY_JITTER recipe has no leading sky frame, so the recipe subtracts the mode of the first sky frame from the first target frame, rather than interpolating between the bracketting sky frames as occurs in the standard version. The sequence of frames can also end on the source.

The spatial distortion correction in the core jitter recipes uses the ATOOLS package in addition to those engines listed in the generic documentation.

Aperture photometry accesses both the UKIRT Faint-standard and Persson HST lists.

E.6 Michelle

DIFFERENCE_STATS, POL_ANGLE_NOD_CHOP, POL_QU_FIRST_NOD_CHOP, and
POL_NOD_CHOP only apply to Michelle.

ARRAY_TESTS calculates and files both an average bias frame and the read noise in the calibration system. There is no logging. Checks are made that appropriate waveforms are selected.

E.7 NACO

The scope of the recipes is similar to that for ISAAC. No attempt has been made to reduce any coronographic data with the standard recipes.

Registration is critical for such small point-spread functions to match well. Therefore the minimum number of contiguous pixels above the threshold to be counted as a fiducial source for automatic registration is increased from 9 to 15, and the percentile detection threshold raised from 98% to 99%. These may need further adjustment as a wider selection of observations are processed. The sky co-ordinates are used to aid registration by default.

Aperture photometry accesses both the UKIRT Faint-standard and Persson HST lists.

E.8 NIRI

Tests with 2004 data are limited to thermal data and REDUCE_DARK recipes.

The prelminaries fudge the WCS headers to give a consistent set

A 3-arcsecond aperture is used by default for the thermal imaging aperture photometry.

E.9 UFTI

The FP family of recipes only applies to UFTI.

The sky counts are validated as part of the initial processing.

E.10 UIST

There is no ARRAY_TESTS recipe. Instead there are DARK_AND_BPM and
MEASURE_READNOISE.

There are JITTER_SELF_FLAT variants with a higher registration completeness (0.5 from 0.4) giving purer registration but may rely on the telescope offsets more often.

Measurement of the full-array statistics avoids the outer 5% border, in order to avoid aberrant pixels which can still bias the clipped mean.

Raw polarimetric data are flipped along the second axis to counter a bug in Polpack computing vector orientations for left-handed co-ordinates.