Sigma QUick Infrared Camera User Manual

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 1 WIYN High-Resolution Infrared Camera (WHIRC) Quick Guide to Data Reduction Dick Joyce Ver

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 10 1. Sky flats are best generated from a series of observations which give an appreciable (s

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 11 2.6, 2.7). The smooth variation evident in a cut through one of the dimples (Fig. 2.7) woul

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 12 and use imreplace to set the pixels deviating from what should be a narrow distribution to t

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 13 2.4.1.4 Photo-emitting Defects Photo-emitting defects (PEDs) are generally pixels which bec

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 14 Using gauss with sigma=31 gave a similar result; observers may want to try both of these str

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 15 tapers to near zero at the edges. One can then copy the central 800 × 800 region into the z

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 16 Fig. 2.14: Dome flat for Ks before (left panel) and after (right panel) removal of bad pi

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 17 4. Set pixels below a certain value (say 0.05) to 1.0 to avoid excessively large numbers in

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 18 Because the strength of the OH lines varies during the night, fringes may not be seen in the

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 19 Figure 2.15: IRAF parameter list for the task imcombine to obtain a sky image for the set

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 2 ACRONYMS AND ABBREVIATIONS: ...

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 20 Figure 2.16: Average of sky images in the Paβ filter (left panel), showing evident fringe

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 21 For comparison, we show in Fig. 2.19 fringe templates for the Paβ45 and H filters, to show

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 22 5. Using the appropriate fringe template, the task rmfringe can then be used to remove the

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 23 3.0 Data Reduction 3.1 Standards or Pointlike Objects 1. One will generally have severa

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 24 5. One may analyze the results from each image separately or combine them, using upsqiid o

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 25 During the design of WHIRC, the entire optical system (WIYN telescope, WTTM, and WHIRC) was

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 26 Figure 3.1: Parameter file for the geotran task. 3.3.2 Small Field Mosaics The two bas

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 27 1. Reduce the images to be mosaicked (sky subtraction, flatfielding, etc.) as above and put

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 28 Figure 3.2: Parameter set for the task xyget without distortion correction. The paramete

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 29 Figure 3.3: Parameter set for the task xyget with distortion correction. The parameter

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 3 WIYN High-Resolution Infrared Camera (WHIRC) Data Reduction Guide 1.0 Introduction This do

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 30 3.3.2.2 Combining Images with nircombine The task nircombine (Figure 3.5) will combine the

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 31 b. The parameter ‘infofile’ is the ‘<list>.xycom’ output file from xyget. c. The par

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 32 filtering algorithm. (lower left) Difference of the top two images. Note that the sky sub

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 33 nearby sparse field with a median filtering algorithm. (lower left) Difference of the top

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 34 and that the data be taken in a regular N × M mosaic pattern. The process is a bit cumberso

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 35 just to make the separation of the input images in the output mosaic obvious (Figure 3.10).

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 36 Figure 3.11: Parameter file for the IRAF task irmatch2d. Figure 3.12: Aligned image

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 37 4.0 Appendices 4.1 Appendix A – Observational Test of Pupil Ghost Removal On the (appare

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 38 The sky subtracted images were flattened with both the uncorrected and nopupil flats, yieldi

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 39 Figure 4.1: Plots of the magnitude of a Ks ~ 11 star measured in a 4 arcsec aperture usin

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 4 obtained within a fairly narrow time window. We strongly suggest that observers who generate

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 40 Figure 4.2: The pupil-corrected flattened data from the lower panel of Fig. 4.1, but plott

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 5 2. Scaling: If any of the data were taken with Fowler-4 mode, the pixel values must be norm

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 6 correctly displayed on the image display. ROTOFF is normally 0.0, but at some telescope orie

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 7 2.2 Generating Dome Flats It is generally a good idea to run imstat on the flats just to id

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 8 Figure 2.3: IRAF parameter listing for the imcombine task to combine flatfield images (in

WHIRC Data Reduction Manual Version 2.0, 2014 June 26 9 Figure 2.4: Normalized flat for Ks (left panel) and J (right panel). The significant dif