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KOALA: Kilofibre Optical AAT Lenslet Array ngel R. Lpez-Snchez Australian Astronomical Observatory / Macquarie University @El_Lobo_Rayado 2nd SELGIFS School on IFS Data Analysis Madrid Spain 22 November 2016 2nd SELGIFS School

  1. KOALA: Kilofibre Optical AAT Lenslet Array Ángel R. López-Sánchez Australian Astronomical Observatory / Macquarie University @El_Lobo_Rayado 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 November 2016

  2. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez 3.9m Anglo-Australian T elescope at Siding Spring Observatory

  3. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez 3.9m Anglo-Australian T elescope

  4. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez KOALA: The AAT IFU instrument KOALA , the Kilofibre Optical AAT Lenslet Array , is a wide-field, high efficiency, integral field unit (IFU) designed for use with the bench mounted AAOmega spectrograph on the 3.9m AAT. KOALA has 1000 hexagonal lenslets arranged in a rectangular array. The field of view is selectable: 15.3” x 28.3” , with 0.7” spatial sampling 27.4” x 50.6” with 1.25” spatial sampling To achieve this, KOALA uses a telecentric double-lenslet array fed by interchangeable fore-optics. https://www.aao.gov.au/science/instruments/current/koala/overview

  5. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez KOALA: The AAT IFU instrument The IFU is mounted at the f/8 Cassegrain focus and feeds the AAOmega spectrograph via a 31m fibre run. https://www.aao.gov.au/science/instruments/current/koala/overview

  6. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez KOALA: The AAT IFU instrument KOALA benefits from all of the flexibility of the reconfigurable AAOmega spectrograph . The double beam spectrograph provides user selectable wavelength coverage and resolution using a series of movable, interchangeable gratings . A set of low, medium, and high resolution gratings provide R~1000, R~5000 and R ~ 10000 across the range 3300 Å to 9600 Å. Full spectral coverage is possible in a single exposure with the low-resolution gratings. The fibre spectra are recorded onto the 2K x 4K E2V CCDs with light dispersed along the 2K axis (not the 4K axis). Same spectrograph used for 2dF or SAMI observations.

  7. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez https://www.aao.gov.au/science/instruments/current/AAOmega

  8. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez KOALA: The AAT IFU instrument KOALA uses a double microlens array to feed the fibres. Although it is possible to feed a fibre array directly by placing it at the (magnified) focal plane, a microlens array offers 2 significant advantages: 1. A microlens array has close to 100% filling- factor (96% for KOALA), whereas a fibre array has a limited filling factor due to fibre cladding and packing. 2. A microlens array can be used to form a pupil- image on the face of the fibre, and therefore the coupling into the fibre is more efficient because both the pupil image size and the focal ratio can be matched to those required for efficient coupling into the fibre. The KOALA micro lens arrays. The top image shows the SUSS hexagonal lenslets which face the sk, with a 100-micron grid overlaid. The bottom image shows the second, circular lenslet array which faces the fibres.

  9. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez KOALA: The AAT IFU instrument KOALA offers a rectangular field of view with a selectable scale. The 1000 lenslets of the focal plane are laid out in a rectangle of 40 x 25 lenslets , an aspect ratio of 0.54.

  10. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez KOALA: The AAT IFU instrument The field is oriented such that at position angle of 0º, the long axis is east-west. The position angle is measured north-through east .

  11. Raw data obtained by AAOmega using KOALA • Single 30 min exposure of Blue Compact Dwarf Galaxy POX 4 • Blue arm using 580V grating (3650 - 5700 Å) • Wide field: 27.4” x 50.6” with 1.25” spatial sampling

  12. Raw data obtained by AAOmega using KOALA • Single 30 min exposure of Blue Compact Dwarf Galaxy POX 4 • Blue arm using 580V grating (3650 - 5700 Å)

  13. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Reducing AAOmega data: 2dFdr software 2dFdr is the AAO’s generic data reduction package for all of the observatory’s fibre based spectrographs. 2dFdr currently has modes that reduce data for a number of instruments including 2dF, SPIRAL, KOALA and SAMI feeds for AAOmega, 2dF+HERMES, and 6dF on the UK Schmidt. https://www.aao.gov.au/science/software/2dfdr

  14. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Reducing AAOmega data: 2dFdr software 2dFdr is the AAO’s generic data reduction package for all of the observatory’s fibre based spectrographs. 2dFdr currently has modes that reduce data for a number of instruments including 2dF, SPIRAL, KOALA and SAMI feeds for AAOmega, 2dF+HERMES, and 6dF on the UK Schmidt. https://www.aao.gov.au/science/software/2dfdr

  15. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Reducing AAOmega data: 2dFdr software 2dFdr is the AAO’s generic data reduction package for all of the observatory’s fibre based spectrographs. 2dFdr currently has modes that reduce data for a number of instruments including 2dF, SPIRAL, KOALA and SAMI feeds for AAOmega, 2dF+HERMES, and 6dF on the UK Schmidt. https://www.aao.gov.au/science/software/2dfdr

  16. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Reducing AAOmega data: 2dFdr software 2dFdr is the AAO’s generic data reduction package for all of the observatory’s fibre based spectrographs. 2dFdr currently has modes that reduce data for a number of instruments including 2dF, SPIRAL, KOALA and SAMI feeds for AAOmega, 2dF+HERMES, and 6dF on the UK Schmidt. https://www.aao.gov.au/science/software/2dfdr

  17. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Reducing AAOmega data: 2dFdr software Once bias, dark, arc and flat-field frames are obtained, producing the wavelength- calibrated, full reduced frame just takes few minutes (auto-reduction pipeline). Reduced single 30 min blue (580V) frame produced by 2dFdr of POX 4. The resulting fits file has a size of 2048 (spectral axis) x 1000 (spaxels)

  18. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Problem: Avoiding dead spaxels It is recommended to slightly offset the field between individual frames to avoid dead spaxels. This means individual frames can’t be directly combined using 2dFdr…. A Python script that provides offsets between spaxels for a given position angle.

  19. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Solution: Python scripts I’m currently developing new Python scripts that combine and/or mosaic observations of a single source, deal with the spatial rebinning of the data onto a square spatial grid (i.e. cubing), and correct for atmospheric differential refraction. I expect these scripts to be completely functional by Semester 17A .

  20. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Python scripts to get KOALA combined data Combined data for 3 x 1800 s exposures of POX 4 using the 580V grating. The resulting fits file has a size of 2048 (spectral axis) x 1107 (spaxels) . This is still work in progress…

  21. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Python scripts to get KOALA combined data Map of the [O III] 5007 emission in POX 4

  22. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Python scripts to get KOALA combined data Map of the [O III] 5007 emission in POX 4, identifying spaxel 318

  23. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Python scripts to get KOALA combined data Wavelength-calibrated (but not flux-calibrated) of spaxel 318 (POX 4 centre)

  24. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Python scripts to get KOALA combined data Wavelength-calibrated (but not flux-calibrated) of spaxel 318 (POX 4 centre)

  25. 2nd SELGIFS School on IFS Data Analysis – Madrid – Spain – 22 Nov 2016 Ángel R. López-Sánchez Python scripts to get KOALA combined data Wavelength-calibrated (but not flux-calibrated) of spaxel 318 (POX 4 centre)

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