1. 1 Calibration Screen Development Claire Cramer Brian Stalder Gautham Narayan Christopher Stubbs Department of Physics Harvard University Claire Cramer Brian Stalder Gautham Narayan Christopher Stubbs Department of Physics Harvard University Keith Lykke Steve Brown Allan Smith NIST John Tonry Jeff Morgan Ken Chambers PanSTARRS Keith Lykke Steve Brown Allan Smith NIST John Tonry Jeff Morgan Ken Chambers PanSTARRS

2. 2OverviewOverview ObjectivesObjectives StatusStatus ChallengesChallenges PlansPlans ObjectivesObjectives StatusStatus ChallengesChallenges PlansPlans

3. 3ObjectivesObjectives We hope to achieve unprecedented precision in LSST photometry.We hope to achieve unprecedented precision in LSST photometry. This requires knowingThis requires knowing Relative sensitivity of apparatus vs. wavelength Transmission of atmosphere. Our plan is to use a NIST-calibrated photodiode as the primary flux sensitivity reference.Our plan is to use a NIST-calibrated photodiode as the primary flux sensitivity reference. We will use full-aperture illumination of the system to map out each pixel’s response vs. wavelength, for each LSST filter.We will use full-aperture illumination of the system to map out each pixel’s response vs. wavelength, for each LSST filter. (Measurement of atmospheric transmission is a distinct issue, for a later conversation)(Measurement of atmospheric transmission is a distinct issue, for a later conversation) We hope to achieve unprecedented precision in LSST photometry.We hope to achieve unprecedented precision in LSST photometry. This requires knowingThis requires knowing Relative sensitivity of apparatus vs. wavelength Transmission of atmosphere. Our plan is to use a NIST-calibrated photodiode as the primary flux sensitivity reference.Our plan is to use a NIST-calibrated photodiode as the primary flux sensitivity reference. We will use full-aperture illumination of the system to map out each pixel’s response vs. wavelength, for each LSST filter.We will use full-aperture illumination of the system to map out each pixel’s response vs. wavelength, for each LSST filter. (Measurement of atmospheric transmission is a distinct issue, for a later conversation)(Measurement of atmospheric transmission is a distinct issue, for a later conversation)

4. 4 Detectors are better characterized than any celestial source!  nm QE Spectrum of Vega NIST photodiode QE

5. 5 Basic Concept Back-illuminated diffuser Monitoring photodiode LSST aperture focal plane

6. 6 Demonstration of the concept at CTIO Measured full system transmission using a tunable laser and NIST diode.Measured full system transmission using a tunable laser and NIST diode. This was not a permanent installation.This was not a permanent installation. Measured full system transmission using a tunable laser and NIST diode.Measured full system transmission using a tunable laser and NIST diode. This was not a permanent installation.This was not a permanent installation.

7. 7 Tunable laser (400 nm - 2 microns) from Opotek Second harmonic (532 nm) generator Mixer (to 355 nm) 1.064 micron NdYAG pulsed pump laser Tunable downconverter Second harmonic (532 nm) generator Mixer (to 355 nm) 1.064 micron NdYAG pulsed pump laser Tunable downconverter

8. 8

9. 9 A/D converter module Photdiode preamp USB extender Integrator electronics Calibrated photodiode Beam launch optics Optical Fiber

10. 10 Preliminary results from this approach Relative system response vs. wavelength for CTIO Mosaic imager 100 x 100 pixel block average Multiple points at 800 nm show repeatability of 0.4% Relative system response vs. wavelength for CTIO Mosaic imager 100 x 100 pixel block average Multiple points at 800 nm show repeatability of 0.4%, nm, nm T

11. 11 Actual data from CTIO R Band Colored Glass Filter System throughput Filtered/blank=filter only, nm, nm

12. 12 950 nm

13. 13 960 nm

14. 14 970 nm

15. 15 980 nm

16. 16 990 nm

17. 17 1000 nm

18. 18 1010 nm

19. 19 1020 nm

20. 20 Position Dependence in Response 780 nm 890 nm 780 nm 890 nm

21. 21 This approach requires 1.Photodiode monitor & circuit 2.Tunable light source with adequate intensity 3.Uniform radiance screen, to ~10%. An adjustable source of illumination across the screen would be nice! 4.Calibration pipeline that exploits these data. 5.Dark dome (or at least uniform illumination) 1.Photodiode monitor & circuit 2.Tunable light source with adequate intensity 3.Uniform radiance screen, to ~10%. An adjustable source of illumination across the screen would be nice! 4.Calibration pipeline that exploits these data. 5.Dark dome (or at least uniform illumination)

22. 22

23. 23 We are building a DLP-driven flatfield screen Hacked DLP digital projector, optical fiber Transmissive screen Diverging mirrors Tunable source We can currently generate a 2m dia spot in ~26 inches depth I expect we can fill LSST screen uniformly with 2m depth

24. 24 Transferring uniform radiance Flat, by def. Non-uniform Iteratively flattened reciprocal

25. 25ChallengesChallenges We can add a collimator, to restrict angles of emission to the FOV of camera, but then uniformity measurement is difficult.We can add a collimator, to restrict angles of emission to the FOV of camera, but then uniformity measurement is difficult. Need optimized optical surfaces for reflectors to project decent spot in minimal standoff distance.Need optimized optical surfaces for reflectors to project decent spot in minimal standoff distance. Tunable light sources below 400nm are difficult.Tunable light sources below 400nm are difficult. Don’t yet know requisite cadence of filter transmission measurements.Don’t yet know requisite cadence of filter transmission measurements. Plan to ship v1.0 to PanSTARRS in May.Plan to ship v1.0 to PanSTARRS in May. We can add a collimator, to restrict angles of emission to the FOV of camera, but then uniformity measurement is difficult.We can add a collimator, to restrict angles of emission to the FOV of camera, but then uniformity measurement is difficult. Need optimized optical surfaces for reflectors to project decent spot in minimal standoff distance.Need optimized optical surfaces for reflectors to project decent spot in minimal standoff distance. Tunable light sources below 400nm are difficult.Tunable light sources below 400nm are difficult. Don’t yet know requisite cadence of filter transmission measurements.Don’t yet know requisite cadence of filter transmission measurements. Plan to ship v1.0 to PanSTARRS in May.Plan to ship v1.0 to PanSTARRS in May.

26. 26 Selected References Stubbs & Tonry “Toward 1% Photometry: End-to-End Calibration of Astronomical Telescopes and Detectors”Stubbs & Tonry “Toward 1% Photometry: End-to-End Calibration of Astronomical Telescopes and Detectors” ApJ 646, 1436 (2006) Stubbs et al. “Preliminary Results from Detector-Based Throughput Calibration of the CTIO Mosaic Imager and Blanco Telescope Using a Tunable Laser” astro-ph/0609260 (2006)Stubbs et al. “Preliminary Results from Detector-Based Throughput Calibration of the CTIO Mosaic Imager and Blanco Telescope Using a Tunable Laser” astro-ph/0609260 (2006) Stubbs et al, “Toward More Precise Survey Photometry for PanSTARRS and LSST: Measuring Directly the Optical Transmission Spectrum of the Atmosphere” PASP 119, 1163 (2007)Stubbs et al, “Toward More Precise Survey Photometry for PanSTARRS and LSST: Measuring Directly the Optical Transmission Spectrum of the Atmosphere” PASP 119, 1163 (2007) Technical Memo on Screen Design Considerations. C. Stubbs Dev 2007.Technical Memo on Screen Design Considerations. C. Stubbs Dev 2007. Stubbs & Tonry “Toward 1% Photometry: End-to-End Calibration of Astronomical Telescopes and Detectors”Stubbs & Tonry “Toward 1% Photometry: End-to-End Calibration of Astronomical Telescopes and Detectors” ApJ 646, 1436 (2006) Stubbs et al. “Preliminary Results from Detector-Based Throughput Calibration of the CTIO Mosaic Imager and Blanco Telescope Using a Tunable Laser” astro-ph/0609260 (2006)Stubbs et al. “Preliminary Results from Detector-Based Throughput Calibration of the CTIO Mosaic Imager and Blanco Telescope Using a Tunable Laser” astro-ph/0609260 (2006) Stubbs et al, “Toward More Precise Survey Photometry for PanSTARRS and LSST: Measuring Directly the Optical Transmission Spectrum of the Atmosphere” PASP 119, 1163 (2007)Stubbs et al, “Toward More Precise Survey Photometry for PanSTARRS and LSST: Measuring Directly the Optical Transmission Spectrum of the Atmosphere” PASP 119, 1163 (2007) Technical Memo on Screen Design Considerations. C. Stubbs Dev 2007.Technical Memo on Screen Design Considerations. C. Stubbs Dev 2007.