1. Li, Ting Texas A&M University DePoy, Darren Texas A&M University Burke, David SLAC Kessler, Richard University of Chicago Marshall, Jennifer Texas A&M University Wise, Jason Texas A&M University Rheault, J-P Texas A&M University Boada, Steven Texas A&M University Carona, Don Texas A&M University Apr 16, 2011 Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

2. WHY we are building aTmCam? -- Motivation HOW we are going to build it? -- Method WHAT we have done so far? -- Results we will we do next? -- Future Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

3. Instrument Earth’s Atmosphere Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

4. Model the atmospheric transmission spectrum by libRadTran with different amount of precipitable water Hansen & Caimanque, 1975 (PASP) Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

5. Atmospheric Transmission is time, airmass and location dependent. Calibration stars have the different spectra as the program objects, e.g. SNs, Galaxies, etc. Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

6. Kessler DES docdb 5723

7. Kessler DES docdb 5723

8. WHY? Atmospheric transmission spectrum in real-time Reach a sub-1% precision photometry How? What? Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

9. Data Reduction for Spectroscopy = - - Instrument Sensitivity Atmospheric Transmission Raw data Spectrum Obtained from observing standard stars Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

10. Data Reduction for Spectroscopy = - - Observing standard stars = - - Instrument Sensitivity Atmospheric Transmission Raw data Spectrum Instrument Sensitivity Atmospheric Transmission Raw dataSpectrum Obtained from observing standard stars Obtained from Instrument Calibration System Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

11. WHY? Atmospheric transmission spectrum in real-time Reach a sub-1% precision photometry How?  Measure the standard star with a Calibrated Spectrograph? What? Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

12. WHY? Atmospheric transmission spectrum in real-time Reach a sub-1% precision photometry How? Χ Measure the standard star with a Calibrated Spectrograph? Photometry is always easier than spectroscopy! What? Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

13. Molecular/Rayleigh scattering Aerosol scattering Molecular absorption Cloud Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

14. Molecular/Rayleigh scattering Pressure Aerosol scattering Molecular absorption Cloud Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

15. Molecular/Rayleigh scattering Aerosol scattering Aerosol optical depth Molecular absorption Cloud Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

16. Molecular/Rayleigh scattering Aerosol scattering Molecular absorption Oxygen Cloud Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

17. Molecular/Rayleigh scattering Aerosol scattering Molecular absorption Oxygen Ozone Cloud Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

18. Molecular/Rayleigh scattering Aerosol scattering Molecular absorption Oxygen Ozone Water Cloud Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

19. pressureozonewater aerosol Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

20. Ratios from the simulation by libRadTran

21. WHY? Atmospheric transmission spectrum in real-time Reach a sub-1% precision photometry How? Measure the standard star with a Calibrated Spectrograph Multi Narrowband Imager Get the best fit model in the database Robotic, automatic multi-imaging system  aTmCam What? Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

22. WHY? Atmospheric transmission spectrum in real-time Reach a sub-1% precision photometry How? Measure the standard star with a Calibrated Multi Narrowband Imager Get the best fit model in the database Robotic, automatic multi-imaging system  aTmCam What?  Can we replace the spectrograph with imager? Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

23. Prototype aTmCam SBIG Camera Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012 Jaz Spectrograph Wedged Prisms + Narrowband Filters

24. Observing Vega at Texas A&M Observatory Red: Direct measurement from spectrograph Green: Best fit model picked by the ratios from Narrow-band Imager Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

25. Observing Vega at McDonald Observatory Green: Best fit model picked by the measurements from Spectrograph Black: Best fit model picked by the ratios from Narrow-band Imager Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

26. WHY? Atmospheric transmission spectrum in real-time Reach a sub-1% precision photometry How? Measure the standard star with a Calibrated Multi Narrowband Imager Get the best fit model in the database Robotic, automatic multi-imaging system  aTmCam What? We can replace the spectrograph with imager. Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

27. WHY? Atmospheric transmission spectrum in real-time Reach a sub-1% precision photometry How? Measure the standard star with a Calibrated Multi Narrowband Imager Get the best fit model in the database Robotic, automatic multi-imaging system  aTmCam What? We can replace the spectrograph with imager. Do we need to measure the atmospheric throughput at each field of the survey? If not, then how close? Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

28. Temporal or angular parameter of the variation Need to be answered in CTIO with REAL aTmCam 20-30 nights observation at CTIO this fall 3-4 telescopes and cameras Currently working on building a software system on: Target acquisition Simultaneously image taking ISMAIL: Imaging Software for Munnerlyn Astronomical Instrumentation Lab Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

29. Mount Control Panel Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

30. Camera Control Panel Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

31. WHY? Atmospheric transmission spectrum in real-time Reach a sub-1% precision photometry How? Measure the standard star with a Calibrated Multi Narrowband Imager Get the best fit model in the database Robotic, automatic multi-imaging system  aTmCam What? We can replace the spectrograph with imager. We will know whether or not we need to measure the atmospheric throughput at each field of the survey. Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012

32. WHY? Atmospheric transmission spectrum in real-time Reach a sub-1% precision photometry How? Measure the standard star with a Calibrated Multi Narrowband Imager Get the best fit model in the database Robotic, automatic multi-imaging system  aTmCam What? We can replace the spectrograph with imager. We will know whether or not we need to measure the atmospheric throughput at each field of the survey. Calibration & Standardization of Large Surveys & Missions in Astronomy & Astrophysics Conference @ FermiLab, 16-19 April 2012