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Testing a New Astronomical Data Reduction Technique on ER CEPHEIUS

Testing a New Astronomical Data Reduction Technique on ER CEPHEIUS. Robert Parish Stephen F. Austin State University Department of Physics and Astronomy Parishrj@titan.sfasu.edu. Different Types of Eclipsing Binaries. Obtaining Data. Variable Star. V(t). Telescope. Obtaining Data.

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Testing a New Astronomical Data Reduction Technique on ER CEPHEIUS

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  1. Testing a New Astronomical Data Reduction Technique on ER CEPHEIUS Robert Parish Stephen F. Austin State University Department of Physics and Astronomy Parishrj@titan.sfasu.edu

  2. Different Types of Eclipsing Binaries

  3. Obtaining Data Variable Star V(t) Telescope

  4. Obtaining Data Variable Star D(t) = A(t)V(t) Telescope

  5. Obtaining Data D(t) = A(t)V(t) D(t) = A(t)V(t)+S(t) Telescope

  6. Obtaining Data D(x,y,t)=F(x,y) [A(t)V(t)+S(t)] Telescope D(x,y,t)=N(x,y) + F(x,y) [A(t)V(t)+S(t)] Noise

  7. Current Technique ND(x,y) F(x,y) D Dp NB(x,y) D(x,y,t)

  8. Current Technique Sky Brightness Variable Star S Dp Comparison Star C

  9. Current Technique – Problems • Obtaining a Proper Flat Field • Sky Flats, Box Flats, “Shirt Flats” • Maintaining CCD temperature Between Dark and Light Frames • Variable System Noise • Incorrect Calibration Procedures

  10. A New Approach • Fix Current Technique Problems by • Eliminating the need for dark, flat and bias frames • Removing user error by automating the calibration process

  11. A New Approach @ time t @ time t+Δt

  12. A New Approach D S C

  13. A New Approach D S C

  14. A New Approach - Derivation D D C C S S

  15. ER CEP. in NGC188

  16. Testing – Check Star

  17. Testing – Variable 3

  18. Visual Band • Published Period1 • P = .30652d • Approximate Period Calculations: • Conventional Method • P = .2857d • New Approach • P = .2860d • Percent Difference • .11% or 25.92seconds

  19. Running Average

  20. Screen Shot of Application

  21. Running Average with Theory

  22. Convergent Solutions • Using Starlight Pro and Excel • Recalculate the solution based on minute changes in chosen parameters • Linear Least Squares formula used to calculate the error between the Average Light Curve and Theoretical Solution • 3D Plots of Parameter 1, Parameter 2, and Error

  23. i = 81° Error = .0406

  24. T1 >100k + T2 Error = .0391

  25. R2 = .328 T2 = 4640K Error = .0380

  26. q = .506 T2 = 4640K Error = .0374

  27. ER Cepheius Starlight Pro Model i = 81° q = .506 R1= .439 T1= 4740K R2 = .328 T2 = 4640K Error = .0334 Animation Created with StarLight Pro http://www.midnightkite.com/binstar.html

  28. References (UPDATE THIS PAGE) 1. X.B. Zhang, “A CCD Photometric Survey of Variable Stars in the Field of NGC188,” Astron. J. 123, pp.1548, 2002. 2.R.M. Branly, “Light Curve Solutions for Eclipsing Binaries in NGC 188,” Astro. Sp. Sci235, pp.149-160, 1996. 3. W.H. Richardson, “Bayesian-based iterative method of image restoration,” J. Opt. Soc. Amer. 62, pp.55-59, 1972. 4. L.B. Lucy, “An iterative technique for the rectification of observed distribution,” Astron. J. 79, pp.745-754, 1974. 5. J.L. Starck, Astronomical Image and Data Analysis, Springer, 2002. 6. R. Wodaski, The New CCD Astronomy, New Astronomy Press, 2002.

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