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Experiments and Design of a wavelength calibration procedure for MOSFIRE

Experiments and Design of a wavelength calibration procedure for MOSFIRE. CfAO Mainland Internship Program. Principal Investigator: David Guerrero, Cal Poly SLO Research Advisor: Ian McLean, UCLA Research Supervisors: Emily Rice, UCLA Jason Weiss, UCLA August 11, 2006. MOSFIRE.

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Experiments and Design of a wavelength calibration procedure for MOSFIRE

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  1. Experiments and Design of a wavelength calibration procedure for MOSFIRE CfAO Mainland Internship Program Principal Investigator: David Guerrero, Cal Poly SLO Research Advisor: Ian McLean, UCLA Research Supervisors: Emily Rice, UCLA Jason Weiss, UCLA August 11, 2006

  2. MOSFIRE • Large (4,000 lb) cryogenic Multi-Object Spectrometer for the near Infra-Red (~ 0.97-2.45 µm) • $ 12 M project over 4 years. • Being developed for the W.M. Keck Observatory by UCLA, CIT, and UCSC.

  3. Slit Mechanism (CSU) • Based on a prototype developed by the Suisse Center for Electronics and Materials (CSEM) for James Webb Space Telescope. • 46 bars 46 slits • Advantages: • Multi-Object Observation • Reduced Integration time • Increased efficiency • Real-time configurable mask • Disadvantages: • No tilted slits • No more than 1 slit/row • Increased complexity to calibrate

  4. The Big Picture MOSFIRE Proposal Design Testing Shipping Preliminary Design Modeling Fabrication/Assembly Optical Electronic Mechanical Software Calibration Procedure

  5. Analysis of Problem Based on NIRSPEC calibration procedure, assist in modeling MOSFIRE wavelength calibration. • Spatial Calibration • Spectral Calibration OH Lines

  6. Problem Solving Approach • Find a relationship between the different slit configurations and the corresponding position of their spectra on the detector. • Using arc lamps inside the instrument would mean a financial and opto-mechanical challenge. ACHIEVED!

  7. Project as a whole Create an IDL application that calculates the exact position and linear dispersion of spectrum on the detector Investigate Physics involved in the optics system Design a friendly user interface for the input and output of results Develop an IDL code that does the math

  8. Physics Behind Optics System

  9. Basic IDL Code CONSTANTS Blaze angle(B)=22.61˚ Groove density(T)=110.5 l/mm Focal length of Collimator (Fcoll)=1813 mm Focal length of Camera (Fcam)=250 mm Spectrograph angle (Q) =40.0˚ VARIABLES Order (m) = 3,4,5, or 6 Grating Angle (GA) = 42.614˚ or 41.524˚ Field angle (FA) = -180 to180 arcsec Reciprocal Linear Dispersion (RLD)= Ả/mm Central λ= 2*sin(B)*cos(Q/2) m*T RLD = 107*cos(Q-GA) m* Fcam*T

  10. Graphical User Interface (GUI) Input Fields Output Fields

  11. References • Mclean, Ian. “Electronic Imaging in Astronomy Detectors and Instrumentation.” Wiley & Praxis. West Sussex, England, 1997. • “Building IDL Applications” Research Systems, Inc. April, 1998. • “IDL Reference Guide” Vol. 1 & 2. Research Systems, Inc. March, 1997. • www.astro.ucla.edu/~irlab/mosfire/ • http://www2.keck.hawaii.edu/inst/nirspec/manual/nirspec_manual.html • www.gemini.edu • www.stsci.edu • www.answers.com/topic/infrared-astronomy • http://cfao.ucolick.org/

  12. Acknowledgements • Special thanks to Prof. Ian McLean, Emily Rice, Jason Weiss, and all the personnel at the Infra-Red Lab at UCLA for their valuable help during my research experience. • Funding provided through the CfAO a NSFSTC, AST-987683 THANKS!

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