Colavita, M. M. and Serabyn, E. and Millan-Gabet, R. and Koresko, C. D. and Akeson, R. L. and Booth, A. J. and Mennesson, B, P. and Ragland, S. D. and Appleby, E. C. and Berkey, B. C. and Cooper, A. and Crawford, S. L. and Creech-Eakman, M. J. and Dahl, W. and Felizardo, C. and Garcia-Gathright, J. I. and Gathright, J. T. and Herstein, J. S. and Hovland, E. E. and Hrynevych, M. A. and Ligon, E. R. and Medeiros, D. W. and Moore, J. D. and Morrison, D. and Paine, C. G. and Palmer, D. L. and Panteleeva, T. and Smith, B. and Swain, M. R. and Smythe, R. F. and Summers, K. R. and Tsubota, K. and Tyau, C. and Vasisht, G. and Wetherell, E. and Wizinowich, P. L. and Woillez, J. M. (2009) Keck Interferometer Nuller Data Reduction and On-Sky Performance. Publications of the Astronomical Society of the Pacific, 121 (884). pp. 1120-1138. ISSN 0004-6280 http://resolver.caltech.edu/CaltechAUTHORS:20091020-102522322
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We describe the Keck Interferometer nuller theory of operation, data reduction, and on-sky performance, particularly as it applies to the nuller exozodiacal dust key science program that was carried out between 2008 February and 2009 January. We review the nuller implementation, including the detailed phasor processing involved in implementing the null-peak mode used for science data and the sequencing used for science observing. We then describe the Level 1 reduction to convert the instrument telemetry streams to raw null leakages, and the Level 2 reduction to provide calibrated null leakages. The Level 1 reduction uses conservative, primarily linear processing, implemented consistently for science and calibrator stars. The Level 2 processing is more flexible, and uses diameters for the calibrator stars measured contemporaneously with the interferometer’s K-band cophasing system in order to provide the requisite accuracy. Using the key science data set of 462 total scans, we assess the instrument performance for sensitivity and systematic error. At 2.0 Jy we achieve a photometrically-limited null leakage uncertainty of 0.25% rms per 10 minutes of integration time in our broadband channel. From analysis of the Level 2 reductions, we estimate a systematic noise floor for bright stars of ~0.2% rms null leakage uncertainty per observing cluster in the broadband channel. A similar analysis is performed for the narrowband channels. We also provide additional information needed for science reduction, including details on the instrument beam pattern and the basic astrophysical response of the system, and references to the data reduction and modeling tools.
|Additional Information:||© 2009 Astronomical Society of the Pacific. Received 2009 June 13; accepted 2009 August 4; published 2009 September 16. The Keck Interferometer is funded by the National Aeronautics and Space Administration (NASA). Observations presented were obtained at theW. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of theW. M. Keck Foundation. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, and at the NASA Exoplanet Science Institute, California Institute of Technology, under contract with NASA.|
|Official Citation:||Keck Interferometer Nuller Data Reduction and On-Sky Performance M. M. Colavita, E. Serabyn, R. Millan-Gabet, C. D. Koresko, R. L. Akeson, A. J. Booth, B. P. Mennesson, S. D. Ragland, E. C. Appleby, B. C. Berkey, A. Cooper, S. L. Crawford, M. J. Creech-Eakman, W. Dahl, C. Felizardo, J. I. Garcia-Gathright, J. T. Gathright, J. S. Herstein, E. E. Hovland, M. A. Hrynevych, E. R. Ligon, D. W. Medeiros, J. D. Moore, D. Morrison, C. G. Paine, D. L. Palmer, T. Panteleeva, B. Smith, M. R. Swain, R. F. Smythe, K. R. Summers, K. Tsubota, C. Tyau, G. Vasisht, E. Wetherell, P. L. Wizinowich, and J. M. Woillez Publications of the Astronomical Society of the Pacific 2009 121:884, 1120-1138|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||26 Oct 2009 20:07|
|Last Modified:||26 Dec 2012 11:29|
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