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Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane

  • Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou

S. Kent et al 2023 The Astronomical Journal 166 .

  • Provider: AAS Journals

Caption: Figure 10.

Amplitude of the two nonaxisymmetric modes in Figure 4 in the distortion model for a set of 210 exposures taken at various ADC settings. The quantity plotted is the residual between the measured coefficient and that predicted by the telescope optical model. Left: E mode. Right: B mode. Turbulence affects the amplitude of the former (rms scatter of 2.4 μm) but not the latter (rms scatter of 0.3 μm).

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