Figure 13 from NULLING DATA REDUCTION AND ON-SKY PERFORMANCE OF THE LARGE BINOCULAR TELESCOPE INTERFEROMETER

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NULLING DATA REDUCTION AND ON-SKY PERFORMANCE OF THE LARGE BINOCULAR TELESCOPE INTERFEROMETER

Authors: D. Defrère, P. M. Hinz, B. Mennesson, W. F. Hoffmann, R. Millan-Gabet, A. J. Skemer, V. Bailey, W. C. Danchi, E. C. Downey, O. Durney, P. Grenz, J. M. Hill, T. J. McMahon, M. Montoya, E. Spalding, A. Vaz, O. Absil, P. Arbo, H. Bailey, G. Brusa, G. Bryden, S. Esposito, A. Gaspar, C. A. Haniff, G. M. Kennedy, J. M. Leisenring, L. Marion, M. Nowak, E. Pinna, K. Powell, A. Puglisi, G. Rieke, A. Roberge, E. Serabyn, R. Sosa, K. Stapeldfeldt, K. Su, A. J. Weinberger, and M. C. Wyatt

2016 The Astrophysical Journal 824 66.

Provider: AAS Journals

Caption: Figure 13.

Measured photometric sensitivity for various representative nights of the commissioning phase (same notation as in Figure 10). The solid line shows the theoretical sensitivity for readout noise only (i.e., 400 e−/pixel, Hoffmann et al. 2014), while the gray shaded area shows the sensitivity for readout noise and background noise (assuming a thermal background flux in the range of 1–2 Jy pixel⁻¹). The vertical dashed line indicates the integration time for which the background noise dominates the readout noise (assuming a thermal background level of 1.5 Jy pixel⁻¹).

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