Proceedings Article | 28 June 2006
E. Serabyn, A. Booth, M. Colavita, S. Crawford, J. Garcia, J. Gathright, M. Hrynevych, C. Koresko, R. Ligon, B. Mennesson, T. Panteleeva, S. Ragland, K. Summers, W. Traub, K. Tsubota, E. Wetherell, P. Wizinowich, J. Woillez
Proc. SPIE. 6268, Advances in Stellar Interferometry
KEYWORDS: Stars, Data modeling, Interferometers, Cameras, Remote sensing, Adaptive optics, Keck Observatory, K band, Nulling interferometry, Visibility
The Keck Interferometer Nuller (KIN) is now largely in place at the Keck Observatory, and functionalities and
performance are increasing with time. The main goal of the KIN is to examine nearby stars for the presence of exozodiacal
emission, but other sources of circumstellar emission, such as disks around young stars, and hot exoplanets are
also potential targets. To observe with the KIN in nulling mode, knowledge of the intrinsic source spectrum is essential,
because of the wide variety of wavelengths involved in the various control loops - the AO system operates at visible
wavelengths, the pointing loops use the J-band, the high-speed fringe tracker operates in the K-band, and the nulling
observations take place in the N-band. Thus, brightness constraints apply at all of these wavelengths. In addition, source
structure plays a role at both K-band and N-band, through the visibility. In this talk, the operation of the KIN is first
briefly described, and then the sensitivity and performance of the KIN is summarized, with the aim of presenting an
overview of the parameter space accessible to the nuller. Finally, some of the initial observations obtained with the KIN
are described.
