Proceedings Article | 8 July 2014
F. Garzón, N. Castro-Rodríguez, M. Insausti, L. López-Martín, Peter Hammersley, M. Barreto, P. Fernández, E. Joven, P. López, A. Mato, H. Moreno, M. Núñez, J. Patrón, J. Rasilla, P. Redondo, J. Rosich, S. Pascual, R. Grange
Proc. SPIE. 9147, Ground-based and Airborne Instrumentation for Astronomy V
KEYWORDS: Infrared sensors, Near infrared, Telescopes, Sensors, Spectroscopy, Imaging spectroscopy, Image filtering, Astronomical imaging, Multiplexers, Molybdenum
EMIR is one of the first common user instruments for the GTC, the 10 meter telescope operating at the Roque de los
Muchachos Observatory (La Palma, Canary Islands, Spain). EMIR is being built by a Consortium of Spanish and French
institutes led by the Instituto de Astrofísica de Canarias (IAC). EMIR is primarily designed to be operated as a MOS in
the K band, but offers a wide range of observing modes, including imaging and spectroscopy, both long slit and
multiobject, in the wavelength range 0.9 to 2.5 μm. This contribution reports on the results achieved so far during the
verification phase at the IAC prior to its shipment to the GTC for being commissioned, which is due by mid 2015. After
a long period of design and fabrication, EMIR finally entered into its integration phase by mid 2013. Soon after this, the
verification phase at the IAC was initiated aimed at configuring and tuning the EMIR functions, mostly the instrument
control system, which includes a sophisticated on line data reduction pipeline, and demonstrating the fulfillment of the
top level requirements. We have designed an ambitious verification plan structured along the three kind of detectors at
hand: the MUX and the engineering and scientific grade arrays. The EMIR subsystems are being integrated as they are
needed for the purposes of the verification plan. In the first stage, using the MUX, the full optical system, but with a
single dispersive element out of the three which form the EMIR suite, the two large wheels mounting the filters and the
pseudo-grisms, plus the detector translation unit holding the MUX, were mounted. This stage was mainly devoted to
learn about the capabilities of the instrument, define different settings for its basic operation modes and test the accuracy,
repeatability and reliability of the mechanisms. In the second stage, using the engineering Hawaii2 FPA, the full set of
pseudo-grisms and band filters are mounted, which means that the instrument is fully assembled except for the cold slit
unit, a robotic reconfigurable multislit mask system capable of forming multislit pattern of 55 different slitlets in the
EMIR focal plane. This paper will briefly describe the principal units and features of the EMIR instrument as the main
results of the verification performed so far are discussed. The development and fabrication of EMIR is funded by
GRANTECAN and the Plan Nacional de Astronomía y Astrofísica (National Plan for Astronomy and Astrophysics,
Spain).
