We report the results on the EMIR1 (Espectrógrafo Multiobjeto Infra-Rojo) performances after the commissioning period of the instrument at the Gran Telescopio Canarias (GTC). 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. 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). After an extensive and intensive period of system verification at the IAC, EMIR was shipped to the GTC on May 2016 for its integration at the Nasmyth platform. Once in the observatory, several tests were conducted to ensure the functionality of EMIR at the telescope, in particular that of the ECS (EMIR Control System) which has to be fully embedded into the GCS (GTC Control System) so as to become an integral part of it. During the commissioning, the main capabilities of EMIR and its combined operation with the GTC are tested and the ECS are modified to its final form. This contribution reports on the details of the EMIR operation at the GTC obtained so far, on the first commissioning period.
EMIR (Espectrógrafo Multiobjeto Infrarrojo) is a wide-field, near-infrared, multi-object spectrograph, with image
capabilities, which will be located at the Nasmyth focus of GTC (Gran Telescopio Canarias). It will allow observers to
obtain many intermediate resolution spectra simultaneously, in the nIR bands Z, J, H, K. A multi-slit mask unit will be
used for target acquisition.
This paper shows an overview of EMIR Data Factory System which main functionality is to receive raw images from
DAS (Data Acquisition system), collect FITS header keywords, store images to database and propagate images to other
GCS (GTC Control System) components to produce astronomical data. This system follows the standards defined by the
telescope to permit the integration of this software on the GCS. The Data Factory System needs the DAS, the Sequencer,
GUI and the Monitor Manager subsystems to operate. DAS generates images and sends them to the Data Factory.
Sequencer and GUI (Graphical User Interface) provide information about instrument and observing program. The
Monitor Manager supplies information about telescope and instrument state.
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,
EMIR is the NIR imager and multiobject spectrograph being built as a common user instrument for the GTC and it is
currently entering in the integration and verification phase at system level. EMIR is being built by a Consortium of
Spanish and French institutes led by the IAC.
In this paper we describe the readout modes of EMIR detector, a Hawaii2 FPA, after two full calibrations campaigns.
Besides the standard set of modes (reset-read, CDS, Fowler, Follow-up the ramp), the modified SDSU-III hardware and
home made software will also offer high dynamic range readout modes, which will improve the ability of the instrument
to sound densely populated areas which often are made of objects with large differences in brightness. These new high
dynamic range modes are: single readout with very short integration time, window mode and combination of both. The
results show that the new modes behave linearly with different exposition times, improve the maximum frame rate and
increase the saturation limit in image mode for EMIR instrument.
We describe the on-board electronics chain and the on-ground data processing pipeline that will operate on data from the
Herschel-SPIRE photometer to produce calibrated astronomical products. Data from the three photometer arrays will be
conditioned and digitised by on-board electronics and sent to the ground with no further on-board data processing. On
the ground, the data pipeline will process the data from point source, jiggle-map, and scan-map observations in a fully
automatic manner, producing measured flux densities (for point source observations) or maps. It includes calculation of
the bolometer voltages from the raw telemetry, glitch removal, and corrections for various effects including time
constants associated with the detectors and electronics, electrical and optical crosstalk, detector temperature drifts, flatfielding,
and non-linear response of the bolometers to strong sources. Flux density calibration will be with respect to
standard astronomical sources with the planets Uranus and Neptune being adopted as the baseline primary standards.
The pipeline will compute estimated values of in-beam flux density for a standard flat νS(ν) source spectrum.