- Day-one instruments
- Current visitor instruments
- Second generation instruments
- Next generation instruments
A defining aspect of the scientific success of any telescope installation is its ability to deliver cutting-edge data through novel instrumentation. An exciting and extensive instrumentation development program exists for GTC. The telescope can currently host up to two instruments for its Nasmyth foci. Further instruments may be installed in the two folded-Cassegrain foci that are currently being prepared, and ultimately also in the main Cassegrain focus.
In order to maximise the scientific return from the GTC, telescope is prepared to accept visitor instruments as they can bring additional capabilities to the GTC not available with the suite of facility instruments. The procedures for proposing a Visitor Instrument to the GTC, and the rationale for visiting instruments are explained in this document.
Also, of interest for any possible instrument developer, the discussion on the general roules for the distribution of Guaranteed time, both for facility instruments and visitor instruments, are described here.
On this table a summary of present and future GTC instrumentation is given (instruments available for the ongoing semester are highlighted in green).
|0.36 - 1 µm||Common-user instrument.
Operational since 2009.
It will be dismounted at the arrival of GTCAO in mid-2018, and will be moved to main Cassegrain station once available (estimated in mid-2019).
|7.8 x 7.8 arcmin field.
Broad- medium- and narrow-band imaging.
Tunable filter imaging.
Fast photometry capabilities.
Long-slit and multi-object spectroscopy.
Spectral resolutions 300 to 2500.
(later Folded Cass-E)
|8 - 25 µm||Common-user instrument.
Operational from 2012 to 2016.
Decomissioned in April 2016. Back to the telescope in Folded Cass E station by late-2017, sharing this focal station with CIRCE until the arrival of MIRADAS in mid-2019.
|26 x 19 arcsec field.
Imaging and long-slit spectroscopy.
Spectral resolutions 175 to 1300.
Imaging and spectral polarimetry.
|1 - 2.5 µm||Visitor instrument (University of Florida).
Operational since September 2015. It will share this focal station with CanariCam until the arrival of MIRADAS in mid-2019.
|3.4 x 3.4 arcmin field.
Imaging and polarimetry.
Upgradable to spectroscopy.
|1 - 2.5 µm||Common-user instrument.
Installed on May 2016. Operational by the end of 2016.
|6.67 x 6.67 arcmin field (imaging).
4 x 6.67 arcmin field (spectroscopy).
Broad- and narrow-band imaging.
Long-slit and multi-object spectroscopy through configurable cold slits.
Spectral resolution 3500 - 4000.
Fed from OSIRIS
|0.4 - 0.7µm||Visitor instrument currently developed by IAC.||Point-source fiber spectroscopy.
High spectral stability.
Spectral resolution 25000
|0.4 - 1 µm||Common-user instrument.
To be installed in March 2017. Operational by September 2017.
|3.5 x 3.5 arcmin field (MOS mode) and 12.5 x 11.3 arcsec (IFU mode).
Up to 100 objects simultaneous through positionable fibres.
Spectral resolution 6000 to 18700.
|1 - 2.5 µm||Common-user instrument.
To be installed in late-2018. Operational mid-2019.
|Imaging and integral-field spectroscopy.
spectral resolution 1500 to 30000.
Diffraction limited performance in combination with the GTC adaptive optics unit. Imaging (FoV 20x20 or 40x40 arcsec) and integral field spectroscopy (FoV up to 2.6 x 2.4 arcsec)
|1 - 2.5 µm||Common-user instrument.
To be installed in mid-2019. Operational early 2020.
|Up to 12 targets via deployable probe arms, each feeding a 3.7 x 1.2 arcsec field of view.
Multi-object spectroscopy with up to 12 objects.
Spectral resolution 20000.
The first two instruments were delivered to GTC to populate the Nasmyth-A and -B focal stations. The very first instrument for scientific use was OSIRIS, which started operation when the telescope commenced its scientific life, in March 2009. OSIRIS works in the optical wavelength range and can be used for high-quality imaging and longs-slit as well as multi-object spectroscopy. The arrival of GTCAO+FRIDA in late-2018 will occupy the Nasmyth-B focal station and will move OSIRIS to main Cassegrain focus of the telescope.
The second instrument CanariCam came on-line in 2012, after a long period of preparing the telescope for it (in particular the chopping motion of the secondary mirror and achieving getting the primary mirror segments in phase). CanariCam is a thermal infrared camera and spectrograph with polarimetry and coronography capabilities. CanariCam was in operation up to April 2016, when it was removed from the Nasmyth A focus to be placed in one of the folded Cassegrain focal stations later, or share it with another instrument.
These first two instruments have been developed by consortia formed by several research centers. The consortium that developed OSIRIS was led by the Instituto de Astrofísica de Canarias (IAC), with the participation of the IA-UNAM, IFCA and IAA. CanariCam was built by the University of Florida.
Current visitor instruments
In December 2014 we received and installed the first visitor instrument, CIRCE, from the University of Florida. This instrument, designed and built on initiative by Prof. Eikenberry, was commissioned along 2015 and will deliver important near-IR imaging capability to the telescope. The instrument may be upgraded for spectroscopy. Although being formally a visiting instrument, it was made available to the general community since September 2015.
A second visiting instrument, HORS, has been developed at the IAC (PI: Dr. Carlos Allende Prieto) and it will be commissioned along 2016. This instrument will deliver high-resolution spectra of point sources in the optical wavelength range. It is expected to be highly stable, which is of interest for science projects such as studies of extra-solar planets.
Second generation instruments
The next common-user instrument that is being built for the GTC is EMIR, a multi-object spectrograph and imager for the near infrared. With its cryogenic configurable slit unit and medium spectral resolution this instrument is expected to become one of the work-horse instruments. EMIR is being developed by a consortium led by the IAC and will arrive at the telescope in early 2016 for its on-sky commissioning.
FRIDA is another instrument for GTC that is being developed. FRIDA, will make use of the GTC Adaptive Optics system, being able to take pictures in broad-band and narrow-band filters, as well as facilitate integral-field spectroscopy in the spectral range of 0.9 - 2.5 μm. FRIDA is a project led by the Instituto de Astronomía de la Universidad Nacional Autónoma de México (UNAM) in partnership with the Instituto de Astrofísica de Canarias (IAC), the University of Florida (UF), and the Universidad Complutense de Madrid (UCM). The instrument is in its phase of construction and is scheduled to arrive at the telescope in 2018.
Next generation instruments
Development of instrumentation is a long process and hence for its planning one must look several years into the future. In order to help define the progression needed to keep GTC scientifically competitive throughout the decade ahead of the year 2008, an independent panel was tasked with analyzing GTC´s future instrumentation needs. Recommendations provided by this work panel can be found here.
Based on the outcome of this study, it was decided to proceed with the development of two medium-dispersion spectrographs, one in the visible range and another in the near infrared, to be implemented in the telescope around the middle of the next decade (2015/2016).
After a competitive process, in late 2010 the MEGARA and
Currently MEGARA has successfully completed the review of its final design and is progressing at full steam its construction phase. Current schedule shows the installation of MEGARA in the GTC by March 2017.
MIRADAS has successfully completed the review of its preliminary design and is nearly to complete its final design. Its construction phase will be initiated after the successful review of its final design. Current schedule shows the installation of MIRADAS in the GTC at mid-2019.
Last modified: 02 December 2016