Change page style:
NIRI (Near InfraRed Imager and spectrograph) - Gemini North
Capability: 1-5 micron wavelength seeing-limited, Natural Guide Star (NGS) Adaptive Optics (AO), or Laser Guide Star (LGS) AO imaging
NIRI is an near-IR imager/spectrometer operating over the 1 to 5um wavelength regime. The instrument is cryogenic and is cooled by two Leybold closed-cycle cooler units to an IR array operating temperature of around 30-35K. All optical elements inside the NIRI cryostat are cooled and, in general, will reach operating temperatures of around 60 to 80K. Since NIRI is cryogenic, the cryostat is pumped and cryo-cooled to a pressure better than 10^-5 torr.
Professional and Educational Tours
The repair of the Gemini North laser system is proceeding but insufficient progress has been made to offer the laser this month. Because all but one NIFS program requires the laser, this also means we will not be doing the NIFS/NIRI swap this month, as previously planned. NIRI will remain on the telescope and NIFS will not be available. We remain optimistic that we will be on-line for the planned February NIFS+LGS run. Updates will be posted.
Natural Seeing (Non-Adaptive Optics) Guided Observations:
NIRI standalone (i.e., without AO) requires the use of a peripheral wavefront sensor for both imaging and spectroscopy. PWFS2 is preferred over PWFS1, as it can be used on fainter guide stars, can run at a higher frequency for a given guide star, works better under windy and cloudy conditions, and is smaller and thus vignettes less of the field of view.
f/6 imaging: PWFS2 guide star should be located >5' from the target
The Gemini North laser system has developed a hardware fault. We are working on a repair which is proceeding quite well but the final prognosis is still not known. January's NIFS+LGS run is delayed and shortened, and may even have to be cancelled. We are optimistic that we will be on-line for the planned February NIFS+LGS run. Updates will be posted.
Gemini composite image of the field around FRB 121102 (indicated). The dwarf host galaxy was imaged, and spectroscopy performed, using the Gemini Multi-Object Spectrograph (GMOS) on the Gemini North telescope on Maunakea in Hawai'i. Data was obtained on October 24-25 and November 2, 2016. Image Credit: Gemini Observatory/AURA/NSF/NRC.
The FLAMINGOS-2 team strongly recommends that PIs read this section and also that they start from the automatically-generated OT templates for FLAMINGOS-2 OT library when preparing F2 observations. The library contains detailed instructions for customising the template observations: changing targets, standard stars, slit widths, etc. This web page is intended to explain the various OT components in depth:
Observations with the TEXES instrument are taken somewhat differently than those of the regular Gemini instruments. The OT setup for TEXES observations are relatively simple and are used only for two purposes: first, they define the target and the guide star; second, they indicate various basic items of the TEXES configuration (cross-disperser, total requested length of the observation, slit orientation, and central wavelength).
This page guides you through the main steps and considerations for configuring TEXES observations in the Observing Tool: