This section describes how to prepare IGRINS-2 observations using the Gemini Observing Tool (OT). Basic information on the OT is available here.
The baseline calibrations for IGRINS-2 include Telluric standards, flatfields, and zenith sky observations. The required Night Basecal Time per observation is automatically calculated by the PIT and already includes the time needed for the standard telluric observations.
The following baseline calibrations are shared by all IGRINS-2 programs observed during a given night. Applicants should not include time for these baseline calibrations in their Phase I proposals:
The 2025A Gemini Observatory Call for Proposals has been released. Proposals are being accepted for observations from 1 February, 2025 to 31 July, 2025. Gemini North and Gemini South are expected to have 165 and 155 nights available for science, respectively. A new version of the Phase I Tool (PIT) has been released to support proposal submissions.
The IGRINS-2 optical system is designed to achieve a broad simultaneous wavelength coverage while maintaining a spectral resolving power of ~45,000. The IGRINS-2 optical layout is shown in Figure 1.
IGRINS-2 uses a silicon immersion echelle grating as the main disperser and volume phase holographic (VPH) gratings as the cross-dispersers. The instrument covers the H and K bands simultaneously in a single exposure.
IGRINS-2 has a single slit with a size of 0.33" x 5".
IGRINS-2 is equipped with a Slit Viewing Camera (SVC), which considerably reduces acquisition times and permits real-time monitoring of the telescope tracking and guiding performance.
The IGRINS-2 Integration Time Calculator for spectroscopy can be used to determine exposure times, S/N ratios, background levels for a wide range of source properties, and observing conditions.
Papers describing aspects of IGRINS-2:
IGRINS-2 is operated in a single, high-resolution spectroscopic mode. This mode provides full wavelength coverage between 1.49-1.80 μm (H-band) and between 1.96-2.46 μm (K-band) region at a spectral resolution of R~45,000. These two spectroscopic channels, composed of two separate detectors (H- and K-bands), are being obtained simultaneously.
IGRINS-2 makes use of a silicon immersion grating as the main disperser and two VPH gratings as cross-dispersers. The resulting resolving power is R~45,000.
The coverages of the different orders in which the light is dispersed are provided below.
The final evaluation of the instrument performance is in the process of being completed. However, the following table provides preliminary estimates for the signal-to-noise ratio for 3,600s (6x600s) integration on a point source in the 70%-ile image quality, 50%-ile cloud cover (clear).
The Phase I Tool (PIT) is the software application used by PIs to submit proposals for observing with IGRINS-2 at the Gemini Telescope, as well as for all other Gemini instruments.
In order to minimize common errors when creating a new IGRINS-2 program, PIs are encouraged to pay particular attention to the following aspects of the Phase I preparation.
IGRINS-2 has a single configuration available for all observations, providing wavelength coverage of 1.49-1.80 micron (H-band) and 1.96-2.46 micron (K-band) with a resolving power of R~45,000.
Gemini 2024B observing programs and schedule have been announced!
Notification emails were sent to successful PIs on Jun 13, 2024. Please check the schedules page for more information.
Note that the latest version of the Observing Tool is required to access and update 2024B programs.
Image: International Gemini Observatory/NOIRLab/NSF/AURA/ M. Rodriguez, T.A. Rector, J. Miller, M. Zamani & D. de Martin
The 2024B Gemini Observing Tool is now available for download. This update is required to access the Gemini Observing Databases.
The Installation Instructions are linked on the Observing Tool web page, and we recommend that everyone download their programs from the databases rather than import from saved XMLs.