powerful capability will be unique to GIRMOS
as no other 8- to 10-meter-class observatory
has a workhorse MOAO instrument. The primary scientific questions that will
benefit greatly from the multiplexing capa-
bilities of GIRMOS are:
The current design parameters of the instru-
ment concept are given in the table below.
The instrument will also offer simultaneous
imaging capability that is at a slightly lower
resolution compared to the Gemini South
Adaptive Optics Imager (GSAOI). The chosen
design significantly increases the speed of
integral field spectrograph surveys for sci-
ence projects that target areas with high
source densities, such as detailed observa-
tions of distant galaxies. • Low- and high-mass star formation within
the Milky Way
Additionally, GIRMOS will be the first multi-
object infrared integral field spectrograph
to offer a high spectral resolution mode that
enables key science not possible on exist-
ing AO-fed spectrographs, particularly those
relating to the chemodynamics of astro-
nomical objects. This unique combination
of multiplexing integral field spectrographs
with high spatial and spectral resolution will
make GIRMOS the forefront survey instru-
ment for a broad range of topics in astro-
nomical research.
• The search for intermediate-mass black
hole formation in central regions of globu-
lar clusters
• The formation process of the Milky Way’s su-
permassive black hole and its environment
• The nature of optical, infrared, radio, and
gravitational-wave transients
• Relative roles of internal processes and en-
vironment at the peak of galaxy formation
• Galaxies, black holes, and globular cluster
formation processes at “Cosmic Dawn”
• Ultra-high angular resolution studies of
distant galaxies aided by gravitational
lensing
• Relationship between cold gas, star for-
mation, and dynamics in galaxies at high
redshift
GIRMOS will also be a powerful scientific
and technical pathfinder for the Thirty Me-
ter Telescope’s (TMT) Infrared Multi-Object
Telescope Feed
Gemini 8.1-meter MCAO f/33 beam Individual IFS field of view
(arcseconds)
1.06 × 1.06
2.1 × 2.1
4.2 × 4.2
8.4 × 8.4 (all IFS combined)
MOAO Performance > 50% encircled energy within 0.1’’ IFS Spatial Pixel Size (milliarcseconds)
(H and K bands)
25 × 25
50 × 50
100 × 100
100 × 100 (all IFS combined)
Field of Regard 2’ diameter patrol field Spectral Resolution (R) 3,000 or 8,000
Wavelength Range 1.1−2.4 μm (J, H, or K bands) Spectrograph Throughput > 40%
Number of IFSs
4 (with a goal of 8)
Detector
4,096 × 4,096 HAWAI‘I-4RG
for 4 spectral channels
Imager Field of View 100 × 100’’ Imager Plate Scale (milliarcseconds) 25
Imager Wavelength 1.1−2.4 μm (J, H, or K bands)
Range Imager Detector
January 2019 / 2018 Year in Review
4,096 × 4,096 HAWAI‘I-4RG
GeminiFocus
47