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MIRMOS has a large field of view (13’ x 3’) in multi-object mode with 92 configurable slits
MIRMOS has a large field of view (13’ x 3’) in multi-object mode with 92 configurable slits
(Left): The MIRMOS field of view in Y, J, H, and K bands compared to the size of the moon.
Magellan/MIRMOS is 5x faster than any existing infrared spectrograph for multiband surveys
Magellan/MIRMOS is 5x faster than any existing infrared spectrograph for multiband surveys
(Right:) A comparison of the information grasp of MIRMOS to other existing and planned IR spectrographs.
The MIRMOS IFU with its large field of view (26” x 20”) will provide a completely unique facility worldwide.
The MIRMOS IFU with its large field of view (26” x 20”) will provide a completely unique facility worldwide.
(Left): The field of view of the MIRMOS IFU compared to other current and forthcoming NIR IFUs on large telescopes.
A dichroic tree splits light into four spectroscopic channels, providing simultaneous spectroscopy across the full near-infrared spectrum.
A dichroic tree splits light into four spectroscopic channels, providing simultaneous spectroscopy across the full near-infrared spectrum.
(Right:) A solid model of MIRMOS. Light enters through the corrector on the left, passes through the CSU, is collomated, hits the dichroic tree, and ends in one of four spectroscopic channels or in the through slit imager.
An I-band imaging channel will be used for mask alignment and to constrain clouds/hazes in exoplanet atmospheres.
An I-band imaging channel will be used for mask alignment and to constrain clouds/hazes in exoplanet atmospheres.
(Left:) A ray diagram showing the 4 spectrograph channels along with the through slit I-band imager which sits below the four spectoscopic cameras.
MIRMOS uses low-scatter VPH gratings to minimize contributions to the interline background and employs ultra-fast (f /1.5) cameras to reach the background limit quickly.
MIRMOS uses low-scatter VPH gratings to minimize contributions to the interline background and employs ultra-fast (f /1.5) cameras to reach the background limit quickly.
(Right:) A solid model of one of the spectroscopic f/1.5 cameras.
A large configurable slit unit to be designed and fabricated by CSEM, who also designed and fabricated the slit unit for MOSFIRE.
A large configurable slit unit to be designed and fabricated by CSEM, who also designed and fabricated the slit unit for MOSFIRE.
(Left:) A view of the mechanical bars which will form the MIRMOS slits. (Image Credit: CSEM)
Wide-field (26”x20”) integral-field spectroscopy will be enabled by an image slicer which slides in and out of the field of view.
Wide-field (26”x20”) integral-field spectroscopy will be enabled by an image slicer which slides in and out of the field of view.
(Left:) A 3D rendering of the light path for the slicer and reformatting optics.
An insertable diffuser will enable spectrophotometry that approaches the photon noise limit for high-precision observations of the atmospheres of extrasolar planets.
An insertable diffuser will enable spectrophotometry that approaches the photon noise limit for high-precision observations of the atmospheres of extrasolar planets.
(Left:) Image from Stefansson et al. 2017 of an optical diffuser installed on the Astrophysical Research Consortium Telescope Imaging Camera (ARCTIC) on the ARC 3.5 m Telescope at Apache Point Observatory.
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