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Surveying the Atmospheres of Extrasolar Planets
Surveying the Atmospheres of Extrasolar Planets
In addition to faint-object spectroscopy, MIRMOS is designed for high spectrophotometric-precision spectroscopy of bright targets like TESS stars that host planets.
In addition to faint-object spectroscopy, MIRMOS is designed for high spectrophotometric-precision spectroscopy of bright targets like TESS stars that host planets.
(Right:) Video showing how a diffuser can stabilize the PSF of the telescope allowing for higher prevision observations of bright stars. MIRMOS will be the first spectrograph equipped with a diffuser. (Video Credit: Guðmundur Kári Stefánsson)
MIRMOS's goal for spectrophotometric precision would deliver atmospheric constraints that are competitive with space-based instruments like JWST.
MIRMOS's goal for spectrophotometric precision would deliver atmospheric constraints that are competitive with space-based instruments like JWST.
(Left:) Simulated observations of the transmission spectrum of a a cool Neptune-sized planet from HST, JWST, and MIRMOS. Even if MIRMOS reaches only 150 ppm precision in diffuser-assisted observations (gray points), it will enable secure detection of spectral modulation at levels never before achieved in ground-based spectroscopy.
MIRMOS can observe atmospheres of planets with a wide range of radii and temperatures providing a critical tool for surveying planets for atmospheric signals.
MIRMOS can observe atmospheres of planets with a wide range of radii and temperatures providing a critical tool for surveying planets for atmospheric signals.
(Right:) A forecasted population of exoatmosphere targets that could be discovered with TESS and would be observable with MIRMOS.
Galaxies from Cosmic Noon to Reionization
Galaxies from Cosmic Noon to Reionization
The field of view and high level of multiplexing proposed for MIRMOS are required to trace galaxies in various environments across cosmic time.
The field of view and high level of multiplexing proposed for MIRMOS are required to trace galaxies in various environments across cosmic time.
(Right:) The history of reionization in a simulation from Ocvirk et al. 2018. Time increases to the right, while the vertical axis shows one spatial dimension. Black regions are neutral and blue are ionized. The FOV of MIRMOS is compared to other existing and planned instruments (Finkelstein et al 2019). Only MIRMOS probes the scales of ionized bubbles throughout reionization. And with it's broad wavelength coverage MIRMOS can simultaneously observe Ly-alpha and metal emission lines for galaxies with z>6.3.
The MIRMOS FOV will cover typical size scales of ionized bubbles at z~7 (as shown above) and a few pointings with MIRMOS can cover protoclusters at Cosmic Noon (left).
The MIRMOS FOV will cover typical size scales of ionized bubbles at z~7 (as shown above) and a few pointings with MIRMOS can cover protoclusters at Cosmic Noon (left).
(Left:) An image of a large overdensity assembling during Cosmic Noon compared to the MIRMOS field of view. The image shows a 2D slice in redshift from the 3D tomographic reconstruction of the z~2 Lyman-alpha forrest from the LATIS survey (Newman et al. 2020).
MIRMOS's broad wavelength coverage makes it ideal for studying galaxies at a wide range of redshifts.
MIRMOS's broad wavelength coverage makes it ideal for studying galaxies at a wide range of redshifts.
(Right:) NIR Spectroscopy is required to measure rest-optical emission from HII regions and rest-optical absorption lines from quiescent galaxies at cosmic noon, as well as UV emission lines for reionization-epoch galaxies. These spectral features encode a plethora of physical processes, critical to our understanding of galaxy evolution.
MIRMOS's large FOV and broad wavelength coverage result in a dramatic increase in survey speed making dramatic scientific gains possible.
MIRMOS's large FOV and broad wavelength coverage result in a dramatic increase in survey speed making dramatic scientific gains possible.
(Left:) A proposed 45 night program with Magellan/MIRMOS will result in world-leading surveys for (1) reionization epoch galaxies including simultaneous constrains on Lya and other UV emission lines, (2) typical star-forming galaxies including spectral coverage of all strong optical emission lines and (3) quiescent galaxies with sufficient S/N spectroscopy to characterize stellar absorption features.
Mapping the Kinematics of Circumgalactic Gas
Mapping the Kinematics of Circumgalactic Gas
The MIRMOS IFU will enable 3D mapping of gas within the circumgalactic and circum-QSO medium at 1 < z < 3.
The MIRMOS IFU will enable 3D mapping of gas within the circumgalactic and circum-QSO medium at 1 < z < 3.
MIRMOS will characterize this gas using rest-optical emission lines. Because optical emission lines are optically thin (unlike UV resonance lines), this emission traces the kinematics of the gas, providing unparalleled data on cosmic gas flows. Further, this emission will help to constrain the mass within the CGM/CQM as well as the processes which create this emission and that seen in the rest-UV. (Right:) The MIRMOS IFU FOV (black rectangle) is overlaid on pioneering optical IFU observations of two low-redshift circumgalactic nebulae (Chen et al. 19 and Johnson et al 2018). MIRMOS will detect and resolve emission nebulae like this at redshifts 1-3 for the first time.
Characterizing Sources from Wide-Field Surveys
Characterizing Sources from Wide-Field Surveys
MIRMOS will be the most powerful NIR follow-up facility for newly-discovered sources from the Rubin Observatory, SPT-3G, WFIRST, etc. due to its broad wavelength coverage, IFU capability, and southern location.
MIRMOS will be the most powerful NIR follow-up facility for newly-discovered sources from the Rubin Observatory, SPT-3G, WFIRST, etc. due to its broad wavelength coverage, IFU capability, and southern location.
(Left:) An example of a potential strong lens system from More et al 2012 with half of the MIRMOS IFU FOV overlaid. Possible spectra of a candidate lensed galaxy at various possible redshifts are shown with realistic noise for a 15 minute MIRMOS observation. The broad bandpass ensures the presence of multiple detectable emission lines for 1 < z < 3 sources within a short exposure.
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