The TolTEC project: a millimeter wavelength imaging polarimeter (Conference Presentation)

Wilson, Grant; Ade, Peter A. R.; Aretxaga, I.; Austermann, J. E.; Bardin, Joseph C.; Barry, P. S.; Beall, James A.; Berthoud, Marc; Braeley, Alan; Bryan, Sean; Burkott, Alexandra; Bussan, John; Castillo, E.; Chávez, M.; DeNigris, Natalie; Doyle, S.; Eiben, M.; Ferrusca, D.; Fissel, Laura M.; Gao, Jiansong; Gear, Walter Kieran; Gómez, Valentín Bote; Gordon, Sam; Groppi, Chris; Gutermuth, Robert; Kuczarski, Stephen; Hosseini, Mohsen; Offner, Stella S. R.; Pope, Alexandra; Schloerb, F. Peter; Souccar, Kamal; Tang, Yuping; Wallace, Gary; Yun, Min S.; Mauskopf, Philip Daniel; Kelso, Rhys; Knapp, Jacob; Lunde, Emily; Mani, H. S.; Mathewson, Justin; Scannapieco, Evan; Underhill, M. M.; Hubmayr, Johannes; Hughes, D. H.; Montoya, Ivan Rodriguez; Sánchez, David; Velázquez, Miguel; Ventura, S.; Pascale, Enzo; Rowe, S.; Tucker, C.; Novak, Giles; McMahon, Jeff; Simon, Sara M.

doi:10.1117/12.2313347

Cited by 5 publications

(3 citation statements)

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“…46 Others plotted are BLAST-TNG, 47 FIFI+LS (proposed), HIRMES, 48 MAKO, 49,50 NIKA2, 51 OLIMPO, 52 OST-OSS, 53 PACS, 54 SAFARI-p, 55 SAFARI, 56 SCUBA2, 57 SPIRE, 58 SuperSpec, 59 STARFIREp, 46,60 STARFIRE, 61 and TolTEC. 62 In addition to its own scientific program, GEP fills an important role between the detector technology achievable in the next few years and possible future flagships such as OST. Color is used to indicate the CMOS technology node while font size indicates suitability for use in the space radiation environment.…”

Section: Disclosuresmentioning

confidence: 99%

Galaxy Evolution Probe

Glenn

Bradford

Rosolowsky

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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The Galaxy Evolution Probe (GEP) is a concept for a mid-and far-infrared space observatory to measure key properties of large samples of galaxies with large and unbiased surveys. GEP will attempt to achieve zodiacal light and Galactic dust emission photon backgroundlimited observations by utilizing a 6-K, 2.0-m primary mirror and sensitive arrays of kinetic inductance detectors (KIDs). It will have two instrument modules: a 10 to 400 μm hyperspectral imager with spectral resolution R ¼ λ∕Δλ ≥ 8 (GEP-I) and a 24 to 193 μm, R ¼ 200 grating spectrometer (GEP-S). GEP-I surveys will identify star-forming galaxies via their thermal dust emission and simultaneously measure redshifts using polycyclic aromatic hydrocarbon emission lines. Galaxy luminosities derived from star formation and nuclear supermassive black hole accretion will be measured for each source, enabling the cosmic star formation history to be measured to much greater precision than previously possible. Using optically thin far-infrared fine-structure lines, surveys with GEP-S will measure the growth of metallicity in the hearts of galaxies over cosmic time and extraplanar gas will be mapped in spiral galaxies in the local universe to investigate feedback processes. The science case and mission architecture designed to meet the science requirements is described, and the KID and readout electronics state of the art and needed developments are described. This paper supersedes the GEP concept study report cited in it by providing new content, including: a summary of recent mid-infrared KID development, a discussion of microlens array fabrication for mid-infrared KIDs, and additional context for galaxy surveys. The reader interested in more technical details may want to consult the concept study report. © The Authors. Published by SPIE under a Creative Commons Attribution 4.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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Section: Disclosuresmentioning

confidence: 99%

Galaxy Evolution Probe

Glenn

Bradford

Rosolowsky

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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“…We will use the same FPGA-based readout originally developed for the BLAST-TNG instrument 25 and further developed for TIM and other instruments fielding large-format KID arrays. 26…”

Section: Kids Arraysmentioning

confidence: 99%

Upgrading the Field-Imaging Far-Infrared Line Spectrometer for the Stratospheric Observatory for Infrared Astronomy with kinetic inductance detectors: enabling large sample (extragalactic) surveys

Colditz

Looney

Bigiel

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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We present the initial design, performance improvements, and science opportunities for an upgrade to the Field-Imaging Far-Infrared Line Spectrometer (FIFI-LS). FIFI-LS efficiently measures fine structure cooling lines, delivering critical constraints of the interstellar medium and star-forming environments. The Stratospheric Observatory for Infrared Astronomy (SOFIA) provides the only far-infrared (FIR) observational capability in the world, making FIFI-LS a workhorse for FIR lines, combining optimal spectral resolution and a wide velocity range. Its continuous coverage of 51 to 203 μm makes FIFI-LS a versatile tool to investigate a multitude of diagnostic lines within our galaxy and in extragalactic environments. The sensitivity and field of view (FOV) of FIFI-LS are limited by its 90s-era photoconductor arrays. These limits can be overcome by upgrading the instrument using the latest developments in kinetic inductance detectors (KIDs). KIDs provide sensitivity gains in excess of 1.4 and allow larger arrays, enabling an increase in pixel count by an order of magnitude. This increase allows a wider FOV and instantaneous velocity coverage. The upgrade provides gains in point source observation speed by a factor >2 and in mapping speed by a factor >3.5, enabled by the improved sensitivity and pixel count. This upgrade has been proposed to NASA in response to the 2018 SOFIA Next Generation Instrumentation call. © The Authors. Published by SPIE under a Creative Commons Attribution 4.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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“…The project is reviewed more broadly in these proceedings. 1 The optical design of the TolTEC uses mirrors, lenses, and dichroics to simultaneously couple a 4 arcminute diameter field of view onto three single-band focal planes at 150, 220, and 280 GHz. The optical design and detector properties, as well as a data-driven model of the atmospheric emission of the LMT site, inform an instrument sensitivity model we developed to aid in observing planning.…”

Section: Introductionmentioning

confidence: 99%

Optical design of the TolTEC millimeter-wave camera

Bryan

Austermann

Ferrusca

et al. 2018

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX

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TolTEC is a new camera being built for the 50-meter Large Millimeter-wave Telescope (LMT) in Puebla, Mexico to survey distant galaxies and star-forming regions in the Milky Way. The optical design simultaneously couples the field of view onto focal planes at 150, 220, and 280 GHz. The optical design and detector properties, as well as a data-driven model of the atmospheric emission of the LMT site, inform the sensitivity model of the integrated instrument. This model is used to optimize the instrument design, and to calculate the mapping speed as an early forecast of the science reach of the instrument.

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The TolTEC project: a millimeter wavelength imaging polarimeter (Conference Presentation)

Cited by 5 publications

References 0 publications

Galaxy Evolution Probe

Galaxy Evolution Probe

Upgrading the Field-Imaging Far-Infrared Line Spectrometer for the Stratospheric Observatory for Infrared Astronomy with kinetic inductance detectors: enabling large sample (extragalactic) surveys

Optical design of the TolTEC millimeter-wave camera

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