Full-Array Noise Performance of Deployment-Grade SuperSpec mm-Wave On-Chip Spectrometers

Karkare, K. S.; Barry, P. S.; Bradford, C. M.; Chapman, Scott; Doyle, S.; Glenn, J.; Gordon, Sam; Hailey-Dunsheath, S.; Janssen, R. M. J.; Kovács, A.; Leduc, H. G.; Mauskopf, Philip Daniel; McGeehan, Ryan; Redford, J.; Shirokoff, E.; Tucker, C.; Wheeler, Jordan; Žmuidzinas, J.

doi:10.1007/s10909-020-02407-4

Cited by 33 publications

(29 citation statements)

References 15 publications

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“…So far, we have outlined the rich and diverse science enabled by TIME, a first-generation [C II] LIM experiment. In the future, we anticipate the sensitivity, in part limited by the number of spectrometers on TIME, can be advanced by the development of a more densely populated focal plane empowered by on-chip mm-wave spectrometers (Redford et al 2018;Endo et al 2019;Karkare et al 2020). A nextgeneration TIME experiment, TIME-NG, can have an increased number of spectrometers by at least a factor of 10.…”

Section: Next-generation [C Ii] Lim Experimentsmentioning

confidence: 99%

Probing Cosmic Reionization and Molecular Gas Growth with TIME

Sun

Chang

Uzgil

et al. 2021

ApJ

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Line intensity mapping (LIM) provides a unique and powerful means to probe cosmic structures by measuring the aggregate line emission from all galaxies across redshift. The method is complementary to conventional galaxy redshift surveys that are object-based and demand exquisite point-source sensitivity. The Tomographic Ionized-carbon Mapping Experiment (TIME) will measure the star formation rate (SFR) during cosmic reionization by observing the redshifted [C II] 158 µm line (6 z 9) in the LIM regime. TIME will simultaneously study the abundance of molecular gas during the era of peak star formation by observing the rotational CO lines emitted by galaxies at 0.5 z 2. We present the modeling framework that predicts the constraining power of TIME on a number of observables, including the line luminosity function, and the auto-and cross-correlation power spectra, including synergies with external galaxy tracers. Based on an optimized survey strategy and fiducial model parameters informed by existing observations, we forecast constraints on physical quantities relevant to reionization and galaxy evolution, such as the escape fraction of ionizing photons during reionization, the faint-end slope of the galaxy luminosity function at high redshift, and the cosmic molecular gas density at cosmic noon. We discuss how these constraints can advance our understanding of cosmological galaxy evolution at the two distinct cosmic epochs for TIME, starting in 2021, and how they could be improved in future phases of the experiment.

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Section: Next-generation [C Ii] Lim Experimentsmentioning

confidence: 99%

Probing Cosmic Reionization and Molecular Gas Growth with TIME

Sun

Chang

Uzgil

et al. 2021

ApJ

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“…Example instrumental pathfinders are now abundant in the literature. [59][60][61][62][63][64][65][66][67][68]…”

Section: Proposed Instrumentationmentioning

confidence: 99%

The Atacama large aperture submillimeter telescope (AtLAST) concept

Klaassen

Mroczkowski²,

Bryan

et al. 2020

Ground-Based and Airborne Telescopes VIII

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The coldest and densest structures of gas and dust in the Universe have unique spectral signatures across the (sub-)millimetre bands (ν ≈ 30 − 950 GHz). The current generation of single dish facilities has given a glimpse of the potential for discovery, while sub-mm interferometers have presented a high resolution view into the finer details of known targets or in small-area deep fields. However, significant advances in our understanding of such cold and dense structures are now hampered by the limited sensitivity and angular resolution of our sub-mm view of the Universe at larger scales. In this context, we present the case for a new transformational astronomical facility in the 2030s, the Atacama Large Aperture Submillimetre Telescope (AtLAST). AtLAST is a concept for a 50-m-class single dish telescope, with a high throughput provided by a 2 deg -diameter Field of View, located on a high, dry site in the Atacama with good atmospheric transmission up to ν ∼ 1 THz, and fully powered by renewable energy. We envision AtLAST as a facility operated by an international partnership with a

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“…Statistical approaches applied to existing ALMA data sets, such as the power spectrum analysis (as demonstrated in Uzgil et al 2019 andKeating et al 2020), provide efficient tools for probing low-fidelity emission from faint galaxies below survey detection thresholds. Data sets from line intensity mappingtailored to this statistical approach-will also be available from ongoing and future experiments using instruments with a large field of view on single-dish telescopes (e.g., EoR-Spec (Cothard et al 2020); SuperSpec (Redford et al 2018;Karkare et al 2020); CONCERTO (Lagache et al 2018); TIME (Sun et al 2020)) to probe aggregate [C II] emission at the highest redshifts.…”

Section: Discussionmentioning

confidence: 99%

The ALMA Spectroscopic Survey in the HUDF: A Search for [C ii] Emitters at 6 ≤ z ≤ 8

Uzgil

Oesch

Walter

et al. 2021

ApJ

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The Atacama Large Millimeter/submillimeter Array (ALMA) Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS) Band 6 scan (212–272 GHz) covers potential [C ii] emission in galaxies at 6 ≤ z ≤ 8 throughout a 2.9 arcmin2 area. By selecting on known Lyα emitters (LAEs) and photometric dropout galaxies in the field, we perform targeted searches down to a 5σ [C ii] luminosity depth L [C II] ∼ 2.0 × 108 L ⊙, corresponding roughly to star formation rates (SFRs) of 10–20 M ⊙ yr−1 when applying a locally calibrated conversion for star-forming galaxies, yielding zero detections. While the majority of galaxies in this sample are characterized by lower SFRs, the resulting upper limits on [C ii] luminosity in these sources are consistent with the current literature sample of targeted ALMA observations of z = 6–7 LAEs and Lyman-break galaxies (LBGs), as well as the locally calibrated relations between L [C ii] and SFR—with the exception of a single [C ii]-deficient, UV-luminous LBG. We also perform a blind search for [C ii]-bright galaxies that may have been missed by optical selections, resulting in an upper limit on the cumulative number density of [C ii] sources with L [C II] > 2.0 × 108 L ⊙ (5σ) to be less than 1.8 × 10−4 Mpc−3 (90% confidence level). At this luminosity depth and volume coverage, we present an observed evolution of the [C ii] luminosity function from z = 6–8 to z ∼ 0 by comparing the ASPECS measurement to literature results at lower redshift.

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Full-Array Noise Performance of Deployment-Grade SuperSpec mm-Wave On-Chip Spectrometers

Cited by 33 publications

References 15 publications

Probing Cosmic Reionization and Molecular Gas Growth with TIME

Probing Cosmic Reionization and Molecular Gas Growth with TIME

The Atacama large aperture submillimeter telescope (AtLAST) concept

The ALMA Spectroscopic Survey in the HUDF: A Search for [C ii] Emitters at 6 ≤ z ≤ 8

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