Hafnium Films and Magnetic Shielding for TIME, A mm-Wavelength Spectrometer Array
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Final Accepted Manuscript
Author
Hunacek, J.Bock, J.
Bradford, C. M.
Butler, V.
Chang, T.-C.
Cheng, Y.-T.
Cooray, A.
Crites, A.
Frez, C.
Hailey-Dunsheath, S.
Hoscheit, B.
Kim, D. W.
Li, C.-T.
Marrone, D.
Moncelsi, L.
Shirokoff, E.
Steinbach, B.
Sun, G.
Trumper, I.
Turner, A.
Uzgil, B.
Weber, A.
Zemcov, M.
Affiliation
Univ ArizonaIssue Date
2018-04-06
Metadata
Show full item recordPublisher
SPRINGER/PLENUM PUBLISHERSCitation
Hunacek, J., Bock, J., Bradford, C.M. et al. J Low Temp Phys (2018) 193: 893. https://doi.org/10.1007/s10909-018-1906-3Rights
© Springer Science+Business Media, LLC, part of Springer Nature 2018.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
TIME is a mm-wavelength grating spectrometer array that will map fluctuations of the 157.7-mm emission line of singly ionized carbon ([CII]) during the epoch of reionization (redshift z similar to 5-9). Sixty transition-edge sensor (TES) bolometers populate the output arc of each of the 32 spectrometers, for a total of 1920 detectors. Each bolometer consists of gold absorber on a similar to 3 x 3 mm silicon nitride micro-mesh suspended near the corners by 1 x 1 x 500 mu m silicon nitride legs targeting a photon-noise-dominated NEP similar to 1 x 10-(17) W/root Hz. Hafnium films are explored as a lower-T-c alternative to Ti (500 mK) for TIME TESs, allowing thicker support legs for improved yield. Hf T-c is shown to vary between 250 and 450 mK when varying the resident Ar pressure during deposition. Magnetic shielding designs and simulations are presented for the TIME first-stage SQUIDs. Total axial field suppression is predicted to be 5 x 10(7).Note
12 month embargo; published online: 6 April 2018ISSN
0022-22911573-7357
Version
Final accepted manuscriptSponsors
National Science Foundation Graduate Research Fellowship [DGE-1144469]; National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship [1602677]Additional Links
http://link.springer.com/10.1007/s10909-018-1906-3ae974a485f413a2113503eed53cd6c53
10.1007/s10909-018-1906-3
