[ { "id": "authors:nbhh4-w3j74", "collection": "authors", "collection_id": "nbhh4-w3j74", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220411-225204179", "type": "monograph", "title": "BICEP Array: 150 GHz detector module development", "author": [ { "family_name": "Schillaci", "given_name": "A.", "orcid": "0000-0002-0512-1042", "clpid": "Schillaci-Alessandro" }, { "family_name": "Ade", "given_name": "P. A. R.", "orcid": "0000-0002-5127-0401" }, { "family_name": "Ahmed", "given_name": "Z." }, { "family_name": "Amiri", "given_name": "M." }, { "family_name": "Barkats", "given_name": "D." }, { "family_name": "Basu Thakur", "given_name": "R.", "orcid": "0000-0002-3351-3078", "clpid": "Basu-Thakur-Ritoban" }, { "family_name": "Bischoff", "given_name": "C. A.", "orcid": "0000-0001-9185-6514" }, { "family_name": "Beck", "given_name": "D." }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Buza", "given_name": "V.", "orcid": "0000-0002-1345-4322" }, { "family_name": "Cheshire", "given_name": "J." }, { "family_name": "Connors", "given_name": "J.", "orcid": "0000-0002-6094-2943" }, { "family_name": "Cornelison", "given_name": "J." }, { "family_name": "Crumrine", "given_name": "M." }, { "family_name": "Cukierman", "given_name": "A.", "orcid": "0000-0002-7471-719X" }, { "family_name": "Denison", "given_name": "E." }, { "family_name": "Dierickx", "given_name": "M.", "orcid": "0000-0002-3519-8593" }, { "family_name": "Duband", "given_name": "L." }, { "family_name": "Eiben", "given_name": "M." }, { "family_name": "Fatigoni", "given_name": "S.", "orcid": "0000-0002-3790-7314" }, { "family_name": "Filippini", "given_name": "J. P.", "orcid": "0000-0001-8217-6832" }, { "family_name": "Giannakopoulos", "given_name": "C." }, { "family_name": "Goeckner-Wald", "given_name": "N." }, { "family_name": "Goldfinger", "given_name": "D." }, { "family_name": "Grayson", "given_name": "J. A." }, { "family_name": "Grimes", "given_name": "P." }, { "family_name": "Hall", "given_name": "G.", "orcid": "0000-0002-6299-8385" }, { "family_name": "Halal", "given_name": "G." }, { "family_name": "Halpern", "given_name": "M.", "orcid": "0000-0002-1760-0868" }, { "family_name": "Hand", "given_name": "E." }, { "family_name": "Harrison", "given_name": "S." }, { "family_name": "Henderson", "given_name": "S." }, { "family_name": "Hildebrandt", "given_name": "S. R.", "orcid": "0000-0003-0220-0009", "clpid": "Hildebrant-Sergi-R" }, { "family_name": "Hilton", "given_name": "G. C.", "orcid": "0000-0003-4247-467X" }, { "family_name": "Hubmayr", "given_name": "J.", "orcid": "0000-0002-2781-9302" }, { "family_name": "Hui", "given_name": "H.", "orcid": "0000-0001-5812-1903", "clpid": "Hui-Howard" }, { "family_name": "Irwin", "given_name": "K. D.", "orcid": "0000-0002-2998-9743" }, { "family_name": "Kang", "given_name": "J." }, { "family_name": "Karkare", "given_name": "K. S.", "orcid": "0000-0002-5215-6993" }, { "family_name": "Kefeli", "given_name": "S.", "clpid": "Kefeli-Sinan" }, { "family_name": "Kovac", "given_name": "J. M." }, { "family_name": "Kuo", "given_name": "C. L." }, { "family_name": "Lau", "given_name": "K." }, { "family_name": "Leitch", "given_name": "E. M." }, { "family_name": "Lennox", "given_name": "A." }, { "family_name": "Megerian", "given_name": "K. G.", "clpid": "Megerian-Krikor-G" }, { "family_name": "Miller", "given_name": "O. Y.", "clpid": "Miller-Oli-Y" }, { "family_name": "Minutolo", "given_name": "L.", "orcid": "0000-0002-4876-112X", "clpid": "Minutolo-Lorenzo" }, { "family_name": "Moncelsi", "given_name": "L.", "orcid": "0000-0002-4242-3015", "clpid": "Moncelsi-Lorenzo" }, { "family_name": "Nakato", "given_name": "Y." }, { "family_name": "Namikawa", "given_name": "T.", "orcid": "0000-0003-3070-9240" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "O'Brient", "given_name": "R.", "orcid": "0000-0002-4987-6375", "clpid": "O'Brient-Roger-C" }, { "family_name": "Palladino", "given_name": "S." }, { "family_name": "Petroff", "given_name": "M." }, { "family_name": "Precup", "given_name": "N." }, { "family_name": "Prouve", "given_name": "T." }, { "family_name": "Pryke", "given_name": "C." }, { "family_name": "Racine", "given_name": "B.", "orcid": "0000-0001-8861-3052" }, { "family_name": "Reintsema", "given_name": "C. D." }, { "family_name": "Schmitt", "given_name": "B. L." }, { "family_name": "Singari", "given_name": "B." }, { "family_name": "Soliman", "given_name": "A.", "clpid": "Soliman-Ahmed" }, { "family_name": "St. Germaine", "given_name": "T." }, { "family_name": "Steinbach", "given_name": "B.", "orcid": "0000-0001-6544-7469", "clpid": "Steinbach-Bryan-A" }, { "family_name": "Sudiwala", "given_name": "R. V." }, { "family_name": "Thompson", "given_name": "K. L." }, { "family_name": "Tucker", "given_name": "C." }, { "family_name": "Turner", "given_name": "A. D.", "clpid": "Turner-Anthony-D" }, { "family_name": "Umilta", "given_name": "C.", "orcid": "0000-0002-6805-6188" }, { "family_name": "Verges", "given_name": "C." }, { "family_name": "Vieregg", "given_name": "A. G." }, { "family_name": "Wandui", "given_name": "A.", "orcid": "0000-0002-8232-7343", "clpid": "Wandui-Albert-K" }, { "family_name": "Weber", "given_name": "A. C.", "clpid": "Weber-Alexis-C" }, { "family_name": "Wiebe", "given_name": "D. V." }, { "family_name": "Willmert", "given_name": "J." }, { "family_name": "Wu", "given_name": "W. L. K.", "orcid": "0000-0001-5411-6920" }, { "family_name": "Yang", "given_name": "E." }, { "family_name": "Yoon", "given_name": "K. W." }, { "family_name": "Young", "given_name": "E." }, { "family_name": "Yu", "given_name": "C." }, { "family_name": "Zeng", "given_name": "L." }, { "family_name": "Zhang", "given_name": "C.", "orcid": "0000-0001-8288-5823", "clpid": "Zhang-Cheng" }, { "family_name": "Zhang", "given_name": "S.", "clpid": "Zhang-S" } ], "abstract": "The BICEP/Keck Collaboration is currently leading the quest to the highest sensitivity measurements of the polarized CMB anisotropies on degree scale with a series of cryogenic telescopes, of which BICEP Array is the latest Stage-3 upgrade with a total of \u223c32,000 detectors. The instrument comprises 4 receivers spanning 30 to 270 GHz, with the low-frequency 30/40 GHz deployed to the South Pole Station in late 2019. The full complement of receivers is forecast to set the most stringent constraints on the tensor to scalar ratio r. Building on these advances, the overarching small-aperture telescope concept is already being used as the reference for further Stage-4 experiment design.\nIn this paper I will present the development of the BICEP Array 150 GHz detector module and its fabrication requirements, with highlights on the high-density time division multiplexing (TDM) design of the cryogenic circuit boards. The low-impedance wiring required between the detectors and the first-stage SQUID amplifiers is crucial to maintain a stiff voltage bias on the detectors. A novel multi-layer FR4 Printed Circuit Board (PCB) with superconducting traces, capable of reading out up to 648 detectors, is presented along with its validation tests.\nI will also describe an ultra-high density TDM detector module we developed for a CMB-S4-like experiment that allows up to 1,920 detectors to be read out. TDM has been chosen as the detector readout technology for the Cosmic Microwave Background Stage-4 (CMB-S4) experiment based on its proven low-noise performance, predictable costs and overall maturity of the architecture. The heritage for TDM is rooted in mm- and submm-wave experiments dating back 20 years and has since evolved to support a multiplexing factor of 64x in Stage-3 experiments.", "doi": "10.48550/arXiv.2111.14785", "publisher": "arXiv", "publication_date": "2021-11-29" }, { "id": "authors:tchrr-zkf51", "collection": "authors", "collection_id": "tchrr-zkf51", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210809-205942459", "type": "monograph", "title": "Measurements of the Zodiacal Light Absolute Intensity through Fraunhofer Absorption Line Spectroscopy with CIBER", "author": [ { "family_name": "Korngut", "given_name": "P. M.", "clpid": "Korngut-Phillip-M" }, { "family_name": "Kim", "given_name": "M. G.", "clpid": "Kim-Min-Gyu" }, { "family_name": "Arai", "given_name": "T.", "clpid": "Arai-Toshiaki" }, { "family_name": "Bangale", "given_name": "P.", "orcid": "0000-0002-3886-3739", "clpid": "Bangale-Priyadarshini" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-Asantha" }, { "family_name": "Cheng", "given_name": "Y. T.", "orcid": "0000-0002-5437-0504", "clpid": "Cheng-Yun-Ting" }, { "family_name": "Feder", "given_name": "R.", "orcid": "0000-0002-9330-8738", "clpid": "Feder-Richard-M" }, { "family_name": "Hristov", "given_name": "V.", "clpid": "Hristov-Viktor-V" }, { "family_name": "Lanz", "given_name": "A.", "orcid": "0000-0003-2565-1558", "clpid": "Lanz-Alicia" }, { "family_name": "Lee", "given_name": "D. H.", "clpid": "Lee-D-H" }, { "family_name": "Levenson", "given_name": "L.", "clpid": "Levenson-Louis" }, { "family_name": "Matsumoto", "given_name": "T.", "orcid": "0000-0001-6066-5221", "clpid": "Matsumoto-Toshio" }, { "family_name": "Matsuura", "given_name": "S.", "orcid": "0000-0002-5698-9634", "clpid": "Matsuura-Shuji" }, { "family_name": "Nguyen", "given_name": "C.", "orcid": "0000-0001-9368-3186", "clpid": "Nguyen-Chi-H" }, { "family_name": "Sano", "given_name": "K.", "orcid": "0000-0002-6468-8532", "clpid": "Sano-Kei" }, { "family_name": "Tsumura", "given_name": "K.", "orcid": "0000-0001-7143-6520", "clpid": "Tsumura-Kohji" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-Michael" } ], "abstract": "Scattered sunlight from the interplanetary dust (IPD) cloud in our Solar system presents a serious foreground challenge for spectro-photometric measurements of the Extragalactic Background Light (EBL). In this work, we report on measurements of the absolute intensity of the Zodiacal Light (ZL) using the novel technique of Fraunhofer line spectroscopy on the deepest 8542 Angstrom line of the near-infrared CaII absorption triplet. The measurements are performed with the Narrow Band Spectrometer (NBS) aboard the Cosmic Infrared Background Experiment (CIBER) sounding rocket instrument. We use the NBS data to test the accuracy of two ZL models widely cited in the literature; the Kelsall and Wright models, which have been used in foreground removal analyses that produce high and low EBL results respectively. We find a mean reduced \u03c7\u00b2 of 3.5 for the Kelsall model and a \u03c7\u00b2 of 2.0 for the Wright model. The best description of our data is provided by a simple modification to the Kelsall model which includes a free ZL offset parameter. This adjusted model describes the data with a reduced \u03c7\u00b2 of 1.5 and yields an inferred offset amplitude of 46 \u00b1 19 nW m\u207b\u00b2 sr\u207b\u00b9 extrapolated to 12500 \u00c5. These measurements elude to the potential existence of a dust cloud component in the inner Solar system whose intensity does not strongly modulate with the Earth's motion around the Sun.", "doi": "10.48550/arXiv.2104.07104", "publisher": "arXiv", "publication_date": "2021-04-14" }, { "id": "authors:kke2y-c4d85", "collection": "authors", "collection_id": "kke2y-c4d85", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200312-132341532", "type": "monograph", "title": "Thermal Kinetic Inductance Detectors for Millimeter-Wave Astrophysics", "author": [ { "family_name": "Wandui", "given_name": "A.", "orcid": "0000-0002-8232-7343", "clpid": "Wandui-Albert" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Frez", "given_name": "C.", "clpid": "Frez-Clifford" }, { "family_name": "Hollister", "given_name": "M. I.", "clpid": "Hollister-Matthew-I" }, { "family_name": "Minutolo", "given_name": "L.", "orcid": "0000-0002-4876-112X", "clpid": "Minutolo-Lorenzo" }, { "family_name": "Nguyen", "given_name": "H.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Steinbach", "given_name": "B.", "clpid": "Steinbach-Bryan-A" }, { "family_name": "Turner", "given_name": "A. D.", "clpid": "Turner-Anthony-D" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" }, { "family_name": "O'Brient", "given_name": "R.", "clpid": "O'Brient-Roger-C" } ], "abstract": "Thermal Kinetic Inductance Detectors (TKIDs) combine the excellent noise performance of traditional bolometers with a radio frequency (RF) multiplexing architecture that enables the large detector counts needed for the next generation of millimeter-wave instruments. Here we present dark prototype TKID pixels that demonstrate a noise equivalent power NEP = 2\u00d710\u207b\u00b9\u2077\u221aW/Hz with a 1/f knee at 0.1 Hz, suitable for background-limited noise performance at 150 GHz from a ground-based site. We discuss the optimizations in the device design and fabrication techniques to realize optimal electrical performance and high quality factors at a bath temperature of 250 mK.", "doi": "10.48550/arXiv.2001.08887", "publisher": "arXiv", "publication_date": "2020-01-24" }, { "id": "authors:2bt5f-4f288", "collection": "authors", "collection_id": "2bt5f-4f288", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190925-135806088", "type": "monograph", "title": "PICO: Probe of Inflation and Cosmic Origins", "author": [ { "family_name": "Hanany", "given_name": "Shaul", "clpid": "Hanany-S" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Pearson", "given_name": "Tim", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "O'Brient", "given_name": "Roger", "clpid": "O'Brient-R-C" }, { "family_name": "Rocha", "given_name": "Gra\u00e7a", "orcid": "0000-0002-4150-8076", "clpid": "Rocha-G-M" } ], "abstract": "The Probe of Inflation and Cosmic Origins (PICO) is an imaging polarimeter that will scan the sky for 5 years in 21 frequency bands spread between 21 and 799 GHz. It will produce full-sky surveys of intensity and polarization with a final combined-map noise level of 0.87 \u03bcK arcmin for the required specifications, equivalent to 3300 Planck missions, and with our current best-estimate would have a noise level of 0.61 \u03bcK arcmin (6400 Planck missions). PICO will either determine the energy scale of inflation by detecting the tensor to scalar ratio at a level r = 5\u00d710^(\u22124) (5\u03c3), or will rule out with more than 5\u03c3 all inflation models for which the characteristic scale in the potential is the Planck scale. With LSST's data it could rule out all models of slow-roll inflation. PICO will detect the sum of neutrino masses at >4\u03c3, constrain the effective number of light particle species with \u0394N_(eff) < 0.06 (2\u03c3), and elucidate processes affecting the evolution of cosmic structures by measuring the optical depth to reionization with errors limited by cosmic variance and by constraining the evolution of the amplitude of linear fluctuations \u03c3_8(z) with sub-percent accuracy. Cross-correlating PICO's map of the thermal Sunyaev-Zeldovich effect with LSST's gold sample of galaxies will precisely trace the evolution of thermal pressure with z. PICO's maps of the Milky Way will be used to determine the make up of galactic dust and the role of magnetic fields in star formation efficiency. With 21 full sky legacy maps in intensity and polarization, which cannot be obtained in any other way, the mission will enrich many areas of astrophysics. PICO is the only single-platform instrument with the combination of sensitivity, angular resolution, frequency bands, and control of systematic effects that can deliver this compelling, timely, and broad science.", "doi": "10.48550/arXiv.1902.10541", "publication_date": "2019-02-26" }, { "id": "authors:rj92b-6ch67", "collection": "authors", "collection_id": "rj92b-6ch67", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191004-143142963", "type": "monograph", "title": "Measurements of Degree-Scale B-mode Polarization with the BICEP/Keck Experiments at South Pole", "author": [ { "family_name": "Ade", "given_name": "P. A. R.", "orcid": "0000-0002-5127-0401", "clpid": "Ade-P-A-R" }, { "family_name": "Aikin", "given_name": "R. W.", "clpid": "Aikin-R-W" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Brevik", "given_name": "J. A.", "clpid": "Brevik-J-A" }, { "family_name": "Hildebrandt", "given_name": "S. R.", "clpid": "Hildebrant-S-R" }, { "family_name": "Hui", "given_name": "H.", "clpid": "Hui-Howard" }, { "family_name": "Irwin", "given_name": "K. D.", "clpid": "Irwin-K-D" }, { "family_name": "Kefeli", "given_name": "S.", "clpid": "Kefeli-S" }, { "family_name": "Lueker", "given_name": "M.", "clpid": "Lueker-M" }, { "family_name": "Moncelsi", "given_name": "L.", "orcid": "0000-0002-4242-3015", "clpid": "Moncelsi-Lorenzo" }, { "family_name": "O'Brient", "given_name": "R.", "clpid": "O'Brient-R" }, { "family_name": "Schillaci", "given_name": "A.", "clpid": "Schillaci-A" }, { "family_name": "Soliman", "given_name": "A.", "clpid": "Soliman-A" }, { "family_name": "Staniszewski", "given_name": "Z. K.", "clpid": "Staniszewski-Z-K" }, { "family_name": "Steinbach", "given_name": "B.", "clpid": "Steinbach-B" }, { "family_name": "Teply", "given_name": "G. P.", "clpid": "Teply-G-P" }, { "family_name": "Wandui", "given_name": "A.", "clpid": "Wandui-A" }, { "family_name": "Zhang", "given_name": "C.", "orcid": "0000-0001-8288-5823", "clpid": "Zhang-C" }, { "literal": "BICEP Collaboration" }, { "literal": "Keck Collaboration" } ], "abstract": "The BICEP and Keck Array experiments are a suite of small-aperture refracting telescopes observing the microwave sky from the South Pole. They target the degree-scale B-mode polarization signal imprinted in the Cosmic Microwave Background (CMB) by primordial gravitational waves. Such a measurement would shed light on the physics of the very early universe. While BICEP2 observed for the first time a B-mode signal at 150 GHz, higher frequencies from the Planck satellite showed that it could be entirely due to the polarized emission from Galactic dust, though uncertainty remained high. Keck Array has been observing the same region of the sky for several years, with an increased detector count, producing the deepest polarized CMB maps to date. New detectors at 95 GHz were installed in 2014, and at 220 GHz in 2015. These observations enable a better constraint of galactic foreground emissions, as presented here. In 2015, BICEP2 was replaced by BICEP3, a 10 times higher throughput telescope observing at 95 GHz, while Keck Array is now focusing on higher frequencies. In the near future, BICEP Array will replace Keck Array, and will allow unprecedented sensitivity to the gravitational wave signal. High resolution observations from the South Pole Telescope (SPT) will also be used to remove the lensing contribution to B-modes.", "doi": "10.48550/arXiv.1807.02199", "publication_date": "2018-07-05" }, { "id": "authors:3m3f9-mrb52", "collection": "authors", "collection_id": "3m3f9-mrb52", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-154905435", "type": "monograph", "title": "Science Impacts of the SPHEREx All-Sky Optical to Near-Infrared Spectral Survey II: Report of a Community Workshop on the Scientific Synergies Between the SPHEREx Survey and Other Astronomy Observatories", "author": [ { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "de la Torre", "given_name": "Sylvain", "orcid": "0000-0002-0839-2884", "clpid": "de-la-Torre-S" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Teplitz", "given_name": "Harry", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Werner", "given_name": "Michael", "clpid": "Werner-M-W" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Chang", "given_name": "Tzu-Ching", "clpid": "Chang-Tzu-Ching" }, { "family_name": "Crill", "given_name": "Brendan", "orcid": "0000-0002-4650-8518", "clpid": "Crill-B-P" }, { "family_name": "Korngut", "given_name": "Phil", "clpid": "Korngut-P-M" }, { "family_name": "Scoville", "given_name": "Nick Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" } ], "abstract": "SPHEREx is a proposed NASA MIDEX mission selected for Phase A study. SPHEREx would carry out the first all-sky spectral survey in the near infrared. At the end of its two-year mission, SPHEREx would obtain 0.75-to-5\u03bcm spectra of every 6.2 arcsec pixel on the sky, with spectral resolution R>35 and a 5-\u03c3 sensitivity AB>19 per spectral/spatial resolution element. More details concerning SPHEREx are available at http://spherex.caltech.edu. The SPHEREx team has proposed three specific science investigations to be carried out with this unique data set: cosmic inflation, interstellar and circumstellar ices, and the extra-galactic background light. Though these three themes are undoubtedly compelling, they are far from exhausting the scientific output of SPHEREx. Indeed, SPHEREx would create a unique all-sky spectral database including spectra of very large numbers of astronomical and solar system targets, including both extended and diffuse sources. These spectra would enable a wide variety of investigations, and the SPHEREx team is dedicated to making the data available to the community to enable these investigations, which we refer to as Legacy Science. To that end, we have sponsored two workshops for the general scientific community to identify the most interesting Legacy Science themes and to ensure that the SPHEREx data products are responsive to their needs. In February of 2016, some 50 scientists from all fields met in Pasadena to develop these themes and to understand their implications for the SPHEREx mission. The 2016 workshop highlighted many synergies between SPHEREx and other contemporaneous astronomical missions, facilities, and databases. Consequently, in January 2018 we convened a second workshop at the Center for Astrophysics in Cambridge to focus specifically on these synergies. This white paper reports on the results of the 2018 SPHEREx workshop.", "doi": "10.48550/arXiv.1805.05489", "publication_date": "2018-05-14" }, { "id": "authors:r05zt-vgh73", "collection": "authors", "collection_id": "r05zt-vgh73", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180807-104642184", "type": "monograph", "title": "Characterization and Improvement of the Thermal Stability of TES Bolometers", "author": [ { "family_name": "Sonka", "given_name": "Rita", "clpid": "Sonka-R" }, { "family_name": "Bock", "given_name": "James J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Megerian", "given_name": "Krikor G.", "clpid": "Megerian-K-G" }, { "family_name": "Steinbach", "given_name": "Bryan A.", "clpid": "Steinbach-B-A" }, { "family_name": "Turner", "given_name": "Anthony D.", "clpid": "Turner-A-D" }, { "family_name": "Zhang", "given_name": "Cheng", "orcid": "0000-0001-8288-5823", "clpid": "Zhang-Cheng" } ], "abstract": "We study the mechanism of instability in transition edge sensor (TES) bolometers used for ground based observations of the Cosmic Microwave Background (CMB) at 270GHz. The instability limits the range of useful operating resistances of the TES down to \u224850% of R_n, and due to variations in detector properties and optical loading within a column of multiplexed detectors, limits the effective on sky yield. Using measurements of the electrical impedance of the detectors, we show the instability is due to the increased bolometer leg G for higher-frequency detection inducing decoupling of the palladium-gold heat capacity from the thermistor. We demonstrate experimentally that the limiting thermal resistance is due to the small cross sectional area of the silicon nitride bolometer island, and so is easily fixed by layering palladium-gold over an oxide protected TES. The resulting detectors can be biased down to a resistance \u224810% of R_n.", "doi": "10.48550/arXiv.1712.05496", "publication_date": "2017-12-15" }, { "id": "authors:ts3gk-d8y56", "collection": "authors", "collection_id": "ts3gk-d8y56", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180914-101943065", "type": "monograph", "title": "Science Impacts of the SPHEREx All-Sky Optical to Near-Infrared Spectral Survey: Report of a Community Workshop Examining Extragalactic, Galactic, Stellar and Planetary Science", "author": [ { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Werner", "given_name": "Michael", "clpid": "Werner-M-W" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bull", "given_name": "Philip", "clpid": "Bull-P" }, { "family_name": "Crill", "given_name": "Brendan", "orcid": "0000-0002-4650-8518", "clpid": "Crill-B-P" }, { "family_name": "de Putter", "given_name": "Roland", "clpid": "de-Putter-R" }, { "family_name": "Eifler", "given_name": "Tim", "orcid": "0000-0002-1894-3301", "clpid": "Eifler-T-F" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Korngut", "given_name": "Phillip", "clpid": "Korngut-P-M" }, { "family_name": "Nguyen", "given_name": "Hien", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Rhodes", "given_name": "Jason", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" } ], "abstract": "SPHEREx is a proposed SMEX mission selected for Phase A. SPHEREx will carry out the first all-sky spectral survey and provide for every 6.2\" pixel a spectra between 0.75 and 4.18 \u03bcm [with R\u223c41.4] and 4.18 and 5.00 \u03bcm [with R\u223c135]. The SPHEREx team has proposed three specific science investigations to be carried out with this unique data set: cosmic inflation, interstellar and circumstellar ices, and the extra-galactic background light. It is readily apparent, however, that many other questions in astrophysics and planetary sciences could be addressed with the SPHEREx data. The SPHEREx team convened a community workshop in February 2016, with the intent of enlisting the aid of a larger group of scientists in defining these questions. This paper summarizes the rich and varied menu of investigations that was laid out. It includes studies of the composition of main belt and Trojan/Greek asteroids; mapping the zodiacal light with unprecedented spatial and spectral resolution; identifying and studying very low-metallicity stars; improving stellar parameters in order to better characterize transiting exoplanets; studying aliphatic and aromatic carbon-bearing molecules in the interstellar medium; mapping star formation rates in nearby galaxies; determining the redshift of clusters of galaxies; identifying high redshift quasars over the full sky; and providing a NIR spectrum for most eROSITA X-ray sources. All of these investigations, and others not listed here, can be carried out with the nominal all-sky spectra to be produced by SPHEREx. In addition, the workshop defined enhanced data products and user tools which would facilitate some of these scientific studies. Finally, the workshop noted the high degrees of synergy between SPHEREx and a number of other current or forthcoming programs, including JWST, WFIRST, Euclid, GAIA, K2/Kepler, TESS, eROSITA and LSST.", "doi": "10.48550/arXiv.1606.07039", "publication_date": "2016-06-22" }, { "id": "authors:vjtnf-xxt92", "collection": "authors", "collection_id": "vjtnf-xxt92", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180911-163142346", "type": "monograph", "title": "An Empirical Approach to Cosmological Galaxy Survey Simulation: Application to SPHEREx Low-Resolution Spectroscopy", "author": [ { "family_name": "Stickley", "given_name": "Nathaniel R.", "clpid": "Stickley-N-R" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Masters", "given_name": "Daniel", "orcid": "0000-0001-5382-6138", "clpid": "Masters-D-C" }, { "family_name": "de Putter", "given_name": "Roland", "clpid": "de-Putter-R" }, { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" } ], "abstract": "Highly accurate models of the galaxy population over cosmological volumes are necessary in order to predict the performance of upcoming cosmological missions. We present a data-driven model of the galaxy population constrained by deep 0.1-8 \u03bcm imaging and spectroscopic data in the COSMOS survey, with the immediate goal of simulating the spectroscopic redshift performance of the proposed SPHEREx mission. SPHEREx will obtain over the full-sky R\u223c41 spectrophotometry at moderate spatial resolution (\u223c6\") over the wavelength range 0.75-4.18 \u03bcm and R\u223c135 over the wavelength range 4.18-5 \u03bcm. We show that our simulation accurately reproduces a range of known galaxy properties, encapsulating the full complexity of the galaxy population and enables realistic, full end-to-end simulations to predict mission performance. Finally, we discuss potential applications of the simulation framework to future cosmology missions and give a description of released data products.", "doi": "10.48550/arXiv.1606.06374", "publication_date": "2016-06-21" }, { "id": "authors:bnfw6-v6e90", "collection": "authors", "collection_id": "bnfw6-v6e90", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190213-132441192", "type": "monograph", "title": "Mapping the Epoch of Reionization with C+ Line Tomography", "author": [ { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "Charles M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" } ], "abstract": "Our KISS program has laid the theoretical foundations for probing the epoch of reionization with C+\ntomography measurements, developed unique lithographed millimeter-wave spectrometer technology,\nand initiated a first-light C+ experiment named TIME-Pilot. With KISS support we have carried out the\nfollowing investigations:\n1) Developed the case for line intensity mapping methods to study the epoch of reionization\nusing singly ionized carbon (C+), typically the most luminous emission line in galaxies. The\ntheoretical studies not only explored the amplitude of the signal, and the usefulness in\ndetermining physical properties of the partially ionized intergalactic medium, but also the\neffects of foreground confusion from low-redshift galaxies. Our team made the first\ncalculations of C+ clustering fluctuations from the reionization epoch, and estimated the\neffect of foreground galaxy confusion, largely from CO line emission at z ~ 1. We also\nauthored the first papers on tomographic measurements with the Ly\uf061 emission line, which\nshows great promise for near-infrared intensity mapping measurements with the SPHEREx\nSMEX mission concept.\n2) Developed a complete design for a first-detection instrument of [CII] large-scale clustering\nemission named TIME-Pilot, based on an array of 32 novel waveguide spectrometers. The\nspectrometers are mounted in a linear array in two polarizations, and observations are\ncarried out by scanning the detectors in a 1-deg linear strip, which maximizes depth (small\nsurvey area) while preserving sensitivity on large scales (long scan length).\n3) Demonstrated the key waveguide spectrometer technology, which confines radiation in 2\ndimensions and the power propagates between parallel plates and is dispersed and\ncollimated by a curved grating. The waveguide spectrometers greatly reduce the mass and\nvolume that would otherwise be required with a conventional 3-d grating spectrometer.\n4) Demonstrated a prototype superconducting detector array. These high-sensitivity\nsuperconducting bolometers are mounted on the focal surface across multiple\nspectrometers, and read out by superconducting current amplifiers. The devices present\nunique micro-machining challenges to produce edge-butted sub-arrays that do not leave\nspectral gaps between channels.\n5) Completed the full cryogenic system for the instrument. We commandeered an existing 4\nK cryostat from another project, and added cooling stages to an ultimate temperature of\n220 mK to meet the TIME-Pilot cooling requirements. The system is fully tested and\noperational.\n6) Formed a partnership with ASIAA in Taiwan, led by Tzu-Ching Chang who attended the\noriginal KISS study. ASIAA is providing major hardware components for the TIME-Pilot\ninstrument, and in the past year have developed a prototype of the spectrometer, and\nprocured cables and cryogenic coolers. ASIAA has also become the managing institution\nfor the James Clerk Maxwell Telescope (JCMT) in Hawaii, and ideal facility for carrying out\nobservations with the instrument.", "doi": "10.26206/BWNS-7F04", "publication_date": "2016-03-22" }, { "id": "authors:2q184-ja103", "collection": "authors", "collection_id": "2q184-ja103", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-130227932", "type": "monograph", "title": "A complete view of galaxy evolution: panchromatic luminosity functions and the generation of metals", "author": [ { "family_name": "Blain", "given_name": "Andrew W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Bertoldi", "given_name": "Frank", "orcid": "0000-0002-1707-1775", "clpid": "Bertoldi-F" }, { "family_name": "Bock", "given_name": "James", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "Matt", "clpid": "Bradford-M-C" }, { "family_name": "Dowell", "given_name": "C. Darren", "clpid": "Dowell-C-D" }, { "family_name": "Glenn", "given_name": "Jason", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "family_name": "Goldsmith", "given_name": "Paul", "orcid": "0000-0002-6622-8396", "clpid": "Goldsmith-P-F" }, { "family_name": "Harwit", "given_name": "Martin", "clpid": "Harwit-M" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Smith", "given_name": "J. D.", "orcid": "0000-0003-1545-5078", "clpid": "Smith-J-D-T" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Stacey", "given_name": "Gordon", "clpid": "Stacey-G-J" }, { "family_name": "Vieira", "given_name": "Joaquin", "clpid": "Vieira-J-D" }, { "family_name": "Yun", "given_name": "Min", "orcid": "0000-0001-7095-7543", "clpid": "Yun-Min-S" }, { "family_name": "Zmuidzinas", "given_name": "Jonas", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "When and how did galaxies form and their metals accumulate? Over the last decade, this has moved from an archeological question to a live investigation: there is now a broad picture of the evolution of galaxies in dark matter halos: their masses, stars, metals and supermassive blackholes. Galaxies have been found and studied in which these formation processes are taking place most vigorously, all the way back in cosmic time to when the intergalactic medium (IGM) was still largely neutral. However, the details of how and why the interstellar medium (ISM) in\ndistant galaxies cools, is processed, recycled and enriched in metals by stars, and fuels active\ngalactic nuclei (AGNs) remain uncertain. In particular, the cooling of gas to fuel star formation,\nand the chemistry and physics of the most intensely active regions is hidden from view at optical\nwavelengths, but can be seen and diagnosed at mid- & far-infrared (IR) wavelengths. Rest-frame\nIR observations are important first to identify the most luminous, interesting and important\ngalaxies, secondly to quantify accurately their total luminosity, and finally to use spectroscopy to\ntrace the conditions in the molecular and atomic gas out of which stars form. In order to map out\nthese processes over the full range of environments and large-scale structures found in the\nuniverse - from the densest clusters of galaxies to the emptiest voids \u2013 we require tools for deep,\nlarge area surveys, of millions of galaxies out to z~5, and for detailed follow-up spectroscopy.\nThe necessary tools can be realized technically. Here, we outline the requirements for gathering\nthe crucial information to build, validate and challenge models of galaxy evolution.", "doi": "10.48550/arXiv.0903.1272", "publication_date": "2009-03-06" } ]