SQUID-Based Microwave Cavity Search for Dark-Matter Axions

Asztalos, S. J.; Carosi, G.; Hagmann, C.; Kinion, D.; Bibber, K. van; Hotz, M.; Rosenberg, L.; Rybka, G.; Hoskins, J.; Hwang, Jungseek; Sikivie, P.; Tanner, D. B.; Bradley, Richard F.; Clarke, John

doi:10.1103/physrevlett.104.041301

Cited by 692 publications

(597 citation statements)

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“…Fig. 3 shows initial ADMX results with SQUID amplifiers but not at dilution refrigerator temperatures (10). In more detail, Fig.…”

Section: Overview: Present Limits On Dark-matter Axionsmentioning

confidence: 99%

Dark-matter QCD-axion searches

Rosenberg

2015

Proc. Natl. Acad. Sci. U.S.A.

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In the late 20th century, cosmology became a precision science. Now, at the beginning of the next century, the parameters describing how our universe evolved from the Big Bang are generally known to a few percent. One key parameter is the total mass density of the universe. Normal matter constitutes only a small fraction of the total mass density. Observations suggest this additional mass, the dark matter, is cold (that is, moving nonrelativistically in the early universe) and interacts feebly if at all with normal matter and radiation. There's no known such elementary particle, so the strong presumption is the dark matter consists of particle relics of a new kind left over from the Big Bang. One of the most important questions in science is the nature of this dark matter. One attractive particle dark-matter candidate is the axion. The axion is a hypothetical elementary particle arising in a simple and elegant extension to the standard model of particle physics that nulls otherwise observable CP-violating effects (where CP is the product of charge reversal C and parity inversion P) in quantum chromo dynamics (QCD). A light axion of mass 10 −(6-3) eV (the invisible axion) would couple extraordinarily weakly to normal matter and radiation and would therefore be extremely difficult to detect in the laboratory. However, such an axion is a compelling dark-matter candidate and is therefore a target of a number of searches. Compared with other particle dark-matter candidates, the plausible range of axion dark-matter couplings and masses is narrowly constrained. This focused search range allows for definitive searches, where a nonobservation would seriously impugn the dark-matter QCD-axion hypothesis. Axion searches use a wide range of technologies, and the experiment sensitivities are now reaching likely dark-matter axion couplings and masses. This article is a selective overview of the current generation of sensitive axion searches. Not all techniques and experiments are discussed, but I hope to give a sense of the current experimental landscape of the search for dark-matter axions.What Makes Up the Dark Matter? One of the great discoveries of the last century is that the vast majority of all matter in the universe is made of something other than dust, planets, gas, etc., which is the ordinary matter we see around us. From observations, we now have an accurate accounting of the dark-matter fraction of the universe at around one-quarter of its total energy density, with almost all of the remaining mass and energy density of the universe being the mysterious "dark energy." From Milky Way galactic observations, our nearby dark-matter density is around one-half of proton mass per cubic centimeter.Observational constraints imposed by structure formation in the Universe plus the remnant light-isotope abundance from primordial nucleosynthesis suggest the dark matter is a new exotic particle relic left over from the Big Bang. Interestingly, light axions, with masses much less than that of the electron, have dark matter-like p...

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“…Fig. 3 shows initial ADMX results with SQUID amplifiers but not at dilution refrigerator temperatures (10). In more detail, Fig.…”

Section: Overview: Present Limits On Dark-matter Axionsmentioning

confidence: 99%

Dark-matter QCD-axion searches

Rosenberg

2015

Proc. Natl. Acad. Sci. U.S.A.

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“…In this letter we present a microwave frequency TWPA with 4 GHz of bandwidth and an order of magnitude more saturation power than the best JPA. This device is compatible with scaling to much larger qubit systems through multiplexed measurement, and may find applications outside quantum information such as astrophysics detectors [12,22] At microwave frequencies the TWPA can be thought of as a transmission line where the propagation velocity is controlled by varying the individual circuit parameters of inductance or capacitance per unit length [24,25]. This is typically achieved by constructing a signal line with a current dependent (nonlinear) inductance.…”

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confidence: 99%

Traveling wave parametric amplifier with Josephson junctions using minimal resonator phase matching

White

Mutus

Hoi

et al. 2015

Applied Physics Letters

166

174

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Josephson parametric amplifiers have become a critical tool in superconducting device physics due to their high gain and quantum-limited noise. Traveling wave parametric amplifiers (TWPAs) promise similar noise performance while allowing for significant increases in both bandwidth and dynamic range. We present a TWPA device based on an LC-ladder transmission line of Josephson junctions and parallel plate capacitors using low-loss amorphous silicon dielectric. Crucially, we have inserted λ/4 resonators at regular intervals along the transmission line in order to maintain the phase matching condition between pump, signal, and idler and increase gain. We achieve an average gain of 12 dB across a 4 GHz span, along with an average saturation power of -92 dBm with noise approaching the quantum limit.The Josephson parametric amplifier [1][2][3][4][5][6][7] (JPA) is a critical tool for high fidelity state measurement in superconducting qubits [8][9][10] as it allows parametric amplification with near quantum-limited noise [11]. Despite its success, the JPA has typically been used only for single frequency measurements due to lower bandwidth and saturation power. A promising approach to scaling superconducting qubit experiments is frequency multiplexing [12][13][14], which requires additional bandwidth and dynamic range for each measurement tone. Simultaneous amplification of up to five multiplexed tones has been achieved with a JPA [15-17] but was only possible with the Impedance-transformed parametric amplifier [18] (IMPA). This highly engineered JPA provides much larger bandwidth and saturation power but pushes the resonant design to its low Q limit.To extend this frequency multiplexed approach for future experiments, we have adopted the distributed design of the traveling wave parametric amplifier (TWPA) [19]. Fiber-optic TWPAs have already demonstrated high gain, dynamic range, and bandwidth while reaching the quantum-limit of added noise [20,21]. In this letter we present a microwave frequency TWPA with 4 GHz of bandwidth and an order of magnitude more saturation power than the best JPA. This device is compatible with scaling to much larger qubit systems through multiplexed measurement, and may find applications outside quantum information such as astrophysics detectors [12,22] At microwave frequencies the TWPA can be thought of as a transmission line where the propagation velocity is controlled by varying the individual circuit parameters of inductance or capacitance per unit length [24,25]. This is typically achieved by constructing a signal line with a current dependent (nonlinear) inductance. Like the JPA, a large enough pump tone will modulate this inductance, coupling the pump (ω p ) to a signal (ω s ) and idler (ω i ) tone via frequency mixing such that ω s + ω i = 2ω p . Unlike the JPA however, the TWPA has no resonant structure so gain, bandwidth, and dynamic range are determined by the coupled mode equations of a nonlinear transmission line [23]. In addition to allowing more bandwidth and saturation power...

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“…On cooling, the HEMT amplifier's residual noise temperature, though low enough for many applications, sticks stubbornly at a few kelvin 17 . Though this "HEMT plateau" can be lowered somewhat by employing lower device powers 18 , it has motivated the successful development of resonant SQUID-based devices 17 offering substantially lower noise temperatures, albeit over more limited bandwidths. But with both HEMTs or SQUIDs, the attainment of millikelvin noise temperatures demands sub-kelvin refrigeration, as supplied by a dilution refrigerator or its equivalent.…”

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confidence: 99%