To study and control the behaviour of the spins of electrons that are moving through a metal or semiconductor is an outstanding challenge in the field of 'spintronics', where possibilities for new electronic applications based on the spin degree of freedom are currently being explored. Recently, electrical control of spin coherence and coherent spin precession during transport was studied by optical techniques in semiconductors. Here we report controlled spin precession of electrically injected and detected electrons in a diffusive metallic conductor, using tunnel barriers in combination with metallic ferromagnetic electrodes as spin injector and detector. The output voltage of our device is sensitive to the spin degree of freedom only, and its sign can be switched from positive to negative, depending on the relative magnetization of the ferromagnetic electrodes. We show that the spin direction can be controlled by inducing a coherent spin precession caused by an applied perpendicular magnetic field. By inducing an average precession angle of 180 degrees, we are able to reverse the sign of the output voltage.

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We find that stray infrared light from the 4 K stage in a cryostat can cause significant loss in superconducting resonators and qubits. For devices shielded in only a metal box, we measured resonators with quality factors Q = 10 5 and qubits with energy relaxation times T1 = 120 ns, consistent with a stray light-induced quasiparticle density of 170-230 µm −3 . By adding a second black shield at the sample temperature, we found about an order of magnitude improvement in performance and no sensitivity to the 4 K radiation. We also tested various shielding methods, implying a lower limit of Q = 10 8 due to stray light in the light-tight configuration.Quantum information processing in superconducting circuits is performed at very low temperatures, so energy loss due to quasiparticles is expected to vanish because their density diminishes exponentially with decreasing temperature. As energy relaxation times saturate for superconducting quantum circuits and planar resonators, reaching values on the order of 1-10 µs [1-4], recent experiments have suggested that this may be due to excess non-equilibrium quasiparticles; measurements on phase qubit coherence [5,6], tunneling in charge qubits [7], resonator quality factors [3,4] and quasiparticle recombination times [8,9] are compatible with an excess quasiparticle density on the order of 10-100 µm −3 , possibly arising from stray light, cosmic rays, background radioactivity, or the slow heat release of defects.In this Letter, we demonstrate that stray infrared light gives significant loss in resonators and qubits, and is sometimes the dominant limitation in our present experiments. We also show quantitatively how a combination of infrared shielding techniques removes the influence of stray infrared light, and that the required shielding is beyond what is generally used. The effectiveness of the various techniques is investigated by methodically changing and testing them. With our new light-tight setup, the quality factors of Al superconducting resonators improve dramatically by a factor of 20, as shown in Fig. 1. We also show that shielding improves phase qubit coherence.Loss in a superconducting resonator with frequency f is controlled by the quasiparticle density n qp [10] (for kT ≪ hf )with ∆ the energy gap, D(E F ) the two-spin density of states, and α the kinetic inductance fraction, which depends on geometry. Importantly, excess quasiparticles can limit quality factors, in particular at the low temperatures at which resonators and qubits are operated.Measurements on the temperature dependence of resonator quality factors indicate the presence of an additional loss term, as shown in Fig. 1. Here we plot quality factors of coplanar waveguide (CPW) Al resonators. The open symbols are measured when simply placing the sample in a sample box in a cryostat, with no special measures against stray light. Above a temperature of 200 mK the quality factors decrease exponentially, consistent with a thermal quasiparticle density (dashed line, Eq. 1). At low temperatures a plateau ...

We have directly measured quasiparticle number fluctuations in a thin film superconducting Al resonator in thermal equilibrium. The spectrum of these fluctuations provides a measure of both the density and the lifetime of the quasiparticles. We observe that the quasiparticle density decreases exponentially with decreasing temperature, as theoretically predicted, but saturates below 160 mK to 25-55=m 3 . We show that this saturation is consistent with the measured saturation in the quasiparticle lifetime, which also explains similar observations in qubit decoherence times. DOI: 10.1103/PhysRevLett.106.167004 PACS numbers: 74.40.Àn, 07.57.Kp, 74.25.Bt, 74.25.NÀ In a superconductor the density of unpaired electrons (quasiparticles) should vanish when approaching zero temperature [1]. This crucial property promises long decoherence times for superconducting qubits [2] and long relaxation times for highly sensitive radiation detectors [3]. However, relaxation times for resonators [4,5] and qubit decoherence times [6][7][8] were shown to saturate at low temperature. Recent modeling [8,9] suggests that nonequilibrium quasiparticles are the main candidate for this saturation, which was tested qualitatively by injecting quasiparticles into a qubit [10]. A direct measurement of the number of quasiparticles and the energy decay rate in equilibrium at low temperatures would provide new insight in superconductivity at low temperatures, crucially needed in the aforementioned fields.At finite temperature, it follows from thermodynamics that the density of quasiparticles fluctuates around an average value that increases exponentially with temperature [11]. Here we report a measurement of the spectrum of these fluctuations in a single aluminum superconducting film (T c ¼ 1:1 K) in equilibrium, for temperatures from 300 to 100 mK. The number fluctuations show up as fluctuations in the complex conductivity of the film, probed with a microwave resonator. The spectrum of these fluctuations provides a direct measure of the number of quasiparticles in the superconductor. We observe that the quasiparticle density decreases exponentially with decreasing temperature until it saturates at 25-55 m À3 below 160 mK. We prove that the measured saturation of the quasiparticle lifetime to 2.2 ms below 160 mK is consistent with the saturation in quasiparticle density. In addition, our experiment shows that it is possible to reach the fundamental generation-recombination noise limit in detectors based on Al resonators.In a superconductor in thermal equilibrium, the density of quasiparticles per unit volume is given byvalid at k B T < Á, with N 0 the single spin density of states at the Fermi level (1:72 Â 10 10 m À3 eV À1 for Al), k B Boltzmann's constant, T the temperature, and Á the energy gap of the superconductor. Two quasiparticles with opposite spins and momenta can be generated from a Cooper pair by a phonon with an energy larger than the energy gap. When two quasiparticles recombine into a Cooper pair, a phonon is emitted. These proce...

Future observations of cosmic microwave background (CMB) polarisation have the potential to answer some of the most fundamental questions of modern physics and cosmology, including: What physical process gave birth to the Universe we see today? What are the dark matter and dark energy that seem to constitute 95% of the energy density of the Universe? Do we need extensions to the standard model of particle physics and fundamental interactions? Is the ΛCDM cosmological scenario correct, or are we missing an essential piece of the puzzle? In this paper, we list the requirements for a future CMB polarisation survey addressing these scientific objectives, and discuss the design drivers of the CORE space mission proposed to ESA in answer to the "M5" call for a medium-sized mission. The rationale and options, and the methodologies used to assess the mission's performance, are of interest to other future CMB mission design studies. CORE has 19 frequency channels, distributed over a broad frequency range, spanning the 60-600 GHz interval, to control astrophysical foreground emission. The angular resolution ranges from 2 to 18 , and the aggregate CMB sensitivity is about 2 µK.arcmin. The observations are made with a single integrated focal-plane instrument, consisting of an array of 2100 cryogenically-cooled, linearly-polarised detectors at the focus of a 1.2-m aperture cross-Dragone telescope. The mission is designed to minimise all sources of systematic effects, which must be controlled so that no more than 10 −4 of the intensity leaks into polarisation maps, and no more than about 1% of E-type polarisation leaks into B-type modes. CORE observes the sky from a large Lissajous orbit around the Sun-Earth L2 point on an orbit that offers stable observing conditions and avoids contamination from sidelobe pick-up of stray radiation originating from the Sun, Earth, and Moon. The entire sky is observed repeatedly during four years of continuous scanning, with a combination of three rotations of the spacecraft over different timescales. With about 50% of the sky covered every few days, this scan strategy provides the mitigation of systematic effects and the internal redundancy that are needed to convincingly extract the primordial B-mode signal on large angular scales, and check with adequate sensitivity the consistency of the observations in several independent data subsets. CORE is designed as a "near-ultimate" CMB polarisation mission which, for optimal complementarity with ground-based observations, will perform the observations that are known to be essential to CMB polarisation science and cannot be obtained by any other means than a dedicated space mission. It will provide well-characterised, highly-redundant multi-frequency observations of polarisation at all the scales where foreground emission and cosmic variance dominate the final uncertainty for obtaining precision CMB science, as well as 2 angular resolution maps of high-frequency foreground emission in the 300-600 GHz frequency range, essential for complementarity w...