Planck 2013 results. XXXI. Consistency of the Planck data

The Planck design and scanning strategy provide many levels of redundancy that can be exploited to provide tests of internal consistency. One of the most important is the comparison of the 70 GHz (amplifier) and 100 GHz (bolometer) channels. Based on different instrument technologies, with feeds located differently in the focal plane, analysed independently by different teams using different software, and near the minimum of diffuse foreground emission, these channels are in effect two different experiments. The 143 GHz channel has the lowest noise level on Planck, and is near the minimum of unresolved foreground emission. In this paper, we analyse the level of consistency achieved in the 2013 Planck data. We concentrate on comparisons between the 70, 100, and 143 GHz channel maps and power spectra, particularly over the angular scales of the first and second acoustic peaks, on maps masked for diffuse Galactic emission and for strong unresolved sources. Difference maps covering angular scales from 8° to 15′ are consistent with noise, and show no evidence of cosmic microwave background structure. Including small but important corrections for unresolved-source residuals, we demonstrate agreement (measured by deviation of the ratio from unity) between 70 and 100 GHz power spectra averaged over 70 ≤ ℓ ≤ 390 at the 0.8% level, and agreement between 143 and 100 GHz power spectra of 0.4% over the same ℓ range. These values are within and consistent with the overall uncertainties in calibration given in the Planck 2013 results. We also present results based on the 2013 likelihood analysis showing consistency at the 0.35% between the 100, 143, and 217 GHz power spectra. We analyse calibration procedures and beams to determine what fraction of these differences can be accounted for by known approximations or systematicerrors that could be controlled even better in the future, reducing uncertainties still further. Several possible small improvements are described. Subsequent analysis of the beams quantifies the importance of asymmetry in the near sidelobes, which was not fully accounted for initially, affecting the 70/100 ratio. Correcting for this, the 70, 100, and 143 GHz power spectra agree to 0.4% over the first two acoustic peaks. The likelihood analysis that produced the 2013 cosmological parameters incorporated uncertainties larger than this. We show explicitly that correction of the missing near sidelobe power in the HFI channels would result in shifts in the posterior distributions of parameters of less than 0.3σ except for As, the amplitude of the primordial curvature perturbations at 0.05 Mpc-1, which changes by about 1σ. We extend these comparisons to include the sky maps from the complete nine-year mission of the Wilkinson Microwave Anisotropy Probe (WMAP), and find a roughly 2% difference between the Planck and WMAP power spectra in the region of the first acoustic peak

Detection chain and electronic readout of the QUBIC instrument

The Q and U Bolometric Interferometer for Cosmology (QUBIC) Technical Demonstrator (TD) aiming to shows the feasibility of the combination of interferometry and bolometric detection. The electronic readout system is based on an array of 128 NbSi Transition Edge Sensors cooled at 350mK readout with 128 SQUIDs at 1K controlled and amplified by an Application Specific Integrated Circuit at 40K. This readout design allows a 128:1 Time Domain Multiplexing. We report the design and the performance of the detection chain in this paper. The technological demonstrator unwent a campaign of test in the lab. Evaluation of the QUBIC bolometers and readout electronics includes the measurement of I-V curves, time constant and the Noise Equivalent Power. Currently the mean Noise Equivalent Power is ~ 2 x 10⁻¹⁶ W/√Hz

Detection chain and electronic readout of the QUBIC instrument

The Q and U Bolometric Interferometer for Cosmology (QUBIC) Technical Demonstrator (TD) aiming to shows the feasibility of the combination of interferometry and bolometric detection. The electronic readout system is based on an array of 128 NbSi Transition Edge Sensors cooled at 350mK readout with 128 SQUIDs at 1K controlled and amplified by an Application Specific Integrated Circuit at 40K. This readout design allows a 128:1 Time Domain Multiplexing. We report the design and the performance of the detection chain in this paper. The technological demonstrator unwent a campaign of test in the lab. Evaluation of the QUBIC bolometers and readout electronics includes the measurement of I-V curves, time constant and the Noise Equivalent Power. Currently the mean Noise Equivalent Power is ~ 2 x 10⁻¹⁶ W/√Hz

Mapping neurotransmitter systems to the structural and functional organization of the human neocortex

Neurotransmitter receptors support the propagation of signals in the human brain. How receptor systems are situated within macro-scale neuroanatomy and how they shape emergent function remain poorly understood, and there exists no comprehensive atlas of receptors. Here we collate positron emission tomography data from more than 1,200 healthy individuals to construct a whole-brain three-dimensional normative atlas of 19 receptors and transporters across nine different neurotransmitter systems. We found that receptor profiles align with structural connectivity and mediate function, including neurophysiological oscillatory dynamics and resting-state hemodynamic functional connectivity. Using the Neurosynth cognitive atlas, we uncovered a topographic gradient of overlapping receptor distributions that separates extrinsic and intrinsic psychological processes. Finally, we found both expected and novel associations between receptor distributions and cortical abnormality patterns across 13 disorders. We replicated all findings in an independently collected autoradiography dataset. This work demonstrates how chemoarchitecture shapes brain structure and function, providing a new direction for studying multi-scale brain organization.</p

Etude des différentes composantes de la polarisation du ciel en vue de l'observation du Fond Diffus Cosmologique avec le satellite Planck

This thesis is dedicated to the measurement of the Cosmic Microwave Background (CMB) anisotropies and to the characterization of its Galactic foregrounds. This work has been done in the framework of the Planck satellite data analysis preparation.First, a general introduction to cosmology and to CMB is presented. An overview of the current cosmological measurements is given and the Archeops, WMAP and Planck experiments are introduced. Part two is devoted to the effect of a primordial magnetic field on CMB polarization. We derive the angular power spectra of this effect and give a superior limit on the nowadays intensity of this field using the WMAP data.In a third part, we present the analysis we have performed using the Archeops data. First, we show the Gaussian nature of the temperature data measured at 143 GHz, constraining the non-linear coupling factor and systematic residuals and then, using the polarized data from the 353 GHz channel, we show the first measurement of the polarized diffuse emission of dust at large angular scales.In a fourth part, we present an original component separation method allowing to extract the various physical contributions from multi-frequency observations, in both temperature and polarization. Performances of the method are intensively tested using Planck sky simulations.Finally, we focus on the modelization of the polarized Galactic emissions of synchrotron and dust and we compare our simulations of these emissions to the Archeops and WMAP polarized data.Cette thèse est dédiée à la mesure des anisotropies du Fond Diffus Cosmologique (CMB) ainsi qu'à la caractérisation des émissions d'avant-plan. Les travaux que nous avons entrepris s'inscrivent dans le cadre de la préparation à l'analyse et à l'exploitation des données du satellite Planck.L'exposé débute par une introduction à la cosmologie et au CMB. Un état des lieux des mesures cosmologiques est dressé et les expériences Archeops, WMAP et Planck sont présentées.Une deuxième partie est consacrée à l'effet d'un champ magnétique primordial sur la polarisation du CMB. Nous y dérivons les spectres de puissance angulaire de cet effet et nous donnons une limite supérieure sur l'intensité actuelle de ce champ à l'aide des données de WMAP.Dans une troisième partie, nous présentons les analyses effectuées à partir des mesures de l'expérience Archeops. D'une part, nous montrons le caractère gaussien des données en température à 143 GHz, contraignant ainsi le paramètre de couplage non linéaire et les résidus systématiques et d'autre part, à l'aide des données à 353 GHz, nous montrons la première mesure de l'émission diffuse polarisée de la poussière galactique à grande échelle.Une quatrième partie présente une méthode de séparation de composantes permettant d'extraire les différentes contributions physiques à partir d'observations multifréquences, en température et en polarisation. Nous caractérisons ses performances sur des simulations du ciel vu par Planck.Enfin, dans une dernière partie, nous nous attachons à modéliser les émissions galactiques polarisées du synchrotron et de la poussière et nous comparons ces émissions simulées aux données des expériences Archeops et WMAP