Planck est un satellite de l'ESA lancé en 2009, qui avais pour mission de faire une carte de très grande précision du rayonnement fossile de l'Univers, afin de mieux comprendre comment il s'est formé. Cet objectif ambitieux nécessite un niveau de maîtrise extrême des effets instrumentaux. Cependant en cours de mission il s'est avéré que le composant responsable de la numérisation des données scientifiques introduisait un bisais important qui compromettait l'exploitation scientifique des données de l'instrument Planck/HFI. Ce travail décris comment ce biais a été compris et corrigé avec succès. Une analyse très poussée a été conduite sur les détecteurs du satellite, la chaine cryogénique embarquée et le composant de numérisation lui même. Ce qui a nécessité une méthodologie spécifique afin de télécharger les données nécessaire depuis le satellite avant sa fin de mission et son décommissionnement. / Planck is an ESA spacecraft launched in 2009, its mission goal was to map with an exquisite precision the first light of Universe, to help understanding how it has formed. This ambitious objective requires a very high level of control on the instrumental effects. During the mission, it has been found that the component responsible of the digitization of scientific data introduced an unexpectedly high bias effect, preventing full exploitation of data from the Planck/HFI instrument. The present work relates how this bias effect was understood and successfully corrected for. A very deep analysis of the spacecraft detectors, the cryogenic chain, and the digitization component has been performed, which required a specific methodology to gather data from the spacecraft before the end of the mission and its decommissioning.

PILOT (Polarized Instrument for Long wavelength Observation of the Tenuous interstellar medium) est une expérience embarquée en ballon stratosphérique destinée à la mesure de l'émission polarisée de notre galaxie dans le submillimétrique. La charge pointée de PILOT est composée d'un télescope au foyer duquel est placée une caméra embarquant 2048 bolomètres, refroidis à 300 mK, mesurant dans deux bandes spectrales (240 µm et 550 µm) et deux polarisations. La détection de la polarisation est réalisée à l'aide d'un polariseur placé à 45° dans le faisceau, le décomposant en deux composantes polarisées orthogonales chacune détectée par un bloc détecteur, et d'une lame demi-onde rotative. L'Institut d'Astrophysique Spatiale (Orsay, France) est responsable de la réalisation, de l'intégration, des tests et de l'étalonnage spectral de la caméra. Pour cela deux bancs de mesures sont développés, un pour les essais d'imagerie et de polarisation, et un pour l'étalonnage spectral. L'expérimentation permet de valider l'alignement des optiques froides, de caractériser la qualité optique des images, de caractériser les réponses temporelles et en intensité des détecteurs, et de mesurer la réponse spectrale de la caméra. Un modèle photométrique de l'instrument est développé simulant les différentes configurations pour les essais d'étalonnage spectral, d'imagerie en laboratoire, et en vol, ceci afin d'estimer la puissance totale reçue par chaque pixel du détecteur de chaque configuration. Cette puissance totale est issue de l'émission thermique de l'instrument, de l'atmosphère et des sources observées en vol ou de l'environnement du laboratoire. Une campagne de tests a permis de caractériser et d'étalonner la caméra de l'expérience PILOT. Les premières images dans le domaine du submillimétrique ont été révélées, et les premières réponses spectrales mesurées. Suite à la caractérisation et l'étalonnage spectral, la caméra est alignée avec le miroir primaire sur la nacelle CNES pour des caractérisations et des étalonnages en polarisation de l'instrument complet. Le premier vol est prévu pour le milieu de l'année 2014. / The Polarized Instrument for Long wavelength Observation of the Tenuous interstellar medium (PILOT) is a balloon borne experiment designed to measure the polarized emission from dust grains in the galaxy in the submillimeter range. The payload is composed of a telescope at the optical focus of which is placed a camera using 2048 bolometers cooled to 300 mK. The camera performs polarized optical measurements in two spectral bands (240 µm and 550 µm). The polarization measurement is based on a cryogenic rotating half-wave plate and a fixed mesh grid polarizer placed at 45° separating the beam into two orthogonal polarized components each detected by a detector array. The Institut d'Astrophysique Spatiale (Orsay, France) is responsible for the design, integration, tests and spectral calibration of the camera. Two optical benches have been designed for its imaging and polarization characterization and spectral calibration. Theses setups allow to validate the alignment of the camera cryogenic optics, to check the optical quality of the images, to characterize the time and intensity response of the detectors, and to measure the overall spectral response. A numerical photometric model of the instrument was developed for the optical configuration during calibration tests (spectral), functional tests (imager) on the ground, and flight configuration at the telescope focus, giving an estimate of the optical power received by the detectors for each configuration. The tests campaign validates the PILOT camera characterization and calibration. It delivered the first submillimeter images and the first spectral responses. Next, the camera will be aligned and integrated with the primary mirror of the telescope on the CNES gondola, for characterization and optical polarization calibration of the complete instrument. The first flight is now planned for mid 2014.

Les particules cosmiques sont émises par différentes sources galactiques et sont composées de protons et de noyaux d'hélium. Ces éléments interagissent avec les matériaux et y déposent leur énergie par interaction nucléaire. L'instrument Planck/HFI a observé le ciel depuis l'espace dans le but de cartographier le fond diffus cosmologique. Pour cela, HFI embarque un plan focal refroidit à 100 mK composé de 54 bolomètres. Le flux de particules cosmiques, interagissant avec les composants des détecteurs (thermomètre, grille, wafer), chauffe ponctuellement les capteurs (glitches) ce qui entraine une dégradation du signal scientifique. Leur étude a révélé un autre effet thermique caractérisé par un chauffage global du plan focal de l'ordre du microkelvin, les High Coincidence Events (HCE). Deux familles de HCE ont été isolées dans les données : les rapides, générés par des gerbes de particules secondaires formées dans les couches externes du satellite et interagissant avec l'ensemble de l'instrument HFI ; les lents, généré par la vaporisation d'hélium formant un lien thermique ponctuel entre le plan focal et l'étage à 1,6 K lui faisant face. L'exposition d'une matrice de bolomètres TES à une source de particules α a démontré une réponse similaire mais également des glitches simultanés entre les pixels.Ces recherches démontrent que les particules cosmiques et les gerbes de particules doivent être étudiées afin d'éviter des effets thermiques prédominant. Le développement des prochaines générations de détecteurs, devront ainsi prendre en compte ces interactions indissociables d'une mission spatiale et s'en prémunir. / Cosmic rays are emitted from different galactic sources and consist of protons and helium nuclei. These elements interact with matter and deposit part of their energy by nuclear interaction.The Planck/HFI instrument observed the sky from space to map the Cosmic Microwave Background. For this purpose, HFI has a focal plane cool down to 100 mK and composed of 54 bolometers. The interactions of the cosmic ray flux with the detectors' components (thermometer, grid and wafer) heat up regularly the sensor (glitches) which leads to a degradation of the scientific signal. Studying them revealed another thermal effect characterized by a thermal increase of the entire focal plane up to the microkelvin range, the High Coincidence Events (HCE).Two HCE famillies were separated: the fast ones, generated by cosmic ray showers developed in the external layers of the satellite and interacting with the entire HFI instrument and the slow ones, generated by the vaporisation of helium forming a ponctual thermal link between the focal plane and the 1.6 K stage facing it.Exposure of a TES bolometer matrix to an α particules source showed a similar response but also simultaneous glitches on several pixels. This work demonstrates that cosmic rays and particle showers on next low temperature experiments has to be studied to prevent predominating thermal effects from it. The developpement of futur space experiments will have to take these interactions into account to elimiate them from data.

Bolometers are the most sensitive detectors for measuring millimeter and submillimeter wavelength astrophysical signals. Cameras comprised of arrays of bolometers have already made significant contributions to the field of astronomy. A challenge for bolometer cameras is obtaining observations at multiple wavelengths. Traditionally, observing in multiple bands requires a partial disassembly of the instrument to replace bandpass filters, a task which prevents immediate spectral interrogation of a source. More complex cameras have been constructed to observe in several bands using beam splitters and dichroic filters, but the added complexity leads to physically larger instruments with reduced efficiencies. The SPEctral Energy Distribution camera (SPEED) is a new type of bolometer camera designed to efficiently observe in multiple wavebands without the need for excess bandpass filters and beam splitters. SPEED is a ground-based millimeter-wave bolometer camera designed to observe at 2.1, 1.3, 1.1, and 0.85 mm simultaneously. SPEED makes use of a new type of bolometer, the frequency selective bolometer (FSB), to observe all of the wavebands within each of the camera's four pixels. FSBs incorporate frequency selective dipole surfaces as absorbing elements allowing each detector to absorb a single, narrow band of radiation and pass all other radiation with low loss. Each FSB also contains a superconducting transition-edge sensor (TES) that acts as a sensitive thermistor for measuring the temperature of the FSB. This thesis describes the development of the SPEED camera and FSB detectors. The design of the detectors used in the instrument is described as well as the the general optical performance of frequency selective dipole surfaces. Laboratory results of both the optical and thermal properties of millimeter-wave FSBs are also presented. The SPEED instrument and its components are highlighted and the optical design of the optics which couple SPEED to the Heinrich Hertz Telescope is given. This thesis concludes with an introduction to the jiggle mapping data analysis of bolometer instruments like SPEED.

Thanks to high Tc of 40 K, high Jc of > 10^7 A.cm^-2, and no weak link behavior across the grain boundary in MgB2 material. This highest Tc among all conventional BCS superconductors, and better material properties of MgB2 compared to high Tc cuprate superconductors makes this material attractive for many applications including, but not limited to, power cables, Josephson junction based electronic devices, SRF cavities, THz sensors and single photon counters. Ultrathin superconducting films are a key element in various detectors utilized in remote sensing over a large part of the entire electromagnetic spectrum. The superconducting hot electron bolometer (HEB) mixer is a crucial detector for high-resolution spectroscopy at THz frequencies. The state-of-the-art NbN phonon-cooled HEB mixers have a relatively narrow (IF) bandwidth ~ 3- 4 GHz as a direct result of the poor acoustic transparency of the film-substrate interface and low sound velocity in NbN reducing the phonon escape time in the film. Alternatively, MgB2 displays a very short τe-ph ~ ps. The phonon escape time is also short due to the high sound velocity in the material (~ 7 Km.s^-2) thus giving rise to a broader IF bandwidth. Also, smaller magnetic penetration depth (λ ≈ 40 nm) of MgB2 makes material of choices for single photon detector application. The response time of an SNSPD is proportional to the square of its magnetic penetration depth λ. Therefore, MgB2 may potentially operate 10-fold faster than the NbN (λ =200 nm) based SNSPD. In this work, I present my effort to fabricate high quality ultrathin superconducting MgB2 films on 6H-SiC (0001) substrates, and study their superconducting and electronic properties. C- epitaxial 10 nm showed Tc of above 36 K, while residual resistivity of up to 26 μΩ.cm was achieved. Critical currents of more than 6 × 10^6 A · cm^−2 at 20 K have been measured for the films with thicknesses iv ranging from 10 to 100 nm. Fishtail structures have been observed in the magnetic field dependence of the critical current density for the thinnest of these films, indicating the presence of defects, which act as vortex pinning centers. From the magnetic field dependence, an average distance between adjacent pinning centers of 35 nm has been obtained for the thinnest films. Ultrathin film as thin as 1.8 nm (6 unit cells) can be achieved by Hybrid Physical-Chemical Vapor Deposition (HPCVD) followed by low angle Ar ion milling. These post processed films exhibit better superconducting properties compared to directly grown films. The 1.8 nm, showed Tc > 28 K and Jc > 10^6 A/cm^2 4 K. The surface roughness of the films was significantly improved and the suppression of Tc from the bulk value is much slower in milled films than in as-grown films. These results show the great potential of these ultrathin films for superconducting devices and present a possibility to explore superconductivity in MgB2 at the 2D limit. Finally, I measured the upper critical field of MgB2 films of various thickness and extracted their thickness dependent in-plane intraband diffusivities by using Gurevich model developed for two-band MgB2 superconductor in dirty limit. Results showed that π band diffusivity (Dπ) decreases rapidly from 71.12 cm^2/s for 100 nm film to 4.6 cm^2/s for 5 nm film where as �� band diffusivity (����) decreases much slower from 2.8 cm^2/s for 100 nm film to 0.8 cm^2/s for 5 nm film. This larger Dπ than ���� indicates the cleaner π band. / Physics

Noise in electronic circuits can sometimes cause problems. It is especially problematic in for example high sensitive sensors and high end audio and video equipment. In audio and video equipment the noise will make its way into the sound and picture reducing the overall quality. Sensors that are constructed to sense extremely small changes can only pick up changes larger than the noise floor of the circuit. By lowering the noise, sensors can achieve higher accuracy.  This thesis presents an ultra low noise solution of the biasing circuitry to the bolometer used in one of FLIR Systems high end cameras. The bolometer uses different adjustable direct current voltage sources and is extremely sensitive to noise. The purpose is to improve the picture quality and the thermal measurement resolution. A prototype circuit was constructed and in the end of the thesis a final circuit with successful result will be presented.

L’objectif de cette thèse est le développement des détecteurs pour la microscopie champproche électromagnétique pour deux domaines fréquentiels. Pour le domaine des microondesnous présentons des micro-antennes non conventionnelles basées sur un guidagecoplanaire et l’effet de pointe. Nous pr´esentons les différentes étapes de la conceptionet de la réalisation avec les techniques de micro-fabrication. L’évaluation de leur performancea été obtenue avec une confrontation des résultats de mesure et de cartographie surdes éléments passifs et ceux d’une modélisation d’intégration finie. Pour le domaine desTérahertz, nous avons réalisé des micro-bolométres à température ambiante. Dans le butd’améliorer l’absorption de ces d´etecteurs, leur conception a été basée sur l’étude théoriquede l’absorption d’une onde électromagnétique en incidence normale sur un empilement descouches métalliques et diélectrique. Deux versions ont été réalisées et caractérisées é l’aidedes sources électroniques qui peuvent atteindre 1, 1 THz en continue. Les performancesde ces d´etecteurs en termes de bruit, de sensibilit´e et de temps de r´eponse sont mises enexergue. / The objective of this thesis is the development of detectors for near-field microscopy fortwo electromagnetic frequency domains. For microwave domain we present unconventionalmicro-antennas based on coplanar line and point effect. We present the different stages ofthe design and implementation with micro-fabrication technique. The evaluation of theirperformance was obtained with a comparison of measurement results and mapping ofpassive elements and those of a model of finite integration. For the THz domain, we performedroom temperature micro-bolometers. In order to improve the absorption of thesedetectors, their design was based on the theoretical study of the absorption of an electromagneticwave normally incident on a stack of metal and dielectric layers. Two versionswere prepared and characterized using electronic sources that can reach continuous 1,1THz. The performance of these detectors in terms of noise, sensitivity and time responseare highlighted.

Nous avons développé un récepteur hétérodyne terahertz (THz) compact et ultra-sensible à base de laser à cascade quantique (QCL) comme oscillateur local et de bolomètre à électron chaud (HEB) comme mélangeur. Le récepteur est basé sur un nouveau concept pour le couplage quasi-optique entre l'oscillateur local et le mélangeur ce qui a permis de ne pas utiliser de lame semi-réfléchissante pour la superposition du signal provenant du QCL et du signal à détecter. Le mélangeur utilisé est un HEB en nitrure de niobium avec une antenne planaire formée d’une double hélice log-spiral. Le HEB est monté sur la partie plane d’une lentille convexe en silicium. L’oscillateur local est un QCL que nous avons développé avec un système de contre-réaction répartie du troisième ordre avec une faible dissipation thermique, un faisceau peu divergent et un fonctionnement mono-mode à la fréquence cible de 2.7 THz. Le couplage entre l’oscillateur local et le mélangeur HEB a également été amélioré en couplant le QCL avec une fibre creuse en diélectrique ce qui a permis d’améliorer la directivité du faisceau laser à 55 dBi. Grâce aux précédents résultats, nous avons obtenu un récepteur THz hétérodyne compact qui présente une sensibilité proche de l’état de l’art à 2.7 THz. / We demonstrate an ultra-compact Terahertz (THz) heterodyne detec- tion system based on a quantum cas- cade laser (QCL) as local oscillator and a hot electron bolometer (HEB) for the mixing. It relies on a new opti- cal coupling scheme where the local oscillator signal is coupled through the air side of the planar HEB an- tenna, while the signal to be de- tected is coupled to the HEB through the lens. This technique allows us to suppress the beam splitter usu- ally employed for heterodyne mea- surements. The mixer is a Niobium Nitride HEB with a log-spiral planar antenna on silicon and mounted on the back of a plano-convex silicon lens. We have developed a low power consumption and low beam di- vergence 3rd-order distributed feed- back laser with single mode emis- sion at the target frequency of 2.7 THz to be used as local oscillator for the heterodyne receiver. The cou- pling between the QC laser and the the HEB has been further optimized, using a dielectric hollow waveguide that reliably increases the laser beam directivity up to 55 dBi. Upon the high beam quality, sufficient output power in a single mode at the tar- geted frequency and low power dissi- pation of our local oscillator, we have build an ultra compact THz hetero- dyne receiver with sensitivity close to the state of the art at 2.7 THz.

<p>Thermistor material can be used to fabricate un-cooled IR detectors their figure of merit is the Temperature Coefficient of Resistance (TCR). Ge dots in Si can act as a thermistor material and they have a theoretical TCR higher than for SiGe layers but they suffer from intermixing of Si into the Ge dots. Ge dots were grown on unstrained or strained Si layers and relaxed or strained SiGe layers at temperatures of 550 and 600°C by reduced pressure chemical vapor deposition (RPCVD). Both single and multilayer structures where grown and characterized. To achieve a strong signal in a thermal detector a uniform shape and size distribution of the dots is desired. In this thesis work, an endeavor has been to grow uniform Ge dots with small standard deviation of their size. Scanning electron microscopy (SEM) and Atomic force microscopy (AFM) have been used to characterize the size and shape distribution of Ge dots. Ge contents measured with Raman spectroscopy are higher at lower growth temperatures. Simulation of TCR for the most uniform sample grown at 600°C give 4.43%/K compared to 3.85%/K for samples grown at 650°C in a previous thesis work.</p><p>Strained surfaces increases dot sizes and make dots align in crosshatched pattern resulting in smaller density, this effect increases with increasing strain.</p><p>Strain from buried layers of Ge dots in a multilayer structure make dots align vertically. This alignment of Ge dots was very sensitive to the thickness of the Si barrier layer. The diameter of dots increase for each period in a multilayer structure. When dots are capped by a Si layer at the temperature of 600°C intermixing of Si into the Ge dot occurs and the dot height decrease.</p>

Thermistor material can be used to fabricate un-cooled IR detectors their figure of merit is the Temperature Coefficient of Resistance (TCR). Ge dots in Si can act as a thermistor material and they have a theoretical TCR higher than for SiGe layers but they suffer from intermixing of Si into the Ge dots. Ge dots were grown on unstrained or strained Si layers and relaxed or strained SiGe layers at temperatures of 550 and 600°C by reduced pressure chemical vapor deposition (RPCVD). Both single and multilayer structures where grown and characterized. To achieve a strong signal in a thermal detector a uniform shape and size distribution of the dots is desired. In this thesis work, an endeavor has been to grow uniform Ge dots with small standard deviation of their size. Scanning electron microscopy (SEM) and Atomic force microscopy (AFM) have been used to characterize the size and shape distribution of Ge dots. Ge contents measured with Raman spectroscopy are higher at lower growth temperatures. Simulation of TCR for the most uniform sample grown at 600°C give 4.43%/K compared to 3.85%/K for samples grown at 650°C in a previous thesis work. Strained surfaces increases dot sizes and make dots align in crosshatched pattern resulting in smaller density, this effect increases with increasing strain. Strain from buried layers of Ge dots in a multilayer structure make dots align vertically. This alignment of Ge dots was very sensitive to the thickness of the Si barrier layer. The diameter of dots increase for each period in a multilayer structure. When dots are capped by a Si layer at the temperature of 600°C intermixing of Si into the Ge dot occurs and the dot height decrease.