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1. Pilot optical alignment

Author

Nicolas Ponthieu, F. Pajot, J. M. Nicot, M. Chaigneau, G. Parot, Giorgio Savini, Y. André, M. Bouzit, Nicolas Bray, Johan Montel, C. Tucker, J.-P. Dubois, J. Martignac, J. Aumont, Maria Salatino, O. Simonella, V. Buttice, Bruno Maffei, R. J. Laureijs, R. Misawa, J.-Ph. Bernard, Frederi Mirc, B. Mot, J. Narbonne, Silvia Masi, O. Boulade, C. Engel, Etienne Perot, E. Doumayrou, A. Caillat, J. A. Tauber, C. Coudournac, A. Hughes, I. Ristorcelli, Y. Lepennec, S. Maestre, Pierre Tapie, Y. Longval, P. de Bernardis, F. Bousquet, G. Foenard, S. Grabarnik, Giampaolo Pisano, G. Roudil, P. Etcheto, P. Gélot, B. Leriche, Muriel Saccoccio, J. P. Crussaire, J. Pimentao, C. Marty, Matthew Joseph Griffin, Peter A. R. Ade, L. Baustista, M. Charra, F. Douchin, J.-P. Torre, L. Rodriguez, L. Montier, Peter Charles Hargrave, B. Crane, W. Marty, and G. Versepuech

Subjects
Physics, Optical alignment, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), Galaxy, Interstellar medium, Wavelength, Long wavelength, Optics, business, Astrophysics::Galaxy Astrophysics, Dust emission, Ontario canada
Abstract

PILOT (Polarized Instrument for Long wavelength Observations of the Tenuous interstellar medium) is a balloonborne astronomy experiment designed to study the polarization of dust emission in the diffuse interstellar medium in our Galaxy. The PILOT instrument allows observations at wavelengths 240 μm (1.2THz) with an angular resolution about two arc-minutes. The observations performed during the first flight in September 2015 at Timmins, Ontario Canada, have demonstrated the optical performances of the instrument.

Published
2017

2. The PILOT optical alignment for its first flight

Author

G. Roudil, B. Mot, Y. Longval, W. Marty, J. Aumont, R. Misawa, A. Caillat, Y. Lepennec, E. Doumayrou, G. Foënard, J. A. Tauber, A. Hughes, G. Parot, L. Montier, J. Pimentao, M. Chaigneau, F. Pajot, J.-Ph. Bernard, B. Crane, Johan Montel, B. Leriche, M. Bouzit, Nicolas Bray, V. Buttice, Nicolas Ponthieu, Pierre Tapie, Isabelle Ristorcelli, J. M. Nicot, Muriel Saccoccio, Giorgio Savini, F. Douchin, P. deBernardis, C. Coudournac, Frederi Mirc, J. Martignac, Etienne Perot, Bruno Maffei, J.-P. Torre, C. Engel, A. Mangilli, L. Rodriguez, Peter Charles Hargrave, S. Maestre, Y. André, Silvia Masi, L. Bautista, P. Etcheto, C. Marty, S. Stever, S. Grabarnik, Maria Salatino, O. Simonella, Giampaolo Pisano, J.-P. Dubois, Carole Tucker, P. Gélot, René J. Laureijs, F. Bousquet, Matthew Joseph Griffin, Peter A. R. Ade, J. Narbonne, Christopher Tibbs, and O. Boulade

Subjects
Cryostat, Optical alignment, Physics::Optics, Aerospace Engineering, Astrophysics, 01 natural sciences, law.invention, 010309 optics, Primary mirror, Optics, law, Polarization, 0103 physical sciences, Optical instrumentation, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Gregorian telescope, business.industry, Submillimeter telescope, Polarization (waves), Galaxy, Interstellar medium, Wavelength, Space and Planetary Science, business
Abstract

PILOT is a balloon-borne astronomy experiment designed to study the polarization of dust emission in the diffuse interstellar medium in our Galaxy at wavelengths 240 and 550 µm with an angular resolution of about two arc-min. PILOT optics is composed of an off-axis Gregorian telescope and a refractive re-imager system. All these optical elements, except the primary mirror, are in a cryostat cooled to 3K. We used optical and 3D measurements combined with thermo-elastic modeling to perform the optical alignment. This paper describes the system analysis, the alignment procedure, and finally the performances obtained during the first flight in September 2015

Published
2017

3. The optical performance of the PILOT instrument from ground end‐to‐end tests

Author

Y. Longval, O. Boulade, Maria Salatino, O. Simonella, René J. Laureijs, Nicolas Ponthieu, B. Leriche, Y. André, L. Bautista, J. Narbonne, J. A. Tauber, J. P. Dubois, Muriel Saccoccio, Carole Tucker, G. Roudil, Matthew Joseph Griffin, Peter A. R. Ade, Giorgio Savini, Isabelle Ristorcelli, J. Pimentao, L. Rodriguez, A. Caillat, B. Mot, M. Bouzit, A. Hughes, Peter Charles Hargrave, C. Engel, F. Bousqet, J. Montel, B. Maffei, E. Doumayrou, Silvia Masi, J.-P. Bernard, D. Alina, S. Maestre, G. Foënard, P. de Bernardis, L. Montier, M. Chaigneau, J. Aumont, R. Misawa, M. Charra, F. Douchin, W. Marty, Etienne Perot, C. Marty, V. Buttice, S. Grabarnik, Giampaolo Pisano, F. Pajot, B. Crane, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Point spread function, Image quality, Far infrared, 01 natural sciences, 010309 optics, Optics, Polarization, 0103 physical sciences, PILOT, Straylight, 010303 astronomy & astrophysics, QB, Remote sensing, Cosmic dust, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Linear polarization, business.industry, Detector, Interstellar dust, Astronomy and Astrophysics, Space and Planetary Science, Polarization (waves), Wavelength, Cardinal point, business
Abstract

International audience; The Polarized Instrument for Long‐wavelength Observation of the Tenuous interstellar medium (PILOT) is a balloon‐borne astronomy experiment designed to study the linear polarization of thermal dust emission in two photometric bands centred at wavelengths 240 mu m (1.2 THz) and 550 mu m (545 GHz), with an angular resolution of a few arcminutes. Several end‐to‐end tests of the instrument were performed on the ground between 2012 and 2014, in order to prepare for the first scientific flight of the experiment that took place in September 2015 from Timmins, Ontario, Canada. This paper presents the results of those tests, focussing on an evaluation of the instrument's optical performance. We quantify image quality across the extent of the focal plane, and describe the tests that we conducted to determine the focal plane geometry, the optimal focus position, and sources of internal straylight. We present estimates of the detector response, obtained using an internal calibration source, and estimates of the background intensity and background polarization.

Published
2017

4. Following lithiation fronts in paramagnetic electrodes with in situ magnetic resonance spectroscopic imaging

Author

Vincent Sarou-Kanian, Elodie Salager, J. B. Leriche, Michaël Deschamps, Jean-Marie Tarascon, Philippe Melin, Mingxue Tang, Michel Ménétrier, Réseau sur le stockage électrochimique de l'énergie (RS2E), Université de Picardie Jules Verne (UPJV)-Institut de Chimie du CNRS (INC)-Aix Marseille Université (AMU)-Université de Pau et des Pays de l'Adour (UPPA)-Université de Nantes (UN)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Collège de France (CdF (institution))-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Université Grenoble Alpes (UGA)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Ecole Nationale Supérieure de Chimie de Montpellier (ENSCM), Conditions Extrêmes et Matériaux : Haute Température et Irradiation (CEMHTI), Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université d'Orléans (UO), Laboratoire réactivité et chimie des solides - UMR CNRS 7314 (LRCS), Université de Picardie Jules Verne (UPJV)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Institut de Chimie de la Matière Condensée de Bordeaux (ICMCB), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut Polytechnique de Bordeaux-Université de Bordeaux (UB), Advanced Lithium Energy Storage Systems - ALISTORE-ERI (ALISTORE-ERI), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Chaire Chimie du solide et énergie, Chimie du solide et de l'énergie (CSE), Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU), the European Commission through the European Regional Development Fund (ERDF/FEDER) in region Centre (France), RS2E network, ANR-10-LABX-0076,STORE-EX,Laboratory of excellency for electrochemical energy storage(2010), ANR-14-CE05-0015,ASTORIX,Absorbeurs Solaires haute Température Oxydo-Résistants mIcroteXturés(2014), Université de Nantes (UN)-Aix Marseille Université (AMU)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Collège de France (CdF (institution))-Université de Picardie Jules Verne (UPJV)-Ecole Nationale Supérieure de Chimie de Montpellier (ENSCM)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Pau et des Pays de l'Adour (UPPA)-Institut de Chimie du CNRS (INC)-Université de Montpellier (UM)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Université Grenoble Alpes (UGA), Université d'Orléans (UO)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Université de Picardie Jules Verne (UPJV)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Université de Bordeaux (UB)-Institut Polytechnique de Bordeaux-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Collège de France - Chaire Chimie du solide et énergie, and Collège de France (CdF (institution))-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
In situ, Battery (electricity), Materials science, Field (physics), Science, General Physics and Astronomy, 02 engineering and technology, 010402 general chemistry, 01 natural sciences, Article, General Biochemistry, Genetics and Molecular Biology, Paramagnetism, Nuclear magnetic resonance, Hardware_GENERAL, Electronics, Multidisciplinary, business.industry, Magnetic resonance spectroscopic imaging, General Chemistry, [CHIM.MATE]Chemical Sciences/Material chemistry, Magnetic field gradient, 021001 nanoscience & nanotechnology, 0104 chemical sciences, Electrode, Optoelectronics, 0210 nano-technology, business
Abstract

Li-ion batteries are invaluable for portable electronics and vehicle electrification. A better knowledge of compositional variations within the electrodes during battery operation is, however, still needed to keep improving their performance. Although essential in the medical field, magnetic resonance imaging of solid paramagnetic battery materials is challenging due to the short lifetime of their signals. Here we develop the scanning image-selected in situ spectroscopy approach, using the strongest commercially available magnetic field gradient. We demonstrate the 7Li magnetic resonance spectroscopic image of a 5 mm-diameter operating battery with a resolution of 100 μm. The time-resolved image-spectra enable the visualization in situ of the displacement of lithiation fronts inside thick paramagnetic electrodes during battery operation. Such observations are critical to identify the key limiting parameters for high-capacity and fast-cycling batteries. This non-invasive technique also offers opportunities to study devices containing paramagnetic materials while operating., Magnetic resonance imaging is a promising non-invasive approach to visualize paramagnetic materials in devices, but the short lifetime of signals currently limits its use. Here, the authors develop an approach which overcomes this hurdle to spectroscopically image lithiation fronts during battery operation.

Published
2016

5. Synthèse des recommandations pour le traitement de l’incontinence urinaire féminine non neurologique

Author

L. Peyrat, P. Berlizot, V. Cardot, E. Delorme, Loic Lenormand, B Leriche, R. Yiou, A. Vidart, S. Conquy, L. Boccon Gibod, P. Ballanger, François Richard, J.-F. Hermieu, P. Debodinance, F. Cour, E. Ragni, and A. Cortesse

Subjects
business.industry, Urology, Medicine, business, Humanities
Abstract

Resume Ces deux dernieres decennies ont permis de voir apparaitre de nouveaux traitements medicaux ou chirurgicaux revolutionnant la prise en charge de l’incontinence urinaire feminine non neurologique. De nombreuses etudes souvent prospectives randomisees, avec des reculs suffisants, ont permis de valider les bons choix therapeutiques en dehors des effets de mode et des pressions commerciales. L’Association Francaise d’Urologie, par le biais de son Comite d’Urologie et de Pelviperineologie de la Femme, propose ses recommandations. Celles-ci ont ete etablies par un groupe d’experts des specialites concernees (Urologues, Gynecologues, Reeducateurs), a partir d’une revue de la litterature, mais en tenant compte des pratiques quotidiennes universitaires et liberales. Entre Evidence Base Medicine et realite du terrain, ces recommandations essayent de proposer des attitudes realistes et applicables.

Published
2010

6. Recommandations pour la prise en charge rééducative de l’incontinence urinaire non neurologique de la femme

Author

B. Leriche and S. Conquy

Subjects
medicine.medical_specialty, Pelvic floor, Rehabilitation, business.industry, Urology, medicine.medical_treatment, MEDLINE, Uterine prolapse, Urinary incontinence, Biofeedback, medicine.disease, Session (web analytics), medicine.anatomical_structure, medicine, Physical therapy, Medical prescription, medicine.symptom, business
Abstract

Pelvic floor rehabilitation is prescribed as first-line treatment for women with stress urinary incontinence, particularly in cases of urinary incontinence with no first-degree uterine prolapse, with poor-quality perineal testing results or inverted perineal command. Prescription of 15 sessions should suffice to evaluate the possibilities of improving the incontinence. The sessions can be continued if the patient feels she is progressing but has not reached sufficient results. With no progression despite properly conducted rehabilitation, the question of whether to continue the physical therapy arises. Currently, therapists determine the number of sessions. They are better apt to know whether sessions should be pursued and should relay a report to the prescribing physician. This type of rehabilitation is within the domain of physical therapists. Midwives can be responsible for postpartum rehabilitation. On the other hand, the importance of the patient's role in the results and their maintenance is well known. Occasionally a few sessions some time after the initial sessions can serve to verify the acquisitions and motivate the patient in her personal contribution to this rehabilitation. The work of the physical therapist cannot be substituted with Keat-type home electrostimulation. The physical therapist plays an important role in the overall management of this condition. Currently, in absence of demonstrated efficacy, self-administration of electrostimulation is not recommended. In urge incontinence, the rehabilitation approach will be used concomitantly with prescription of anticholergics with behavioral therapy and bladder biofeedback work. In addition, low-frequency electrostimulation can be done during the session. Starting with 10-12 sessions is sufficient. In all cases, rehabilitation should take a multidisciplinary approach and be integrated into a medical and/or surgical management plan.

Published
2010

7. Prise en charge neurochirurgicale de la paraplégie tuberculeuse : à propos de six cas

Author

S. Taha, B. Leriche, K. Doe, L. Nogues, and M. Lopes

Subjects
Spondylodiscitis, medicine.medical_specialty, business.industry, medicine.medical_treatment, Kyphosis, Laminectomy, Perioperative, medicine.disease, Surgery, Spinal decompression, medicine, Neurology (clinical), Complication, business, Paraplegia, Rare disease
Abstract

Tuberculosis is a rare disease in economically developed countries. Paraplegia is one of its severe complications, occurring in cases of spondylodiscitis with compressive epiduritis and/or pathological fracture of vertebral bodies with subacute kyphosis. Six patients aged 15–75 years were treated in our department from May 2005 to April 2006 by the same operator (L.N.) for paraplegia complicating Pott's disease. Patients’ neurologic function at admission and their outcomes three and 12 months after surgery were graded using the Frankel classification. MRI showed a single lesion in five cases and skip lesions in one case. Standard antituberculosis chemotherapy was started immediately within the first week of admission in five patients following a 12-month regimen. Principles of surgical treatment were ventral spinal cord decompression (with or without dorsal stage procedure), immediate grafting, correction of subacute spinal deformity and instrumentation in all cases. The diagnosis of Mycobacterium tuberculosis was confirmed by laboratory investigations in four cases and by histopathological examination in all cases. One patient who had undergone prior isolated laminectomy performed by an on call team presented neurological deterioration and progressive kyphosis. Neurological outcome improved in five patients. Four of them were able to walk unaided within the first three months after surgery. No perioperative complication occurred. In paraplegia complicating vertebral tuberculosis, overall neurological outcome appeared to be good in case of delayed emergency surgical management combined with antituberculosis chemotherapy.

Published
2009

8. Bolometers at CEA: ARTEMIS and beyond

Author

B. Horeau, P. O. Lagage, C. Delisle, D. Rabanus, J. Relland, O. Boulade, C. De Breuck, Pascal André, E. Doumayrou, L. Rodriguez, Didier Dubreuil, V. Minier, E. Ercolani, P. Gallais, J. Martignac, M. Talvard, Vincent Reveret, G. Willmann, François Visticot, E. Pantin, P. Agnèse, B. Leriche, M. Lortholary, and Y. Le-Pennec

Subjects
Physics, business.industry, Bolometer, Detector, General Engineering, Astronomy and Astrophysics, Astrophysics, Cryogenics, Space exploration, law.invention, Telescope, Space and Planetary Science, law, Electronics, Aerospace engineering, business
Abstract

ArTeMiS is a bolometer camera that will be installed at the APEX submillimeter telescope in Chile in 2010. This instrument will be a powerful tool for scientists with its three focal planes that will operate simultaneously in background limited conditions at 200, 350 and 450 microns (5760 pixels in total). A prototype called p-ArTeMiS has been tested at APEX in 2007 and thanks to its good performances, the team has been able to conduct scientific projects in star formation and on debris disks. This paper summarises the details of the ArTeMiS project, with a description of the detectors, the optics, the cryogenics and the electronics. We will also present the undergoing studies at CEA on detectors for the future submillimeter space missions.

Published
2009

9. Large Bolometer Arrays with Superconducting NbSi Sensors for Future Space Experiments

Author

M. Giard, L. Bergé, F. Pajot, B. Leriche, J. P. Torre, S. Lefranc, L. Dumoulin, E. Bréelle, Y. Atik, M. Piat, D. Santos, N. Marsot, Benoit Belier, Alain Benoit, C. Evesque, C. Hoffmann, D. Prêle, Yun Jin, Philippe Camus, T. Durand, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'électronique fondamentale (IEF), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Cryogénie (Cryo), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de photonique et de nanostructures (LPN), Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Cryo - Cryogénie, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics::Instrumentation and Detectors, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Multiplexing, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, law, 0103 physical sciences, Microelectronics, General Materials Science, Sensitivity (control systems), [SPI.NANO]Engineering Sciences [physics]/Micro and nanotechnologies/Microelectronics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Superconductivity, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Cardinal point, Optoelectronics, Millimeter, Transition edge sensor, business
Abstract

International audience; New techniques in microelectronics allow to build large arrays of bolometers filling the focal plane of submillimeter and millimeter telescopes. The expected sensitivity increase is the key for the next generation of space experiments in this wavelength range. Superconducting bolometers offer currently the best prospects in terms of sensitivity and multiplexed readout. We present here the developments led in France based on NbSi alloy thermometers. The manufacturing process of a 23 pixel array and the test setup are described.

Published
2008

10. Modeling of Single Electron Charging in Nanocrystal Memories

Author

Y. Leroy, B. Leriche, A.S. Cordan, Jung, Marie-Anne, Institut d'Electronique du Solide et des Systèmes (InESS), and Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS)

Subjects
Materials science, Condensed Matter::Other, business.industry, Transistor, Doping, Nanotechnology, Charge (physics), Condensed Matter::Mesoscopic Systems and Quantum Hall Effect, Symmetry (physics), Computer Science Applications, Theoretical Computer Science, law.invention, Condensed Matter::Materials Science, Nanocrystal, law, Excited state, Optoelectronics, Electrical and Electronic Engineering, business, Quantum tunnelling, Communication channel
Abstract

A three-dimensional model is proposed to describe single electron charging into the nanocrystals that compose the floating gate of a metal-oxide-semiconductor transistor. It is built on the physical and geometrical parameters of the device. If the nanocrystals have a cylindrical symmetry, the 3D approach can be analytically reduced to a 2D model. Different effects that play an important part on single electron charging, such as the electrostatic coupling between two nanocrystals and the doping density of the channel, are analysed. Moreover the necessity of including the excited states of the nanocrystals and the subbands of the channel is shown. Finally the tunneling times to charge the nanocrystals in the floating gate from the channel are simulated and discussed.

Published
2006

11. Electrostatic coupling between nanocrystals in a quantum flash memory

Author

A.S. Cordan, B. Leriche, Y. Leroy, Institut d'Electronique du Solide et des Systèmes (InESS), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), and Jung, Marie-Anne

Subjects
Materials science, business.industry, Oxide, Electrical engineering, Condensed Matter Physics, Flash memory, Electronic, Optical and Magnetic Materials, chemistry.chemical_compound, Flash (photography), Tunnel effect, chemistry, Nanocrystal, Materials Chemistry, Optoelectronics, Electrical and Electronic Engineering, business, Layer (electronics), Quantum, Quantum tunnelling
Abstract

In quantum flash memories, the floating gate is a nanocrystal (NC) layer which can be charged from the channel. To our knowledge, no attempt has been carried out to evaluate the interactions between nanocrystals inside a layer. On the contrary, since the NCs are commonly supposed to be independent, reduced systems of single NC are often considered. In our model and simulations, we show that the NC charging is not only related to relevant thicknesses (tunnel, oxide) and NC radii, but also to the electrostatic coupling that exists between two nanocrystals inside the floating gate layer.

Published
2006

12. Méningite lymphocytaire : Listeria monocytogenes, une étiologie à ne pas négliger chez l'enfant immunocompétent

Author

R. Mesnage, L. Houdon, A. Edmar, Patrick Gérardin, S. Picot, B. Leriche, J. Comoy, and H. Flodrops

Subjects
Gynecology, medicine.medical_specialty, Listeria monocytogenes, business.industry, Lymphocytic meningitis, Pediatrics, Perinatology and Child Health, medicine, medicine.disease_cause, medicine.disease, business, Meningitis
Abstract

Resume Les meningites a listeria chez l'enfant immunocompetent sont exceptionnelles et ne sont pas denuees de complications. Observation. - Nous rapportons le cas d'une meningite lymphocytaire decapitee par la vancomycine chez une fillette de sept ans. Le diagnostic de listeriose cerebromeningee a ete porte sur l'apparition secondaire d'une hydrocephalie due a une arachnoidite au niveau de la jonction du troisieme ventricule et de l'aqueduc de Sylvius. Conclusion. – Cette observation souligne l'interet d'associer de l'amoxicilline a l'antibiotherapie probabiliste de toute meningite lymphocytaire sans bacterie identifiee, avec un important syndrome inflammatoire biologique, chez l'enfant immunocompetent compris.

Published
2005

13. Traitement des rectocèles et des élytrocèles par voie abdominale : apport de la laparoscopie

Author

O Daville, J.P Grandjean, B Seket, P Dubernard, R Chircop, J.P Galaup, J. F. Lapray, and B Leriche

Subjects
Gynecology, medicine.medical_specialty, Anorectal disease, business.industry, medicine, Surgery, business
Abstract

Resume But de l’etude. – Le but du travail est de rapporter les resultats de la promontofixation rectale associee a une douglassectomie dans le traitement des rectoceles et des elytroceles. Materiel et methodes. – Il s’agissait d’une etude retrospective concernant 72 patientes operees par le meme operateur a vocation coloproctologique entre 1992 et 2002. Une intervention par laparotomie avait ete realisee 37 fois entre 1992 et 2001. La voie laparoscopique a ete adoptee chez 35 patientes entre 1995 et 2002. Une promontofixation rectale fut realisee par une seule bandelette prothetique fixee sur la face anterolaterale droite du rectum et au ligament commun prevertebral. La meme bandelette fut aussi utilisee pour fixer l’appareil genital. Les gestes urinaires associes furent tres frequents, soit therapeutiques soit prophylactiques. Resultats. – Les resultats a distance furent apprecies pour 63 malades qui avaient un recul superieur a un an. Il n’y avait aucune malade perdue de vue. Le recul moyen fut de 58 mois. Une recidive de la tumefaction vaginale fut notee chez deux patientes. On nota que la promontofixation ameliore la dyschesie dans 80 % des cas, les troubles de la continence anale dans 95 % des cas et l’incontinence urinaire associee dans 70 % des cas. Conclusion. – L’approche abdominale est le traitement de choix des volumineuses rectoceles et elytroceles associees a d’autres troubles de la statique pelvienne notamment a un prolapsus rectal interne et/ou a une descente importante du plancher pelvien. L’abord par cœlioscopie ajoute ses avantages avec une moindre morbidite et aussi une amelioration du resultat fonctionnel.

Published
2004

14. The ArT\'eMiS wide-field submillimeter camera: preliminary on-sky performances at 350 microns

Author

Bruno Maffei, Agnès Arnaud, Louis Rodriguez, Jean-Charles Cigna, J. Relland, Patrick Agnese, Jean Le Pennec, B. Leriche, Lionel Duband, Luc Dumaye, Wilfried Rabaud, Eric Doumayrou, Vincent Reveret, Michel Talvard, Elodie Groult, Pascal Gallais, P. Andre, L. Clerc, Jérôme Martignac, Carlos De Breuck, Didier Dubreuil, Thierry Jourdan, François Visticot, Michel Lortholary, Aurélie Vandeneynde, Cyrille Delisle, and Eric Ercolani

Subjects
Physics, business.industry, media_common.quotation_subject, Bolometer, Uranus, Photometer, 01 natural sciences, 7. Clean energy, law.invention, 010309 optics, Telescope, Cardinal point, Optics, 13. Climate action, Sky, law, 0103 physical sciences, Calibration, Millimeter, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, media_common
Abstract

ArTeMiS is a wide-field submillimeter camera operating at three wavelengths simultaneously (200, 350 and 450 microns). A preliminary version of the instrument equipped with the 350 microns focal plane, has been successfully installed and tested on APEX telescope in Chile during the 2013 and 2014 austral winters. This instrument is developed by CEA (Saclay and Grenoble, France), IAS (France) and University of Manchester (UK) in collaboration with ESO. We introduce the mechanical and optical design, as well as the cryogenics and electronics of the ArTeMiS camera. ArTeMiS detectors are similar to the ones developed for the Herschel PACS photometer but they are adapted to the high optical load encountered at APEX site. Ultimately, ArTeMiS will contain 4 sub-arrays at 200 microns and 2x8 sub-arrays at 350 and 450 microns. We show preliminary lab measurements like the responsivity of the instrument to hot and cold loads illumination and NEP calculation. Details on the on-sky commissioning runs made in 2013 and 2014 at APEX are shown. We used planets (Mars, Saturn, Uranus) to determine the flat-field and to get the flux calibration. A pointing model was established in the first days of the runs. The average relative pointing accuracy is 3 arcsec. The beam at 350 microns has been estimated to be 8.5 arcsec, which is in good agreement with the beam of the 12 m APEX dish. Several observing modes have been tested, like On-The-Fly for beam-maps or large maps, spirals or raster of spirals for compact sources. With this preliminary version of ArTeMiS, we concluded that the mapping speed is already more than 5 times better than the previous 350 microns instrument at APEX. The median NEFD at 350 microns is 600 mJy.s1/2, with best values at 300 mJy.s1/2. The complete instrument with 5760 pixels and optimized settings will be installed during the first half of 2015., Comment: 11 pages, 11 figures. Presented at SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, June 24, 2014. To be published in Proceedings of SPIE Volume 9153

Published
2014

15. Thermal architecture design tests for the Planck/HFI instrument

Author

M. Piat, J.-P. Torre, J. P. Crussaire, J.-M. Lamarre, B. Leriche, and Alain Benoit

Subjects
Physics, Nuclear and High Energy Physics, business.industry, media_common.quotation_subject, Bolometer, Architecture design, law.invention, Wavelength, symbols.namesake, Optics, law, Sky, Thermal, symbols, Satellite, Millimeter, Planck, business, Instrumentation, media_common
Abstract

The ESA satellite project Planck is designed to survey the sky at sub-millimetre and millimetre wavelengths in a drift scan mode. The High-Frequency Instrument (HFI) will use 48 bolometers cooled to 100 mK by a dilution cooler. In this paper, we describe how the scan strategy leads to requirements on the 0.1 K stage temperature stability and how a combination of a passive and an active system can be used to approach this specification.

Published
2000

16. Calibration and first light of the Diabolo photometer at the Millimetre and Infrared Testa Grigia Observatory

Author

J. P. Lepeltier, G. Recouvreur, G. Mainella, J. P. Bernard, Alain Benoit, B. Vozzi, J. P. Crussaire, Francois-Xavier Désert, Noël Coron, J.-P. Torre, B. Leriche, V. Soglasnova, F. Zagury, J.-M. Lamarre, J. Narbonne, R. Pons, P. de Marcillac, M. Giard, Jacques Leblanc, M. De Petris, F. Pajot, G. Jegoudez, A. De Luca, Jean-Loup Puget, P. de Bernardis, G. Dambier, G. Serra, S. Pujol, Jacques Delabrouille, Centre de Recherches sur les Très Basses Températures (CRTBT), Université Joseph Fourier - Grenoble 1 (UJF)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut Laue-Langevin (ILL), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-Université Joseph Fourier - Grenoble 1 (UJF), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, and ILL

Subjects
cosmic microwave background, media_common.quotation_subject, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Telescope, Optics, law, Observatory, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, media_common, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Astrophysics (astro-ph), Bolometer, First light, Photometer, Radio continuum, observations, 13. Climate action, Sky, Millimeter, photometers, business, Secondary mirror
Abstract

We have designed and built a large-throughput dual channel photometer, Diabolo. This photometer is dedicated to the observation of millimetre continuum diffuse sources, and in particular, of the Sunyaev-Zel'dovich effect and of anisotropies of the 3K background. We describe the optical layout and filtering system of the instrument, which uses two bolometric detectors for simultaneous observations in two frequency channels at 1.2 and 2.1 mm. The bolometers are cooled to a working temperature of 0.1 K provided by a compact dilution cryostat. The photometric and angular responses of the instrument are measured in the laboratory. First astronomical light was detected in March 1995 at the focus of the new Millimetre and Infrared Testa Grigia Observatory (MITO) Telescope. The established sensitivity of the system is of 7 mK_RJ s^1/2$. For a typical map of at least 10 beams, with one hour of integration per beam, one can achieve the rms values of y_SZ ~ 7 10^-5 and the 3K background anisotropy Delta T/T ~ 7 10^-5, in winter conditions. We also report on a novel bolometer AC readout circuit which allows for the first time total power measurements on the sky. This technique alleviates (but does not forbid) the use of chopping with a secondary mirror. This technique and the dilution fridge concept will be used in future scan--modulated space instrument like the ESA Planck mission project., 10 pages, LaTeX, 12 figures, accepted for publication in Astronomy and Astrophysics Supplement Series

Published
2000

17. [Untitled]

Author

G. Serra, I. Ristorcelli, B. Leriche, J.-M. Lamarre, M. Giard, F. Pajot, H. Safa, and G. Recouvreur

Subjects
Physics, Segmented mirror, business.industry, Cassegrain reflector, Astronomy and Astrophysics, Translation (geometry), Rotation, law.invention, Primary mirror, Telescope, Optical axis, Optics, Interference (communication), Space and Planetary Science, law, business
Abstract

PRONAOS is a balloon-borne system dedicated to astronomical observations in the submillimeter range (180µm - 1050µm) based on the use of a 2m Cassegrain telescope. The primary mirror consists of six CFRP (Carbon Fiber Reinforced Plastic) panels, each being positioned by three actuators. The rotation angles of the panels have been measured in the visible range with the help of a CCD and digital centroiding techniques that were necessary because of the light scattering on the CFRP mirror. The translation movements (along the optical axis) of the panels have been measured with an interference technique in the submillimeter range. Both visible and submillimeter measurements were also necessary to determine the alignment of the telescope - focal instrument system with the star sensor. The whole alignment process leads to a precision of ±8″ for the rotation angles and ±7µm for the translation of each panel, sufficient for a qualification of the system.

Published
1997

18. The PILOT experiment for the measurement of interstellar dust polarization : the camera ground calibration

Author

Julien Bernard, V. Buttice, A. Caillat, M. Bouzit, Jean-Pierre Dubois, Y. Longval, B. Crane, C. Marty, Marc Chaigneau, B. Leriche, and F. Pajot

Subjects
Physics, business.industry, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Optical power, Spectral bands, Polarizer, Polarization (waves), law.invention, Telescope, Optics, law, business, Cosmic dust, Remote sensing
Abstract

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 45o 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.

Published
2012

19. SPM, a submillimeter photometer for PR0NAOS

Author

J. Mangin, J.-M. Lamarre, J. P. Lepeltier, C. Bourguignon, A. De Luca, G. Serra, H. Lagardere, J.-P. Torre, J. Narbonne, B. Leriche, R. Peyturaux, J. P. Bernard, J. Reigner, X. Desert, G. Jegoudez, R. Pons, J. Leblanc, M. Barthelemy, Francois Boulanger, J.-L. Puget, M. Glard, L. Delille, J. C. Renault, C. Lizambert, F. Pajot, G. Guyot, G. Dambier, G. Recouvreur, E. Korczak, J. P. Crussaire, C. Rioux, I. Ristorcelli, and C. Plaisant

Subjects
Cryostat, Physics, Liquid helium, business.industry, Bolometer, Photometer, Spectral bands, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Electronic, Optical and Magnetic Materials, law.invention, Telescope, Interstellar medium, Optics, law, Calibration, business
Abstract

SPM is a multi-channels photometer designed to obtain the best sensitivity at the focus of the 2 m balloon-borne PRONAOS telescope. Its scientific goals include the measurement of cosmological background anisotropy, which is important for understanding the origin of the structure in the universe and the observation of cold solid matter in the interstellar medium as an indicator of the physical conditions that prevail in star forming regions. SPM consists of warm optics that ensure beam switching and in-flight calibration, a liquid helium cryostat that contains filters and the 3 He cooled bolometers, and electronics for housekeeping and data handling. The spectral bands are 180–240 μm, 240–340 μm, 340–540 μm and 540–1200 μm. They are defined by dichroics, which allows simultaneous observations in the four bands. The expected NEΔT in flight is significantly less than 1 mK in all the bands. SPM will fly with PRONAOS in May 1994.

Published
1994

20. NbSi TES Array and Readout: Development and Characterization

Author

S. Marnieros, F. Pajot, F Gadot, B. Leriche, G. Bordier, L. Dumoulin, Benoit Belier, C. Evesque, J. Q. Zhong, Laurent Bergé, M. Piat, E. Bréelle, Sheng-Cai Shi, Y. Atik, D. Prêle, F. Voisin, J. Martino, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'électronique fondamentale (IEF), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris

Subjects
Materials science, Physics::Instrumentation and Detectors, Slot antenna, Integrated circuit, Cryogenics, BiCMOS, 01 natural sciences, 7. Clean energy, law.invention, cryogenic electronics, Sensor array, law, 0103 physical sciences, transition edge sensors, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Electrical and Electronic Engineering, 010306 general physics, Antenna coupling, 010303 astronomy & astrophysics, business.industry, Amplifier, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Electronic, Optical and Magnetic Materials, [PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], Optoelectronics, Transition edge sensor, SiGe analog integrated circuits, business, bolometers
Abstract

We are developing a detection system based on a NbSi Transition Edge Sensor (TES) bolometer array. A thermo-mechanical architecture accomodates the array and the cryogenic stage of the readout. We model the coupling of the TES bolometer to the radiation by means of twin slot antenna. We present the latest design of the cryogenic readout which includes a BiCMOS SiGe integrated circuit at 4 K controlling a Superconducting Quantum Interference Device (SQUID) amplifier.

Published
2011

21. Large submillimeter and millimeter detector arrays for astronomy: development of NbSi superconducting bolometers

Author

F. Pajot, L. Dumoulin, J. Martino, G. Bordier, B. Leriche, D. Prêle, J. Zhong, Y. Atik, E. Bréelle, Sheng-Cai Shi, C. Evesque, S. Marnieros, F. Voisin, Laurent Bergé, Benoit Belier, M. Piat, and F. Gadot

Subjects
Physics, Physics::Instrumentation and Detectors, business.industry, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Radiation, Multiplexer, law.invention, Telescope, Cardinal point, Optics, law, Optoelectronics, Millimeter, Astrophysics::Earth and Planetary Astrophysics, Antenna (radio), business, Astrophysics::Galaxy Astrophysics
Abstract

The achievement of the Planck and Herschel space missions in the submillimeter and millimeter range was made possible by a continuous effort on detector developments. Now limited by the intrinsic fluctuations of the radiation coming from the astronomical sources themselves, the sensitivity improvement requires the development of large arrays of detectors filling the focal plane of the telescopes. We present here the development of a TES array using NbSi sensors on SiN membranes. The readout electronics is based on SQUIDs and a cooled SiGe ASIC multiplexer. The detector is coupled with the input radiation by means of antenna. The present goal performance is adapted for the realisation of a ground based millimeter camera.

Published
2010

22. Planck pre-launch status: The HFI instrument, from specification to actual performance

Author

Peter A. R. Ade, V. Yurchenko, F. Piacentini, R. Pons, M. Nexon, G. Recouvreur, Christopher G. Paine, C. Dumesnil, Philippe Camus, J. Pahn, O. Perdereau, M. Tristram, Sarah E. Church, M.-A. Miville-Deschênes, A. Coulais, J. J. Bock, F.-X. Désert, J. Lande, G. Serra, J. F. Macías-Pérez, F. Pajot, J.-L. Beney, F. Bouchet, Simon Prunet, J.-P. Torre, C. Leroy, N. Ponthieu, Bruno Maffei, E. Bréelle, M. Giard, B. P. Crill, J.-L. Puget, L. Vibert, W. A. Holmes, T. C. Koch, E. Hivon, J. Haissinski, R. V. Sudiwala, B. Mansoux, L. Montier, K. Dassas, C. Renault, C. Evesque, R. S. Bhatia, Alain Benoit, J. Charra, Sophie Henrot-Versille, W. C. Jones, Y. Blanc, P. de Bernardis, A. Arondel, F. Couchot, C. Rosset, Martin Crook, C. Marty, Stéphane Plaszczynski, B. Leriche, Etienne Pointecouteau, D. Rambaud, D. Santos, J.-F. Sygnet, M. Charra, Tom Bradshaw, J.-M. Delouis, I. Ristorcelli, P. Eng, Jan Tauber, Thierry Maciaszek, Karim Benabed, H. Lagardère, D. Yvon, A. Moneti, J. Narbonne, Giorgio Savini, Andrew E. Lange, X. Dupac, Y. Longval, A. Catalano, R. Gispert, P. de Marcillac, P. Lami, George Efstathiou, C. Mercier, Silvia Masi, Jacques Delabrouille, J. A. Murphy, Ken Ganga, J.-Ph. Bernard, M. Piat, Adam Woodcraft, J.-M. Lamarre, G. Guyot, L. Guglielmi, P. Stassi, J.-J. Fourmond, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, PLANCK, École normale supérieure - Paris (ENS Paris), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Hélium : du fondamental aux applications (HELFA), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Cryogénie (Cryo), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Cryo - Cryogénie, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)

Subjects
cosmic microwave background, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Point source, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Cosmic background radiation, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Radio spectrum, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, techniques: photometric, Optics, law, space vehicles: instruments, submillimeter: general, techniques: polarimetric, 0103 physical sciences, Calibration, Planck, 010303 astronomy & astrophysics, QB, Physics, 010308 nuclear & particles physics, business.industry, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, symbols, business
Abstract

Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planck mission. It will observe the whole sky in six bands in the 100 GHz–1 THz range.\ud \ud Aims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental sources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide full maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels or accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests and calibration.\ud \ud Methods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly: (i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions; (iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques.\ud \ud Results. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based calibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification.

Published
2010

23. Status of the ArTeMiS camera to be installed on APEX

Author

P. O. Lagage, B. Leriche, J. Relland, O. Boulade, Pascal André, B. Horeau, M. Lortholary, C. De Breuck, M. Talvard, Eric Ercolani, Vincent Reveret, Didier Dubreuil, L. Rodriguez, P. Gallais, Y. Le-Pennec, D. Rabanus, E. Doumayrou, J. Martignac, and P. Agnèse

Subjects
Physics, Pixel, business.industry, media_common.quotation_subject, Bolometer, Cassegrain reflector, Photometer, Particle detector, law.invention, Photometry (optics), Wavelength, Optics, law, Sky, business, media_common, Remote sensing
Abstract

The ArTeMiS submillimetric camera will observe simultaneously the sky at 450, 350 and 200 μm using 3 different focal planes made of 2304, 2304 and 1152 bolometric pixels respectively. This camera will be mounted in the Cassegrain cabin of APEX, a 12 m antenna located on the Chajnantor plateau, Chile. To realize the bolometric arrays, we have adapted the Silicon processing technology used for the Herschel-PACS photometer to account for higher incident fluxes and longer wavelengths from the ground. In addition, an autonomous cryogenic system has been designed to cool the 3 focal planes down to 300 mK. Preliminary performances obtained in laboratory with the first of 3 focal planes are presented. Latest results obtained in 2009 with the P-ArTeMiS prototype camera are also discussed, including massive protostellar cores and several star forming regions that have been clearly identified and mapped.

Published
2010

24. Development of NbSi TES bolometer arrays for submillimeter astronomy

Author

F. Pajot, D. Prêle, Y. Atik, M. Piat, S. Marnieros, C. Evesque, F. Voisin, Stéphane Collin, L. Dumoulin, B. Leriche, Benoit Belier, Laurent Bergé, and E. Bréelle

Subjects
Physics, Physics::Instrumentation and Detectors, business.industry, Terahertz radiation, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Readout electronics, Submillimetre astronomy, law.invention, law, Optoelectronics, Millimeter, Space astronomy, business, Ultra sensitive
Abstract

Future ground and space astronomy experiments will require large arrays of sensitive detectors in the submillimeter and millimeter ranges. Superconducting Transition Edge Sensors (TES) are currently under development in many institutes to be used as ultra sensitive bolometers. We are investigating co-evaporated NbSi thin films TES arrays. We present here the characterisation and laboratory performances of an array and its readout electronics.

Published
2009

25. Recent results obtained on the APEX 12 m antenna with the ArTeMiS prototype camera

Author

M. Talvard, V. Revéret, V. Minier, G. Willmann, O. Boulade, J. Martignac, E. Pantin, C. De Breuck, M. Lortholary, D. Rabanus, L. Rodriguez, J. Relland, E. Ercolani, Pascal André, P. O. Lagage, Patrick Agnese, B. Leriche, B. Horeau, Didier Dubreuil, Y. Le-Pennec, P. Gallais, and E. Doumayrou

Subjects
Physics, Pixel, business.industry, Bolometer, Photometer, Particle detector, law.invention, Telescope, Optics, Cardinal point, Observatory, law, Onsala Space Observatory, business, Remote sensing
Abstract

ArTeMiS is a camera designed to operate on large ground based submillimetric telescopes in the 3 atmospheric windows 200, 350 and 450 µm. The focal plane of this camera will be equipped with 5760 bolometric pixels cooled down at 300 mK with an autonomous cryogenic system. The pixels have been manufactured, based on the same technology processes as used for the Herschel-PACS space photometer. We review in this paper the present status and the future plans of this project. A prototype camera, named P-ArTeMiS, has been developed and successfully tested on the KOSMA telescope in 2006 at Gornergrat 3100m, Switzerland. Preliminary results were presented at the previous SPIE conference in Orlando (Talvard et al, 2006). Since then, the prototype camera has been proposed and successfully installed on APEX, a 12 m antenna operated by the Max Planck Institute fur Radioastronomie, the European Southern Observatory and the Onsala Space Observatory on the Chajnantor site at 5100 m altitude in Chile. Two runs have been achieved in 2007, first in March and the latter in November. We present in the second part of this paper the first processed images obtained on star forming regions and on circumstellar and debris disks. Calculated sensitivities are compared with expectations. These illustrate the improvements achieved on P-ArTeMiS during the 3 experimental campaigns.

Published
2008

26. Characterization of NbSi films for TES bolometers

Author

C. Evesque, M. Piat, E. Bréelle, D. Prêle, B. Leriche, L. Dumoulin, Benoit Belier, Y. Atik, Laurent Bergé, F. Voisin, and F. Pajot

Subjects
Cryostat, Resistive touchscreen, Materials science, Fabrication, business.industry, Bolometer, Niobium, chemistry.chemical_element, Particle detector, law.invention, SQUID, chemistry, law, Optoelectronics, Thin film, business
Abstract

Future space experiments will require large arrays of sensitive detectors in the submillimeter and millimeter range. Superconducting transition-edge sensors (TESs) are currently under heavy development to be used as ultra sensitive bolometers. In addition to good performance, the choice of material depends on long term stability (both physical and chemical) along with a good reproducibility and uniformity in fabrication. For this purpose we are investigating the properties of co-evaporated NbSi thin films. NbSi is a well-known alloy for use in resistive thermometers. We present a full low temperature characterization of superconductive NbSi films. In order to tune the critical temperature of the NbSi thermometers down to the desired range, we have to adjust the concentration of niobium in the NbSi alloy. Tests are made using 4He-cooled cryostats, 300mK 3He mini-fridges, Resistance Bridges and commercial SQUID. Measured parameters are the critical temperature, the sharpness of the transition. Noise measurements are on-going.

Published
2008

27. Characterization of NbSi TES on a 23-Pixel Array

Author

F. Pajot, M. Piat, Laurent Bergé, F. Voisin, Y. Atik, C. Evesque, D. Prêle, L. Dumoulin, E. Bréelle, B. Leriche, Benoit Belier, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut d'électronique fondamentale (IEF), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)

Subjects
Wheatstone bridge, Materials science, Niobium, chemistry.chemical_element, 01 natural sciences, Temperature measurement, law.invention, 010309 optics, law, 0103 physical sciences, Electrical and Electronic Engineering, 010306 general physics, Resistive touchscreen, business.industry, NbSi, Bolometer, transition edge sensor, Array, Condensed Matter Physics, Electronic, Optical and Magnetic Materials, SQUID, [PHYS.COND.CM-S]Physics [physics]/Condensed Matter [cond-mat]/Superconductivity [cond-mat.supr-con], chemistry, Thermometer, [PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], Optoelectronics, Transition edge sensor, business, bolometers
Abstract

International audience; Instrumental progress allowed the development of bolometric detectors adapted to submillimeter and millimeter wavelengths. Superconducting transition-edge sensors (TESs) are currently under heavy development to be used as ultra sensitive bolometers. In addition to good performance, the choice of material depends on long term stability (both physical and chemical) along with a good reproducibility and uniformity in fabrication. For this purpose we are investigating the properties of NbSi thin films and have already developed arrays of NbSi TES. NbSi is a well-known alloy for use in resistive thermometers. We present a low temperature characterization of the NbSi films on a 23-pixel array. In order to tune the critical temperature of the NbSi thermometers down to the desired range, we have to adjust the concentration of Niobium in the NbSi alloy. In this experiment, we set for a Niobium concentration of 15 percent, to be able to run tests at a convenient temperature larger than 300 miliKelvin. Tests are made using Helium4-cooled cryostats, 300 miliKelvin Helium3 mini-fridges, resistance bridge and a commercial SQUID with its readout circuit. Parameters being measured are: critical temperature, resistance, sharpness of the transition given by the alpha parameter and noise measurements. The multiplexing is also developed to prepare the final chain for noise measurements on 23 pixel bolometers array.

Published
2008

28. Development of Large Bolometer Arrays for Submillimeter and Millimeter Astronomy

Author

D. Prêle, Y. Atik, Aurélien Benoit, F. Pajot, M. Piat, Yong Jin, C. Evesque, M. Giard, Ph. Camus, D. Santos, L. Dumoulin, B. Bélier, B. Leriche, and S. Lefranc

Subjects
Physics, business.industry, Bolometer, Detector, Astronomy, Integrated circuit, Submillimetre astronomy, Space exploration, law.invention, Cardinal point, law, Microelectronics, Millimeter, business
Abstract

Access to new microelectronics facilities allows the development of large bolometer arrays for astronomy. The expected sensitivity increase is the key for the next generation of cameras at the focal plane of submillimeter and millimeter telescopes. We present here the research led in France in this domain.

Published
2008

29. ArTeMiS: filled bolometer arrays for next generation sub-mm telescopes

Author

O. Boulade, Patrick Agnese, C. Walter, M. Talvard, M. Lortholary, C. Veyssiere, V. Minier, Aurélien Benoit, Didier Dubreuil, Pascal André, V. Revéret, F. Pajot, G. Durand, Jean Lepennec, B. Leriche, P. O. Lagage, B. Horeau, J. Martignac, E. Doumayrou, L. Vigroux, L. Rodriguez, Nicola Schneider, P. Gallais, and J. Stutzki

Subjects
Physics, business.industry, Bolometer, Detector, Field of view, law.invention, Telescope, Radio telescope, Observational astronomy, Optics, law, Infrared window, Angular resolution, business
Abstract

Astronomical observations at sub-millimetre wavelengths are limited either by the angular resolution of the telescope or by the sensitivity and field of view of the detector array. New generation of radio telescopes, such as the ALMA-type antennas on Chajnantor plateau in Chile, can overcome these limitations if they are equipped with large detector arrays made of thousands of sensitive bolometer pixels. Instrumentation developments undertaken at CEA and based on the all silicon technology of CEA/Leti are able to provide such large detector arrays. The ArTeMiS project consists in developing a camera for ground-based telescopes that operates in two sets of atmospheric windows at 200-450 μm (channel 1) and 800-1200 μm (channel 2). ArTeMiS-1 consists in grid bolometer arrays similar to those developed by CEA for the Herschel Space Observatory. A prototype camera operating in this first atmospheric window was installed and successfully tested in March 2006 on the KOSMA telescope at Gornergrat (Switzerland) in collaboration with the University of Cologne. ArTeMiS-2 will consist either in antenna-coupled bolometer arrays or specific mesh bolometer arrays. By the end of 2008, ArTeMiS cameras could be operated on 10m-class telescopes on the Chajnantor ALMA site, e.g., APEX, opening new scientific prospects in the study of the early phases of star formation and in cosmology, in the study of the formation of large structures in the universe. At longer term, installation of such instrumentation at Dome-C in Antarctica is also under investigation. The present status of the ArTeMiS project is detailed in this paper.

Published
2006

30. Superconducting NbSi thermometers for use in TES devices

Author

M. Piat, S. Lefranc, B. Leriche, L. Bergé, L. Dumoulin, J.-P. Torre, C. Evesque, F. Pajot, E. Bréelle, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Masataka Ohkubo, Kazuhisa Mitsuda and Hiroyuki Takahashi, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Superconductivity, Physics, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Nuclear and High Energy Physics, Resistive touchscreen, Condensed matter physics, business.industry, Bolometer, NbSi, 02 engineering and technology, 021001 nanoscience & nanotechnology, 01 natural sciences, law.invention, law, Superconducting, 0103 physical sciences, Optoelectronics, 95.55.Rg, 010306 general physics, 0210 nano-technology, business, Instrumentation
Abstract

We present here preliminary results for superconducting NbSi thermometers to be used in TES devices. These thermometers are being made by the CSNSM/IN2P3 in Orsay, France, in parallel to resistive NbSi thermometers, a more common use for this alloy. The critical temperature of these devices is easily tuneable. We present here devices operated and tested at 300 mK using a 3He fridge.

Published
2006

31. Calorimetric detection of THz radiation from femtosecond filaments in air

Author

G. Méchain, Michel Franco, Bernard Prade, B. Leriche, André Mysyrowicz, Stylianos Tzortzakis, Laboratoire d'optique appliquée (LOA), École Nationale Supérieure de Techniques Avancées (ENSTA Paris)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Materials science, Physics and Astronomy (miscellaneous), Kinetics, Physics::Optics, General Physics and Astronomy, 02 engineering and technology, 01 natural sciences, law.invention, terahertz, 020210 optoelectronics & photonics, Optics, Physics::Plasma Physics, law, Thz radiation, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, 010306 general physics, Quantum optics, [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], business.industry, Far-infrared laser, General Engineering, Plasma, Laser, filamentation, Physics::Space Physics, Femtosecond, business, Ultrashort pulse
Abstract

International audience; Calorimetric measurements of the THz radiation from plasma filaments created in air by intense IR fs laser pulses were performed. The decay kinetics of the THz radiation from this extended plasma source is shown to be different from that of a localized air plasma source produced by the same laser.

Published
2004

32. Design and tests of high sensitivity NTD Ge thermometers for the Planck-High Frequency Instrument

Author

J.-M. Lamarre, F. Langlet, M. Piat, B. Leriche, J. W. Beeman, J. P. Crussaire, J. P. Torre, R. S. Bhatia, and Porter, F. Scott

Subjects
Physics, Frequency response, Phonon, business.industry, Bolometer, Analytical chemistry, Thermal fluctuations, Temperature measurement, law.invention, Optics, law, Thermometer, Thermal, Interfacial thermal resistance, business
Abstract

The High Frequency Instrument of Planck needs high sensitivity semi-conductors at low temperature to monitor the temperature of the bolometer plate. We have modeled such thermometers by using a semi-analytical approach of Anderson insulators, taking into account both the electrical field and the electron/phonon decoupling effects. The optimized design uses convenient NTD Ge material and has larger dimension than the initial design. The first measurements of these optimized thermometers showed a significant thermal de-coupling effect due to Kapitza resistance with its mechanical support. Nevertheless, a sensitivity of about 8 nK.Hz^(–0.5), not far from the predicted one, was obtained. The noise spectrum of the thermometer was flat down to 1 Hz, dominated at lower frequency by the thermal fluctuations.

Published
2002

33. ELISA: A small balloon Experiment for a Large Scale Survey in the Sub-millimeter

Author

F. Boulanger, J. Ph. Bernard, I. Ristorcelli, A. Abergel, J.-P. Torre, G. Lagache, M. Armengaud, B. Stepnik, J.-M. Lamarre, M. Giard, C. Meny, J. P. Crussaire, B. Leriche, and Y. Longval

Subjects
Physics, Cryostat, Infrared astronomy, business.industry, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, law.invention, Primary mirror, Telescope, Optics, law, Astrophysics::Earth and Planetary Astrophysics, Space research, business, Secondary mirror, Astrophysics::Galaxy Astrophysics
Abstract

This paper presents the technical aspects and scientific objectives of the balloon-borne Experiment for Large Infrared Survey Astronomy (ELISA). The emphasis is put upon the synergies existing between the ELISA project and future space missions, both with respect to technical and scientific aspects. ELISA is a small balloon project for an experiment dedicated to measure the Far-Infrared to Sub-millimeter continuum emission of dust over a large fraction of the sky, with unprecedented sensitivity and angular resolution. The primary mirror of the telescope, similar to the one used for the Top-Hat mission, will have a diameter of 1 m, ensuring an angular resolution of about 3.5′. PACS-type bolometer arrays will be used in four photometric bands centered at 170, 240, 400, and 650 μm and providing a 22′×45′ instantaneous field of view per channel. A liquid He cryostat will host the cold optics, including the secondary mirror of the telescope, as well as the detectors, which will be cooled to 0.3 K using an He3 ...

Published
2002

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