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13 results on '"François Visticot"'

1. Characterization of the focal plane of the microchannel X-ray telescope at the metrology beamline of SOLEIL synchrotron for the space astronomy mission SVOM

Author

Aline Meuris, Benjamin Schneider, Hugo Allaire, David Baudin, Ion Cojocari, Paulo Da Silva, Eric Doumayrou, Diego Götz, Philippe Ferrando, Philippe Laurent, Michel Lortholary, Pascal Mercère, Frédéric Pinsard, Marin Prieur, Thibault Pichon, Léna Provost, Diana Renaud, Nicolas Renault-Tinacci, Timothée Tollet, François Visticot, Département d'Astrophysique (ex SAP) (DAP), 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, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Phénomènes aux Hautes Energies (PHE), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
[PHYS]Physics [physics], Nuclear and High Energy Physics, Instrumentation
Published
2023

2. AIRS: ARIEL IR spectrometer status

Author

Jérôme Martignac, Jérôme Amiaux, Michel Berthé, Christophe Cara, Cyrille Delisles, Achrène Direk, Luc Dumaye, Jean Fontignie, Alain Goestschy, Benoît Horeau, Norma Hurtado, Duc-Dat Huyn, Grégory Kaszubiak, Pierre-Olivier Lagage, Isabelle Le Mer, Michel Lortholary, Vincent Moreau, Salima Mouzali, Patrick Mulet, François Nico, Thibault Pichon, Léna Provost, Diana Renaud, Victor Schwartz, Michel Talvard, Thierry Tourrette, François Visticot, Axel Arhancet, Damien Bachet, Nicolas Berton, Mickael Lacroix, Hervé Le Provost, Olivier Tellier, Anne Philippon, Clémence De Jabrun, Jean-Pierre Dubois, François Langlet, Dylan Le Claire, Benoît Lecomte, Marc Ollivier, Stéphane Tosti, Vincent Lapeyrère, Marion Bonafous, Jérôme Parisot, Jean-Michel Réess, Didier Zegadanin, Jean-Philipe Beaulieu, Virginie Batista, Pierre Drossart, Salma Fahmy, Delphine Jollet, Ludovic Puig, Thierry Tirolien, Pascale Danto, Gilles Hervet, Oceane Maisonnave, Paul Eccleston, Georgia Bishop, Rachel Drumond, Andrew Caldwell, Martin Caldwell, Lucile Desjonqueres, Martin Whalley, Enzo Pascale, Gianluca Morgante, Mauro Focardi, Emanuele Pace, and Anna-Maria Di Giorgio

Published
2022

3. B-BOP, the SPICA Imaging Polarimeter

Author

Sylvain Martin, Marc Sauvage, Michel Berthé, Laurent Dussopt, S. Bounissou, Pierre-Antoine Frugier, J. Martignac, Didier Dubreuil, Marcos Chimeno, O. Gevin, Lionel Duband, A. Aliane, Jean-Yves Plesseria, Louis Rodriguez, Amala Demonti, V. Goudon, Benoit Marquet, François Visticot, Xavier de la Broïse, Jacques Delabrouille, Vincent Reveret, Javier Pérez, Eric Doumayrou, Camille Gennet, Josefina Torres Redondo, Obaïd Adami, X. F. Navick, H. Kaya, Albrecht Poglitsch, Cyrille Delisle, and Paco Najarro

Subjects
Physics, business.industry, Linear polarization, Bolometer, Detector, Polarimetry, FOS: Physical sciences, Polarimeter, Spica, Spectral bands, Polarization (waves), 7. Clean energy, law.invention, Optics, law, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We present the B-BOP instrument, a polarimetric camera on board the future ESA-JAXA SPICA far-infrared space observatory. B-BOP will allow the study of the magnetic field in various astrophysical environments thanks to its unprecedented ability to measure the linear polarization of the submillimeter light. The maps produced by B-BOP will contain not only information on total power, but also on the degree and the angle of polarization, simultaneously in three spectral bands (70, 200 and 350 microns). The B-BOP detectors are ultra-sensitive silicon bolometers that are intrinsically sensitive to polarization. Their NEP is close to 10E-18 W/sqrt(Hz). We will present the optical and thermal architectures of the instrument, we will detail the bolometer design and we will show the expected performances of the instrument based on preliminary lab work., 10 pages, 6 figures, SPIE proceeding: Astronomical Telescopes + Instrumentation 2020

Published
2021

4. Characterization of the detection chain of the Micro-channel X-ray Telescope

Author

Luc Dumaye, Tony Lavanant, Frédéric Pinsard, Benjamin Schneider, Aline Meuris, Isabelle Le Mer, Diana Renaud, Thierry Tourrette, Marin Prieur, Francesco Ceraudo, François Nico, Michel Lortholary, Norbert Meidinger, François Visticot, D. Gotz, Eric Doumayrou, Alain Goetschy, Danilo Mießner, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Max-Planck-Institut für Extraterrestrische Physik (MPE), and Max-Planck-Gesellschaft

Subjects
Physics, Cryostat, [PHYS]Physics [physics], Nuclear and High Energy Physics, X-ray spectroscopy, Silicon, 010308 nuclear & particles physics, business.industry, Detector, chemistry.chemical_element, X-ray telescope, 01 natural sciences, law.invention, Telescope, Optics, chemistry, law, 0103 physical sciences, Electronics, Spectral resolution, business, 010303 astronomy & astrophysics, Instrumentation
Abstract

This paper describes the first performance tests and characterization of the detection chain of the Micro-channel X-ray Telescope (MXT), one of the instruments on board the French-Chinese mission SVOM for the study of Gamma-Ray Bursts. The MXT detector consists of a back-illuminated 450 µm -thick fully-depleted frame-store silicon pnCCD, operating in the 0 . 2 − 10 keV energy range. Featuring an imaging area of ≈ 4 cm 2 , the device is read out in parallel by two CAMEX ASICs and is powered and controlled by its dedicated Front-End Electronics. A complete setup based on a cryostat and a multi-energy X-ray source have been designed for the characterization of the detection chain. The tests, performed at ≈ −65 ° C , demonstrate a spectral resolution of (82 ± 2) eV at 1.5 keV as well as a 200 eV low-level threshold. Both of those results are in compliance with the performance requirements of the instrument.

Published
2020

5. Optimal X-ray filters for EDXRF analysis

Author

Diana Renaud, Olivier Limousin, Daniel Maier, François Visticot, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics - Instrumentation and Detectors, Trace (linear algebra), FOS: Physical sciences, 01 natural sciences, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, 0302 clinical medicine, Optics, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation, Mathematical Physics, Filter material, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, business.industry, Scattering, X-ray, Instrumentation and Detectors (physics.ins-det), Filter (signal processing), Physics - Medical Physics, Medical Physics (physics.med-ph), business, Beam (structure), Voltage
Abstract

International audience; This work presents a semi-analytical approach to answer the question of optimal beam filtering in the case of EDXRF measurements with an X-ray tube. A collection of programs, called xfilter, is presented that is capable to find the optimal filter material and the optimal scattering angle for all possible combinations of trace elements and target materials. The tube voltage can be either set fixed or be another parameter to optimize. The concepts of the calculations are introduced in a general manner and demonstrated with a specific example, the detection of gold Kα 1 XRF within human tissue. The comparison between the calculation results and an EDXRF measurement shows excellent agreement.

Published
2020

6. Second generation of portable gamma camera based on Caliste CdTe hybrid technology

Author

Vincent Schoepff, Olivier Limousin, Daniel Maier, François Visticot, Cyrille Delisle, Charly Mahe, Frederick Carrel, Guillaume Amoyal, Geoffrey Daniel, Fabrice Soufflet, C. Blondel, A. Meuris, J. Martignac, O. Gevin, M.C. Vassal, Pierre-Anne Bausson, Département d'Astrophysique (ex SAP) (DAP), 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, École des Ponts ParisTech (ENPC), Département d'Electronique, des Détecteurs et d'Informatique pour la Physique (ex SEDI) (DEDIP), Laboratoire Capteurs et Architectures Electroniques (LCAE), Département Métrologie Instrumentation & Information (DM2I), Laboratoire d'Intégration des Systèmes et des Technologies (LIST), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Laboratoire d'Intégration des Systèmes et des Technologies (LIST), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 3D Plus, ANR-11-RSNR-0016,ORIGAMIX,lOcalisation de la Radioactivité par Imageurs GAMma Pixellisés(2011), Laboratoire d'Intégration des Systèmes et des Technologies (LIST (CEA)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Laboratoire d'Intégration des Systèmes et des Technologies (LIST (CEA))

Subjects
Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Gamma imaging, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, FOS: Physical sciences, Real time imaging, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, 030218 nuclear medicine & medical imaging, law.invention, CALISTE-O, spectrometry, 03 medical and health sciences, 0302 clinical medicine, law, sensor, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Field-programmable gate array, nuclear instrumentation, Gamma camera, Compton camera, Physics, ORIGAMIX, instrumentation, 010308 nuclear & particles physics, business.industry, Detector, Volume (computing), gamma camera, Instrumentation and Detectors (physics.ins-det), CdTe, Physics - Medical Physics, Cadmium telluride photovoltaics, ARM architecture, Power consumption, radioactivity, Medical Physics (physics.med-ph), business, ionizing radiation, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, Computer hardware, CALISTE-HD
Abstract

In the framework of a national funded program for nuclear safety, a first prototype of portable gamma camera was built and tested. It integrates a Caliste-HD CdTe-hybrid detector designed for space X-ray astronomy coupled with a new system-on-chip based acquisition system (FPGA and ARM microprocessor) and thermo-electrical coolers for a use at room temperature. The complete gamma part of the camera fits in a volume of 15 x 15 x 40 cm^3 for a mass lower than 1 kg and a power consumption lower than 10 W. Localization and spectro-identification of radionuclides in a contaminated scene were demonstrated during several test campaigns. A new generation of system is under development taking into account feedback experience from in-situ measurements and integrating a new generation of sensor cost-optimized by industrial applications called Caliste-O. Caliste-O holds a 16 x 16 pixel detector of 14 x 14 mm^2 and 2 mm thick with 8 full-custom front-end IDeF-X HD ASICs. Two prototypes were fabricated and tested. The paper will present the results of in-situ measurements with the first gamma camera, the spectroscopic performance of Caliste-O and the design of the second generation of gamma camera which aims for real time imaging and spectro-identification., 6 pages, 7 figures

Published
2018

8. The Euclid STM VIS focal plane assembly: from the integration to the qualification tests (Conference Presentation)

Author

Diana Renaud, Philippe Ferrando, Cédric Thizy, Jean-Yves Roussé, François Visticot, Patrice Charon, Thierry Tourrette, Mark Cropper, Sylvie Liébecq, Saeeda Awan, Luc Dumaye, Ruyman Azzollini, Vincent Hennion, Michel Berthé, Jean Fontignie, J. Martignac, Jean-Michel Joubert, Arnaud Roger, Ashraf Al-Bahlawan, T. Hunt, B. Horeau, Nicolas Solenne, Damien Bachet, Pascal Contrepois, Magdalena B. Szafraniec, Michael Carty, Dominique Gibier, Pascale Danto, Valérie Samain, S. Pottinger, Thierry Orduna, Duc-Dat Huynh, and Jérôme Amiaux

Subjects
Engineering drawing, Presentation, Cardinal point, Computer science, media_common.quotation_subject, Qualification testing, media_common
Published
2018

9. Characterizing filaments in regions of high-mass star formation: High-resolution submilimeter imaging of the massive star-forming complex NGC 6334 with ArT\'eMiS

Author

V. Revéret, L. Rodriguez, J. Martignac, Michel Lortholary, Cyrille Delisle, Frédérique Motte, Didier Dubreuil, Doris Arzoumanian, P. Palmeirim, Eric Doumayrou, J. Le Pennec, François Visticot, H. Roussel, Tracey Hill, D. Russeil, Annie Zavagno, C. De Breuck, Nicola Schneider, A. Roy, Nicolas Peretto, Y. Shimajiri, Sylvain Bontemps, J. Tigé, Pascal Gallais, M. Hennemann, Vincent Minier, M. Talvard, Vera Konyves, Ph. André, Luc Dumaye, K. L. J. Rygl, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Magmas et Volcans (LMV), Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet [Saint-Étienne] (UJM)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), 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 de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Synthèse Organique (Hétérochimie organique, organoéléments et matériaux) (LSOHOOM), Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Procédés, Matériaux et Energie Solaire (PROMES), Université de Perpignan Via Domitia (UPVD)-Centre National de la Recherche Scientifique (CNRS), FORMATION STELLAIRE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département d'Astrophysique (ex SAP) (DAP), 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, Department of Mechanical Engineering, University of Bristol [Bristol], Toyota Technological Institute at Chicago [Chicago] (TTIC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Centre National d’Études Spatiales [Paris] (CNES), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), 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), Centre National de la Recherche Scientifique (CNRS)-Université Jean Monnet [Saint-Étienne] (UJM)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Centre National de la Recherche Scientifique (CNRS), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP)

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, Gravitation, Protein filament, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, Star formation, Molecular cloud, Bolometer, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Interstellar medium, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA]
Abstract

Herschel observations of nearby molecular clouds suggest that interstellar filaments and prestellar cores represent two fundamental steps in the star formation process. The observations support a picture of low-mass star formation according to which ~ 0.1 pc-wide filaments form first in the cold interstellar medium, probably as a result of large-scale compression of interstellar matter by supersonic turbulent flows, and then prestellar cores arise from gravitational fragmentation of the densest filaments. Whether this scenario also applies to regions of high-mass star formation is an open question, in part because Herschel data cannot resolve the inner width of filaments in the nearest regions of massive star formation. We used the bolometer camera ArTeMiS on the APEX telescope to map the central part of the NGC6334 complex at a factor of > 3 higher resolution than Herschel at 350 microns. Combining ArTeMiS data with Herschel data allowed us to study the structure of the main filament of the complex with a resolution of 8" or < 0.07 pc at d ~ 1.7 kpc. Our study confirms that this filament is a very dense, massive linear structure with a line mass ranging from ~ 500 Msun/pc to ~ 2000 Msun/pc over nearly 10 pc. It also demonstrates that its inner width remains as narrow as W ~ 0.15 +- 0.05 pc all along the filament length, within a factor of < 2 of the characteristic 0.1 pc value found with Herschel for lower-mass filaments in the Gould Belt. While it is not completely clear whether the NGC 6334 filament will form massive stars or not in the future, it is two to three orders of magnitude denser than the majority of filaments observed in Gould Belt clouds, and yet has a very similar inner width. This points to a common physical mechanism for setting the filament width and suggests that some important structural properties of nearby clouds also hold in high-mass star forming regions., 10 pages, 6 figures. A&A, in press

Published
2016

10. 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

11. Optical design for the 450, 350, and 200 µm ArTeMiS camera

Author

Pascal Gallais, Didier Dubreuil, J. Martignac, Jean Christian Toussaint, Giampaolo Pisano, Vincent Reveret, Bruno Maffei, Vic Haynes, Norma Hurtado, Thierry Lerch, Philippe André, Louis Rodriguez, Jean Le Pennec, Michel Lortholary, François Visticot, Michel Talvard, and Cyrille Delisle

Subjects
instrumentation, Physics, Cryostat, business.industry, Cassegrain reflector, alignment, Field of view, Diamond turning, optical design, law.invention, Optical axis, Telescope, ArTeMiS, imager, submillimeter wavelength, Cardinal point, Optics, law, Focus (optics), business
Abstract

ArTeMiS is a submillimeter camera planned to work simultaneously at 450 μm, 350 μm and 200 μm by use of 3 focal planes of, respectively, 8, 8 and 4 bolometric arrays, each one made of 16 x18 pixels. In July 2013, with a preliminary setting reduced to 4 modules and to the 350 μm band, ArTeMiS was installed successfully at the Cassegrain focus of APEX, a 12 m antenna located on the Chajnantor plateau, Chile. After the summary of the scientific requirements, we describe the main lines of the ArTeMiS nominal optical design with its rationale and performances. This optical design is highly constrained by the room allocation available in the Cassegrain cabin. It is an all-reflective design including a retractable pick off mirror, a warm Fore Optics to image the focal plane of the telescope inside the cryostat, and the cold optics. The large size of the field of view at the focal plane of the telescope, 72 mm x 134 mm for the 350 μm and 450 μm beams, leads to the use of biconical toroidal mirrors. In this way, the nominal image quality obtained on the bolometric arrays is only just diffraction limited at some corners of the field of view. To keep a final PSF as much uniform as possible across the field of view, we have used the technic of manufacturing by diamond turning to machine the mirrors. This approach, while providing high accuracy on the shape of the mirrors, made easier the control of the two sub units, the Fore Optics and the cold optics, in the visible domain and at room temperature. Moreover, the use of the similar material (Aluminium alloy 6061) for the optical bench and the mirrors with their mount ensures a homothetic shrinking during the cooling down. The alignment protocol, drew up at the early step of the study, is also presented. It required the implementation of two additional mechanisms inside the cryostat to check the optical axis of the cold optics, in the real conditions of operation of ArTeMiS. In this way, it was possible to pre-align the Fore Optics sub unit with respect to the cold optics. Finally, despite the high constraints of the operating conditions of APEX, this protocol allowed to align ArTeMiS with respect to the telescope in a single adjustment. The first images obtained on the sky, Saturn with its rings, are given.

Published
2014

12. Cryogenic system for the ArTeMiS large sub millimeter camera

Author

J. Le Pennec, M. Talvard, L. Duband, E. Ercolani, J. Relland, J. Martignac, Thierry Jourdan, L. Clerc, and François Visticot

Subjects
Cryostat, Physics, business.industry, Detector, Bolometer, Cassegrain reflector, law.invention, Telescope, Optical axis, Optics, law, Millimeter, Photonics, business
Abstract

A new photonic camera has been developed in the framework of the ArTeMis project (Bolometers architecture for large field of view ground based telescopes in the sub-millimeter). This camera scans the sky in the sub-millimeter range at simultaneously three different wavelengths, namely 200 μm, 350 μm, 450 μm, and is installed inside the APEX telescope located at 5100m above sea level in Chile. Bolometric detectors cooled to 300 mK are used in the camera, which is integrated in an original cryostat developed at the low temperature laboratory (SBT) of the INAC institut. This cryostat contains filters, optics, mirrors and detectors which have to be implemented according to mass, size and stiffness requirements. As a result the cryostat exhibits an unusual geometry. The inner structure of the cryostat is a 40 K plate which acts as an optical bench and is bound to the external vessel through two hexapods, one fixed and the other one mobile thanks to a ball bearing. Once the cryostat is cold, this characteristic enabled all the different elements to be aligned with the optical axis. The cryogenic chain is built around a pulse tube cooler (40 K and 4 K) coupled to a double stage helium sorption cooler (300 mK). The cryogenic and vacuum processes are managed by a Siemens PLC and all the data are showed and stored on a CEA SCADA system. This paper describes the mechanical and thermal design of the cryostat, its command control, and the first thermal laboratory tests. This work was carried out in collaboration with the Astrophysics laboratory SAp of the IRFU institut. SAp and SBT have installed the camera in July 2013 inside the Cassegrain cabin of APEX.

Published
2014

13. 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

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