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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

5. 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

6. An N-band test bench for the METIS coronagraphic masks

Author

Michel Lortholary, Derek Ives, Salima Mouzali, Olivier Absil, Luc Dumaye, Thierry Orduna, Jean Christophe Barrière, Pascal Gallais, Eric Pantin, Christian Delacroix, Samuel Ronayette, and Mikael Karlsson

Subjects
Test bench, business.industry, Computer science, Phase mask, High contrast imaging, 01 natural sciences, Circumstellar disk, Exoplanet, law.invention, 010309 optics, Telescope, Phase plate, law, 0103 physical sciences, Metis, Aerospace engineering, business, 010303 astronomy & astrophysics
Abstract

METIS is one of the first three instruments for the ELT, Europe’s next-generation ground-based telescope. It will offer imaging, coronagraphy and spectroscopy in the L, M and N bands for general-purpose science in astrophysics. Among its main science drivers are circumstellar disks and extrasolar planets observations, which requires demanding high contrast imaging techniques. In that framework, METIS will be equipped with state-of-the-art phase mask coronagraphs: Apodizing Phase Plate (APP) and Annular Grooves Phase Mask (AGPM). Manufacturing the AGPM coronagraphs is a complex process that requires performance assessment with specific testing before implementation into the instrument. At Department of Astrophysics (CEA Saclay, France), responsible for the testing of the N-band AGPMs, a previously available test bench with a telescope simulator and cryogenic facility has been upgraded to comply with the AGPM tests requirements. This paper presents these requirements and describes the test bench design adopted. Then, based on preliminary results, we discuss the original solutions that permitted to reach our goals.

Published
2020

7. 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

9. Latest results and prospects of the ArTeMiS camera on APEX

Author

Eric Doumayrou, Eric Ercolani, V. Revéret, Michel Lortholary, L. Rodriguez, L. Clerc, J. Relland, L. Dumaye, F. Roussel, C. De Breuck, M. Talvard, P. Gallais, Y. Le-Pennec, D. Dubreuil, F. Schuller, F. Visticot, C. Delisle, Agnès Arnaud, Ph. André, J. Martignac, and Lionel Duband

Subjects
Telescope, Pixel, business.industry, Computer science, law, Frame (networking), Detector, Spica, business, Optical coupling, Computer hardware, law.invention, Apex (geometry)
Abstract

We present the latest results obtained with the wide-field submillimeter camera ArTeMiS that is operating on APEX since July 2013. This camera is presently equipped with 1870 pixels at 350 μm and 800 pixels at 450 μm simultaneously. ArTeMiS is a PI-camera open to the ESO and Swedish community. It has already taken a part in the 2016-2017 scientific results of APEX. So far, it offers the best performance in terms of mapping speed at 350 and 450 μm in the southern hemisphere. Major improvements of the APEX telescope have been achieved at the end of 2017, requiring a complete removal of the instruments in the C-Cabin. In the meantime, the ArTeMiS camera has been kept safe at the ALMA Operations Support Facility (OSF) building. We took advantage of this re-installation to improve a bit more the optical coupling of detectors. We present here the present status of the camera. Since APEX operation is now guaranteed until the end of 2022, our prospects are to install in time new detectors presently developed at CEA/Leti in the frame of R&D developments made for the future SPICA space mission. Those detectors, which have new polarization capabilities, are also presented.

Published
2018

10. 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

11. HERSCHEL—PACS Bolometer Arrays for Submillimeter Ground-Based Telescopes

Author

Eric Doumayrou, V. Revéret, L. Rodriguez, Patrick Agnese, B. Horeau, Pascal Gallais, Michel Lortholary, O. Boulade, Jean Le Pennec, Philippe André, Michel Talvard, and Jérome Martignac

Subjects
Physics, Spectrometer, business.industry, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Photodetector, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Photometer, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Submillimetre astronomy, law.invention, Telescope, Optics, law, Infrared window, Astrophysics::Solar and Stellar Astrophysics, General Materials Science, business, Astrophysics::Galaxy Astrophysics
Abstract

The Herschel Space Observatory will carry onboard a new kind of bolometric architecture for the PACS (Photodetector Array Camera and Spectrometer) submillimeter photometer. These new generation CCD-like multiplexed bolometer arrays are buttable and enable the conception of large fully sampled focal planes either for space or for ground-based telescopes. We present here some development for ground-based applications in the context of the ARTEMIS (ARchitecture de bolometres pour des TElescopes sub-MIllimetriques au Sol) project. We have developed an electro-thermal numerical model that simulates the performances of these semiconducting bolometers under specific ground-based conditions (different wavelengths and background powers for example). This model permits to determine the optimal parameters for each condition and shows that the bolometers can be background limited in each atmospheric transmission window between 200 and 450 microns. We also describe the optical system that provides a high optical efficiency in each submillimeter atmospheric window. Astronomical observations made with a prototype on the APEX telescope are presented.

Published
2008

12. 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

13. Antarctic observations at long wavelengths with the IRAIT-ITM Telescope at Dome C

Author

Carlos Abia, Christian Walter, Christophe Leroy-Dos Santos, L. Rodriguez, Giuliano Nucciarelli, Jean Marc Christille, Yann Reinert, D. Tavagnacco, A. Valentini, Paul Lotrus, Vincent Minier, Laurent Fromont, Oscar Straniero, Xavier Joffrin, Michel Lortholary, Pascal Tremblin, Maurizio Busso, Gilles Durand, Patrice Charron, Zalpha Challita, Min Kyong Kwon, Mauro Dolci, Samuel Ronayette, Mathieu Condamin, Eric Doumayrou, and Gino Tosti

Subjects
Meteorology, media_common.quotation_subject, Bolometer, Cryocooler, Snow, law.invention, Summer season, Telescope, Wavelength, Dome (geology), law, Sky, Environmental science, media_common, Remote sensing
Abstract

We illustrate the status of the international infra-red telescope IRAIT-ITM, a project developed thanks to an Italian- Spanish-French collaboration and now sited at the Dome C Antarctic base. The telescope and its subsystems were installed at DomeC by a team of Italian and French scientists. The 80 cm telescope is placed on a small snow hill next to a laboratory of astronomy. The operations started in January 2013, with the Nasmyth focal planes equipped with the midinfrared camera AMICA for 1.25 to 25 μm and the sub-millimetre camera CAMISTIC for observation of the sky noise at 200 and 350 μm using a bolometer camera. During 2013 the two winter-overs worked mainly on technological duties, learning how to operate the telescope, while temperatures decreased down to -80°C. The cryogenic systems could be operated respectively at 0.25K and 4K at all times, with satisfactory use of the heat from the compressors of the cryocoolers to the warm-up the laboratory through a closed loop glycol system. The lack of tests and reliability in extreme conditions of some components and difficult access to maintenance hampered regular observations below -50°C. Using the lessons of this first winter, the summer team improves the robustness of the failing systems and ease the access to maintenance. The winter 2014 is the first one with programmed observations. Because of power restrictions, the two instruments are used each one at a time by periods of 2 weeks. The Camistic camera continues to observe the stability of the sky at a fixed altitude in chopping mode and performs skydips. The TCS is being upgraded in order to prepare the next summer season with extensive observations of the sun with Camistic.

Published
2014

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. Antarctic observations at long wavelengths with the IRAIT-ITM Telescope at Dome CGround-based and Airborne Telescopes V

Author

Stepp, Larry M., Roberto, Gilmozzi, Hall, Helen J., Durand, Gilles A., Pascal, Tremblin, Vincent, Minier, Yann, Reinert, Christophe Leroy dos Santos, Louis, Rodriguez, Xavier, Joffrin, Busso, Maurizio Maria, Tosti, Gino, Nucciarelli, Giuliano, Mauro, Dolci, Oscar, Straniero, Angelo, Valentini, Carlos, Abia, Jean Marc Christille, Eric, Doumayrou, Michel, Lortholary, Patrice, Charron, Paul, Lotrus, Christian, Walter, Samuel, Ronayette, Zalpha, Challita, Laurent, Fromont, Mathieu, Condamin, Min Kyong Kwon, and Daniele, Tavagnacco

Published
2014

16. Evidence of triggered star formation in G327.3-0.6. Dust-continuum mapping of an infrared dark cloud with P-ArTéMiS

Author

Friedrich Wyrowski, Didier Dubreuil, G. Hamon, Vincent Minier, Per Bergman, Frédérique Motte, J. Martignac, P. O. Lagage, M. Talvard, Eric Doumayrou, H. Roussel, Michel Lortholary, O. Boulade, J. Le Pennec, Hans Olofsson, Ph. André, L. Rodriguez, G. Willmann, V. Revéret, Pascal Gallais, 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 de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], ESO, European Southern Observatory (ESO), Max-Planck-Institut für Radioastronomie (MPIFR), 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), ANR, ArTéMiS, ANR-08-PANH-0002,ARTEMIS,Action de Réduction du Temps de dEmarrage et d'optiMIsation des systèmes de puissance à pile à combustible pour le Secours électrique(2008), 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and ANR: ArTéMiS,ArTéMiS

Subjects
Infrared, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, law.invention, 010309 optics, Telescope, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Protostar, HII region, Infrared dark cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Star formation, Molecular cloud, Astronomy and Astrophysics, star: formation, Galactic plane, Astrophysics - Astrophysics of Galaxies, Stars, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, 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

Aims. Expanding HII regions and propagating shocks are common in the environment of young high-mass star-forming complexes. They can compress a pre-existing molecular cloud and trigger the formation of dense cores. We investigate whether these phenomena can explain the formation of high-mass protostars within an infrared dark cloud located at the position of G327.3-0.6 in the Galactic plane, in between two large infrared bubbles and two HII regions. Methods: The region of G327.3-0.6 was imaged at 450 ? m with the CEA P-ArT\'eMiS bolometer array on the Atacama Pathfinder EXperiment telescope in Chile. APEX/LABOCA and APEX-2A, and Spitzer/IRAC and MIPS archives data were used in this study. Results: Ten massive cores were detected in the P-ArT\'eMiS image, embedded within the infrared dark cloud seen in absorption at both 8 and 24 ?m. Their luminosities and masses indicate that they form high-mass stars. The kinematical study of the region suggests that the infrared bubbles expand toward the infrared dark cloud. Conclusions: Under the influence of expanding bubbles, star formation occurs in the infrared dark areas at the border of HII regions and infrared bubbles., Comment: 4 pages

Published
2009

17. First 450-micron dust continuum mapping of the massive star-forming region NGC 3576 with the P-ArTeMiS bolometer camera

Author

V. Revéret, G. Hamon, C. De Breuck, L. Rodriguez, Michel Lortholary, J. Stutzki, Eric Pantin, Pascale Andre, Pascal Gallais, O. Boulade, Cormac Purcell, J. Le Pennec, Didier Dubreuil, J. Martignac, P. O. Lagage, Tracey Hill, Nicola Schneider, M. Miller, Vincent Minier, Eric Doumayrou, Sylvain Bontemps, H. Roussel, M. Talvard, 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), Solar-Terrestrial Centre of Excellence [Brussels] (STCE), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Chemical Laboratories, University of Cambridge [UK] (CAM), Swinburne University of Technology (Hawthorn campus), Aquatic Environment Research Centre, Department of geography, 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), 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 des matériaux et du génie physique (LMGP ), Institut National Polytechnique de Grenoble (INPG)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Informatique de Nantes Atlantique (LINA), Mines Nantes (Mines Nantes)-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), ESO, European Southern Observatory (ESO), Chimie Et Interdisciplinarité : Synthèse, Analyse, Modélisation (CEISAM), Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), Station Expérimentale de Guernévez, Institut National de la Recherche Agronomique (INRA), Department of Health Sciences Research [Mayo Clinic] (HSR), Mayo Clinic, Laboratoire Hétérochimie Fondamentale et Appliquée (LHFA), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie de Toulouse (ICT-FR 2599), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), 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), 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 des matériaux et du génie physique (LMGP), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG), School of Physics, Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), and Université Fédérale Toulouse Midi-Pyrénées

Subjects
ISM: structure, Continuum (design consultancy), [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, ISM: clouds, law.invention, 010309 optics, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], law, 0103 physical sciences, Protostar, submillimeter, 010303 astronomy & astrophysics, Physics, stars: formation, Star formation, Astrophysics (astro-ph), Bolometer, Astronomy and Astrophysics, Galaxy, Stars, Space and Planetary Science, stars: circumstellar matter, ISM: individual objects: NGC 3576
Abstract

Context: The earliest phases of massive star formation are currently much debated. Aims. In an effort to make progress, we took a census of Class0-like protostellar dense cores in the NGC 3576 region, one of the nearest and most luminous embedded sites of high-mass star formation in the Galaxy. Methods: We used the P-ArTeMiS bolometer camera on the APEX telescope to produce the first 450-micron dust continuum map of the filamentary dense clump associated with NGC 3576. Results: Combining our 450-micron observations with existing data at other wavelengths, we have identified seven massive protostellar sources along the NGC 3576 filament and placed them in the M_env - L_bol evolutionary diagram for protostars. Conclusions: Comparison with theoretical evolutionary tracks suggests that these seven protostellar sources will evolve into massive stars with masses M* ~ 15-50 Msun. Four sources are classified as candidate high-mass Class 0 objects, two sources as massive Class I objects, and one source appears to be at an intermediate stage., 9 pages, 2 figures + 2 online figures, 2 online tables. Accepted for publication in A&A (Letters)

Published
2008

18. Cosmic ray identification and rejection in the EPIC-MOS cameras onboard XMM-Newton: results from flight data

Author

Jean Luc Sauvageot, Claude Pigot, Philippe Ferrando, and Michel Lortholary

Subjects
Physics, Physics::Instrumentation and Detectors, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Flux, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, EPIC, Space radiation, Cardinal point, Optics, business, Flight data
Abstract

We have analysed the tracks left by cosmic-ray particles on the CCDs of the EPIC-MOS cameras onboard XMM-Newton. These tracks could be entirely visualized by using a special operation test mode, and their characterization could be performed. This has allowed to measure the cosmic-ray flux at the level of the focal plane, as well as the fraction of the CCD surface which is sterilized by the cosmic-ray impacts. The relation between this fraction and parameters transmitted to the ground during normal observations has been established.

Published
2003

19. Characterization in the laboratory of VISIR, the mid-infrared imager and spectrometer for the VLT

Author

Anton Schoenmaker, Arnaud Claret, Arie N. de Jong, S. Damstra, Yves Lussignol, Eddy Elswijk, Charles Lyraud, Jan-Willem Pel, Gilles Durand, Johan Pragt, Philippe Galdemard, Gabby Kroes, Didier Dubreuil, Martial Authier, Jean Belorgey, Jean-Francois Gournay, Pierre-Olivier Lagage, Michel Lortholary, Yvon Rio, C. Veyssiere, and Eric Pantin

Subjects
Physics, Very Large Telescope, Spectrometer, Observatory, Infrared, Instrumentation, Mid infrared, Spectral resolution, Remote sensing
Abstract

In this paper, we present the status of VISIR, the mid-infrared instrument to be installed in 2003 at theCassegrain focus of MELIPAL, one of the four 8-meter telescopes of the European Very Large Telescope. Thiscryogenic instrument, optimized for diffraction-limited performance in both mid-infrared atmospheric windows(N and Q band), combines imaging capabilities over a field up to about 1x1 arcmin 2 , and long-slit (0.5 arcmin)grating spectroscopy with various spectral resolutions up to R=25000 at 10 m and 12500 at 20 m. Thecontract to design and build VISIR was signed in November 1996 between the European Southern Observatory(ESO) and a French-Dutch consortium of institutes led by Service d'Astrophysique of Commissariat a l'EnergieAtomique (CEA). A key step in the project has been passed in December 2001, with the first infrared images inthe laboratory and in April 2002 with the first infrared spectra in the laboratory. We present the results of thelaboratorytests of the instrument, which is scheduled to be shipped to Paranal at the end of 2002.Keywords : infrared, instrumentation, imager, spectrometer, VLT.

Published
2003

20. HERSCHEL—PACS Bolometer Arrays for Submillimeter Ground-Based Telescopes.

Author

Philippe André, Michel Talvard, Louis Rodriguez, Olivier Boulade, Eric Doumayrou, Pascal Gallais, Benoit Horeau, Jean Le Pennec, Michel Lortholary, Jérome Martignac, and Patrick Agnèse

Subjects
SPACE (Architecture), COMPOSITION in architecture, URBAN planning, SPACE perception
Abstract

Abstract   The Herschel Space Observatory will carry onboard a new kind of bolometric architecture for the PACS (Photodetector Array Camera and Spectrometer) submillimeter photometer. These new generation CCD-like multiplexed bolometer arrays are buttable and enable the conception of large fully sampled focal planes either for space or for ground-based telescopes. We present here some development for ground-based applications in the context of the ARTEMIS (ARchitecture de bolomètres pour des TElescopes sub-MIllimétriques au Sol) project. We have developed an electro-thermal numerical model that simulates the performances of these semiconducting bolometers under specific ground-based conditions (different wavelengths and background powers for example). This model permits to determine the optimal parameters for each condition and shows that the bolometers can be background limited in each atmospheric transmission window between 200 and 450 microns. We also describe the optical system that provides a high optical efficiency in each submillimeter atmospheric window. Astronomical observations made with a prototype on the APEX telescope are presented. [ABSTRACT FROM AUTHOR]

Published
2008

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