« Un pasteur de son peuple… »

National audienceEn 1761, Bernard Aymable Dupuy (1707-† 1789) alors maître de musique de la collégiale Saint-Sernin de Toulouse compose une Idylle Un pasteur de son peuple pour célébrer l’intronisation de Monseigneur Arthur Richard Dillon (1721-† 1806) à l’archevêché de Toulouse. Cette pièce de circonstance d’une réelle qualité musicale est un portrait en musique du prélat qui fut également le dernier président des États du Languedoc. La pièce fut rejouée dans la grande salle des Synodes de Narbonne en 2009 à l’occasion du retour du corps de Monseigneur Dillon mort en exil en Angleterre. Seulement connue par un très beau volume conservé par la bibliothèque municipale de Toulouse, la partition de l’Idylle a été éditée en 2008 par le Centre de Musique Baroque de Versailles

Submillimetre/TeraHertz Astronomy at Dome C with CEA filled bolometer array

Submillimetre/TeraHertz (e.g. 200, 350, 450 microns) astronomy is the prime technique to unveil the birth and early evolution of a broad range of astrophysical objects. A major obstacle to carry out submm observations from ground is the atmosphere. Preliminary site testing and atmospheric transmission models tend to demonstrate that Dome C could offer the best conditions on Earth for submm/THz astronomy. The CAMISTIC project aims to install a filled bolometer-array camera with 16x16 pixels on IRAIT at Dome C and explore the 200-$\mu$m windows for potential ground-based observations.Comment: 6 page

La Maîtrise de la cathédrale Notre-Dame de Rodez aux XVIIe et XVIIIe siècles

L'étude des baux d'engagement des maîtres de musique de la cathédrale de Rodez aux XVIIe et XVIIIe siècles, ainsi que les délibérations du chapitre donnent une image la vie quotidienne à la maîtrise, et de son évolution sur la période considérée. Au fil de ces contrats, apparaissent la vie des enfants de chœur et des musiciens, les modalités de l'apprentissage, le fonctionnement et les pratiques musicales au service de cette vénérable institution

Scanamorphos: a map-making software for Herschel and similar scanning bolometer arrays

Scanamorphos is one of the public softwares available to post-process scan observations performed with the Herschel photometer arrays. This post-processing mainly consists in subtracting the total low-frequency noise (both its thermal and non-thermal components), masking high-frequency artefacts such as cosmic ray hits, and projecting the data onto a map. Although it was developed for Herschel, it is also applicable with minimal adjustment to scan observations made with some other imaging arrays subjected to low-frequency noise, provided they entail sufficient redundancy; it was successfully applied to P-Artemis, an instrument operating on the APEX telescope. Contrary to matrix-inversion softwares and high-pass filters, Scanamorphos does not assume any particular noise model, and does not apply any Fourier-space filtering to the data, but is an empirical tool using purely the redundancy built in the observations -- taking advantage of the fact that each portion of the sky is sampled at multiple times by multiple bolometers. It is an interactive software in the sense that the user is allowed to optionally visualize and control results at each intermediate step, but the processing is fully automated. This paper describes the principles and algorithm of Scanamorphos and presents several examples of application.Comment: This is the final version as accepted by PASP (on July 27, 2013). A copy with much better-quality figures is available on http://www2.iap.fr/users/roussel/herschel

Catalogue de l'oeuvre de Bernard Aymable DUPUY (1707-1789)

Le compositeur toulousain Bernard Aymable Dupuy (1707 † 1789) laisse à la postérité une œuvre importante bien que largement méconnue. Le maître de musique de Saint-Sernin de Toulouse eut une longue vie, il s’éteint à l’âge de 82 ans, et ses compositions couvrent une période allant de 1728 à 1789, année de sa mort. Le catalogue de son œuvre est précédé d’une introduction qui replace le compositeur et ses productions dans le contexte de l’époque, et donne une vision d’ensemble des quelques 70 pièces répertoriées à ce jour. Majoritairement spirituelle, mais pas uniquement, cette production est resté inédite jusqu’à ces dernières années, où quelques pièces choisies ont été éditées par le Centre de Musique Baroque de Versailles. Les manuscrits de Dupuy sont conservés dans différentes bibliothèques : Bibliothèque nationale de France, bibliothèque municipale de Toulouse, Bibliothèque Méjane d’Aix-en-Provence, bibliothèque Inguimbertine de Carpentras, bibliothèque municipale de Montpellier et Société des Lettres Sciences et Arts de l’Aveyron. Le catalogue analyse chaque pièce, présentant pour chaque mouvement l’effectif, l’incipit (musical et littéraire) le détail de la source, le texte et une courte note concernant la structure musicale

Recent Development of MESSINE, a 3D Eddy Current Model

In the 1996 QNDE Conference, we presented a parametric forward model [1], which has been recently named MESSINE (Model for Electromagnetic Simplified Simulation In Nondestructive Evaluation), to predict eddy current signal. The proposed model first discretizes the eddy current distribution into current loops. A parametric description of the shape of these loops is given according to the observation of the results obtained with a three-dimensional finite element code which provides a realistic distribution of the induced currents. The loops’ inductances and resistances are then calculated. By considering the system constituted of the coil and the current loops as a « multi-transformer», their current intensity is determined. The impedance change, which is the component of the eddy current signal, can then be deduced. The model was validated in the case of axisymmetric configurations. Comparisons with both analytical (Dodd and Deeds [2]) and numerical models showed very good agreements. Then the proposed model was applied to three-dimensional configurations. Impedance changes of a coil along rectangular through-wall slot were calculated. Comparisons with experimental results show a fairly good agreement for the impedance change phases, but a poorer one for the impedance change amplitudes. Investigations were made to improve the parametric description of the current loop deformation. One of the solutions to improve the parametric description is presented here

Evidence of triggered star formation in G327.3-0.6. Dust-continuum mapping of an infrared dark cloud with P-ArT\'eMiS

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 page

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

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 915

Probing the structure of a massive filament: ArTéMiS 350 and 450 μm mapping of the integral-shaped filament in Orion A

Context. The Orion molecular cloud is the closest region of high-mass star formation. It is an ideal target for investigating the detailed structure of massive star-forming filaments at high resolution and the relevance of the filament paradigm for the earliest stages of intermediate- to high-mass star formation. Aims. Within the Orion A molecular cloud, the integral-shaped filament (ISF) is a prominent, degree-long structure of dense gas and dust with clear signs of recent and ongoing high-mass star formation. Our aim is to characterise the structure of this massive filament at moderately high angular resolution (8′′ or ~0.016 pc) in order to measure the intrinsic width of the main filament, down to scales well below 0.1 pc, which has been identified as the characteristic width of filaments. Methods. We used the ArTéMiS bolometer camera at APEX to map a ~0.6 × 0.2 deg2 region covering OMC-1, OMC-2, and OMC-3 at 350 and 450 μm. We combined these data with Herschel-SPIRE maps to recover extended emission. The combined Herschel-ArTéMiS maps provide details on the distribution of dense cold material, with a high spatial dynamic range, from our 8′′ resolution up to the transverse angular size of the map, ~10-15′. By combining Herschel and ArTéMiS data at 160, 250, 350, and 450 μm, we constructed high-resolution temperature and H2 column density maps. We extracted radial intensity profiles from the column density map in several representative portions of the ISF, which we fitted with Gaussian and Plummer models to derive their intrinsic widths. We also compared the distribution of material traced by ArTéMiS with that seen in the higher-density tracer N2H+(1-0) that was recently observed with the ALMA interferometer. Results. All the radial profiles that we extracted show a clear deviation from a Gaussian, with evidence for an inner plateau that had not previously been seen clearly using Herschel-only data. We measure intrinsic half-power widths in the range 0.06-0.11 pc. This is significantly larger than the Gaussian widths measured for fibres seen in N2H+, which probably only traces the dense innermost regions of the large-scale filament. These half-power widths are within a factor of two of the value of ~0.1 pc found for a large sample of nearby filaments in various low-mass star-forming regions, which tends to indicate that the physical conditions governing the fragmentation of pre-stellar cores within transcritical or supercritical filaments are the same over a large range of masses per unit length. © F. Schuller et al. 2021

Probing the role of protostellar feedback in clustered star formation. Mapping outflows in the collapsing protocluster NGC 2264-C

The role played by protostellar feedback in clustered star formation is still a matter of debate. In particular, protostellar outflows have been proposed as a source of turbulence in cluster-forming clumps, which may provide support against global collapse for several free-fall times. Here, we seek to test the above hypothesis in the case of the well-documented NGC 2264-C protocluster, byquantifying the amount of turbulence and support injected in the surrounding medium by protostellar outflows. Using the HERA heterodyne array on the IRAM 30m telescope, we carried out an extensive mapping of NGC 2264-C in the three molecular line transitions 12CO(2-1), 13CO(2-1), and C18O(2-1). We found widespread high-velocity 12CO emission, testifying to the presence of eleven outflow lobes, closely linked to the compact millimeter continuum sources previously detected in the protocluster. We carried out a detailed analysis of the dynamical parameters of these outflows, including a quantitative evaluation of the overall momentum flux injected in the cluster-forming clump. These dynamical parameters were compared to the gravitational and turbulent properties of the clump. We show that the population of protostellar outflows identified in NGC 2264-C are likely to contribute a significant fraction of the observed turbulence but cannot efficiently support the protocluster against global collapse. Gravity appears to largely dominate the dynamics of the NGC 2264-C clump at the present time. It is however possible that an increase in the star formation rate during the further evolution of the protocluster will trigger sufficient outflows to finally halt the contraction of the cloud.Comment: Accepted for publication in Astronomy & Astrophysics. The quality of figures has been deteriorated to match arXiv size limitatio