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1. 3D extinction mapping of the Milky Way using Convolutional Neural Networks: Presentation of the method and demonstration in the Carina Arm region

Author: Cornu, D., Montillaud, J., Marshall, D. J., Robin, A. C., and Cambrésy, L.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Context. Several methods have been proposed to build 3D extinction maps of the Milky Way (MW), most often based on Bayesian approaches. Although some studies employed machine learning (ML) methods in part of their procedure, or to specific targets, no 3D extinction map of a large volume of the MW solely based on a Neural Network method has been reported so far. Aims. We aim to apply deep learning as a solution to build 3D extinction maps of the MW. Methods. We built a convolutional neural network (CNN) using the CIANNA framework, and trained it with synthetic 2MASS data. We used the Besan\c{c}on Galaxy model to generate mock star catalogs, and 1D Gaussian random fields to simulate the extinction profiles. From these data we computed color-magnitude diagrams (CMDs) to train the network, using the corresponding extinction profiles as targets. A forward pass with observed 2MASS CMDs provided extinction profile estimates for a grid of lines of sight. Results. We trained our network with data simulating lines of sight in the area of the Carina spiral arm tangent and obtained a 3D extinction map for a large sector in this region ($l = 257 - 303$ deg, $|b| \le 5$ deg), with distance and angular resolutions of $100$ pc and $30$ arcmin, respectively, and reaching up to $\sim 10$ kpc. Although each sightline is computed independently in the forward phase, the so-called fingers-of-God artifacts are weaker than in many other 3D extinction maps. We found that our CNN was efficient in taking advantage of redundancy across lines of sight, enabling us to train it with only 9 sightlines simultaneously to build the whole map. Conclusions. We found deep learning to be a reliable approach to produce 3D extinction maps from large surveys. With this methodology, we expect to easily combine heterogeneous surveys without cross-matching, and therefore to exploit several surveys in a complementary fashion., Comment: 7 pages
Published: 2022

2. The Hi-GAL catalogue of dusty filamentary structures in the Galactic Plane

Author: Schisano, E., Molinari, S., Elia, D., Benedettini, M., Olmi, L., Pezzuto, S., Traficante, A., Brescia, M., Cavuoti, S., di Giorgio, A. M., Liu, S. J., Moore, T. J. T., Noriega-Crespo, A., Riccio, G., Baldeschi, A., Becciani, U., Peretto, N., Merello, M., Vitello, F., Zavagno, A., Beltrán, M. T., Cambrésy, L., Eden, D. J., Causi, G. Li, Molinaro, M., Palmeirim, P., Sciacca, E., Testi, L., Umana, G., and Whitworth, A. P.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: The recent data collected by {\it Herschel} have confirmed that interstellar structures with filamentary shape are ubiquitously present in the Milky Way. Filaments are thought to be formed by several physical mechanisms acting from the large Galactic scales down to the sub-pc fractions of molecular clouds, and they might represent a possible link between star formation and the large-scale structure of the Galaxy. In order to study this potential link, a statistically significant sample of filaments spread throughout the Galaxy is required. In this work we present the first catalogue of $32,059$ candidate filaments automatically identified in the Hi-GAL survey of the entire Galactic Plane. For these objects we determined morphological (length, $l^{a}$, and geometrical shape) and physical (average column density, $N_{\rm H_{2}}$, and average temperature, $T$) properties. We identified filaments with a wide range of properties: 2$'$\,$\leq l^{a}\leq$\, 100$'$, $10^{20} \leq N_{\rm H_{2}} \leq 10^{23}$\,cm$^{-2}$ and $10 \leq T\leq$ 35\,K. We discuss their association with the Hi-GAL compact sources, finding that the most tenuous (and stable) structures do not host any major condensation and we also assign a distance to $\sim 18,400$ filaments for which we determine mass, physical size, stability conditions and Galactic distribution. When compared to the spiral arms structure, we find no significant difference between the physical properties of on-arm and inter-arm filaments. We compared our sample with previous studies, finding that our Hi-GAL filament catalogue represents a significant extension in terms of Galactic coverage and sensitivity. This catalogue represents an unique and important tool for future studies devoted to understanding the filament life-cycle., Comment: 38 pages, 29 figures, 3 appendices
Published: 2019
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3. French SKA White Book - The French Community towards the Square Kilometre Array

Author: Acero, F., Acquaviva, J. -T., Adam, R., Aghanim, N., Allen, M., Alves, M., Ammanouil, R., Ansari, R., Araudo, A., Armengaud, E., Ascaso, B., Athanassoula, E., Aubert, D., Babak, S., Bacmann, A., Banday, A., Barriere, K., Bellossi, F., Bernard, J. -P., Bernardini, M. G., Béthermin, M., Blanc, E., Blanchet, L., Bobin, J., Boissier, S., Boisson, C., Boselli, A., Bosma, A., Bosse, S., Bottinelli, S., Boulanger, F., Boyer, R., Bracco, A., Briand, C., Bucher, M., Buat, V., Cambresy, L., Caillat, M., Casandjian, J. -M., Caux, E., Célestin, S., Cerruti, M., Charlot, P., Chassande-Mottin, E., Chaty, S., Christensen, N., Ciesla, L., Clerc, N., Cohen-Tanugi, J., Cognard, I., Combes, F., Comis, B., Corbel, S., Cordier, B., Coriat, M., Courtin, R., Courtois, H., Da Silva, B., Daddi, E., Dallier, R., Dartois, E., Demyk, K., Denis, J. -M., Denis, L., Djannati-Ataï, A., Donati, J. -F., Douspis, M., van Driel, W., Korso, M. N. El, Falgarone, E., Fantina, A., Farges, T., Ferrari, A., Ferrari, C., Ferrière, K., Flamary, R., Gac, N., Gauffre, S., Genova, F., Girard, J., Grenier, I., Griessmeier, J. -M., Guillard, P., Guillemot, L., Gulminelli, F., Gusdorf, A., Habart, E., Hammer, F., Hennebelle, P., Herpin, F., Hervet, O., Hughes, A., Ilbert, O., Janvier, M., Josselin, E., Julier, A., Lachaud, C., Lagache, G., Lallement, R., Lambert, S., Lamy, L., Langer, M., Larzabal, P., Lavaux, G., Bertre, T. Le, Fèvre, O. Le, Tiec, A. Le, Lefloch, B., Lehnert, M., Lemoine-Goumard, M., Levrier, F., Limousin, M., Lis, D., López-Sepulcre, A., Macias-Perez, J., Magneville, C., Marcowith, A., Margueron, J., Marquette, G., Marshall, D., Martin, L., Mary, D., Masson, S., Maurogordato, S., Mazauric, C., Mellier, Y., Miville-Deschênes, M. -A., Montier, L., Mottez, F., Mourard, D., Nesvadba, N., Nezan, J. -F., Noterdaeme, P., Novak, J., Ocvirk, P., Oertel, M., Olive, X., Ollier, V., Palanque-Delabrouille, N., Pandey-Pommier, M., Pennec, Y., Pérault, M., Peroux, C., Petit, P., Pétri, J., Petiteau, A., Pety, J., Pratt, G. W., Puech, M., Quertier, B., Raffin, E., Harison, S. Rakotozafy, Rawson, S., Renaud, M., Revenu, B., Richard, C., Richard, J., Rincon, F., Ristorcelli, I., Rodriguez, J., Schultheis, M., Schimd, C., Semelin, B., Sol, H., Starck, J. -L., Tagger, M., Tasse, C., Theureau, G., Torchinsky, S., Vastel, C., Vergani, S. D., Verstraete, L., Vigouroux, X., Vilmer, N., Vilotte, J. -P., Webb, N., Ysard, N., and Zarka, P.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The "Square Kilometre Array" (SKA) is a large international radio telescope project characterised, as suggested by its name, by a total collecting area of approximately one square kilometre, and consisting of several interferometric arrays to observe at metric and centimetric wavelengths. The deployment of the SKA will take place in two sites, in South Africa and Australia, and in two successive phases. From its Phase 1, the SKA will be one of the most formidable scientific machines ever deployed by mankind, and by far the most impressive in terms of data throughput and required computing power. With the participation of almost 200 authors from forty research institutes and six private companies, the publication of this French SKA white paper illustrates the strong involvement in the SKA project of the French astronomical community and of a rapidly growing number of major scientific and technological players in the fields of Big Data, high performance computing, energy production and storage, as well as system integration., Comment: Editor in chief: C. Ferrari; Editors: M. Alves, S. Bosse, S. Corbel, A. Ferrari, K. Ferri\`ere, S. Gauffre, E. Josselin, G. Lagache, S. Lambert, G. Marquette, J.-M. Martin, M.-A. Miville-Desch\^enes, L. Montier, B. Semelin, G. Theureau, S. Vergani, N. Vilmer, P. Zarka; Original file with high resolution figures at SKA-France link: https://ska-france.oca.eu/images/SKA-France-Media/FWB_051017.pdf
Published: 2017

4. Multi-temperature mapping of dust structures throughout the Galactic Plane using the PPMAP tool with Herschel Hi-GAL data

Author: Marsh, K. A., Whitworth, A. P., Lomax, O., Ragan, S. E., Becciani, U., Cambresy, L., Di Giorgio, A., Eden, D., Elia, D., Kacsuk, P., Molinari, S., Palmeirim, P., Pezzuto, S., Schneider, N., Sciacca, E., and Vitello, F.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We describe new Hi-GAL based maps of the entire Galactic Plane, obtained using continuum data in the wavelength range 70-500 $\mu$m. These maps are derived with the PPMAP procedure, and therefore represent a significant improvement over those obtained with standard analysis techniques. Specifically they have greatly improved resolution (12 arcsec) and, in addition to more accurate integrated column densities and mean dust temperatures, they give temperature-differential column densities, i.e., separate column density maps in twelve distinct dust temperature intervals, along with the corresponding uncertainty maps. The complete set of maps is available on-line. We briefly describe PPMAP and present some illustrative examples of the results. These include (a) multi-temperature maps of the Galactic HII region W5-E, (b) the temperature decomposition of molecular cloud column-density probability distribution functions, and (c) the global variation of mean dust temperature as a function of Galactocentric distance. Amongst our findings are: (i) a strong localised temperature gradient in W5-E in a direction orthogonal to that towards the ionising star, suggesting an alternative heating source and providing possible guidance for models of the formation of the bubble complex, and (ii) the overall radial profile of dust temperature in the Galaxy shows a monotonic decrease, broadly consistent both with models of the interstellar radiation field and with previous estimates at lower resolution. However, we also find a central temperature plateau within ~ 6 kpc of the Galactic centre, outside of which is a pronounced steepening of the radial profile. This behaviour may reflect the greater proportion of molecular (as opposed to atomic) gas in the central region of the Galaxy., Comment: 14 pages, 12 figures; accepted for publication in MNRAS
Published: 2017
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5. Properties of Hi-GAL clumps in the inner Galaxy]{The Hi-GAL compact source catalogue. I. The physical properties of the clumps in the inner Galaxy ($-71.0^{\circ}< \ell < 67.0^{\circ}$)

Author: Elia, D., Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, S., Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmerim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltrán, M. T., Billot, N., Cambrésy, L., Cesaroni, R., García-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mège, P., Peretto, N., Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., Becciani, U., Brescia, M., Buemi, C., Bufano, F., Butora, R., Cavuoti, S., Costa, A., Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., Leto, P., Causi, G. Li, Marchili, N., Martinavarro-Armengol, S., Mercurio, A., Molinaro, M., Riccio, G., Sano, H., Sciacca, E., Tachihara, K., Torii, K., Trigilio, C., Vitello, F., and Yamamoto, H.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Hi-GAL is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 $\mu$m. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogs presented in Molinari et al. (2016a), covering the portion of Galactic plane $-71.0^{\circ}< \ell < 67.0^{\circ}$. The band-merged catalogue contains 100922 sources with a regular SED, 24584 of which show a 70 $\mu$m counterpart and are thus considered proto-stellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterise different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in proto-stellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to proto-stellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between "on-arm" and "inter-arm" positions., Comment: Accepted by MNRAS
Published: 2017
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6. Spatial distribution of star formation related to ionized regions throughout the inner Galactic plane

Author: Palmeirim, P., Zavagno, A., Elia, D., Moore, T. J. T., Whitworth, A., Tremblin, P., Traficante, A., Merello, M., Russeil, D., Pezzuto, S., Cambrésy, L., Baldeschi, A., Bandieramonte, M., Becciani, U., Benedettini, M., Buemi, C., Bufano, F., Bulpitt, A., Butora, R., Carey, D., Costa, A., Deharveng, L., Di Giorgio, A., Eden, D., Hajnal, A., Hoare, M., Kacsuk, P., Leto, P., Marsh, K., Mège, P., Molinari, S., Molinaro, M., Noriega-Crespo, A., Schisano, E., Sciacca, E., Trigilio, C., Umana, G., and Vitello, F.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present a comprehensive statistical analysis of star-forming objects located in the vicinities of 1 360 bubble structures throughout the Galactic Plane and their local environments. The compilation of ~70 000 star-forming sources, found in the proximity of the ionized (Hii) regions and detected in both Hi-GAL and GLIMPSE surveys, provided a broad overview of the different evolutionary stages of star-formation in bubbles, from prestellar objects to more evolved young stellar objects (YSOs). Surface density maps of star-forming objects clearly reveal an evolutionary trend where more evolved star-forming objects are found spatially located near the center, while younger star-forming objects are found at the edge of the bubbles. We derived dynamic ages for a subsample of 182 Hii regions for which kinematic distances and radio continuum flux measurements were available. We detect ~80% more star-forming sources per unit area in the direction of bubbles than in the surrounding fields. We estimate ~10% clump formation efficiency (CFE) of Hi-GAL clumps in bubbles, twice the CFE in fields not affected by feedback. We find higher CFE of protostellar clumps in younger bubbles, whose density of the bubble shells is higher. We argue that the formation rate from prestellar to protostellar phase is probably higher during the early stages of the bubble expansion. Evaluation of the fragmentation time inside the shell of bubbles advocates the preexistence of clumps in the medium before the bubble, as supported by numerical simulations. Approximately 23% of the Hi-GAL clumps are found located in the direction of a bubble, with 15% for prestellar clumps and 41% for protostellar clumps. We argue that the high fraction of protostellar clumps may be due to the acceleration of the star-formation process cause by the feedback of the (Hii) bubbles., Comment: 15 pages, 12 figures. Accepted for publication by Astronomy and Astrophysics
Published: 2017
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7. Hierarchical progressive surveys. Multi-resolution HEALPix data structures for astronomical images, catalogues, and 3-dimensional data cubes

Author: Fernique, P., Allen, M. G., Boch, T., Oberto, A., Pineau, F-X., Durand, D., Bot, C., Cambresy, L., Derriere, S., Genova, F., and Bonnarel, F.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Scientific exploitation of the ever increasing volumes of astronomical data requires efficient and practical methods for data access, visualisation, and analysis. Hierarchical sky tessellation techniques enable a multi-resolution approach to organising data on angular scales from the full sky down to the individual image pixels. Aims. We aim to show that the Hierarchical progressive survey (HiPS) scheme for describing astronomical images, source catalogues, and three-dimensional data cubes is a practical solution to managing large volumes of heterogeneous data and that it enables a new level of scientific interoperability across large collections of data of these different data types. Methods. HiPS uses the HEALPix tessellation of the sphere to define a hierarchical tile and pixel structure to describe and organise astronomical data. HiPS is designed to conserve the scientific properties of the data alongside both visualisation considerations and emphasis on the ease of implementation. We describe the development of HiPS to manage a large number of diverse image surveys, as well as the extension of hierarchical image systems to cube and catalogue data. We demonstrate the interoperability of HiPS and Multi-Order Coverage (MOC) maps and highlight the HiPS mechanism to provide links to the original data. Results. Hierarchical progressive surveys have been generated by various data centres and groups for ~200 data collections including many wide area sky surveys, and archives of pointed observations. These can be accessed and visualised in Aladin, Aladin Lite, and other applications. HiPS provides a basis for further innovations in the use of hierarchical data structures to facilitate the description and statistical analysis of large astronomical data sets., Comment: 21 pages, 6 figures. Accepted for publication in Astronomy & Astrophysics
Published: 2015
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8. Modeling and predicting the shape of the far-infrared to submillimeter emission in ultra-compact HII regions and cold clumps

Author: Paradis, D., Mény, C., Noriega-Crespo, A., Paladini, R., Bernard, J. -P., Bot, C., Cambrésy, L., Demyk, K., Gromov, V., Rivera-Ingraham, A., and Veneziani, M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Dust properties are very likely affected by the environment in which dust grains evolve. For instance, some analyses of cold clumps (7 K- 17 K) indicate that the aggregation process is favored in dense environments. However, studying warm (30 K-40 K) dust emission at long wavelength ($\lambda$$>$300 $\mu$m) has been limited because it is difficult to combine far infared-to-millimeter (FIR-to-mm) spectral coverage and high angular resolution for observations of warm dust grains. Using Herschel data from 70 to 500 $\mu$m, which are part of the Herschel infrared Galactic (Hi-GAL) survey combined with 1.1 mm data from the Bolocam Galactic Plane Survey (BGPS), we compared emission in two types of environments: ultra-compact HII (UCHII) regions, and cold molecular clumps (denoted as cold clumps). With this comparison we tested dust emission models in the FIR-to-mm domain that reproduce emission in the diffuse medium, in these two environments (UCHII regions and cold clumps). We also investigated their ability to predict the dust emission in our Galaxy. We determined the emission spectra in twelve UCHII regions and twelve cold clumps, and derived the dust temperature (T) using the recent two-level system (TLS) model with three sets of parameters and the so-called T-$\beta$ (temperature-dust emissvity index) phenomenological models, with $\beta$ set to 1.5, 2 and 2.5. We tested the applicability of the TLS model in warm regions for the first time. This analysis indicates distinct trends in the dust emission between cold and warm environments that are visible through changes in the dust emissivity index. However, with the use of standard parameters, the TLS model is able to reproduce the spectral behavior observed in cold and warm regions, from the change of the dust temperature alone, whereas a T-$\beta$ model requires $\beta$ to be known., Comment: Accepted for publication in A&A. 19 pages, 8 figures, 7 tables
Published: 2014
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9. Young stellar clusters in the Rosette molecular cloud. Arguments against triggered star formation

Author: Cambrésy, L., Marton, G., Feher, O., Tóth, L. V., and Schneider, N.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The Rosette complex is a well studied region of the galactic plane which presents the apparent characteristics of a triggered star forming region. This is however still debated as no strong evidence corroborates this statement. We focus on characterizing the young stellar population in the Rosette complex to improve our understanding of the processes that regulate the star formation in this region. We propose an original method that relies on the joint analysis of the star color and density in the near-infrared. It leads to mapping the molecular cloud spatial distribution and detecting the embedded clusters with their characterization in terms of member number and age estimation. We have identified 13 clusters, 2 of which are new discoveries, and we estimate that the total number of young stellar objects in the Rosette ranges between 4000 and 8000 members. We find that the age distribution of the young clusters is not consistent with a general triggered scenario for the star formation in this molecular cloud. This study proves that the Rosette complex evolution is not governed by the influence of its OB star population. It suggests that the simple morphological appearance of an active region is not sufficient to conclude much about the triggering role in the star formation process. Our method of constraining the cluster properties using UKIDSS and WISE data has proven efficient, and studies of other regions of the galactic plane would definitely benefit from this approach., Comment: Accepted for publication in A&A. 11 pages, 10 figures. Language edited version
Published: 2013
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10. Variation of the extinction law in the Trifid nebula

Author: Cambrésy, L., Rho, J., Marshall, D. J., and Reach, W. T.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: In the past few years, the extinction law has been measured in the infrared wavelengths for various molecular clouds and different laws have been obtained. In this paper we seek variations of the extinction law within the Trifid nebula region. Such variations would demonstrate a local dust evolution linked to variation of the environment parameters such as the density or the interstellar radiation field. The extinction values, A_lambda/A_V, are obtained using the 2MASS, UKIDSS and Spitzer/GLIMPSE surveys. The technique is to inter-calibrate color-excess maps from different wavelengths to derive the extinction law and to map the extinction in the Trifid region. We measured the extinction law at 3.6, 4.5, and 5.8 um and we found a transition at A_V ~ 20 mag. Below this threshold the extinction law is as expected from models for R_V=5.5 whereas above 20 mag of visual extinction, it is flatter. Using these results the color-excess maps are converted into a composite extinction map of the Trifid nebula at a spatial resolution of 1 arcmin. A tridimensional analysis along the line-of-sight allowed us to estimate a distance of 2.7 kpc for the Trifid. The comparison of the extinction with the 1.25 mm emission suggests the millimeter emissivity is enhanced in the dense condensations of the cloud. Our results suggest a dust transition at large extinction which has not been reported so far and dust emissivity variations., Comment: Accepted for publication in A&A. 10 pages, 8 figures
Published: 2011
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11. Filamentary structures and compact objects in the Aquila and Polaris clouds observed by Herschel

Author: Men'shchikov, A., André, Ph., Didelon, P., Könyves, V., Schneider, N., Motte, F., Bontemps, S., Arzoumanian, D., Attard, M., Abergel, A., Baluteau, J. -P., Bernard, J. -Ph., Cambrésy, L., Cox, P., Di Francesco, J., di Giorgio, A. M., Griffin, M., Hargrave, P., Huang, M., Kirk, J., Li, J. Z., Martin, P., Minier, V., Miville-Deschênes, M. -A., Molinari, S., Olofsson, G., Pezzuto, S., Roussel, H., Russeil, D., Saraceno, P., Sauvage, M., Sibthorpe, B., Spinoglio, L., Testi, L., Ward-Thompson, D., White, G., Wilson, C. D., Woodcraft, A., and Zavagno, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Our PACS and SPIRE images of the Aquila Rift and part of the Polaris Flare regions, taken during the science demonstration phase of Herschel discovered fascinating, omnipresent filamentary structures that appear to be physically related to compact cores. We briefly describe a new multi-scale, multi-wavelength source extraction method used to detect objects and measure their parameters in our Herschel images. All of the extracted starless cores (541 in Aquila and 302 in Polaris) appear to form in the long and very narrow filaments. With its combination of the far-IR resolution and sensitivity, Herschel directly reveals the filaments in which the dense cores are embedded; the filaments are resolved and have deconvolved widths of 35 arcsec in Aquila and 59 arcsec in Polaris (9000 AU in both regions). Our first results of observations with Herschel enable us to suggest that in general dense cores may originate in a process of fragmentation of complex networks of long, thin filaments, likely formed as a result of an interplay between gravity, interstellar turbulence, and magnetic fields. To unravel the roles of the processes, one has to obtain additional kinematic and polarization information; these follow-up observations are planned., Comment: 7 pages, 2 figures. Accepted for publication in Astronomy and Astrophysics, Herschel Special Issue.
Published: 2010
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12. The Aquila prestellar core population revealed by Herschel

Author: Könyves, V., André, Ph., Men'shchikov, A., Schneider, N., Arzoumanian, D., Bontemps, S., Attard, M., Motte, F., Didelon, P., Maury, A., Abergel, A., Ali, B., Baluteau, J. -P., Bernard, J. -Ph., Cambrésy, L., Cox, P., Di Francesco, J., di Giorgio, A. M., Griffin, M. J., Hargrave, P., Huang, M., Kirk, J., Li, J. Z., Martin, P., Minier, V., Molinari, S., Olofsson, G., Pezzuto, S., Russeil, D., Roussel, H., Saraceno, P., Sauvage, M., Sibthorpe, B., Spinoglio, L., Testi, L., Ward-Thompson, D., White, G., Wilson, C. D., Woodcraft, A., and Zavagno, A.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: The origin and possible universality of the stellar initial mass function (IMF) is a major issue in astrophysics. One of the main objectives of the Herschel Gould Belt Survey is to clarify the link between the prestellar core mass function (CMF) and the IMF. We present and discuss the core mass function derived from Herschel data for the large population of prestellar cores discovered with SPIRE and PACS in the Aquila Rift cloud complex at d ~ 260 pc. We detect a total of 541 starless cores in the entire ~11 deg^2 area of the field imaged at 70-500 micron with SPIRE/PACS. Most of these cores appear to be gravitationally bound, and thus prestellar in nature. Our Herschel results confirm that the shape of the prestellar CMF resembles the stellar IMF, with much higher quality statistics than earlier submillimeter continuum ground-based surveys.
Published: 2010
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13. The Herschel first look at protostars in the Aquila Rift

Author: Bontemps, S., Andre, Ph., Konyves, V., Men'shchikov, A., Schneider, N., Maury, A., Peretto, N., Arzoumanian, D., Attard, M., Motte, F., Minier, V., Didelon, P., Saraceno, P., Abergel, A., Baluteau, J. -P., Bernard, J. -Ph., Cambresy, L., Cox, P., Di Francesco, J., Di Giorgo, A. M., Griffin, M., Hargrave, P., Huang, M., Kirk, J., Li, J., Martin, P., Merin, B., Molinari, S., Olofsson, G., Pezzuto, S., Prusti, T., Roussel, H., Russeil, D., Sauvage, M., Sibthorpe, B., Spinoglio, L., Testi, L., Vavrek, R., Ward-Thompson, D., White, G., Wilson, C., Woodcraft, A., and Zavagno, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: As part of the science demonstration phase of the Herschel mission of the Gould Belt Key Program, the Aquila Rift molecular complex has been observed. The complete ~ 3.3deg x 3.3deg imaging with SPIRE 250/350/500 micron and PACS 70/160 micron allows a deep investigation of embedded protostellar phases, probing of the dust emission from warm inner regions at 70 and 160 micron to the bulk of the cold envelopes between 250 and 500 micron. We used a systematic detection technique operating simultaneously on all Herschel bands to build a sample of protostars. Spectral energy distributions are derived to measure luminosities and envelope masses, and to place the protostars in an M_env - L_bol evolutionary diagram. The spatial distribution of protostars indicates three star-forming sites in Aquila, with W40/Sh2-64 HII region by far the richest. Most of the detected protostars are newly discovered. For a reduced area around the Serpens South cluster, we could compare the Herschel census of protostars with Spitzer results. The Herschel protostars are younger than in Spitzer with 7 Class 0 YSOs newly revealed by Herschel. For the entire Aquila field, we find a total of ~ 45-60 Class 0 YSOs discovered by Herschel. This confirms the global statistics of several hundred Class~0 YSOs that should be found in the whole Gould Belt survey., Comment: 6 pages, 6 figures, publication in A&A
Published: 2010
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14. From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt survey

Author: André, Ph., Men'shchikov, A., Bontemps, S., Könyves, V., Motte, F., Schneider, N., Didelon, P., Minier, V., Saraceno, P., Ward-Thompson, D., Di Francesco, J., White, G., Molinari, S., Testi, L., Abergel, A., Griffin, M., Henning, Th., Royer, P., Merín, B., Vavrek, R., Attard, M., Arzoumanian, D., Wilson, C. D., Ade, P., Aussel, H., Baluteau, J. -P., Benedettini, M., Bernard, J. -Ph., Blommaert, J. A. D. L., Cambrésy, L., Cox, P., Di Giorgio, A., Hargrave, P., Hennemann, M., Huang, M., Kirk, J., Krause, O., Launhardt, R., Leeks, S., Pennec, J. Le, Li, J. Z., Martin, P., Maury, A., Olofsson, G., Omont, A., Peretto, N., Pezzuto, S., Prusti, T., Roussel, H., Russeil, D., Sauvage, M., Sibthorpe, B., Sicilia-Aguilar, A., Spinoglio, L., Waelkens, C., Woodcraft, A., and Zavagno, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We summarize the first results from the Gould Belt survey, obtained toward the Aquila Rift and Polaris Flare regions during the 'science demonstration phase' of Herschel. Our 70-500 micron images taken in parallel mode with the SPIRE and PACS cameras reveal a wealth of filamentary structure, as well as numerous dense cores embedded in the filaments. Between ~ 350 and 500 prestellar cores and ~ 45-60 Class 0 protostars can be identified in the Aquila field, while ~ unbound starless cores and no protostars are observed in the Polaris field. The prestellar core mass function (CMF) derived for the Aquila region bears a strong resemblance to the stellar initial mass function (IMF), already confirming the close connection between the CMF and the IMF with much better statistics than earlier studies. Comparing and contrasting our Herschel results in Aquila and Polaris, we propose an observationally-driven scenario for core formation according to which complex networks of long, thin filaments form first within molecular clouds, and then the densest filaments fragment into a number of prestellar cores via gravitational instability., Comment: 7 pages, 4 figures. Accepted for publication in Astronomy and Astrophysics, Herschel Special Issue
Published: 2010
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15. A Herschel study of the properties of starless cores in the Polaris Flare dark cloud region using PACS and SPIRE

Author: Ward-Thompson, D., Kirk, J. M., André, P., Saraceno, P., Didelon, P., Könyves, V., Schneider, N., Abergel, A., Baluteau, J. -P., Bernard, J. -Ph., Bontemps, S., Cambrésy, L., Cox, P., Di Francesco, J., Di Giorgio, A. M., Griffin, M., Hargrave, P., Huang, M., Li, J. Z., Martin, P., Men'shchikov, A., Minier, V., Molinari, S., Motte, F., Olofsson, G., Pezzuto, S., Russeil, D., Sauvage, M., Sibthorpe, B., Spinoglio, L., Testi, L., White, G., Wilson, C., Woodcraft, A., and Zavagno, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The Polaris Flare cloud region contains a great deal of extended emission. It is at high declination and high Galactic latitude. It was previously seen strongly in IRAS Cirrus emission at 100 microns. We have detected it with both PACS and SPIRE on Herschel. We see filamentary and low-level structure. We identify the five densest cores within this structure. We present the results of a temperature, mass and density analysis of these cores. We compare their observed masses to their virial masses, and see that in all cases the observed masses lie close to the lower end of the range of estimated virial masses. Therefore, we cannot say whether they are gravitationally bound prestellar cores. Nevertheless, these are the best candidates to be potentialprestellar cores in the Polaris cloud region., Comment: 5 pages, 2 figures, accepted by A&A
Published: 2010
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16. Properties of dust and detection of Halpha emission in LDN 1780

Author: del Burgo, C. and Cambresy, L.
Subjects: Astrophysics
Abstract: We present ISOPHOT observations between 60 and 200 microns and a near-infrared extinction map of LDN 1780. We have used the ISOPHOT data together with the 25, 60 and 100 microns IRIS maps to disentangle the warm and cold components of large dust grains that are observed in translucent and dense clouds. The warm and cold components in LDN 1780 have different properties and spatial distributions, with the warm component surrounding the cold component. The cold component is associated with molecular gas at densities of ~1000 cm^-3. The warm component has a uniform colour temperature of 25 K, and the colour temperature of the cold component slightly varies between 15.8 and 17.3 K (beta=2, Delta(T)=0.5 K). The ratio between the 200 microns emission of the cold component and Av is Ic(200)/Av=12.1 MJy/sr/mag and the average ratio tau(200)/Av=2.0x10^-4 mag^-1. The far-infrared emissivity of the warm component is significantly lower than that of the cold component. The Halpha emission and Av correlate very well; a ratio I(Halpha)/Av=2.2 Rayleigh/mag is observed. This correlation indicates the presence of a source of ionisation that can penetrate deeply into the cloud. Using the ratio I(Halpha)/Av we have estimated a ionisation rate for LDN 1780 that results to be ~10^-16 photons/s. We interpret this relatively high value as due to an enhanced cosmic ray flux of ~10 times the standard value. The origin of the cosmic rays could be from supernovae in the Scorpio-Centaurus OB association and/or the runaway zeta Ophiuchus., Comment: 19 pages, 12 figures, accepted for publications in MNRAS
Published: 2006
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17. Luminous AGB stars in nearby galaxies. A study using Virtual Observatory tools

Author: Tsalmantza, P., Kontizas, E., Cambresy, L., Genova, F., Dapergolas, A., and Kontizas, M.
Subjects: Astrophysics
Abstract: Aims. This study focuses on very luminous Mbol<-6.0 mag AGB stars with J-Ks>1.5 mag and H-Ks>0.4 mag in the LMC, SMC, M31, and M33 from 2MASS data. Methods.The data were taken from the 2MASS All-Sky Point Source catalogue archive. We used Virtual Observatory tools and took advantage of its capabilities at various stages in the analysis. Results. It is well known that stars with the colors we selected correspond mainly to carbon stars. Although the most luminous AGBs detected here contain a large number of carbon stars,they are not included in existing catalogues produced from data in the optical domain, where they are not visible since they are dust-enshrouded. A comparison of the AGB stars detected with combined near and mid-infrared data from MSX and 2MASS in the LMC shows that 10% of the bright AGB stars are bright carbon stars never detected before and that the other 50% are OH/IR oxygen rich stars, whereas the 40% that remain were not cross-matched. Conclusions. The catalogues of the most luminous AGB stars compiled here are an important complement to existing data. In the LMC, these bright AGB stars are centrally located, whereas they are concentrated in an active star-formation ring in M31. In the SMC and M33, there are not enough of them to draw definite conclusions, although they tend to be centrally located. Their luminosity functions are similar for the four galaxies we studied., Comment: 16 pages, 12 figures, 4 tables (Appendix A), accepted in A&A
Published: 2005
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18. Surface density of the young cluster IC 348 in the Perseus molecular cloud

Author: Cambresy, L., Petropoulou, V., Kontizas, M., and Kontizas, E.
Subjects: Astrophysics
Abstract: The IC 348 young star cluster contains more than 300 confirmed members. It is embedded in the Perseus molecular cloud, making any clustering analysis subject to an extinction bias. In this work, we derive the extinction map of the cloud and revisit the content of IC 348 through a statistical approach that uses the 2MASS data. Our goal was to address the question of the completeness of IC 348 and of young clusters in general. We performed a combined analysis of the star color and density in this region, in order to establish the surface density map of the cluster. We reached the conclusion that IC 348 has structures up to 25' from the cluster center, and we estimate that about 40 members brighter than Ks=13 mag are still unidentified. Although we cannot use our statistical method to identify these new members individually, the surface density map gives a strong indication of their actual location. They are distributed in the outer regions of the cluster, where very few dedicated observations have been made so far, which is probably why they escaped previous identification. In addition, we propose the existence of a new embedded cluster associated to the infrared source MSX6C G160.2784-18.4216, about 38' south of IC 348., Comment: 5 pages, 5 figures, accepted for publication in A&A
Published: 2005
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19. Large-scale variations of the dust optical properties in the Galaxy

Author: Cambresy, L., Jarrett, T. H., and Beichman, C. A.
Subjects: Astrophysics
Abstract: We present an analysis of the dust optical properties at large scale, for the whole galactic anticenter hemisphere. We used the 2MASS Extended Source Catalog to obtain the total reddening on each galaxy line of sight and we compared this value to the IRAS 100 microns surface brightness converted to extinction by Schlegel et al (1998). We performed a careful examination and correction of the possible systematic effects resulting from foreground star contamination, redshift contribution and galaxy selection bias. We also evaluated the contribution of dust temperature variations and interstellar clumpiness to our method. The correlation of the near-infrared extinction to the far-infrared optical depth shows a discrepancy for visual extinction greater than 1 mag with a ratio A_V(FIR) / A_V(gal) = 1.31 +- 0.06. We attribute this result to the presence of fluffy/composite grains characterized by an enhanced far--infrared emissivity. Our analysis, applied to half of the sky, provides new insights on the dust grains nature suggesting fluffy grains are found not only in some very specific regions but in all directions for which the visual extinction reaches about 1 mag., Comment: 10 pages, 11 figures, accepted for publication in A&A
Published: 2005
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20. Multi-wavelength analysis of the dust emission in the Small Magellanic Cloud

Author: Bot, C., Boulanger, F., Lagache, G., Cambresy, L., and Egret, D.
Subjects: Astrophysics
Abstract: We present an analysis of dust grain emission in the diffuse interstellar medium of the Small Magellanic Cloud (SMC). This study is motivated by the availability of 170 microns ISOPHOT data covering a large part of the SMC, with a resolution enabling to disentangle the diffuse medium from the star forming regions. After data reduction and subtraction of Galactic foreground emission, we used the ISOPHOT data together with HiRes IRAS data and ATCA/Parkes combined HI column density maps to determine dust properties for the diffuse medium. We found a far infrared emissivity per hydrogen atom 30 times lower than the Solar Neighborhood value. The modeling of the spectral energy distribution of the dust, taking into account the enhanced interstellar radiation field, gives a similar conclusion for the smallest grains (PAHs and very small grains) emitting at shorter wavelength. Assuming Galactic dust composition in the SMC, this result implies a difference in the gas-to-dust ratio (GDR) 3 times larger than the difference in metallicity. This low depletion of heavy elements in dust could be specific of the diffuse ISM and not apply for the whole SMC dust if it results from efficient destruction of dust by supernovae explosions., Comment: 11 pages, 10 figures. Accepted for publication in Astronomy & Astrophysics
Published: 2004
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21. Extinction with 2MASS: star counts and reddening toward the North America and the Pelican Nebulae

Author: Cambresy, L., Beichman, C. A., Jarrett, T. H., and Cutri, R. M.
Subjects: Astrophysics
Abstract: We propose a general method for mapping the extinction in dense molecular clouds using 2MASS near-infrared data. The technique is based on the simultaneous utilization of star counts and colors. These two techniques provide independent estimations of the extinction and each method reacts differently to foreground star contamination and to star clustering. We take advantage of both methods to build a large scale extinction map (2.5 x 2.5 degrees) of the North America-Pelican nebulae complex. With Ks star counts and H-Ks color analysis the visual extinction is mapped up to 35 mag. Regions with visual extinction greater than 20 mag account for less than 3% of the total mass of the cloud. Color is generally a better estimator for the extinction than star counts. Nine star clusters are identified in the area, seven of which were previously unknown., Comment: 33 pages, 14 figures, accepted in AJ
Published: 2002
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22. Sub-structure of the outer Galactic Halo from the 2 Micron All Sky Survey

Author: Ibata, R. A., Lewis, G. F., Irwin, M. J., and Cambresy, L.
Subjects: Astrophysics
Abstract: A pole-count analysis of the infrared 2MASS survey is presented, in order to identify faint stream-like structures within the halo of the Milky Way. Selecting stars with colours consistent with M-giant stars, we find a strong over-density of sources on a stream with pole (l=95,b=13), which corresponds to the pole of the orbit of the Sagittarius dwarf galaxy. This great-circle feature of width ~12 degrees, contains 5% of the late M-giants in the Halo. No other stream-like structures are detected in M-giants in the 2MASS Second Incremental Data Release (2IDR), and in particular, we find no evidence for a stellar component to the Magellanic Stream. This suggests that the present accretion rate of low-mass satellites with a luminous component is very low, and the formation of the luminous component of the Halo must have been essentially complete before the accretion of the Sagittarius dwarf galaxy, more than 3Gyr ago. We also search for great-circle streams using almost all high-latitude (|b|>30) sources in the 2IDR dataset. No narrow great-circle streams of width 0.5-2 degrees were found, though we were only sensitive to relatively nearby (<17kpc) remnants of massive (10^6 Msun) globular clusters. If the Galactic potential is close to being spherical, as some recent observations suggest, the lack of observed great-circle streams is consistent with the presence of dark matter substructures in the Halo. Although alternative explanations cannot be ruled out from our analysis of the 2IDR dataset, future experiments with better statistics have the potential to reveal the heating effect of dark matter substructure on stellar streams., Comment: 8 pages, 4 figures, submitted to MNRAS
Published: 2001
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23. Far-infrared dust opacity and visible extinction in the Polaris Flare

Author: Cambresy, L., Boulanger, F., Lagache, G., and Stepnik, B.
Subjects: Astrophysics
Abstract: We present an extinction map of the Polaris molecular cirrus cloud derived from star counts and compare it with the Schlegel et al. (1998) extinction map derived from the far--infrared dust opacity. We find that, within the Polaris cloud, the Schlegel et al. Av values are a factor 2 to 3 higher than the star count values. We propose that this discrepancy results from a difference in $\tau_{FIR}/ A_V$ between the diffuse atomic medium and the Polaris cloud. We use the difference in spectral energy distribution, warm for the diffuse atomic medium, cold for the Polaris cloud, to separate their respective contribution to the line of sight integrated infrared emission and find that the $\tau_{FIR}/ A_V$ of cold dust in Polaris is on average 4 times higher than the Schlegel et al. value for dust in atomic cirrus. This change in dust property could be interpreted by a growth of fluffy particles within low opacity molecular cirrus clouds such as Polaris. Our work suggests that variations in dust emissivity must be taken into account to estimate Av from dust emission wherever cold infrared emission is present (i.e. molecular clouds)., Comment: 9 pages, 7 figures, accepted in A&A
Published: 2001
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24. The Cosmic Infrared Background at 1.25 microns and 2.2 microns using DIRBE and 2MASS: a contribution not due to galaxies ?

Author: Cambresy, L., Reach, W. T., Beichman, C. A., and Jarrett, T. H.
Subjects: Astrophysics
Abstract: Using the 2MASS 2nd Incremental Data Release and the Zodiacal-Subtracted Mission Average maps of COBE/DIRBE, we estimate the cosmic background in the J (1.25 micron) and K (2.2 microns) bands using selected areas representing 550 square degrees of sky. We find a J background of 22.9 \pm 7.0 kJy/sr (54.0 \pm 16.8 nW/m2/sr) and a K background of 20.4 \pm 4.9 kJy/sr (27.8 \pm 6.7 nW/m2/sr). This large scale study shows that the main uncertainty comes from the residual zodiacal emission. The cosmic background we obtain is significantly higher than integrated galaxy counts (3.6 \pm 0.8 kJy/sr and 5.3 \pm 1.2 kJy/sr for J and K, respectively), suggesting either an increase of the galaxy luminosity function for magnitudes fainter than 30 or the existence of another contribution to the cosmic background from primeval stars, black holes, or relic particle decay., Comment: 20 pages, 6 figures, accepted in ApJ
Published: 2001
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25. Mapping of the extinction in Giant Molecular Clouds using optical star counts

Author: Cambresy, L.
Subjects: Astrophysics
Abstract: This paper presents large scale extinction maps of most nearby Giant Molecular Clouds of the Galaxy (Lupus, rho-Ophiuchus, Scorpius, Coalsack, Taurus, Chamaeleon, Musca, Corona Australis, Serpens, IC 5146, Vela, Orion, Monoceros R1 and R2, Rosette, Carina) derived from a star count method using an adaptive grid and a wavelet decomposition applied to the optical data provided by the USNO-Precision Measuring Machine. The distribution of the extinction in the clouds leads to estimate their total individual masses M and their maximum of extinction. I show that the relation between the mass contained within an iso-extinction contour and the extinction is similar from cloud to cloud and allows the extrapolation of the maximum of extinction in the range 5.7 to 25.5 magnitudes. I found that about half of the mass is contained in regions where the visual extinction is smaller than 1 magnitude. The star count method used on large scale (about 250 square degrees) is a powerful and relatively straightforward method to estimate the mass of molecular complexes. A systematic study of the all sky would lead to discover new clouds as I did in the Lupus complex for which I found a sixth cloud of about 10^4 solar masses., Comment: 8 pages, 1 Postscript figure, 12 Gif figures, accepted in A&A
Published: 1999

26. Search for new YSOs in Large Molecular Clouds and extinction mapping using DENIS and optical data

Author: Cambresy, L.
Subjects: Astrophysics
Abstract: I present new results on the extinction and on the YSO content of the Chamaeleon I cloud using the star count method that I have implemented and applied to DENIS and optical data. Application of this method to other nearby Large Molecular Clouds is in progress and is briefly outlined., Comment: 4 pages, 3 figures, To Appear in the proceedings of the conference "Astrophysics With Infrared Surveys: A Prelude to SIRTF"
Published: 1998

27. New Young Stellar Object candidates in the Chamaeleon I molecular cloud discovered by DENIS

Author: Cambresy, L., Copet, E., Epchtein, N., de Batz, B., Borsenberger, J., Fouque, P., Kimeswenger, S., and Tiphene, D.
Subjects: Astrophysics
Abstract: This paper presents an analysis of the nature of point sources discovered by DENIS in an area of 1.5 x 3 degrees around the Chamaeleon I molecular cloud. Most of the 30000 objects detected in the J band are background stars that were previously used to derive an accurate extinction map of the full area (Cambresy et al., 1997) using star count method. In the present work, we investigate the young stellar population of the cloud using the IJK photometric DENIS data. The whole sample of 126 already known YSOs, which are mainly T Tauri stars, are identified in the DENIS catalogue. Besides, we propose 54 sources as new candidates of YSOs. These new faint objects are selected according to their extremely red near infrared colour, that cannot be explained only by the reddening of the cloud. Moreover they are concentrated near to the most obscured areas of the cloud. Although spectroscopic confirmation is badly requested, they are interpreted as probable classical T Tauri stars that have escaped previous spectroscopic, IRAS or X-ray observations and pertaining to the low-end of the luminosity function. Assuming that they are reliable YSOs with massive accretion disks, and using theoretical pre-main-sequence tracks we estimate the age of this sample to be ranging from 5 10^5 to 4 10^6 years, an elapse of time that spans the range between the end of the star formation in the cloud and the maximum life time of the circumstellar disk., Comment: 12 pages, 8 figures, accepted in A&A
Published: 1998

28. Extinction map of the Chamaeleon I molecular cloud with DENIS star counts

Author: Cambresy, L., Epchtein, N., Copet, E., de Batz, B., Kimeswenger, S., Bertre, T. Le, Rouan, D., and Typhene, D.
Subjects: Astrophysics
Abstract: Massive, large scale star counts in the J band provided by the Deep Near Infrared Survey of the Southern Sky (DENIS) are used for the first time to draw out an extinction map of the Chamaeleon I dark cloud. We derived a 2 arcminutes resolution map of the cloud from J star counts within an area of 1.5 x 3 degres around the centre of the cloud using an adaptive grid method and applying a wavelet decomposition. A comparison of our extinction map with the cold contribution of the IRAS 100 microns emission shows an almost perfect matching. It is shown that J star counts supersede optical counts on Schmidt plate where Av > 4., Comment: 4 pages, accepted for publication in Astronomy & Astrophysics Letters
Published: 1997

29. L183 (134N) Dust, Gas and Depletion

Author: Pagani, L., Apponi, A. J., Bacmann, A., Cambrésy, L., Fich, M., Lagache, G., Miville-Deschênes, M. -A., Motte, F., Pardo, J. -R., Pfalzner, Susanne, editor, Kramer, Carsten, editor, Straubmeier, Christian, editor, and Heithausen, Andreas, editor
Published: 2004
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30. A Study of Extinction and Star Formation in the Chamaeleon I Cloud with DENIS

Author: Cambresy, L. and Epchtein, N., editor
Published: 1998
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31. VizieR Online Data Catalog: Distance of HiGAL sources (Mege+, 2021)

Author: Mège, P., Russeil, D., Zavagno, Annie, Elia, D., Molinari, S., Brunt, C.~m., Butora, R., Cambresy, L., Di, Giorgio A.~m., Fenouillet, T., Fukui, Y., Lambert, J.~c., Makai, Z., Merello, M., Meunier, J.~c., Molinaro, M., Moreau, C., Pezzuto, S., Poulin, Y., Schisano, E., Schuller, F., Laboratoire d'Astrophysique de Marseille (LAM), 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), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Astrophysics [Nagoya], Nagoya University, West Virginia University [Morgantown], Departamento de Astronomia (DAS), INAF - Osservatorio Astronomico di Trieste (OAT), Environnement, Ville, Société (EVS), École normale supérieure de Lyon (ENS de Lyon)-École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Université Lumière - Lyon 2 (UL2)-Université Jean Moulin - Lyon 3 (UJML), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-École Nationale des Travaux Publics de l'État (ENTPE)-École nationale supérieure d'architecture de Lyon (ENSAL)-Centre National de la Recherche Scientifique (CNRS), and Max-Planck-Institut für Radioastronomie (MPIFR)
Subjects: Milky Way, Radial velocities, [SDU]Sciences of the Universe [physics], Molecular clouds, Stars: distances
Abstract: Velocity and Distance of HiGAL sources. \\\\(2 data files).
Published: 2020

32. Distance of Hi-GAL sources

Author: Mège, P., primary, Russeil, D., additional, Zavagno, A., additional, Elia, D., additional, Molinari, S., additional, Brunt, C. M., additional, Butora, R., additional, Cambresy, L., additional, Di Giorgio, A. M., additional, Fenouillet, T., additional, Fukui, Y., additional, Lambert, J. C., additional, Makai, Z., additional, Merello, M., additional, Meunier, J. C., additional, Molinaro, M., additional, Moreau, C., additional, Pezzuto, S., additional, Poulin, Y., additional, Schisano, E., additional, and Schuller, F., additional
Published: 2021
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33. What Is SIMBAD, and What Is It Not?

Author: Loup, C., Oberto, A., Allen, M., Lesteven, S., Boch, T., Bot, C., Bonnarel, F., Brouty, M., Brunet, C., Buga, M., Cambresy, L., Delacour, T., Derriere, S., Eisele, A., Fernique, P., Genova, F., Guehenneux, S., Landais, G., Louys, M., Nebot, A., Neuville, M., Ocvirk, P., Perret, E., Pineau, F.-X., Schaaff, A., Siebert, A., Son, E., Vannier, P., Vollmer, B., Vonflie, P., Woelfel, F., and Genova, Françoise
Subjects: [SDU] Sciences of the Universe [physics], [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract: The purpose of the SIMBAD database is to provide the bibliography and some fundamental data on astronomical objects of interest which have been studied in scientific articles. It includes objects of any nature, stars - galaxies - interstellar medium - transient events - etc. SIMBAD is a meta-compilation built from what is published in the literature, and from our expertise on cross-identifications. It is a dynamic database, updated every working day. By construction its content is heterogeneous as data come from any kind of instruments at all wavelengths with any resolution and astrometry, and different names from one publication to another. Thus SIMBAD is not a catalogue, and should not be used as a catalogue. It is not the purpose of SIMBAD to contain “everything”. Especially, lists of uncharacterised sources detected in photometric surveys of any size are usually not processed in SIMBAD. But they are available at CDS in the VizieR database which contains published tables of objects, as well as most very large surveys. The idea now is to use both SIMBAD and VizieR as complementary research tools.
Published: 2019

34. A Study of Extinction and Star Formation in the Chamaeleon I Cloud with DENIS

Author: Cambresy, L., primary
Published: 1998
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35. The cosmic infrared backgroung at 1.25 and 2.2 and microns using DIRBE and 2mass: a contribution not due to galaxies?

Author: Cambresy, L, Reach, W, Beichman, C, and Jarrett, T
Published: 2001

36. Far-Infrared dust opacity and visible extinction

Author: Cambresy, L, Boulander, F, Lagache, G, and Stepnik, B
Published: 2001

37. Far-infrared dust opacity and visible extinction in the Polaris Flare

Author: Cambresy, L
Abstract: UNKNOWN
Published: 2001

38. Extinction with 2MASS: star counts and reddening toward the North America and the Pelican Nebulae

Author: Cutri, R. M, Jarrett, T. H, Beichman, C. A, and Cambresy, L
Abstract: UNKNOWN
Published: 2001

39. Extinction with 2MASS: star counts and reddening toward the North America and the Pelican Nebulae

Author: Cambresy, L, Beichman, C. A, Jarrett, T. H, and Cutri, R. M
Published: 2001

40. French SKA White Book - The French Community towards the Square Kilometre Array

Author: Acero, F., T Acquaviva, J., Adam, R., Aghanim, N., Allen, Mark G., Alves, M., Ammanouil, R., Ansari, R., Araudo, A., Armengaud, E., Ascaso, B., Athanassaoula, E., Aubert, D., Babak, S., Bacmann, A., Banday, A., Barriere, K., Bellossi, F., P Bernard, J., Bernardini, M. G., Bethermin, M., Blanc, E., Blanchet, L., Bobin, J., Samuel Boissier, Boisson, C., Boselli, A., Bosma, A., Bosse, S., Bottinelli, S., Boulanger, F., Remy Boyer, Bracco, A., Briand, C., Bucher, M., Buat, V., Cambresy, L., Caillat, M., M Casandjian, J., Caux, E., Celestin, S., Cerruti, M., Charlot, P., Chassande-Mottin, E., Chaty, S., Christensen, N., Ciesla, L., Clerc, N., Cohen-Tanugi, J., Ismaël Cognard, Combes, F., Comis, B., Corbel, S., Cordier, B., Coriat, M., Courtin, R., Courtois, H., Da Silva, B., Emanuele Daddi, Richard Dallier, Dartois, E., Demyk, K., M Denis, J., Denis, L., Djannati-Atai, A., F Donati, J., Douspis, M., Driel, W., El Korso, M. N., Falgarone, E., Fantina, A. F., Farges, T., Anthony Ferrari, Ferrari, C., Ferrière, K., Flamary, R., Gac, N., Gauffre, S., Genova, F., Girard, J., Grenier, I., Jean-Mathias Grießmeier, Guillard, P., Lucas Guillemot, Gulminelli, F., Gusdorf, A., Habart, E., Hammer, F., Hennebelle, P., Fabrice Herpin, Hervet, O., Hughes, A., Ilbert, O., Janvier, M., Eric Josselin, Julier, A., Lachaud, C., Guilaine Lagache, Lallement, R., Lambert, S., Lamy, L., Pascal Larzabal, Lavaux, G., Le Bertre, T., Le Fèvre, O., Le Tiec, A., Lefloch, B., Lehnert, M., Lemoine-Goumard, M., Levrier, F., Limousin, M., Lis, D., López-Sepulcre, A., Macías-Pérez, J., Magneville, C., Marcowith, A., Jérôme Margueron, Marquette, G., Marshall, D., Martin, L., Mary, D., Masson, S., Maurogordato, S., Mazauric, C., Mellier, Y., A Miville-Deschênes, M., Montier, L., Mottez, F., Mourard, D., Nesvadba, N., F Nezan, J., Noterdaeme, P., Novak, J., Ocvirk, P., Oertel, M., Xavier Olive, Ollier, V., Palanque-Delabrouille, N., Pandey-Pommier, M., Pennec, Y., Perault, M., Peroux, C., Petit, P., Petri, J., Petiteau, A., Pety, J., Pratt, G. W., Puech, M., Benjamin Quertier, Erwan Raffin, Rakotozafy Harison, S., Rawson, S., Renaud, M., Benoît Revenu, Richard, C., Richard, J., Rincon, F., Ristorcelli, I., Rodriguez, J., Schultheis, M., Schimd, C., Semelin, B., Sol, H., L Starck, J., Michel Tagger, Tasse, C., Gilles Theureau, Torchinsky, S., Vastel, C., Vergani, S. D., Verstraete, L., Vigouroux, X., Vilmer, N., P Vilotte, J., Webb, N., Ysard, N., Philippe Zarka, Mathieu Langer, 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 Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), The MITRE corporation, Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire sur les Interactions Véhicules-Infrastructure-Conducteurs (LIVIC), Laboratoire Central des Ponts et Chaussées (LCPC)-Institut National de Recherche sur les Transports et leur Sécurité (INRETS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Agence Universitaire de la Francophonie (AUF), Laboratoire des Bio-Indicateurs Actuels et Fossiles (BIAF), Université d'Angers (UA), Département d'Electronique, des Détecteurs et d'Informatique (ex SEDI) (DEDI), 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, Observatories [Carnegie Institution], Carnegie Institution for Science [Washington], Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), 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 de Recherche en Informatique, Signal et Automatique de Lille (CRIStAL) - UMR 9189 (CRIStAL), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Ecole Centrale de Lille, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Laboratoire d'Énergétique Moléculaire et Macroscopique, Combustion (EM2C), CentraleSupélec-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), M2A 2018, 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), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), RTM - Alpes de Haute Provence - Digne les Bains, ONF - RTM - Alpes de Haute Provence - Digne les Bains, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire Hubert Curien [Saint Etienne] (LHC), Institut d'Optique Graduate School (IOGS)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Détection et de Géophysique (CEA) (LDG), 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)-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), FORMATION STELLAIRE 2018, Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), service hématologie Nantes, Centre hospitalier universitaire de Nantes (CHU Nantes), Groupe de Recherche en Astronomie et Astrophysique du Languedoc (GRAAL), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Erosion torrentielle neige et avalanches (UR ETGR (ETNA)), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), AgroSup Dijon - Institut National Supérieur des Sciences Agronomiques, de l'Alimentation et de l'Environnement, Systèmes et Applications des Technologies de l'Information et de l'Energie (SATIE), École normale supérieure - Rennes (ENS Rennes)-Université Paris-Sud - Paris 11 (UP11)-Conservatoire National des Arts et Métiers [CNAM] (CNAM)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Cachan (ENS Cachan)-Université Gustave Eiffel (UNIV GUSTAVE EIFFEL), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Department of Plant Biology, The Royal Veterinary and Agricultural University, University of Sofia, Thales Alenia Space - TAS (Toulouse, France), Thales (France), Département de Physique des Particules (ex SPP) (DPP), Centre de Recherche Astrophysique de Lyon (CRAL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institut d’Électronique, de Microélectronique et de Nanotechnologie (IEMN) - UMR 8520 (IEMN), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Université Polytechnique Hauts-de-France (UPHF)-Ecole Centrale de Lille-Université Polytechnique Hauts-de-France (UPHF)-Institut supérieur de l'électronique et du numérique (ISEN), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Alcatel Vacuum Technology, ALCATEL, SUBATECH - Radiochimie, Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France, Centre Etud Spatiale Rayonnements Toulouse, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), 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)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Bio-Indicateurs Actuels et Fossiles (BIAF), Département d'Electronique, des Détecteurs et d'Informatique pour la Physique (ex SEDI) (DEDIP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre de Recherche en Informatique, Signal et Automatique de Lille - UMR 9189 (CRIStAL), Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Paris Saclay (COmUE)-Centre National de la Recherche Scientifique (CNRS)-CentraleSupélec, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), 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), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Cachan (ENS Cachan)-Université Paris-Sud - Paris 11 (UP11)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-École normale supérieure - Rennes (ENS Rennes)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Conservatoire National des Arts et Métiers [CNAM] (CNAM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Royal Veterinary and Agricultural University = Kongelige Veterinær- og Landbohøjskole (KVL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Carnegie Institution for Science, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-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), Collège de France - Chaire Galaxies et cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), Laboratoire Hubert Curien (LHC), Institut d'Optique Graduate School (IOGS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Thales Alenia Space [Toulouse] (TAS), THALES [France], Département de Physique des Particules (ex SPP) (DPhP), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), C. Ferrari, G. Lagache, S. Gauffre, G. Marquette, J.-M. Martin, B. Semelin, M. Alves, K. Ferrière, M.-A. Miville-Deschenes, L. Montier, E. Josselin, N. Vilmer, P. Zarka, S. Corbel, S. Vergani, S. Lambert, G. Theureau, S. Bosse, A. Ferrari, and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: Editor in chief: C. Ferrari; Editors: M. Alves, S. Bosse, S. Corbel, A. Ferrari, K. Ferri\`ere, S. Gauffre, E. Josselin, G. Lagache, S. Lambert, G. Marquette, J.-M. Martin, M.-A. Miville-Desch\^enes, L. Montier, B. Semelin, G. Theureau, S. Vergani, N. Vilmer, P. Zarka; Original file with high resolution figures at SKA-France link: https://ska-france.oca.eu/images/SKA-France-Media/FWB_051017.pdf; International audience; The "Square Kilometre Array" (SKA) is a large international radio telescope project characterised, as suggested by its name, by a total collecting area of approximately one square kilometre, and consisting of several interferometric arrays to observe at metric and centimetric wavelengths. The deployment of the SKA will take place in two sites, in South Africa and Australia, and in two successive phases. From its Phase 1, the SKA will be one of the most formidable scientific machines ever deployed by mankind, and by far the most impressive in terms of data throughput and required computing power. With the participation of almost 200 authors from forty research institutes and six private companies, the publication of this French SKA white paper illustrates the strong involvement in the SKA project of the French astronomical community and of a rapidly growing number of major scientific and technological players in the fields of Big Data, high performance computing, energy production and storage, as well as system integration.
Published: 2018

41. French SKA White Book - The French Community towards the Square Kilometre Array

Author: Fabio Acero, Acquaviva, J. -T, Adam, R., Aghanim, N., Allen, M., Alves, M., Ammanouil, R., Ansari, R., Araudo, A., Armengaud, E., Ascaso, B., Athanassaoula, E., Aubert, D., Babak, S., Bacmann, A., Banday, A., Barriere, K., Bellossi, F., Bernard, J. -P, Bernardini, M. G., Béthermin, M., Blanc, E., Blanchet, L., Bobin, J., Boissier, S., Boisson, C., Boselli, A., Bosma, A., Bosse, S., Bottinelli, S., Boulanger, F., Boyer, R., Bracco, A., Briand, C., Bucher, M., Buat, V., Cambresy, L., Caillat, M., Casandjian, J. -M, Caux, E., Célestin, S., Cerruti, M., Charlot, P., Chassande-Mottin, E., Chaty, S., Christensen, N., Ciesla, L., Clerc, N., Cohen-Tanugi, J., Cognard, I., Combes, F., Comis, B., Corbel, S., Cordier, B., Coriat, M., Courtin, R., Courtois, H., Da Silva, B., Daddi, E., Dallier, R., Dartois, E., Demyk, K., Denis, J. -M, Denis, L., Djannati-Ataï, A., Donati, J. -F, Douspis, M., Driel, W., El Korso, M. N., Falgarone, E., Fantina, A., Farges, T., Ferrari, A., Ferrari, C., Ferrière, K., Flamary, R., Gac, N., Gauffre, S., Genova, F., Girard, J., Grenier, I., Griessmeier, J. -M, Guillard, P., Guillemot, L., Gulminelli, F., Gusdorf, A., Habart, E., Hammer, F., Hennebelle, P., Herpin, F., Hervet, O., Hughes, A., Ilbert, O., Janvier, M., Josselin, E., Julier, A., Lachaud, C., Lagache, G., Lallement, R., Lambert, S., Lamy, L., Langer, M., Larzabal, P., Lavaux, G., Le Bertre, T., Le Fèvre, O., Le Tiec, A., Lefloch, B., Lehnert, M., Lemoine-Goumard, M., Levrier, F., Limousin, M., Lis, D., López-Sepulcre, A., Macias-Perez, J., Magneville, C., Marcowith, A., Margueron, J., Marquette, G., Marshall, D., Martin, L., Mary, D., Masson, S., Maurogordato, S., Mazauric, C., Mellier, Y., Miville-Deschênes, M. -A, Montier, L., Mottez, F., Mourard, D., Nesvadba, N., Nezan, J. -F, Noterdaeme, P., Novak, J., Ocvirk, P., Oertel, M., Olive, X., Ollier, V., Palanque-Delabrouille, N., Pandey-Pommier, M., Pennec, Y., Pérault, M., Peroux, C., Petit, P., Pétri, J., Petiteau, A., Pety, J., Pratt, G. W., Puech, M., Quertier, B., Raffin, E., Rakotozafy Harison, S., Rawson, S., Renaud, M., Revenu, B., Richard, C., Richard, J., Rincon, F., Ristorcelli, I., Rodriguez, J., Schultheis, M., Schimd, C., Semelin, B., Sol, H., Starck, J. -L, Tagger, M., Tasse, C., Theureau, G., Torchinsky, S., Vastel, C., Vergani, S. D., Verstraete, L., Vigouroux, X., Vilmer, N., Vilotte, J. -P, Webb, N., Ysard, N., and Zarka, P.
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The "Square Kilometre Array" (SKA) is a large international radio telescope project characterised, as suggested by its name, by a total collecting area of approximately one square kilometre, and consisting of several interferometric arrays to observe at metric and centimetric wavelengths. The deployment of the SKA will take place in two sites, in South Africa and Australia, and in two successive phases. From its Phase 1, the SKA will be one of the most formidable scientific machines ever deployed by mankind, and by far the most impressive in terms of data throughput and required computing power. With the participation of almost 200 authors from forty research institutes and six private companies, the publication of this French SKA white paper illustrates the strong involvement in the SKA project of the French astronomical community and of a rapidly growing number of major scientific and technological players in the fields of Big Data, high performance computing, energy production and storage, as well as system integration., Editor in chief: C. Ferrari; Editors: M. Alves, S. Bosse, S. Corbel, A. Ferrari, K. Ferri\`ere, S. Gauffre, E. Josselin, G. Lagache, S. Lambert, G. Marquette, J.-M. Martin, M.-A. Miville-Desch\^enes, L. Montier, B. Semelin, G. Theureau, S. Vergani, N. Vilmer, P. Zarka; Original file with high resolution figures at SKA-France link: https://ska-france.oca.eu/images/SKA-France-Media/FWB_051017.pdf
Published: 2017

42. The Hi-GAL compact source catalogue.\ud I. The physical properties of the clumps in the inner\ud Galaxy (−71.0 ◦ < ' < 67.0◦)

Author: Elia, D., Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, S., Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, Sarah, Jaffa, Sarah, Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmerim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltran, M. T., Billot, N., Cambresy, L., Cesaroni, R., Garcia-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mege, P., Peretto, Nicolas, Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., and Whitworth, Anthony Peter
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, QB
Abstract: Hi-GAL (Herschel InfraRed Galactic Plane Survey) is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 μm. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogues presented in Molinari et al., covering the portion of Galactic plane −71∘.0 < ℓ < 67∘.0. The band-merged catalogue contains 100 922 sources with a regular SED, 24 584 of which show a 70-μm counterpart and are thus considered protostellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterize different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in protostellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to protostellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between ‘on-arm’ and ‘interarm’ positions.
Published: 2017

43. The spatial distribution of star formation related to ionized regions throughout the Inner Galactic Plane

Author: Palmeirim, P, Zavagno, A, Elia, D, Moore, TJT, Whitworth, A, Tremblin, P, Traficante, A, Merello, M, Russeil, D, Pezzuto, S, Cambresy, L, Baldeschi, A, Bandiermonte, M, Becciani, U, Benedettini, M, Buemi, C, Bufano, F, Bulpitt, A, Butora, R, Carey, D, Costa, A, Deharveng, L, Di Girogio, A, Eden, D, Hajnal, A, Hoare, M, Kacsuk, P, Leto, P, Marsh, K, Mege, P, Molinari, M, Molinaro, M, Noriega-Crespo, A, Schisano, E, Sciacca, E, Trigilio, C, Umana, G, and Vitello, F
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present a comprehensive statistical analysis of star-forming objects located in the vicinities of 1 360 bubble structures throughout the Galactic Plane and their local environments. The compilation of ∼70 000 star-forming sources, found in the proximity of the ionized (Hii) regions, detected in both Hi-GAL and GLIMPSE surveys, provided a broad overview of the different evolutionary stages of star-formation in bubbles, from prestellar objects to more evolved Young Stellar Objects (YSOs). Surface density maps of star-forming objects clearly reveal an evolutionary trend where more evolved star-forming objects (Class II YSO candidates) are found spatially located near the center, while younger star-forming objects are found at the edge of the bubbles. We derived dynamic ages for a sub-sample of 182 H ii regions for which kinematic distances and radio continuum flux measurements were available. We detect approximately 80% more star-forming sources per unit area in the direction of bubbles compared with the surrounding fields. We estimate the Clump Formation Efficiency (CFE) of Hi-GAL clumps in the direction of the shell of the bubbles to be ∼ 10%, around twice the value of the CFE in fields not affected by feedback effects. We find that the higher values of CFE is mostly due to the higher CFE of protostellar clumps, in particular in younger bubbles for which the density of the bubble shells is higher. We argue that the formation rate from prestellar to protostellar phase is probably higher during the early stages of the (H ii ) bubble expansion. Furthermore, we also find a higher fraction of massive YSOs (MYSOs) in bubbles at the early stages of expansion (< 2 Myr) than older bubbles. Evaluation of the fragmentation time inside the shell of bubbles advocate for the pre-existence of clumps in the medium prior to the bubble expansion in order to explain the formation of MYSOs in the youngest H ii regions (< 1 Myr), as supported by numerical simulations. Approximately 23% of Hi-GAL clumps are found located in the direction of a bubble, with 15% for prestellar clumps and 41% for protostellar clumps. We argue that the high fraction of protostellar clumps may be due to the acceleration of the star-formation process cause by the feedback of the (H ii ) bubbles.
Published: 2017

44. The Hi-GAL compact source catalogue - I. The physical properties of the clumps in the inner Galaxy (-71.degrees 0 < l < 67.degrees 0)

Author: Elia, D, Molinari, S, Schisano, E, Pestalozzi, M, Pezzuto, S, Merello, M, Noriega-Crespo, A, Moore, Tjt, Russeil, D, Mottram, Jc, Paladini, R, Strafella, F, Benedettini, M, Bernard, Jp, Di Giorgio, A, Eden, Dj, Fukui, Y, Plume, R, Bally, J, Martin, Pg, Ragan, Se, Jaffa, Se, Motte, F, Olmi, L, Schneider, N, Testi, L, Wyrowski, F, Zavagno, A, Calzoletti, L, Faustini, F, Natoli, P, Palmeirim, P, Piacentini, F, Piazzo, L, Pilbratt, Gl, Polychroni, D, Baldeschi, A, Beltran, Mt, Billot, N, Cambresy, L, Cesaroni, R, Garcia-Lario, P, Hoare, Mg, Huang, M, Joncas, G, Liu, Sj, Maiolo, Bmt, Marsh, Ka, Maruccia, Y, Mege, P, Peretto, N, Rygl, Klj, Schilke, P, Thompson, Ma, Traficante, A, Umana, G, Veneziani, M, Ward-Thompson, D, Whitworth, Ap, Arab, H, Bandieramonte, M, Becciani, U, Brescia, M, Buemi, C, Bufano, F, Butora, R, Cavuoti, S, Costa, A, Fiorellino, E, Hajnal, A, Hayakawa, T, Kacsuk, P, Leto, P, Causi, Gl, Marchili, N, Martinavarro-Armengol, S, Mercurio, A, Molinaro, M, Riccio, G, Sano, H, Sciacca, E, Tachihara, K, Torii, K, Trigilio, C, Vitello, F, and Yamamoto, H
Subjects: Infrared: ISM, extinction, Space and Planetary Science, Dust, Astronomy and Astrophysics, Catalogues, Dust, extinction, ISM: clouds, Local interstellar matter, Submillimetre: ISM, NO
Published: 2017

45. Luminous AGB stars in nearby galaxies

Author: Tsalmantza, P, Kontizas, E, Cambresy, L, Genova, F, Dapergolas, A, Kontizas, M, Tsalmantza, P., Kontizas, E., Cambresy, L., Genova, F., Dapergolas, A., Kontizas, M., and Cambrésy, L.
Subjects: Physics, Point source, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Virtual observatory, Carbon star, Galaxy, Luminosity, Stars, Space and Planetary Science, bepress|Physical Sciences and Mathematics|Astrophysics and Astronomy, Oxygen rich
Abstract: Aims. This study focuses on very luminous Mbol1.5 mag and H-Ks>0.4 mag in the LMC, SMC, M31, and M33 from 2MASS data. Methods.The data were taken from the 2MASS All-Sky Point Source catalogue archive. We used Virtual Observatory tools and took advantage of its capabilities at various stages in the analysis. Results. It is well known that stars with the colors we selected correspond mainly to carbon stars. Although the most luminous AGBs detected here contain a large number of carbon stars,they are not included in existing catalogues produced from data in the optical domain, where they are not visible since they are dust-enshrouded. A comparison of the AGB stars detected with combined near and mid-infrared data from MSX and 2MASS in the LMC shows that 10% of the bright AGB stars are bright carbon stars never detected before and that the other 50% are OH/IR oxygen rich stars, whereas the 40% that remain were not cross-matched. Conclusions. The catalogues of the most luminous AGB stars compiled here are an important complement to existing data. In the LMC, these bright AGB stars are centrally located, whereas they are concentrated in an active star-formation ring in M31. In the SMC and M33, there are not enough of them to draw definite conclusions, although they tend to be centrally located. Their luminosity functions are similar for the four galaxies we studied., Comment: 16 pages, 12 figures, 4 tables (Appendix A), accepted in A&A
Published: 2006

46. The Hi-GAL compact source catalogue - I. The physical properties of the clumps in the inner Galaxy (-71.degrees 0 < l < 67.degrees 0)

Author: Elia, Davide, Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, S., Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmeirim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltran, M. T., Billot, N., Cambresy, L., Cesaroni, R., Garcia-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mege, P., Peretto, N., Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., Becciani, U., Brescia, M., Buemi, C., Bufano, F., Butora, R., Cavuoti, S., Costa, A., Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., Leto, P., Causi, G. Li, Marchili, N., Martinavarro-Armengol, S., Mercurio, A., Molinaro, M., Riccio, G., Sano, H., Sciacca, E., Tachihara, K., Torii, K., Trigilio, C., Vitello, F., Yamamoto, H., Elia, Davide, Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, S., Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmeirim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltran, M. T., Billot, N., Cambresy, L., Cesaroni, R., Garcia-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mege, P., Peretto, N., Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., Becciani, U., Brescia, M., Buemi, C., Bufano, F., Butora, R., Cavuoti, S., Costa, A., Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., Leto, P., Causi, G. Li, Marchili, N., Martinavarro-Armengol, S., Mercurio, A., Molinaro, M., Riccio, G., Sano, H., Sciacca, E., Tachihara, K., Torii, K., Trigilio, C., Vitello, F., and Yamamoto, H.
Abstract: Hi-GAL (Herschel InfraRed Galactic Plane Survey) is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 mu m. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogues presented in Molinari et al., covering the portion of Galactic plane -71.degrees 0 < l < 67.degrees 0. The band-merged catalogue contains 100 922 sources with a regular SED, 24 584 of which show a 70-mu m counterpart and are thus considered protostellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterize different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in protostellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to protostellar, but then it is found to decrease again in themajority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between 'on-arm' and 'interarm' positions.
Published: 2017

47. What Is SIMBAD, and What Is It Not?

Author: Loup, C., Oberto, A., Allen, M., Lesteven, S., Boch, T., Bot, C., Bonnarel, F., Brouty, M., Brunet, C., Buga, M., Cambresy, L., Delacour, T., Derriere, S., Eisele, A., Fernique, P., Genova, F., Guehenneux, S., Landais, G., Louys, M., Nebot, A., Neuville, M., Ocvirk, P., Perret, E., Pineau, F.-X., Schaaff, A., Siebert, A., Son, E., Vannier, P., Vollmer, B., Vonflie, P., Woelfel, F., Laboratoire Chrono-environnement - UFC (UMR 6249) (LCE), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), University of Sofia, RiverLy (UR Riverly), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), and MATIS - Prokaria
Subjects: [SDU]Sciences of the Universe [physics]
Abstract: International audience; The purpose of the SIMBAD database is to provide the bibliography and some fundamental data on astronomical objects of interest which have been studied in scientific articles. It includes objects of any nature, stars - galaxies - interstellar medium - transient events - etc. SIMBAD is a meta-compilation built from what is published in the literature, and from our expertise on cross-identifications. It is a dynamic database, updated every working day. By construction its content is heterogeneous as data come from any kind of instruments at all wavelengths with any resolution and astrometry, and different names from one publication to another. Thus SIMBAD is not a catalogue, and should not be used as a catalogue. It is not the purpose of SIMBAD to contain “everything”. Especially, lists of uncharacterised sources detected in photometric surveys of any size are usually not processed in SIMBAD. But they are available at CDS in the VizieR database which contains published tables of objects, as well as most very large surveys. The idea now is to use both SIMBAD and VizieR as complementary research tools.
Published: 2016

48. SF2A-2016: Semaine de l'Astrophysique Francaise

Author: Reylé, C., Richard, J., Cambresy, L., Deleuil, M., Pécontal, E., Tresse, L., Vauglin, I., Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Astrophysique de Marseille (LAM), 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), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience; Not Available
Published: 2016

49. The Milky Way rotation curve revisited

Author: Russeil, D., primary, Zavagno, A., additional, Mège, P., additional, Poulin, Y., additional, Molinari, S., additional, and Cambresy, L., additional
Published: 2017
Full Text: View/download PDF

50. Athena+: The first deep universe x-ray observatory

Author: Barret, D., Nandra, K., Jonker, P.G., Palacios, A., al., E., Cambresy, L., and Cambresy, L.
Subjects: Astronomy
Abstract: Contains fulltext : 122841.pdf (Publisher’s version ) (Open Access) SF2A-2013 447 p.
Published: 2013

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