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15 results on '"Sauvage, M."'

1. Euclid: Estimation of the Impact of Correlated Readout Noise for Flux Measurements with the Euclid NISP Instrument*

Author

Jiménez Muñoz, A., primary, Macías-Pérez, J., additional, Secroun, A., additional, Gillard, W., additional, Kubik, B., additional, Auricchio, N., additional, Balestra, A., additional, Bodendorf, C., additional, Bonino, D., additional, Branchini, E., additional, Brescia, M., additional, Brinchmann, J., additional, Capobianco, V., additional, Carbone, C., additional, Carretero, J., additional, Casas, R., additional, Castellano, M., additional, Cavuoti, S., additional, Cimatti, A., additional, Cledassou, R., additional, Congedo, G., additional, Conversi, L., additional, Copin, Y., additional, Corcione, L., additional, Costille, A., additional, Cropper, M., additional, Degaudenzi, H., additional, Douspis, M., additional, Dubath, F., additional, Dusini, S., additional, Ealet, A., additional, Franceschi, E., additional, Franzetti, P., additional, Fumana, M., additional, Garilli, B., additional, Gillis, B., additional, Giocoli, C., additional, Grazian, A., additional, Grupp, F., additional, Haugan, S. V. H., additional, Holmes, W., additional, Hormuth, F., additional, Jahnke, K., additional, Kermiche, S., additional, Kiessling, A., additional, Kilbinger, M., additional, Kümmel, M., additional, Kunz, M., additional, Kurki-Suonio, H., additional, Laureijs, R., additional, Ligori, S., additional, Lilje, P. B., additional, Lloro, I., additional, Maiorano, E., additional, Mansutti, O., additional, Marggraf, O., additional, Markovic, K., additional, Massey, R., additional, Medinaceli, E., additional, Mei, S., additional, Meneghetti, M., additional, Meylan, G., additional, Moscardini, L., additional, Niemi, S. M., additional, Padilla, C., additional, Paltani, S., additional, Pasian, F., additional, Pedersen, K., additional, Percival, W. J., additional, Pires, S., additional, Polenta, G., additional, Poncet, M., additional, Popa, L., additional, Pozzetti, L., additional, Raison, F., additional, Rebolo, R., additional, Roncarelli, M., additional, Rossetti, E., additional, Saglia, R., additional, Sauvage, M., additional, Scaramella, R., additional, Schneider, P., additional, Seidel, G., additional, Serrano, S., additional, Sirignano, C., additional, Sirri, G., additional, Tavagnacco, D., additional, Taylor, A. N., additional, Teplitz, H. I., additional, Tereno, I., additional, Toledo-Moreo, R., additional, Valenziano, L., additional, Vassallo, T., additional, Verdoes Kleijn, G. A., additional, Wang, Y., additional, Weller, J., additional, Wetzstein, M., additional, Zamorani, G., additional, and Zoubian, J., additional

Published
2021
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3. An Overview of the Dwarf Galaxy Survey (PASP, 125, 600, [2013])—Corrigendum

Author

Madden, S. C., primary, Rémy-Ruyer, A., additional, Galametz, M., additional, Cormier, D., additional, Lebouteiller, V., additional, Galliano, F., additional, Hony, S., additional, Bendo, G. J., additional, Smith, M. W. L., additional, Pohlen, M., additional, Roussel, H., additional, Sauvage, M., additional, Wu, R., additional, Sturm, E., additional, Poglitsch, A., additional, Contursi, A., additional, Doublier, V., additional, Baes, M., additional, Barlow, M. J., additional, Boselli, A., additional, Boquien, M., additional, Carlson, L. R., additional, Ciesla, L., additional, Cooray, A., additional, Cortese, L., additional, De Looze, I., additional, Irwin, J. A., additional, Isaak, K., additional, Kamenetzky, J., additional, Karczewski, O. Ł., additional, Lu, N., additional, MacHattie, J. A., additional, O’Halloran, B., additional, Parkin, T. J., additional, Rangwala, N., additional, Schirm, M. R. P., additional, Schulz, B., additional, Spinoglio, L., additional, Vaccari, M., additional, Wilson, C. D., additional, and Wozniak, H., additional

Published
2014
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4. An Overview of the Dwarf Galaxy Survey

Author

Madden, S. C., primary, Rémy-Ruyer, A., additional, Galametz, M., additional, Cormier, D., additional, Lebouteiller, V., additional, Galliano, F., additional, Hony, S., additional, Bendo, G. J., additional, Smith, M. W. L., additional, Pohlen, M., additional, Roussel, H., additional, Sauvage, M., additional, Wu, R., additional, Sturm, E., additional, Poglitsch, A., additional, Contursi, A., additional, Doublier, V., additional, Baes, M., additional, Barlow, M. J., additional, Boselli, A., additional, Boquien, M., additional, Carlson, L. R., additional, Ciesla, L., additional, Cooray, A., additional, Cortese, L., additional, de Looze, I., additional, Irwin, J. A., additional, Isaak, K., additional, Kamenetzky, J., additional, Karczewski, O. Ł., additional, Lu, N., additional, MacHattie, J. A., additional, O’Halloran, B., additional, Parkin, T. J., additional, Rangwala, N., additional, Schirm, M. R. P., additional, Schulz, B., additional, Spinoglio, L., additional, Vaccari, M., additional, Wilson, C. D., additional, and Wozniak, H., additional

Published
2013
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5. KINGFISH—Key Insights on Nearby Galaxies: A Far-Infrared Survey withHerschel: Survey Description and Image Atlas1

Author

Kennicutt, R. C., primary, Calzetti, D., additional, Aniano, G., additional, Appleton, P., additional, Armus, L., additional, Beirão, P., additional, Bolatto, A. D., additional, Brandl, B., additional, Crocker, A., additional, Croxall, K., additional, Dale, D. A., additional, Meyer, J. Donovan, additional, Draine, B. T., additional, Engelbracht, C. W., additional, Galametz, M., additional, Gordon, K. D., additional, Groves, B., additional, Hao, C.-N., additional, Helou, G., additional, Hinz, J., additional, Hunt, L. K., additional, Johnson, B., additional, Koda, J., additional, Krause, O., additional, Leroy, A. K., additional, Li, Y., additional, Meidt, S., additional, Montiel, E., additional, Murphy, E. J., additional, Rahman, N., additional, Rix, H.-W., additional, Roussel, H., additional, Sandstrom, K., additional, Sauvage, M., additional, Schinnerer, E., additional, Skibba, R., additional, Smith, J. D. T., additional, Srinivasan, S., additional, Vigroux, L., additional, Walter, F., additional, Wilson, C. D., additional, Wolfire, M., additional, and Zibetti, S., additional

Published
2011
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6. The Herschel Reference Survey

Author

Boselli, A., primary, Eales, S., additional, Cortese, L., additional, Bendo, G., additional, Chanial, P., additional, Buat, V., additional, Davies, J., additional, Auld, R., additional, Rigby, E., additional, Baes, M., additional, Barlow, M., additional, Bock, J., additional, Bradford, M., additional, Castro-Rodriguez, N., additional, Charlot, S., additional, Clements, D., additional, Cormier, D., additional, Dwek, E., additional, Elbaz, D., additional, Galametz, M., additional, Galliano, F., additional, Gear, W., additional, Glenn, J., additional, Gomez, H., additional, Griffin, M., additional, Hony, S., additional, Isaak, K., additional, Levenson, L., additional, Lu, N., additional, Madden, S., additional, O’Halloran, B., additional, Okamura, K., additional, Oliver, S., additional, Page, M., additional, Panuzzo, P., additional, Papageorgiou, A., additional, Parkin, T., additional, Perez-Fournon, I., additional, Pohlen, M., additional, Rangwala, N., additional, Roussel, H., additional, Rykala, A., additional, Sacchi, N., additional, Sauvage, M., additional, Schulz, B., additional, Schirm, M., additional, Smith, M. W. L., additional, Spinoglio, L., additional, Stevens, J., additional, Symeonidis, M., additional, Vaccari, M., additional, Vigroux, L., additional, Wilson, C., additional, Wozniak, H., additional, Wright, G., additional, and Zeilinger, W., additional

Published
2010
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7. Hi-GAL: The Herschel Infrared Galactic Plane Survey

Author

Molinari, S., primary, Swinyard, B., additional, Bally, J., additional, Barlow, M., additional, Bernard, J.-P., additional, Martin, P., additional, Moore, T., additional, Noriega-Crespo, A., additional, Plume, R., additional, Testi, L., additional, Zavagno, A., additional, Abergel, A., additional, Ali, B., additional, André, P., additional, Baluteau, J.-P., additional, Benedettini, M., additional, Berné, O., additional, Billot, N. P., additional, Blommaert, J., additional, Bontemps, S., additional, Boulanger, F., additional, Brand, J., additional, Brunt, C., additional, Burton, M., additional, Campeggio, L., additional, Carey, S., additional, Caselli, P., additional, Cesaroni, R., additional, Cernicharo, J., additional, Chakrabarti, S., additional, Chrysostomou, A., additional, Codella, C., additional, Cohen, M., additional, Compiegne, M., additional, Davis, C. J., additional, de Bernardis, P., additional, de Gasperis, G., additional, Di Francesco, J., additional, di Giorgio, A. M., additional, Elia, D., additional, Faustini, F., additional, Fischera, J. F., additional, Fukui, Y., additional, Fuller, G. A., additional, Ganga, K., additional, Garcia-Lario, P., additional, Giard, M., additional, Giardino, G., additional, Glenn, J:, additional, Goldsmith, P., additional, Griffin, M., additional, Hoare, M., additional, Huang, M., additional, Jiang, B., additional, Joblin, C., additional, Joncas, G., additional, Juvela, M., additional, Kirk, J., additional, Lagache, G., additional, Li, J. Z., additional, Lim, T. L., additional, Lord, S. D., additional, Lucas, P. W., additional, Maiolo, B., additional, Marengo, M., additional, Marshall, D., additional, Masi, S., additional, Massi, F., additional, Matsuura, M., additional, Meny, C., additional, Minier, V., additional, Miville-Deschênes, M.-A., additional, Montier, L., additional, Motte, F., additional, Müller, T. G., additional, Natoli, P., additional, Neves, J., additional, Olmi, L., additional, Paladini, R., additional, Paradis, D., additional, Pestalozzi, M., additional, Pezzuto, S., additional, Piacentini, F., additional, Pomarès, M., additional, Popescu, C. C., additional, Reach, W. T., additional, Richer, J., additional, Ristorcelli, I., additional, Roy, A., additional, Royer, P., additional, Russeil, D., additional, Saraceno, P., additional, Sauvage, M., additional, Schilke, P., additional, Schneider-Bontemps, N., additional, Schuller, F., additional, Schultz, B., additional, Shepherd, D. S., additional, Sibthorpe, B., additional, Smith, H. A., additional, Smith, M. D., additional, Spinoglio, L., additional, Stamatellos, D., additional, Strafella, F., additional, Stringfellow, G., additional, Sturm, E., additional, Taylor, R., additional, Thompson, M. A., additional, Tuffs, R. J., additional, Umana, G., additional, Valenziano, L., additional, Vavrek, R., additional, Viti, S., additional, Waelkens, C., additional, Ward-Thompson, D., additional, White, G., additional, Wyrowski, F., additional, Yorke, H. W., additional, and Zhang, Q., additional

Published
2010
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8. REGIONAL VARIATIONS IN THE DENSE GAS HEATING AND COOLING IN M51 FROM HERSCHEL Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. FAR-INFRARED SPECTROSCOPY

Author

Parkin, T. J., Wilson, C. D., Schirm, M. R. P., Baes, M., Boquien, M., Boselli, A., Cooray, A., Cormier, D., Foyle, K., Karczewski, O. Ł., Lebouteiller, V., Looze, I. de, Madden, S. C., Roussel, H., Sauvage, M., and Spinoglio, L.

Subjects
PHOTONS, GALAXIES, MOLECULAR clouds, INTERSTELLAR molecules, ULTRAVIOLET radiation
Abstract

We present Herschel PACS and SPIRE spectroscopy of the most important far-infrared cooling lines in M51, [C II](158 μm), [N II](122 and 205 μm), [O I](63 and 145 μm), and [O III](88 μm). We compare the observed flux of these lines with the predicted flux from a photon-dominated region model to determine characteristics of the cold gas such as density, temperature, and the far-ultraviolet (FUV) radiation field, G0, resolving details on physical scales of roughly 600 pc. We find an average [C II]/FTIR of 4 × 10–3, in agreement with previous studies of other galaxies. A pixel-by-pixel analysis of four distinct regions of M51 shows a radially decreasing trend in both the FUV radiation field, G0, and the hydrogen density, n, peaking in the nucleus of the galaxy, and then falling off out to the arm and interarm regions. We see for the first time that the FUV flux and gas density are similar in the differing environments of the arm and interarm regions, suggesting that the inherent physical properties of the molecular clouds in both regions are essentially the same. [ABSTRACT FROM AUTHOR]

Published
2013
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9. HERSCHEL* REVEALS MASSIVE COLD CLUMPS IN NGC 7538.

Author

FALLSCHEER, C., REID, M. A., DI FRANCESCO, J., MARTIN, P. G., HILL, T., HENNEMANN, M., NGUYEN-LUONG, Q., MOTTE, F., MEN'SHCHIKOV, A., ANDRÉ, PH., WARD-THOMPSON, D., GRIFFIN, M., KIRK, J., KONYVES, V., RYGL, K. L. J., SADAVOY, S., SAUVAGE, M., SCHNEIDER, N., ANDERSON, L. D., and BENEDETTINI, M.

Subjects
STAR formation, SPECTRAL energy distribution, STELLAR luminosity function, STELLAR mass, INTERSTELLAR medium
Abstract

We present the first overview of the Herschel observations of the nearby high-mass star-forming region NGC 7538, taken as part of the Herschel imaging study of OB young stellar objects (HOBYS) Key Programme. These PACS and SPIRE maps cover an approximate area of one square degree at five submillimeter and far-infrared wavebands. We have identified 780 dense sources and classified 224 of those.With the intention of investigating the existence of cold massive starless or class 0-like clumps that would have the potential to form intermediate- to high-mass stars, we further isolate 13 clumps as the most likely candidates for follow-up studies. These 13 clumps have masses in excess of 40M⊙ and temperatures below 15 K. They range in size from 0.4 pc to 2.5 pc and have densities between 3 × 103 cm−3 and 4 × 104 cm−3. Spectral energy distributions are then used to characterize their energetics and evolutionary state through a luminosity–mass diagram. NGC 7538 has a highly filamentary structure, previously unseen in the dust continuum of existing submillimeter surveys. We report the most complete imaging to date of a large, evacuated ring of material in NGC 7538 which is bordered by many cool sources. [ABSTRACT FROM AUTHOR]

Published
2013
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10. Erratum: "Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample" (2020, ApJ, 889, 150).

Author

Aniano, G., Draine, B. T., Hunt, L. K., Sandstrom, K., Calzetti, D., Kennicutt, R. C., Dale, D. A., Galametz, M., Gordon, K. D., Leroy, A. K., Smith, J.-D. T., Roussel, H., Sauvage, M., Walter, F., Armus, L., Bolatto, A. D., Boquien, M., Crocker, A., De Looze, I., and Meyer, J. Donovan

Subjects
YELLOWTAIL, GALAXIES, DUST, SPACE sciences
Published
2020
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13. MODELING DUST AND STARLIGHT IN GALAXIES OBSERVED BY SPITZER AND HERSCHEL: NGC 628 AND NGC 6946.

Author

Aniano, G., Draine, B. T., Calzetti, D., Dale, D. A., Engelbracht, C. W., Gordon, K. D., Hunt, L. K., Kennicutt, R. C., Krause, O., Leroy, A. K., Rix, H. -W, Roussel, H., Sandstrom, K., Sauvage, M., Walter, F., Armus, L., Bolatto, A. D., Crocker, A., Donovan Meyer, J., and Galametz, M.

Subjects
SPIRAL galaxies, GALAXIES, LUMINOSITY, POLYCYCLIC aromatic hydrocarbons, POLYCYCLIC aromatic compounds
Abstract

We characterize the dust in NGC 628 and NGC 6946, two nearby spiral galaxies in the KINGFISH sample. With data from 3.6 μm to 500 μm, dust models are strongly constrained. Using the Draine & Li dust model (amorphous silicate and carbonaceous grains), for each pixel in each galaxy we estimate (1) dust mass surface density, (2) dust mass fraction contributed by polycyclic aromatic hydrocarbons, (3) distribution of starlight intensities heating the dust, (4) total infrared (IR) luminosity emitted by the dust, and (5) IR luminosity originating in regions with high starlight intensity. We obtain maps for the dust properties, which trace the spiral structure of the galaxies. The dust models successfully reproduce the observed global and resolved spectral energy distributions (SEDs). The overall dust/H mass ratio is estimated to be 0.0082 ± 0.0017 for NGC 628, and 0.0063 ± 0.0009 for NGC 6946, consistent with what is expected for galaxies of near-solar metallicity. Our derived dust masses are larger (by up to a factor of three) than estimates based on single-temperature modified blackbody fits. We show that the SED fits are significantly improved if the starlight intensity distribution includes a (single intensity) “delta function” component. We find no evidence for significant masses of cold dust (T ≲ 12 K). Discrepancies between PACS and MIPS photometry in both low and high surface brightness areas result in large uncertainties when the modeling is done at PACS resolutions, in which case SPIRE, MIPS70, and MIPS160 data cannot be used. We recommend against attempting to model dust at the angular resolution of PACS. [ABSTRACT FROM AUTHOR]

Published
2012
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