Author: "A. Zavagno" / Journal: astronomy and astrophysics - Searchworks@Jio Institute Digital Library Search Results

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102 results on '"A. Zavagno"'

1. Ionization compression impact on dense gas distribution and star formation

Author: Tremblin, P., Schneider, N., Minier, V., Didelon, P., Hill, T., Anderson, L. D., Motte, F., Zavagno, A., André, Ph., Arzoumanian, D., Audit, E., Benedettini, M., Bontemps, S., Csengeri, T., Di Francesco, J., Giannini, T., Hennemann, M., Nguyen Luong, Q., Marston, A. P., Peretto, N., Rivera-Ingraham, A., Russeil, D., Rygl, K. L. J., Spinoglio, L., and White, G. J.
Published: 2014
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2. Dust temperature tracing the ISRF intensity in the Galaxy

Author: Bernard, J.-Ph., primary, Paradis, D., additional, Marshall, D. J., additional, Montier, L., additional, Lagache, G., additional, Paladini, R., additional, Veneziani, M., additional, Brunt, C. M., additional, Mottram, J. C., additional, Martin, P., additional, Ristorcelli, I., additional, Noriega-Crespo, A., additional, Compiègne, M., additional, Flagey, N., additional, Anderson, L. D., additional, Popescu, C. C., additional, Tuffs, R., additional, Reach, W., additional, White, G., additional, Benedetti, M., additional, Calzoletti, L., additional, DiGiorgio, A. M., additional, Faustini, F., additional, Juvela, M., additional, Joblin, C., additional, Joncas, G., additional, Mivilles-Deschenes, M.-A., additional, Olmi, L., additional, Traficante, A., additional, Piacentini, F., additional, Zavagno, A., additional, and Molinari, S., additional
Published: 2010
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3. AHerschelstudy of the properties of starless cores in the Polaris Flare dark cloud region using PACS and SPIRE

Author: Ward-Thompson, D., primary, Kirk, J. M., additional, André, P., additional, Saraceno, P., additional, Didelon, P., additional, Könyves, V., additional, Schneider, N., additional, Abergel, A., additional, Baluteau, J.-P., additional, Bernard, J.-Ph., additional, Bontemps, S., additional, Cambrésy, L., additional, Cox, P., additional, Di Francesco, J., additional, Di Giorgio, A. M., additional, Griffin, M., additional, Hargrave, P., additional, Huang, M., additional, Li, J. Z., additional, Martin, P., additional, Men'shchikov, A., additional, Minier, V., additional, Molinari, S., additional, Motte, F., additional, Olofsson, G., additional, Pezzuto, S., additional, Russeil, D., additional, Sauvage, M., additional, Sibthorpe, B., additional, Spinoglio, L., additional, Testi, L., additional, White, G., additional, Wilson, C., additional, Woodcraft, A., additional, and Zavagno, A., additional
Published: 2010
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4. Galactic cold cores:Herschelstudy of firstPlanckdetections

Author: Juvela, M., primary, Ristorcelli, I., additional, Montier, L. A., additional, Marshall, D. J., additional, Pelkonen, V.-M., additional, Malinen, J., additional, Ysard, N., additional, Tóth, L. V., additional, Harju, J., additional, Bernard, J.-P., additional, Schneider, N., additional, Verebélyi, E., additional, Anderson, L., additional, André, P., additional, Giard, M., additional, Krause, O., additional, Lehtinen, K., additional, Macias-Perez, J., additional, Martin, P., additional, McGehee, P. M., additional, Meny, C., additional, Motte, F., additional, Pagani, L., additional, Paladini, R., additional, Reach, W., additional, Valenziano, L., additional, Ward-Thompson, D., additional, and Zavagno, A., additional
Published: 2010
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5. Herschelobservations of the W43 “mini-starburst”

Author: Bally, J., primary, Anderson, L. D., additional, Battersby, C., additional, Calzoletti, L., additional, DiGiorgio, A. M., additional, Faustini, F., additional, Ginsburg, A., additional, Li, J. Z., additional, Nguyen-Luong, Q., additional, Molinari, S., additional, Motte, F., additional, Pestalozzi, M., additional, Plume, R., additional, Rodon, J., additional, Schilke, P., additional, Schlingman, W., additional, Schneider-Bontemps, N., additional, Shirley, Y., additional, Stringfellow, G. S., additional, Testi, L., additional, Traficante, A., additional, Veneziani, M., additional, and Zavagno, A., additional
Published: 2010
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6. First detection of the methylidyne cation (CH+) fundamental rotational line with theHerschel/SPIRE FTS

Author: Naylor, D. A., primary, Dartois, E., additional, Habart, E., additional, Abergel, A., additional, Baluteau, J.-P., additional, Jones, S. C., additional, Polehampton, E., additional, Ade, P., additional, Anderson, L. D., additional, André, P., additional, Arab, H., additional, Bernard, J.-P., additional, Blagrave, K., additional, Bontemps, S., additional, Boulanger, F., additional, Cohen, M., additional, Compiègne, M., additional, Cox, P., additional, Davis, G., additional, Emery, R., additional, Fulton, T., additional, Gry, C., additional, Huang, M., additional, Joblin, C., additional, Kirk, J. M., additional, Lagache, G., additional, Lim, T., additional, Madden, S., additional, Makiwa, G., additional, Martin, P., additional, Miville-Deschênes, M.-A., additional, Molinari, S., additional, Moseley, H., additional, Motte, F., additional, Okumura, K., additional, Pinheiro Gonçalves, D., additional, Rodón, J. A., additional, Russeil, D., additional, Saraceno, P., additional, Sidher, S., additional, Spencer, L., additional, Swinyard, B., additional, Ward-Thompson, D., additional, White, G. J., additional, and Zavagno, A., additional
Published: 2010
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7. Herschel-SPIRE observations of the Polaris flare: Structure of the diffuse interstellar medium at the sub-parsec scale

Author: Miville-Deschênes, M.-A., primary, Martin, P. G., additional, Abergel, A., additional, Bernard, J.-P., additional, Boulanger, F., additional, Lagache, G., additional, Anderson, L. D., additional, André, P., additional, Arab, H., additional, Baluteau, J.-P., additional, Blagrave, K., additional, Bontemps, S., additional, Cohen, M., additional, Compiegne, M., additional, Cox, P., additional, Dartois, E., additional, Davis, G., additional, Emery, R., additional, Fulton, T., additional, Gry, C., additional, Habart, E., additional, Huang, M., additional, Joblin, C., additional, Jones, S. C., additional, Kirk, J., additional, Lim, T., additional, Madden, S., additional, Makiwa, G., additional, Menshchikov, A., additional, Molinari, S., additional, Moseley, H., additional, Motte, F., additional, Naylor, D. A., additional, Okumura, K., additional, Pinheiro Gonçalves, D., additional, Polehampton, E., additional, Rodón, J. A., additional, Russeil, D., additional, Saraceno, P., additional, Schneider, N., additional, Sidher, S., additional, Spencer, L., additional, Swinyard, B., additional, Ward-Thompson, D., additional, White, G. J., additional, and Zavagno, A., additional
Published: 2010
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8. Herschel-SPIRE spectroscopy of the DR21 molecular cloud core

Author: White, G. J., primary, Abergel, A., additional, Spencer, L., additional, Schneider, N., additional, Naylor, D. A., additional, Anderson, L. D., additional, Joblin, C., additional, Ade, P., additional, André, P., additional, Arab, H., additional, Baluteau, J.-P., additional, Bernard, J.-P., additional, Blagrave, K., additional, Bontemps, S., additional, Boulanger, F., additional, Cohen, M., additional, Compiegne, M., additional, Cox, P., additional, Dartois, E., additional, Davis, G., additional, Emery, R., additional, Fulton, T., additional, Gom, B., additional, Griffin, M., additional, Gry, C., additional, Habart, E., additional, Huang, M., additional, Jones, S., additional, Kirk, J. M., additional, Lagache, G., additional, Leeks, S., additional, Lim, T., additional, Madden, S., additional, Makiwa, G., additional, Martin, P., additional, Miville-Deschênes, M.-A., additional, Molinari, S., additional, Moseley, H., additional, Motte, F., additional, Okumura, K., additional, Pinheiro Gonçalves, D., additional, Polehampton, E., additional, Rodet, T., additional, Rodón, J. A., additional, Russeil, D., additional, Saraceno, P., additional, Sidher, S., additional, Swinyard, B. M., additional, Ward-Thompson, D., additional, and Zavagno, A., additional
Published: 2010
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9. TheHerschel-SPIRE instrument and its in-flight performance

Author: Griffin, M. J., primary, Abergel, A., additional, Abreu, A., additional, Ade, P. A. R., additional, André, P., additional, Augueres, J.-L., additional, Babbedge, T., additional, Bae, Y., additional, Baillie, T., additional, Baluteau, J.-P., additional, Barlow, M. J., additional, Bendo, G., additional, Benielli, D., additional, Bock, J. J., additional, Bonhomme, P., additional, Brisbin, D., additional, Brockley-Blatt, C., additional, Caldwell, M., additional, Cara, C., additional, Castro-Rodriguez, N., additional, Cerulli, R., additional, Chanial, P., additional, Chen, S., additional, Clark, E., additional, Clements, D. L., additional, Clerc, L., additional, Coker, J., additional, Communal, D., additional, Conversi, L., additional, Cox, P., additional, Crumb, D., additional, Cunningham, C., additional, Daly, F., additional, Davis, G. R., additional, De Antoni, P., additional, Delderfield, J., additional, Devin, N., additional, Di Giorgio, A., additional, Didschuns, I., additional, Dohlen, K., additional, Donati, M., additional, Dowell, A., additional, Dowell, C. D., additional, Duband, L., additional, Dumaye, L., additional, Emery, R. J., additional, Ferlet, M., additional, Ferrand, D., additional, Fontignie, J., additional, Fox, M., additional, Franceschini, A., additional, Frerking, M., additional, Fulton, T., additional, Garcia, J., additional, Gastaud, R., additional, Gear, W. K., additional, Glenn, J., additional, Goizel, A., additional, Griffin, D. K., additional, Grundy, T., additional, Guest, S., additional, Guillemet, L., additional, Hargrave, P. C., additional, Harwit, M., additional, Hastings, P., additional, Hatziminaoglou, E., additional, Herman, M., additional, Hinde, B., additional, Hristov, V., additional, Huang, M., additional, Imhof, P., additional, Isaak, K. J., additional, Israelsson, U., additional, Ivison, R. J., additional, Jennings, D., additional, Kiernan, B., additional, King, K. J., additional, Lange, A. E., additional, Latter, W., additional, Laurent, G., additional, Laurent, P., additional, Leeks, S. J., additional, Lellouch, E., additional, Levenson, L., additional, Li, B., additional, Li, J., additional, Lilienthal, J., additional, Lim, T., additional, Liu, S. J., additional, Lu, N., additional, Madden, S., additional, Mainetti, G., additional, Marliani, P., additional, McKay, D., additional, Mercier, K., additional, Molinari, S., additional, Morris, H., additional, Moseley, H., additional, Mulder, J., additional, Mur, M., additional, Naylor, D. A., additional, Nguyen, H., additional, O'Halloran, B., additional, Oliver, S., additional, Olofsson, G., additional, Olofsson, H.-G., additional, Orfei, R., additional, Page, M. J., additional, Pain, I., additional, Panuzzo, P., additional, Papageorgiou, A., additional, Parks, G., additional, Parr-Burman, P., additional, Pearce, A., additional, Pearson, C., additional, Pérez-Fournon, I., additional, Pinsard, F., additional, Pisano, G., additional, Podosek, J., additional, Pohlen, M., additional, Polehampton, E. T., additional, Pouliquen, D., additional, Rigopoulou, D., additional, Rizzo, D., additional, Roseboom, I. G., additional, Roussel, H., additional, Rowan-Robinson, M., additional, Rownd, B., additional, Saraceno, P., additional, Sauvage, M., additional, Savage, R., additional, Savini, G., additional, Sawyer, E., additional, Scharmberg, C., additional, Schmitt, D., additional, Schneider, N., additional, Schulz, B., additional, Schwartz, A., additional, Shafer, R., additional, Shupe, D. L., additional, Sibthorpe, B., additional, Sidher, S., additional, Smith, A., additional, Smith, A. J., additional, Smith, D., additional, Spencer, L., additional, Stobie, B., additional, Sudiwala, R., additional, Sukhatme, K., additional, Surace, C., additional, Stevens, J. A., additional, Swinyard, B. M., additional, Trichas, M., additional, Tourette, T., additional, Triou, H., additional, Tseng, S., additional, Tucker, C., additional, Turner, A., additional, Vaccari, M., additional, Valtchanov, I., additional, Vigroux, L., additional, Virique, E., additional, Voellmer, G., additional, Walker, H., additional, Ward, R., additional, Waskett, T., additional, Weilert, M., additional, Wesson, R., additional, White, G. J., additional, Whitehouse, N., additional, Wilson, C. D., additional, Winter, B., additional, Woodcraft, A. L., additional, Wright, G. S., additional, Xu, C. K., additional, Zavagno, A., additional, Zemcov, M., additional, Zhang, L., additional, and Zonca, E., additional
Published: 2010
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10. Physical properties of the Sh2-104 H II region as seen byHerschel

Author: Rodón, J. A., primary, Zavagno, A., additional, Baluteau, J.-P., additional, Anderson, L. D., additional, Polehampton, E., additional, Abergel, A., additional, Motte, F., additional, Bontemps, S., additional, Ade, P., additional, André, P., additional, Arab, H., additional, Beichman, C., additional, Bernard, J.-P., additional, Blagrave, K., additional, Boulanger, F., additional, Cohen, M., additional, Compiegne, M., additional, Cox, P., additional, Dartois, E., additional, Davis, G., additional, Emery, R., additional, Fulton, T., additional, Gry, C., additional, Habart, E., additional, Halpern, M., additional, Huang, M., additional, Joblin, C., additional, Jones, S. C., additional, Kirk, J., additional, Lagache, G., additional, Lin, T., additional, Madden, S., additional, Makiwa, G., additional, Martin, P., additional, Miville-Deschênes, M.-A., additional, Molinari, S., additional, Moseley, H., additional, Naylor, D., additional, Okumura, K., additional, Orieux, F., additional, Pinheiro Gonçalves, D., additional, Rodet, T., additional, Russeil, D., additional, Saraceno, P., additional, Sidher, S., additional, Spencer, L., additional, Swinyard, B., additional, Ward-Thompson, D., additional, and White, G., additional
Published: 2010
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11. Initial highlights of the HOBYS key program, theHerschelimaging survey of OB young stellar objects

Author: Motte, F., primary, Zavagno, A., additional, Bontemps, S., additional, Schneider, N., additional, Hennemann, M., additional, Di Francesco, J., additional, André, Ph., additional, Saraceno, P., additional, Griffin, M., additional, Marston, A., additional, Ward-Thompson, D., additional, White, G., additional, Minier, V., additional, Men'shchikov, A., additional, Hill, T., additional, Abergel, A., additional, Anderson, L. D., additional, Aussel, H., additional, Balog, Z., additional, Baluteau, J.-P., additional, Bernard, J.-Ph., additional, Cox, P., additional, Csengeri, T., additional, Deharveng, L., additional, Didelon, P., additional, di Giorgio, A.-M., additional, Hargrave, P., additional, Huang, M., additional, Kirk, J., additional, Leeks, S., additional, Li, J. Z., additional, Martin, P., additional, Molinari, S., additional, Nguyen-Luong, Q., additional, Olofsson, G., additional, Persi, P., additional, Peretto, N., additional, Pezzuto, S., additional, Roussel, H., additional, Russeil, D., additional, Sadavoy, S., additional, Sauvage, M., additional, Sibthorpe, B., additional, Spinoglio, L., additional, Testi, L., additional, Teyssier, D., additional, Vavrek, R., additional, Wilson, C. D., additional, and Woodcraft, A., additional
Published: 2010
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12. Herschelobservations of embedded protostellar clusters in the Rosette molecular cloud

Author: Hennemann, M., primary, Motte, F., additional, Bontemps, S., additional, Schneider, N., additional, Csengeri, T., additional, Balog, Z., additional, Di Francesco, J., additional, Zavagno, A., additional, André, Ph., additional, Men'shchikov, A., additional, Abergel, A., additional, Ali, B., additional, Baluteau, J.-P., additional, Bernard, J.-Ph., additional, Cox, P., additional, Didelon, P., additional, di Giorgio, A.-M., additional, Griffin, M., additional, Hargrave, P., additional, Hill, T., additional, Horeau, B., additional, Huang, M., additional, Kirk, J., additional, Leeks, S., additional, Li, J. Z., additional, Marston, A., additional, Martin, P., additional, Molinari, S., additional, Nguyen Luong, Q., additional, Olofsson, G., additional, Persi, P., additional, Pezzuto, S., additional, Russeil, D., additional, Saraceno, P., additional, Sauvage, M., additional, Sibthorpe, B., additional, Spinoglio, L., additional, Testi, L., additional, Ward-Thompson, D., additional, White, G., additional, Wilson, C., additional, and Woodcraft, A., additional
Published: 2010
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13. The physical properties of the dust in the RCW 120 H ii region as seen byHerschel

Author: Anderson, L. D., primary, Zavagno, A., additional, Rodón, J. A., additional, Russeil, D., additional, Abergel, A., additional, Ade, P., additional, André, P., additional, Arab, H., additional, Baluteau, J.-P., additional, Bernard, J.-P., additional, Blagrave, K., additional, Bontemps, S., additional, Boulanger, F., additional, Cohen, M., additional, Compiègne, M., additional, Cox, P., additional, Dartois, E., additional, Davis, G., additional, Emery, R., additional, Fulton, T., additional, Gry, C., additional, Habart, E., additional, Huang, M., additional, Joblin, C., additional, Jones, S. C., additional, Kirk, J. M., additional, Lagache, G., additional, Lim, T., additional, Madden, S., additional, Makiwa, G., additional, Martin, P., additional, Miville-Deschênes, M.-A., additional, Molinari, S., additional, Moseley, H., additional, Motte, F., additional, Naylor, D. A., additional, Okumura, K., additional, Pinheiro Gonçalves, D., additional, Polehampton, E., additional, Saraceno, P., additional, Sauvage, M., additional, Sidher, S., additional, Spencer, L., additional, Swinyard, B., additional, Ward-Thompson, D., additional, and White, G. J., additional
Published: 2010
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14. Clouds, filaments, and protostars: TheHerschel Hi-GAL Milky Way

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, Anderson, L., additional, André, P., additional, Baluteau, J.-P., additional, Battersby, C., additional, Beltrán, M. T., additional, Benedettini, M., additional, Billot, N., additional, Blommaert, J., additional, Bontemps, S., additional, Boulanger, F., additional, Brand, J., additional, Brunt, C., additional, Burton, M., additional, Calzoletti, L., additional, Carey, S., additional, Caselli, P., additional, Cesaroni, R., additional, Cernicharo, J., additional, Chakrabarti, S., additional, Chrysostomou, A., additional, Cohen, M., additional, Compiegne, M., additional, de Bernardis, P., additional, de Gasperis, G., additional, di Giorgio, A. M., additional, Elia, D., additional, Faustini, F., additional, Flagey, N., additional, Fukui, Y., additional, Fuller, G. A., additional, Ganga, K., additional, Garcia-Lario, P., additional, Glenn, J., additional, Goldsmith, P. F., additional, Griffin, M., additional, Hoare, M., additional, Huang, M., additional, Ikhenaode, D., additional, Joblin, C., additional, Joncas, G., additional, Juvela, M., additional, Kirk, J. M., additional, Lagache, G., additional, Li, J. Z., additional, Lim, T. L., additional, Lord, S. D., additional, Marengo, M., additional, Marshall, D. J., additional, Masi, S., additional, Massi, F., additional, Matsuura, M., additional, Minier, V., additional, Miville-Deschênes, M.-A., additional, Montier, L. A., additional, Morgan, L., additional, Motte, F., additional, Mottram, J. C., additional, Müller, T. G., additional, Natoli, P., additional, Neves, J., additional, Olmi, L., additional, Paladini, R., additional, Paradis, D., additional, Parsons, H., additional, Peretto, N., additional, Pestalozzi, M., additional, Pezzuto, S., additional, Piacentini, F., additional, Piazzo, L., additional, Polychroni, D., additional, Pomarès, M., additional, Popescu, C. C., additional, Reach, W. T., additional, Ristorcelli, I., additional, Robitaille, J.-F., additional, Robitaille, T., additional, Rodón, J. A., additional, Roy, A., additional, Royer, P., additional, Russeil, D., additional, Saraceno, P., additional, Sauvage, M., additional, Schilke, P., additional, Schisano, E., additional, Schneider, N., additional, Schuller, F., additional, Schulz, B., additional, Sibthorpe, B., additional, Smith, H. A., additional, Smith, M. D., additional, Spinoglio, L., additional, Stamatellos, D., additional, Strafella, F., additional, Stringfellow, G. S., additional, Sturm, E., additional, Taylor, R., additional, Thompson, M. A., additional, Traficante, A., additional, Tuffs, R. J., additional, Umana, G., additional, Valenziano, L., additional, Vavrek, R., additional, Veneziani, M., additional, Viti, S., additional, Waelkens, C., additional, Ward-Thompson, D., additional, White, G., additional, Wilcock, L. A., additional, Wyrowski, F., additional, Yorke, H. W., additional, and Zhang, Q., additional
Published: 2010
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15. Herschel-SPIRE spectroscopy of G29.96-0.02: Fitting the full SED

Author: Kirk, J. M., primary, Polehampton, E., additional, Anderson, L. D., additional, Baluteau, J.-P., additional, Bontemps, S., additional, Joblin, C., additional, Jones, S. C., additional, Naylor, D. A., additional, Ward-Thompson, D., additional, White, G. J., additional, Abergel, A., additional, Ade, P., additional, André, P., additional, Arab, H., additional, Bernard, J.-P., additional, Blagrave, K., additional, Boulanger, F., additional, Cohen, M., additional, Compiegne, M., additional, Cox, P., additional, Dartois, E., additional, Davis, G., additional, Emery, R., additional, Fulton, T., additional, Gry, C., additional, Habart, E., additional, Huang, M., additional, Lagache, G., additional, Lim, T., additional, Madden, S., additional, Makiwa, G., additional, Martin, P., additional, Miville-Deschênes, M.-A., additional, Molinari, S., additional, Moseley, H., additional, Motte, F., additional, Okumura, K., additional, Pinheiro Gonçalves, D., additional, Rodón, J. A., additional, Russeil, D., additional, Saraceno, P., additional, Sidher, S., additional, Spencer, L., additional, Swinyard, B., additional, and Zavagno, A., additional
Published: 2010
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16. Star formation triggered by H II regions in our Galaxy

Author: Zavagno, A., primary, Anderson, L. D., additional, Russeil, D., additional, Morgan, L., additional, Stringfellow, G. S., additional, Deharveng, L., additional, Rodón, J. A., additional, Robitaille, T. P., additional, Mottram, J. C., additional, Schuller, F., additional, Testi, L., additional, Billot, N., additional, Molinari, S., additional, di Gorgio, A., additional, Kirk, J. M., additional, Brunt, C., additional, Ward-Thompson, D., additional, Traficante, A., additional, Veneziani, M., additional, Faustini, F., additional, and Calzoletti, L., additional
Published: 2010
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17. Evolution of interstellar dust withHerschel. First results in the photodissociation regions of NGC 7023

Author: Abergel, A., primary, Arab, H., additional, Compiègne, M., additional, Kirk, J. M., additional, Ade, P., additional, Anderson, L. D., additional, André, P., additional, Baluteau, J.-P., additional, Bernard, J.-P., additional, Blagrave, K., additional, Bontemps, S., additional, Boulanger, F., additional, Cohen, M., additional, Cox, P., additional, Dartois, E., additional, Davis, G., additional, Emery, R., additional, Fulton, T., additional, Gry, C., additional, Habart, E., additional, Huang, M., additional, Joblin, C., additional, Jones, S. C., additional, Lagache, G., additional, Lim, T., additional, Madden, S., additional, Makiwa, G., additional, Martin, P., additional, Miville-Deschênes, M.-A., additional, Molinari, S., additional, Moseley, H., additional, Motte, F., additional, Naylor, D., additional, Okumura, K., additional, Pinheiro Gonçalves, D., additional, Polehampton, E., additional, Rodon, J., additional, Russeil, D., additional, Saraceno, P., additional, Sauvage, M., additional, Sidher, S., additional, Spencer, L., additional, Swinyard, B., additional, Ward-Thompson, D., additional, White, G. J., additional, and Zavagno, A., additional
Published: 2010
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18. TheHerschelview of star formation in the Rosette molecular cloud under the influence of NGC 2244

Author: Schneider, N., primary, Motte, F., additional, Bontemps, S., additional, Hennemann, M., additional, Di Francesco, J., additional, André, Ph., additional, Zavagno, A., additional, Csengeri, T., additional, Men'shchikov, A., additional, Abergel, A., additional, Baluteau, J.-P., additional, Bernard, J.-Ph., additional, Cox, P., additional, Didelon, P., additional, di Giorgio, A.-M., additional, Gastaud, R., additional, Griffin, M., additional, Hargrave, P., additional, Hill, T., additional, Huang, M., additional, Kirk, J., additional, Könyves, V., additional, Leeks, S., additional, Li, J. Z., additional, Marston, A., additional, Martin, P., additional, Minier, V., additional, Molinari, S., additional, Olofsson, G., additional, Panuzzo, P., additional, Persi, P., additional, Pezzuto, S., additional, Roussel, H., additional, Russeil, D., additional, Sadavoy, S., additional, Saraceno, P., additional, Sauvage, M., additional, Sibthorpe, B., additional, Spinoglio, L., additional, Testi, L., additional, Teyssier, D., additional, Vavrek, R., additional, Ward-Thompson, D., additional, White, G., additional, Wilson, C. D., additional, and Woodcraft, A., additional
Published: 2010
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19. Star formation triggered by the Galactic H II region RCW 120

Author: Zavagno, A., primary, Russeil, D., additional, Motte, F., additional, Anderson, L. D., additional, Deharveng, L., additional, Rodón, J. A., additional, Bontemps, S., additional, Abergel, A., additional, Baluteau, J.-P., additional, Sauvage, M., additional, André, P., additional, Hill, T., additional, and White, G. J., additional
Published: 2010
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20. From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from theHerschelGould Belt Survey

Author: André, Ph., primary, Men'shchikov, A., additional, Bontemps, S., additional, Könyves, V., additional, Motte, F., additional, Schneider, N., additional, Didelon, P., additional, Minier, V., additional, Saraceno, P., additional, Ward-Thompson, D., additional, Di Francesco, J., additional, White, G., additional, Molinari, S., additional, Testi, L., additional, Abergel, A., additional, Griffin, M., additional, Henning, Th., additional, Royer, P., additional, Merín, B., additional, Vavrek, R., additional, Attard, M., additional, Arzoumanian, D., additional, Wilson, C. D., additional, Ade, P., additional, Aussel, H., additional, Baluteau, J.-P., additional, Benedettini, M., additional, Bernard, J.-Ph., additional, Blommaert, J. A. D. L., additional, Cambrésy, L., additional, Cox, P., additional, Di Giorgio, A., additional, Hargrave, P., additional, Hennemann, M., additional, Huang, M., additional, Kirk, J., additional, Krause, O., additional, Launhardt, R., additional, Leeks, S., additional, Le Pennec, J., additional, Li, J. Z., additional, Martin, P. G., additional, Maury, A., additional, Olofsson, G., additional, Omont, A., additional, Peretto, N., additional, Pezzuto, S., additional, Prusti, T., additional, Roussel, H., additional, Russeil, D., additional, Sauvage, M., additional, Sibthorpe, B., additional, Sicilia-Aguilar, A., additional, Spinoglio, L., additional, Waelkens, C., additional, Woodcraft, A., additional, and Zavagno, A., additional
Published: 2010
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21. SPIRE spectroscopy of the prototypical Orion Bar photodissociation region

Author: Habart, E., primary, Dartois, E., additional, Abergel, A., additional, Baluteau, J.-P., additional, Naylor, D., additional, Polehampton, E., additional, Joblin, C., additional, Ade, P., additional, Anderson, L. D., additional, André, P., additional, Arab, H., additional, Bernard, J.-P., additional, Blagrave, K., additional, Bontemps, S., additional, Boulanger, F., additional, Cohen, M., additional, Compiegne, M., additional, Cox, P., additional, Davis, G., additional, Emery, R., additional, Fulton, T., additional, Gry, C., additional, Huang, M., additional, Jones, S. C., additional, Kirk, J., additional, Lagache, G., additional, Lim, T., additional, Madden, S., additional, Makiwa, G., additional, Martin, P., additional, Miville-Deschênes, M.-A., additional, Molinari, S., additional, Moseley, H., additional, Motte, F., additional, Okumura, K., additional, Pinheiro Gonçalves, D., additional, Rodon, J., additional, Russeil, D., additional, Saraceno, P., additional, Sidher, S., additional, Spencer, L., additional, Swinyard, B., additional, Ward-Thompson, D., additional, White, G. J., additional, and Zavagno, A., additional
Published: 2010
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22. Small-scale structure in the Rosette molecular cloud revealed by Herschel

Author: Di Francesco, J., primary, Sadavoy, S., additional, Motte, F., additional, Schneider, N., additional, Hennemann, M., additional, Csengeri, T., additional, Bontemps, S., additional, Balog, Z., additional, Zavagno, A., additional, André, Ph., additional, Saraceno, P., additional, Griffin, M., additional, Men'shchikov, A., additional, Abergel, A., additional, Baluteau, J.-P., additional, Bernard, J.-Ph., additional, Cox, P., additional, Deharveng, L., additional, Didelon, P., additional, di Giorgio, A.-M., additional, Hargrave, P., additional, Huang, M., additional, Kirk, J., additional, Leeks, S., additional, Li, J. Z., additional, Marston, A., additional, Martin, P., additional, Minier, V., additional, Molinari, S., additional, Olofsson, G., additional, Persi, P., additional, Pezzuto, S., additional, Russeil, D., additional, Sauvage, M., additional, Sibthorpe, B., additional, Spinoglio, L., additional, Testi, L., additional, Teyssier, D., additional, Vavrek, R., additional, Ward-Thompson, D., additional, White, G., additional, Wilson, C., additional, and Woodcraft, A., additional
Published: 2010
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23. Filamentary structures and compact objects in the Aquila and Polaris clouds observed byHerschel

Author: Men'shchikov, A., primary, André, Ph., additional, Didelon, P., additional, Könyves, V., additional, Schneider, N., additional, Motte, F., additional, Bontemps, S., additional, Arzoumanian, D., additional, Attard, M., additional, Abergel, A., additional, Baluteau, J.-P., additional, Bernard, J.-Ph., additional, Cambrésy, L., additional, Cox, P., additional, Di Francesco, J., additional, di Giorgio, A. M., additional, Griffin, M., additional, Hargrave, P., additional, Huang, M., additional, Kirk, J., additional, Li, J. Z., additional, Martin, P., additional, Minier, V., additional, Miville-Deschênes, M.-A., additional, Molinari, S., additional, Olofsson, G., additional, Pezzuto, S., additional, Roussel, H., additional, Russeil, D., additional, Saraceno, P., additional, Sauvage, M., additional, Sibthorpe, B., additional, Spinoglio, L., additional, Testi, L., additional, Ward-Thompson, D., additional, White, G., additional, Wilson, C. D., additional, Woodcraft, A., additional, and Zavagno, A., additional
Published: 2010
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24. The Aquila prestellar core population revealed byHerschel

Author: Könyves, V., primary, André, Ph., additional, Men'shchikov, A., additional, Schneider, N., additional, Arzoumanian, D., additional, Bontemps, S., additional, Attard, M., additional, Motte, F., additional, Didelon, P., additional, Maury, A., additional, Abergel, A., additional, Ali, B., additional, Baluteau, J.-P., additional, Bernard, J.-Ph., additional, Cambrésy, L., additional, Cox, P., additional, Di Francesco, J., additional, di Giorgio, A. M., additional, Griffin, M. J., additional, Hargrave, P., additional, Huang, M., additional, Kirk, J., additional, Li, J. Z., additional, Martin, P., additional, Minier, V., additional, Molinari, S., additional, Olofsson, G., additional, Pezzuto, S., additional, Russeil, D., additional, Roussel, H., additional, Saraceno, P., additional, Sauvage, M., additional, Sibthorpe, B., additional, Spinoglio, L., additional, Testi, L., additional, Ward-Thompson, D., additional, White, G., additional, Wilson, C. D., additional, Woodcraft, A., additional, and Zavagno, A., additional
Published: 2010
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25. TheHerschelfirst look at protostars in the Aquila rift

Author: Bontemps, S., primary, André, Ph., additional, Könyves, V., additional, Men'shchikov, A., additional, Schneider, N., additional, Maury, A., additional, Peretto, N., additional, Arzoumanian, D., additional, Attard, M., additional, Motte, F., additional, Minier, V., additional, Didelon, P., additional, Saraceno, P., additional, Abergel, A., additional, Baluteau, J.-P., additional, Bernard, J.-Ph., additional, Cambrésy, L., additional, Cox, P., additional, Di Francesco, J., additional, Di Giorgo, A. M., additional, Griffin, M., additional, Hargrave, P., additional, Huang, M., additional, Kirk, J., additional, Li, J., additional, Martin, P., additional, Merín, B., additional, Molinari, S., additional, Olofsson, G., additional, Pezzuto, S., additional, Prusti, T., additional, Roussel, H., additional, Russeil, D., additional, Sauvage, M., additional, Sibthorpe, B., additional, Spinoglio, L., additional, Testi, L., additional, Vavrek, R., additional, Ward-Thompson, D., additional, White, G., additional, Wilson, C., additional, Woodcraft, A., additional, and Zavagno, A., additional
Published: 2010
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26. The earliest phases of high-mass star formation: the NGC 6334-NGC 6357 complex

Author: Russeil, D., primary, Zavagno, A., additional, Motte, F., additional, Schneider, N., additional, Bontemps, S., additional, and Walsh, A. J., additional
Published: 2010
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27. Near-IR integral field spectroscopy of ionizing stars and young stellar objects on the borders of H II regions

Author: Martins, F., primary, Pomarès, M., additional, Deharveng, L., additional, Zavagno, A., additional, and Bouret, J. C., additional
Published: 2010
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28. Star formation triggered by the Galactic H II region RCW 120

Author: Marc Sauvage, L. Deharveng, Frédérique Motte, Alain Abergel, Sylvain Bontemps, J. A. Rodón, L. D. Anderson, J.-P. Baluteau, Annie Zavagno, Glenn J. White, Ph. André, D. Russeil, T. Hill, 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), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire 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), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), 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)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'Informatique de Nantes Atlantique (LINA), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), Engineering Department, University of Cambridge [UK] (CAM), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN)
Subjects: Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Star formation, Young stellar object, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Spire, Stars, Far infrared, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Protostar, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Low Mass, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: By means of different physical mechanisms, the expansion of HII regions can promote the formation of new stars of all masses. RCW 120 is a nearby Galactic HII region where triggered star formation occurs. This region is well-studied - there being a wealth of existing data - and is nearby. However, it is surrounded by dense regions for which far infrared data is essential to obtain an unbiased view of the star formation process and in particular to establish whether very young protostars are present. We attempt to identify all Young Stellar Objects (YSOs), especially those previously undetected at shorter wavelengths, to derive their physical properties and obtain insight into the star formation history in this region. We use Herschel-PACS and -SPIRE images to determine the distribution of YSOs observed in the field. We use a spectral energy distribution fitting tool to derive the YSOs physical properties. Herschel-PACS and -SPIRE images confirm the existence of a young source and allow us to determine its nature as a high-mass (8-10 MSun) Class 0 object (whose emission is dominated by a massive envelope) towards the massive condensation 1 observed at (sub)-millimeter wavelengths. This source was not detected at 24 micron and only barely seen in the MISPGAL 70 micron data. Several other red sources are detected at Herschel wavelengths and coincide with the peaks of the millimeter condensations. SED fitting results for the brightest Herschel sources indicate that, apart from the massive Class 0 that forms in condensation 1, young low mass stars are forming around RCW 120. The YSOs observed on the borders of RCW 120 are younger than its ionizing star, which has an age of about 2.5 Myr., 5 pqges, 3 figures, accepted by A&A (Special issue on the Herschel first results)
Published: 2010
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29. TheHerschelview of star formation in the Rosette molecular cloud under the influence of NGC 2244

Author: N. Schneider, F. Motte, S. Bontemps, M. Hennemann, J. Di Francesco, Ph. André, A. Zavagno, T. Csengeri, A. Men'shchikov, A. Abergel, J.-P. Baluteau, J.-Ph. Bernard, P. Cox, P. Didelon, A.-M. di Giorgio, R. Gastaud, M. Griffin, P. Hargrave, T. Hill, M. Huang, J. Kirk, V. Könyves, S. Leeks, J. Z. Li, A. Marston, P. Martin, V. Minier, S. Molinari, G. Olofsson, P. Panuzzo, P. Persi, S. Pezzuto, H. Roussel, D. Russeil, S. Sadavoy, P. Saraceno, M. Sauvage, B. Sibthorpe, L. Spinoglio, L. Testi, D. Teyssier, R. Vavrek, D. Ward-Thompson, G. White, C. D. Wilson, A. Woodcraft, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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 Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), 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), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Centre National d’Études Spatiales [Paris] (CNES), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), 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), 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), School of Physics and Astronomy [Cardiff], Cardiff University, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), CITA, University of Toronto, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Stockholm University, 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), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Royal Observatory Edinburgh (ROE), University of Edinburgh, Antarctic Research a European Network for Astrophysics (ARENA), Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, 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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), 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), Université Fédérale Toulouse Midi-Pyrénées, Consiglio Nazionale delle Ricerche (CNR), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), European Space Agency (ESA)-European Space Agency (ESA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and School of Physics and Astronomy
Subjects: Density gradient, Population, FOS: Physical sciences, Astrophysics, Spatial distribution, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, Radiative transfer, education, 010303 astronomy & astrophysics, QB, Physics, education.field_of_study, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Star formation, Molecular cloud, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy Astrophysics
Abstract: The Rosette molecular cloud is promoted as the archetype of a triggered star-formation site. This is mainly due to its morphology, because the central OB cluster NGC 2244 has blown a circular-shaped cavity into the cloud and the expanding HII-region now interacts with the cloud. Studying the spatial distribution of the different evolutionary states of all star-forming sites in Rosette and investigating possible gradients of the dust temperature will help to test the 'triggered star-formation' scenario in Rosette. We use continuum data obtained with the PACS (70 and 160 micron) and SPIRE instruments (250, 350, 500 micron) of the Herschel telescope during the Science Demonstration Phase of HOBYS. Three-color images of Rosette impressively show how the molecular gas is heated by the radiative impact of the NGC 2244 cluster. A clear negative temperature gradient and a positive density gradient (running from the HII-region/molecular cloud interface into the cloud) are detected. Studying the spatial distribution of the most massive dense cores (size scale 0.05 to 0.3 pc), we find an age-sequence (from more evolved to younger) with increasing distance to the cluster NGC 2244. No clear gradient is found for the clump (size-scale up to 1 pc) distribution. The existence of temperature and density gradients and the observed age-sequence imply that star formation in Rosette may indeed be influenced by the radiative impact of the central NGC 2244 cluster. A more complete overview of the prestellar and protostellar population in Rosette is required to obtain a firmer result., Letter in press for Astronomy & Astrophysics Herschel Special Issue
Published: 2010
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30. The earliest phases of high-mass star formation: the NGC 6334-NGC 6357 complex

Author: Andrew Walsh, D. Russeil, Frédérique Motte, Sylvain Bontemps, Nicola Schneider, Annie Zavagno, 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), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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 Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire de Probabilités et Modèles Aléatoires (LPMA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, and Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: 010504 meteorology & atmospheric sciences, Stellar mass, Infrared, Astrophysics, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, regions, Protostar, Basso continuo, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, stars: formation, extinction, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Star formation, Molecular cloud, Astronomy, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Stars, H ii, radio continuum: ISM, Space and Planetary Science, submillimeter: ISM, dust, radio lines: general
Abstract: International audience; Context. Our knowledge of high-mass star formation has been mainly based on follow-up studies of bright sources found by IRAS, and has thus been incomplete for its earliest phases, which are inconspicuous at infrared wavelengths. With a new generation of powerful bolometer arrays, unbiased large-scale surveys of nearby high-mass star-forming complexes now search for the high-mass analog of low-mass cores and class 0 protostars. Aims: Following the pioneering study of Cygnus X, we investigate the star-forming region NGC 6334-NGC 6357 (~1.7 kpc). Methods: We study the complex NGC 6334-NGC 6357 in an homogeneous way following the previous work of Motte and collaborators. We used the same method to extract the densest cores which are the most likely sites for high-mass star formation. We analyzed the SIMBA/SEST 1.2 mm data presented in Munoz and coworkers, which covers all high-column density areas (A v ≥ 15 mag) of the NGC 6334-NGC 6357 complex and extracted dense cores following the method used for Cygnus X. We constrain the properties of the most massive dense cores (M > 100 M_ȯ) using new molecular line observations (as SiO, N2H+,H13CO+, HCO+ (1-0) and CH3CN) with Mopra and a complete cross-correlation with infrared databases (MSX, GLIMPSE, MIPSGAL) and literature. Results: We extracted 163 massive dense cores of which 16 are more massive than 200 M_ȯ. These high-mass dense cores have a typical FWHM size of 0.37 pc, an average mass of M ~ 600 M_ȯ, and a volume-averaged density of ~ 1.5 × 105 cm-3. Among these massive dense cores, 6 are good candidates for hosting high-mass infrared-quiet protostars, 9 cores are classified as high-luminosity infrared protostars, and we find only one high-mass starless clump (~0.3 pc, ~ 4 × 104 cm-3) that is gravitationally bound. Conclusions: Since our sample is derived from a single molecular complex and covers every embedded phase of high-mass star formation, it provides a statistical estimate of the lifetime of massive stars. In contrast to what is found for low-mass class 0 and class I phases, the infrared-quiet protostellar phase of high-mass stars may last as long as their more well known high-luminosity infrared phase. As in Cygnus X, the statistical lifetime of high-mass protostars is shorter than found for nearby, low-mass star-forming regions which implies that high-mass pre-stellar and protostellar cores are in a dynamic state, as expected in a molecular cloud where turbulent and/or dynamical processes dominate. Based on observations made with Mopra telescope. The Mopra telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.Table 1 and Appendix are only available in electronic form at http://www.aanda.orgProfiles as FITS files are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/515/A55
Published: 2010
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31. ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

Author: Schuller, F., Menten, K. M., Contreras, Y., Wyrowski, F., Schilke, P., Bronfman, L., Henning, T., Walmsley, C. M., Beuther, H., Bontemps, S., Cesaroni, R., Deharveng, L., Garay, G., Herpin, F., Lefloch, B., Linz, H., Mardones, D., Minier, V., Molinari, S., Motte, F., Nyman, L.-Å., Reveret, V., Risacher, C., Russeil, D., Schneider, N., Testi, L., Troost, T., Vasyunina, T., Wienen, M., Zavagno, A., Kovacs, A., Kreysa, E., Siringo, G., Weiß, A., Schuller, F., Menten, K. M., Contreras, Y., Wyrowski, F., Schilke, P., Bronfman, L., Henning, T., Walmsley, C. M., Beuther, H., Bontemps, S., Cesaroni, R., Deharveng, L., Garay, G., Herpin, F., Lefloch, B., Linz, H., Mardones, D., Minier, V., Molinari, S., Motte, F., Nyman, L.-Å., Reveret, V., Risacher, C., Russeil, D., Schneider, N., Testi, L., Troost, T., Vasyunina, T., Wienen, M., Zavagno, A., Kovacs, A., Kreysa, E., Siringo, G., and Weiß, A.
Abstract: Context. Thanks to its excellent 5100 m high site in Chajnantor, the Atacama Pathfinder Experiment (APEX) systematically explores the southern sky at submillimeter wavelengths, in both continuum and spectral line emission. Studying continuum emission from interstellar dust is essential to locating the highest density regions in the interstellar medium, and deriving their masses, column densities, density structures, and large-scale morphologies. In particular, the early stages of (massive) star formation remain poorly understood, mainly because only small samples of high-mass proto-stellar or young stellar objects have been studied in detail so far.
Published: 2009
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32. Triggered star formation on the borders of the Galactic Hiiregion RCW 82

Author: Pomarès, M., Zavagno, A., Deharveng, L., Cunningham, M., Jones, P., Kurtz, S., Russeil, D., Caplan, J., Comerón, F., Pomarès, M., Zavagno, A., Deharveng, L., Cunningham, M., Jones, P., Kurtz, S., Russeil, D., Caplan, J., and Comerón, F.
Abstract: Context. We are engaged in a multi-wavelength study of several Galactic H iiregions that exhibit signposts of triggered star formation on their borders, where the collect and collapse process could be at work.
Published: 2009
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33. Triggered star formation on the borders of the Galactic H iiregion RCW 120 ***

Author: Zavagno, A., Pomarès, M., Deharveng, L., Hosokawa, T., Russeil, D., Caplan, J., Zavagno, A., Pomarès, M., Deharveng, L., Hosokawa, T., Russeil, D., and Caplan, J.
Abstract: Context.To investigate the process of star formation triggered by the expansion of an H iiregion, we present a multi-wavelength analysis of the Galactic H iiregion RCW 120 and its surroundings. The collect and collapse model predicts that the layer of gas and dust accumulated between the ionization and shock fronts during the expansion of the H iiregion collapses and forms dense fragments, giving rise to potential sites of massive-star formation.
Published: 2007
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34. Triggered massive-star formation on the borders of Galactic H II regions

Author: Deharveng, L., Lefloch, B., Massi, F., Brand, J., Kurtz, S., Zavagno, A., Caplan, J., Deharveng, L., Lefloch, B., Massi, F., Brand, J., Kurtz, S., Zavagno, A., and Caplan, J.
Abstract: Context.Massive-star formation triggered by the expansion of H iiregions.
Published: 2006
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35. Triggered massive-star formation on the borders of Galactic H II regions

Author: Zavagno, A., Deharveng, L., Comerón, F., Brand, J., Massi, F., Caplan, J., Russeil, D., Zavagno, A., Deharveng, L., Comerón, F., Brand, J., Massi, F., Caplan, J., and Russeil, D.
Abstract: We present SEST-SIMBA 1.2-mm continuum maps and ESO-NTT SOFI JHKSimages of the Galactic H iiregion RCW 79. The millimetre continuum data reveal the presence of massive fragments located in a dust emission ring surrounding the ionized gas. The two most massive fragments are diametrically opposite each other in the ring. The near-IR data, centred on the compact H iiregion located at the south-eastern border of RCW 79, show the presence of an IR-bright cluster containing massive stars along with young stellar objects with near-IR excesses. A bright near- and mid-IR source is detected towards maser emissions, 1.2 pc north-east of the compact H iiregion centre. Additional information extracted from the Spitzer GLIMPSE survey is used to discuss the nature of the bright IR sources observed towards RCW 79. Twelve luminous Class I sources are identified towards the most massive millimetre fragments. All these facts strongly indicate that the massive-star formation observed at the border of the H iiregion RCW 79 has been triggered by its expansion, most probably by the collect and collapse process.
Published: 2006
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36. Triggered massive-star formation at the border of the HIIregion Sh 104

Author: Deharveng, L., Lefloch, B., Zavagno, A., Caplan, J., Whitworth, A. P., Nadeau, D., Martín, S., Deharveng, L., Lefloch, B., Zavagno, A., Caplan, J., Whitworth, A. P., Nadeau, D., and Martín, S.
Abstract: We present millimetre-line imaging of the Galactic H iiregion Sh 104. We show that it is surrounded by a ring of molecular gas and dust. Four large molecular condensations are regularly spaced around the ring. These condensations are themselves fragmented and contain several massive dense cores. A deeply embedded cluster is observed in the near IR towards the largest condensation. It contains at least one massive star ionizing an ultra-compact H iiregion. The Sh 104 region is a good illustration of the “collect and collapse” model for star formation triggered by the expansion of an H iiregion.
Published: 2003
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37. Near-infrared imaging of RAFGL7009S*

Author: Zavagno, A., Deharveng, L., Nadeau, D., Caplan, J., Zavagno, A., Deharveng, L., Nadeau, D., and Caplan, J.
Abstract: RAFGL7009S is a deeply embedded massive young stellar objet (YSO) showing strong ice and saturated silicate absorption features in the mid infrared. It is associated with the ultracompact H iiregion G25.65+1.05, which may be excited by a B1V star. We have obtained JHKimages of a $1\arcmin$field centred on this YSO. In Kwe detect a non-resolved object coinciding with the radio continuum emission peak. Considering the high extinction towards this source ($A_V \geq $100 mag), the observed Kemission is more than 7 mag in excess of that expected for a B1V star. We suggest that this emission is mainly due to scattering of the central zone emission, as recently found for a sample of embedded massive YSOs associated with 3.1 μm H2O ice absorption (Ishii et al. [CITE]). We estimate the YSO's age to be 2$\times$104years. The outflow, the methanol maser emission and the strong ice absorption features suggest the presence of a dense medium very close to the star, possibly a disk.
Published: 2002
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38. ISOCAM 3-12 μm imaging of five galactic compact Hiiregions *

Author: Zavagno, A., Ducci, V., Zavagno, A., and Ducci, V.
Abstract: We present 3-12 μm ISOCAM observations of the five Galactic compact H iiregions Sh 61, Sh 138, Sh 152, Sh 156 and Sh 186. The unidentified infrared bands (UIBs) centred at 3.3, 6.2, 7.7, 8.6 and 11.2 μm -and underlying continuum -are imaged using the SW1, SW2, LW4, LW6 and LW8 filters. Images are also obtained at 5.985, 6.911, 8.222, 10.520 and 12.000 μm using the circular variable filter (CVF). We show that the 5.985 μm emission represents a true continuum reference for the 6.2 μm band, allowing a derivation of this band's properties. Due to uncertainties in the continuum estimates, only lower limits can be given for the 3.3, 7.7 and 11.3 μm band fluxes. These limits agree with previous results found in the literature. The distribution of the bands coincide. The 3.3 μm emission is not observed in high extinction zones, suggesting a lower temperature of the carriers and/or a higher abundance of larger molecules in those zones. The 6.2 μm band emission peaks outside the ionized zone, in the photodissociation region. The 6.2 μm band luminosity correlates with the far UV field intensity, suggesting a UV excitation. We also find a correlation between the spatial distribution of the 6.2 μm band emission and zones of strong 2.122 μm H2emission due to ultraviolet fluorescence. This suggests that both emissions are due to UV excitation. The 6.2 μm emission is slightly closer to the exciting star. This suggests that the band carriers survive in the H izone. The 12 μm emission traces the continuum emission from very small grains, when present, and follows well the distribution of UIB emission. This suggests a link between the two emission carriers. The emission peak observed on the star in Sh 61 and Sh 156 indicates that the continuum from very small grains dominates the emission in highly excited regions.
Published: 2001
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39. Star formation around RCW 120, the perfect bubble

Author: Deharveng, L., Zavagno, A., Schuller, F., Caplan, J., Pomar?s, M., and De Breuck, C.
Abstract: Context. This study deals with the star formation triggered by H?ii?regions.Aims. We wish to take advantage of the very simple morphology of RCW?120?? a perfect bubble?? to understand the mechanisms triggering star formation around an H?ii?region and to establish what kind of stars are formed there.Methods. We present 870??m observations of RCW?120, obtained with the APEX-LABOCA camera. These show the distribution of cold dust, and thus of neutral material. We use Spitzer-MIPS observations at 24??m and 70??m to detect the young stellar objects present in this region and to estimate their evolutionary stages.Results. A layer of dense neutral material surrounds the entire H?ii?region, having been swept up during the region's expansion. This layer has a mass greater than 2000?M?and is fragmented, with massive fragments elongated along the ionization front?(IF). We measured the 24??m flux of 138?sources. Of these, 39 are Class?I or flat-spectrum young stellar objects (YSOs) observed in the direction of the collected layer. We show that several triggering mechanisms are acting simultaneously in the swept-up shell, where they form a second generation of stars. No massive YSOs are detected. However, a massive, compact 870??m core lies adjacent to the IF.?A 70??m source with no 24??m counterpart is detected at the same position. This source is a likely candidate for a Class?0 YSO. Also at 24??m, we detect a chain of about ten regularly spaced Class?I or flat spectrum sources, parallel to the IF, in the direction of the most massive fragment. We suggest that the formation of these YSOs is the result of Jeans gravitational instabilities in the collected layer. Finally, the 870??m emission, the 24??m emission, and the H??emission show the existence of an extended and partially ionized photodissociation region around RCW?120. This demonstrates the long-distance influence of the H?ii?region upon its surrounding medium.
Published: 2009

40. Triggered massive-star formation on the borders of Galactic H?II?regions

Author: Deharveng, L., Lefloch, B., Kurtz, S., Nadeau, D., Pomar?s, M., Caplan, J., and Zavagno, A.
Abstract: Aims. We wish to establish whether sequential star formation is taking place at the periphery of the Galactic H?ii?region Sh2-212.Methods. We present CO millimetre observations of this region obtained at the IRAM 30-m telescope to investigate the distribution of associated molecular material. We also use deep JHK observations obtained at the CFHT to study the stellar content of the region, and radio observations obtained at the VLA to look for the presence of an ultra-compact (UC) H?ii?region and for maser emission.Results. In the optical, Sh2-212 is spherically symmetric around its central exciting cluster. This H?ii?region is located along a molecular filament. A thin, well-defined half ring of molecular material surrounds the brightest part of the H?ii?region at the rear and is fragmented. The most massive fragment (~200?M?) contains a massive young stellar object displaying a near-IR excess; its spectral energy distribution indicates a high-mass (~14?M?), high-temperature (~30?000?K), and high-luminosity (~17?000?L?) source. This object ionizes a UC H?ii?region.Conclusions. Sh2-212 is a good example of massive-star formation triggered via the collect and collapse process. The massive YSO observed at its periphery is a good candidate for a massive star formed in isolation.
Published: 2008

41. Triggered massive-star formation on the borders of Galactic H II regions

Author: L. Deharveng, A. Zavagno, and J. Caplan
Abstract: Young massive stars or clusters are often observed at the peripheries of H ii regions. What triggers star formation at such locations? Among the scenarios that have been proposed, the collect and collapse process is particularly attractive because it permits the formation of massive objects via the fragmentation of the dense shocked layer of neutral gas surrounding the expanding ionized zone. However, until our recent article on Sh 104, it had not been convincingly demonstrated that this process actually takes place. In the present paper we present our selection of seventeen candidate regions for this process; all show high-luminosity near-IR clusters and/or mid-IR point sources at their peripheries. The reality of a collect and collapse origin of these presumably second-generation stars and clusters will be discussed in forthcoming papers, using new near-IR and millimetre observations.
Published: 2005

42. The Herschel⋆view of massive star formation in G035.39–00.33: dense and cold filament of W48 undergoing a mini-starburst⋆⋆

Author: Nguyên Luong, Q., Motte, F., Hennemann, M., Hill, T., Rygl, K. L. J., Schneider, N., Bontemps, S., Men’shchikov, A., André, Ph., Peretto, N., Anderson, L. D., Arzoumanian, D., Deharveng, L., Didelon, P., Di Francesco, J., Griffin, M. J., Kirk, J. M., Könyves, V., Martin, P. G., Maury, A., Minier, V., Molinari, S., Pestalozzi, M., Pezzuto, S., Reid, M., Roussel, H., Sauvage, M., Schuller, F., Testi, L., Ward-Thompson, D., White, G. J., and Zavagno, A.
Abstract: The filament IRDC G035.39–00.33 in the W48 molecular complex is one of the darkest infrared clouds observed by Spitzer. It has been observed by the PACS (70 and 160 μm) and SPIRE (250, 350, and 500 μm) cameras of the Herschel Space Observatory as part of the W48 molecular cloud complex in the framework of the HOBYS key programme. The observations reveal a sample of 28 compact sources (deconvolved FWHM sizes < 0.3 pc) complete down to ~5 M⊙in G035.39–00.33 and its surroundings. Among them, 13 compact sources are massive dense cores with masses >20 M⊙. The cloud characteristics we derive from the analysis of their spectral energy distributions are masses of 20−50 M⊙, sizes of 0.1–0.2 pc, and average densities of 2−20 × 105cm-3, which make these massive dense cores excellent candidates to form intermediate- to high-mass stars. Most of the massive dense cores are located inside the G035.39–00.33 ridge and host IR-quiet high-mass protostars. The large number of protostars found in this filament suggests that we are witnessing a mini-burst of star formation with an efficiency of ~15% and a rate density of ~40 M⊙yr-1kpc-2within ~8 pc2, a large area covering the full ridge. Part of the extended SiO emission observed towards G035.39–00.33 is not associated with obvious protostars and may originate from low-velocity shocks within converging flows, as advocated by previous studies.
Published: 2011
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43. Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites⋆⋆⋆

Author: Hill, T., Motte, F., Didelon, P., Bontemps, S., Minier, V., Hennemann, M., Schneider, N., André, Ph., Men‘shchikov, A., Anderson, L. D., Arzoumanian, D., Bernard, J.-P., di Francesco, J., Elia, D., Giannini, T., Griffin, M. J., Könyves, V., Kirk, J., Marston, A. P., Martin, P. G., Molinari, S., Nguyen Luong, Q., Peretto, N., Pezzuto, S., Roussel, H., Sauvage, M., Sousbie, T., Testi, L., Ward-Thompson, D., White, G. J., Wilson, C. D., and Zavagno, A.
Abstract: We present the first HerschelPACS and SPIRE results of the Vela C molecular complex in the far-infrared and submillimetre regimes at 70, 160, 250, 350, and 500 μm, spanning the peak of emission of cold prestellar or protostellar cores. Column density and multi-resolution analysis (MRA) differentiates the Vela C complex into five distinct sub-regions. Each sub-region displays differences in their column density and temperature probability distribution functions (PDFs), in particular, the PDFs of the “Centre-Ridge” and “South-Nest” sub-regions appear in stark contrast to each other. The Centre-Ridge displays a bimodal temperature PDF representative of hot gas surrounding the HII region RCW 36 and the cold neighbouring filaments, whilst the South-Nest is dominated by cold filamentary structure. The column density PDF of the Centre-Ridge is flatter than the South-Nest, with a high column density tail, consistent with formation through large-scale flows, and regulation by self-gravity. At small to intermediate scales MRA indicates the Centre-Ridge to be twice as concentrated as the South-Nest, whilst on larger scales, a greater portion of the gas in the South-Nest is dominated by turbulence than in the Centre-Ridge. In Vela C, high-mass stars appear to be preferentially forming in ridges, i.e., dominant high column density filaments.
Published: 2011
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44. Characterizing interstellar filaments with Herschel in IC 5146 ⋆⋆⋆

Author: Arzoumanian, D., André, Ph., Didelon, P., Könyves, V., Schneider, N., Men’shchikov, A., Sousbie, T., Zavagno, A., Bontemps, S., Di Francesco, J., Griffin, M., Hennemann, M., Hill, T., Kirk, J., Martin, P., Minier, V., Molinari, S., Motte, F., Peretto, N., Pezzuto, S., Spinoglio, L., Ward-Thompson, D., White, G., and Wilson, C. D.
Abstract: We provide a first look at the results of the HerschelGould Belt survey toward the IC 5146 molecular cloud and present a preliminary analysis of the filamentary structure in this region. The column density map, derived from our 70–500 μm Herscheldata, reveals a complex network of filaments and confirms that these filaments are the main birth sites of prestellar cores. We analyze the column density profiles of 27 filaments and show that the underlying radial density profiles fall off as r-1.5to r-2.5at large radii. Our main result is that the filaments seem to be characterized by a narrow distribution of widths with a median value of 0.10 ± 0.03 pc, which is in stark contrast to a much broader distribution of central Jeans lengths. This characteristic width of ~0.1 pc corresponds to within a factor of ~2 to the sonic scale below which interstellar turbulence becomes subsonic in diffuse gas, which supports the argument that the filaments may form as a result of the dissipation of large-scale turbulence.
Published: 2011
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45. Triggered star formation at the borders of the H ii region Sh 2-217 ⋆

Author: Brand, J., Massi, F., Zavagno, A., Deharveng, L., and Lefloch, B.
Abstract: Context.This paper is part of our ongoing study of star formation at the borders of Galactic H iiregions. In this paper, we report our observations and analysis of Sharpless 217 (Sh 2-217).
Published: 2011
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46. Galactic cold cores

Author: Juvela, M., Ristorcelli, I., Pelkonen, V.-M., Marshall, D. J., Montier, L. A., Bernard, J.-P., Paladini, R., Lunttila, T., Abergel, A., André, Ph., Dickinson, C., Dupac, X., Malinen, J., Martin, P., McGehee, P., Pagani, L., Ysard, N., and Zavagno, A.
Abstract: Context.Within the project Galacticcoldcoreswe are carrying out Herschel photometric observations of cold interstellar clouds detected with the Planck satellite. The three fields observed as part of the Herschel science demonstration phase (SDP) provided the first glimpse into the nature of these sources. The aim of the project is to derive the physical properties of the full cold core population revealed by Planck.
Published: 2011
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47. Giving physical significance to the Hi-GAL data: determining the distance of cold dusty cores in the Milky Way⋆⋆⋆

Author: Russeil, D., Pestalozzi, M., Mottram, J. C., Bontemps, S., Anderson, L. D., Zavagno, A., Beltrán, M. T., Bally, J., Brand, J., Brunt, C., Cesaroni, R., Joncas, G., Marshall, D., Martin, P., Massi, F., Molinari, S., Moore, T., Noriega-Crespo, A., Olmi, L., Thompson, M. A., Wienen, M., and Wyrowski, F.
Abstract: Context.Hi-GAL, an open time key-project of the Herschel satellite, was awarded 343 hours observing time to carry out a 5-band photometric imaging survey at 70, 160, 250, 350, and 500 μm of a |b| ≤ 1° wide strip of the Milky Way Galactic plane in the longitude range −70° ≤ l≤ 70°. Two 2° × 2° fields centred at l= 30° and l= 59° have been observed with the SPIRE and PACS photometric cameras in parallel mode during the Herschel science demonstration phase (SDP). From the images, compact sources are extracted for which the distance must be established in order to determine their physical properties.
Published: 2011
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48. A gallery of bubbles

Author: Deharveng, L., Schuller, F., Anderson, L. D., Zavagno, A., Wyrowski, F., Menten, K. M., Bronfman, L., Testi, L., Walmsley, C. M., and Wienen, M.
Abstract: Context.This study deals with infrared bubbles, the H iiregions they enclose, and triggered massive-star formation on their borders.
Published: 2010
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49. The physical properties of the dust in the RCW 120 H iiregion as seen by Herschel*

Author: Anderson, L. D., Zavagno, A., Rodón, J. A., Russeil, D., Abergel, A., Ade, P., André, P., Arab, H., Baluteau, J.-P., Bernard, J.-P., Blagrave, K., Bontemps, S., Boulanger, F., Cohen, M., Compiègne, M., Cox, P., Dartois, E., Davis, G., Emery, R., Fulton, T., Gry, C., Habart, E., Huang, M., Joblin, C., Jones, S. C., Kirk, J. M., Lagache, G., Lim, T., Madden, S., Makiwa, G., Martin, P., Miville-Deschênes, M.-A., Molinari, S., Moseley, H., Motte, F., Naylor, D. A., Okumura, K., Pinheiro Gonçalves, D., Polehampton, E., Saraceno, P., Sauvage, M., Sidher, S., Spencer, L., Swinyard, B., Ward-Thompson, D., and White, G. J.
Abstract: Context. RCW 120 is a well-studied, nearby Galactic H iiregion with ongoing star formation in its surroundings. Previous work has shown that it displays a bubble morphology at mid-infrared wavelengths, and has a massive layer of collected neutral material seen at sub-mm wavelengths. Given the well-defined photo-dissociation region (PDR) boundary and collected layer, it is an excellent laboratory to study the “collect and collapse” process of triggered star formation. Using HerschelSpace Observatory data at 100, 160, 250, 350, and 500 μm, in combination with Spitzerand APEX-LABOCA data, we can for the first time map the entire spectral energy distribution of an H iiregion at high angular resolution.Aims. We seek a better understanding of RCW 120 and its local environment by analysing its dust temperature distribution. Additionally, we wish to understand how the dust emissivity index, β, is related to the dust temperature.Methods. We determine dust temperatures in selected regions of the RCW 120 field by fitting their spectral energy distribution (SED), derived using aperture photometry. Additionally, we fit the SED extracted from a grid of positions to create a temperature map.Results. We find a gradient in dust temperature, ranging from $\ga$30 K in the interior of RCW 120, to ~20 K for the material collected in the PDR, to ~10 K toward local infrared dark clouds and cold filaments. There is an additional, hotter (~100 K) component to the dust emission that we do not investigate here. Our results suggest that RCW 120 is in the process of destroying the PDR delineating its bubble morphology. The leaked radiation from its interior may influence the creation of the next generation of stars. We find support for an anti-correlation between the fitted temperature and β, in rough agreement with what has been found previously. The extended wavelength coverage of the Herscheldata greatly increases the reliability of this result.
Published: 2010

50. From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the HerschelGould 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., Le Pennec, J., Li, J. Z., Martin, P. G., 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.
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 μm 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 ~300 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 Herschelresults 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.
Published: 2010

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