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31 results on '"Doty S"'

1. Herschel/HIFI spectroscopy of the intermediate mass protostar NGC 7129 FIRS 2

Author

Johnstone, D., primary, Fich, M., additional, McCoey, C., additional, van Kempen, T. A., additional, Fuente, A., additional, Kristensen, L. E., additional, Cernicharo, J., additional, Caselli, P., additional, Visser, R., additional, Plume, R., additional, Herczeg, G. J., additional, van Dishoeck, E. F., additional, Wampfler, S., additional, Bachiller, R., additional, Baudry, A., additional, Benedettini, M., additional, Bergin, E., additional, Benz, A. O., additional, Bjerkeli, P., additional, Blake, G., additional, Bontemps, S., additional, Braine, J., additional, Bruderer, S., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Doty, S. D., additional, Encrenaz, P., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herpin, F., additional, Hogerheijde, M. R., additional, Jacq, T., additional, Jørgensen, J. K., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, Marseille, M., additional, Melnick, G., additional, Neufeld, D., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Pearson, J., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Shipman, R., additional, Tafalla, M., additional, van der Tak, F., additional, Wyrowski, F., additional, Yıldız, U. A., additional, Caux, E., additional, Honingh, N., additional, Jellema, W., additional, Schieder, R., additional, Teyssier, D., additional, and Whyborn, N., additional

Published
2010
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2. Herschel/HIFI observations of high-JCO lines in the NGC 1333 low-mass star-forming region

Author

Yıldız, U. A., primary, van Dishoeck, E. F., additional, Kristensen, L. E., additional, Visser, R., additional, Jørgensen, J. K., additional, Herczeg, G. J., additional, van Kempen, T. A., additional, Hogerheijde, M. R., additional, Doty, S. D., additional, Benz, A. O., additional, Bruderer, S., additional, Wampfler, S. F., additional, Deul, E., additional, Bachiller, R., additional, Baudry, A., additional, Benedettini, M., additional, Bergin, E., additional, Bjerkeli, P., additional, Blake, G. A., additional, Bontemps, S., additional, Braine, J., additional, Caselli, P., additional, Cernicharo, J., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herpin, F., additional, Jacq, T., additional, Johnstone, D., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, Liu, F.-C., additional, Marseille, M., additional, McCoey, C., additional, Melnick, G., additional, Neufeld, D., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Shipman, R., additional, Tafalla, M., additional, Tielens, A. G. G. M., additional, van der Tak, F., additional, Wyrowski, F., additional, Dieleman, P., additional, Jellema, W., additional, Ossenkopf, V., additional, Schieder, R., additional, and Stutzki, J., additional

Published
2010
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3. Herschel/HIFI detections of hydrides towards AFGL 2591

Author

Bruderer, S., primary, Benz, A. O., additional, van Dishoeck, E. F., additional, Melchior, M., additional, Doty, S. D., additional, van der Tak, F., additional, Stäuber, P., additional, Wampfler, S. F., additional, Dedes, C., additional, Yıldız, U. A., additional, Pagani, L., additional, Giannini, T., additional, de Graauw, Th., additional, Whyborn, N., additional, Teyssier, D., additional, Jellema, W., additional, Shipman, R., additional, Schieder, R., additional, Honingh, N., additional, Caux, E., additional, Bächtold, W., additional, Csillaghy, A., additional, Monstein, C., additional, Bachiller, R., additional, Baudry, A., additional, Benedettini, M., additional, Bergin, E., additional, Bjerkeli, P., additional, Blake, G. A., additional, Bontemps, S., additional, Braine, J., additional, Caselli, P., additional, Cernicharo, J., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Goicoechea, J. R., additional, Helmich, F., additional, Herczeg, G. J., additional, Herpin, F., additional, Hogerheijde, M. R., additional, Jacq, T., additional, Johnstone, D., additional, Jørgensen, J. K., additional, Kristensen, L. E., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, Marseille, M., additional, McCoey, C., additional, Melnick, G., additional, Neufeld, D., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Tafalla, M., additional, van Kempen, T. A., additional, Visser, R., additional, and Wyrowski, F., additional

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2010
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4. Variations in H2O+/H2O ratios toward massive star-forming regions

Author

Wyrowski, F., primary, van der Tak, F., additional, Herpin, F., additional, Baudry, A., additional, Bontemps, S., additional, Chavarria, L., additional, Frieswijk, W., additional, Jacq, T., additional, Marseille, M., additional, Shipman, R., additional, van Dishoeck, E. F, additional, Benz, A. O., additional, Caselli, P., additional, Hogerheijde, M. R., additional, Johnstone, D., additional, Liseau, R., additional, Bachiller, R., additional, Benedettini, M., additional, Bergin, E., additional, Bjerkeli, P., additional, Blake, G., additional, Braine, J., additional, Bruderer, S., additional, Cernicharo, J., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Doty, S. D., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herczeg, G. J., additional, Jørgensen, J. K., additional, Kristensen, L. E., additional, Larsson, B., additional, Lis, D., additional, McCoey, C., additional, Melnick, G., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Santiago, J., additional, Saraceno, P., additional, Tafalla, M., additional, van Kempen, T. A., additional, Visser, R., additional, Wampfler, S., additional, Yıldız, U. A., additional, Black, J. H., additional, Falgarone, E., additional, Gerin, M., additional, Roelfsema, P., additional, Dieleman, P., additional, Beintema, D., additional, De Jonge, A., additional, Whyborn, N., additional, Stutzki, J., additional, and Ossenkopf, V., additional

Published
2010
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5. Herschelobservations of the hydroxyl radical (OH) in young stellar objects

Author

Wampfler, S. F., primary, Herczeg, G. J., additional, Bruderer, S., additional, Benz, A. O., additional, van Dishoeck, E. F., additional, Kristensen, L. E., additional, Visser, R., additional, Doty, S. D., additional, Melchior, M., additional, van Kempen, T. A., additional, Yıldız, U. A., additional, Dedes, C., additional, Goicoechea, J. R., additional, Baudry, A., additional, Melnick, G., additional, Bachiller, R., additional, Benedettini, M., additional, Bergin, E., additional, Bjerkeli, P., additional, Blake, G. A., additional, Bontemps, S., additional, Braine, J., additional, Caselli, P., additional, Cernicharo, J., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Giannini, T., additional, de Graauw, Th., additional, Helmich, F., additional, Herpin, F., additional, Hogerheijde, M. R., additional, Jacq, T., additional, Johnstone, D., additional, Jørgensen, J. K., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, Marseille, M., additional, Mc Coey, C., additional, Neufeld, D., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Shipman, R., additional, Tafalla, M., additional, van der Tak, F. F. S., additional, Wyrowski, F., additional, Roelfsema, P., additional, Jellema, W., additional, Dieleman, P., additional, Caux, E., additional, and Stutzki, J., additional

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2010
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6. Water abundances in high-mass protostellar envelopes:Herschelobservations with HIFI

Author

Marseille, M. G., primary, van der Tak, F. F. S., additional, Herpin, F., additional, Wyrowski, F., additional, Chavarría, L., additional, Pietropaoli, B., additional, Baudry, A., additional, Bontemps, S., additional, Cernicharo, J., additional, Jacq, T., additional, Frieswijk, W., additional, Shipman, R., additional, van Dishoeck, E. F., additional, Bachiller, R., additional, Benedettini, M., additional, Benz, A. O., additional, Bergin, E., additional, Bjerkeli, P., additional, Blake, G. A., additional, Braine, J., additional, Bruderer, S., additional, Caselli, P., additional, Caux, E., additional, Codella, C., additional, Daniel, F., additional, Dieleman, P., additional, di Giorgio, A. M., additional, Dominik, C., additional, Doty, S. D., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Gaier, T., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herczeg, G. J., additional, Hogerheijde, M. R., additional, Jackson, B., additional, Javadi, H., additional, Jellema, W., additional, Johnstone, D., additional, Jørgensen, J. K., additional, Kester, D., additional, Kristensen, L. E., additional, Larsson, B., additional, Laauwen, W., additional, Lis, D., additional, Liseau, R., additional, Luinge, W., additional, McCoey, C., additional, Megej, A., additional, Melnick, G., additional, Neufeld, D., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Roelfsema, P., additional, Santiago-García, J., additional, Saraceno, P., additional, Siegel, P., additional, Stutzki, J., additional, Tafalla, M., additional, van Kempen, T. A., additional, Visser, R., additional, Wampfler, S. F., additional, and Yıldız, U. A., additional

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2010
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7. Hydrides in young stellar objects: Radiation tracers in a protostar-disk-outflow system

Author

Benz, A. O., primary, Bruderer, S., additional, van Dishoeck, E. F., additional, Stäuber, P., additional, Wampfler, S. F., additional, Melchior, M., additional, Dedes, C., additional, Wyrowski, F., additional, Doty, S. D., additional, van der Tak, F., additional, Bächtold, W., additional, Csillaghy, A., additional, Megej, A., additional, Monstein, C., additional, Soldati, M., additional, Bachiller, R., additional, Baudry, A., additional, Benedettini, M., additional, Bergin, E., additional, Bjerkeli, P., additional, Blake, G. A., additional, Bontemps, S., additional, Braine, J., additional, Caselli, P., additional, Cernicharo, J., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dieleman, P., additional, Dominik, C., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herczeg, G. J., additional, Herpin, F., additional, Hogerheijde, M. R., additional, Jacq, T., additional, Jellema, W., additional, Johnstone, D., additional, Jørgensen, J. K., additional, Kristensen, L. E., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, Marseille, M., additional, McCoey, C., additional, Melnick, G., additional, Neufeld, D., additional, Nisini, B., additional, Olberg, M., additional, Ossenkopf, V., additional, Parise, B., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Schieder, R., additional, Shipman, R., additional, Stutzki, J., additional, Tafalla, M., additional, Tielens, A. G. G. M., additional, van Kempen, T. A., additional, Visser, R., additional, and Yıldız, U. A., additional

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2010
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8. Water in low-mass star-forming regions withHerschel

Author

Kristensen, L. E., primary, Visser, R., additional, van Dishoeck, E. F., additional, Yıldız, U. A., additional, Doty, S. D., additional, Herczeg, G. J., additional, Liu, F.-C., additional, Parise, B., additional, Jørgensen, J. K., additional, van Kempen, T. A., additional, Brinch, C., additional, Wampfler, S. F., additional, Bruderer, S., additional, Benz, A. O., additional, Hogerheijde, M. R., additional, Deul, E., additional, Bachiller, R., additional, Baudry, A., additional, Benedettini, M., additional, Bergin, E. A., additional, Bjerkeli, P., additional, Blake, G. A., additional, Bontemps, S., additional, Braine, J., additional, Caselli, P., additional, Cernicharo, J., additional, Codella, C., additional, Daniel, F., additional, de Graauw, Th., additional, di Giorgio, A. M., additional, Dominik, C., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Giannini, T., additional, Goicoechea, J. R., additional, Helmich, F., additional, Herpin, F., additional, Jacq, T., additional, Johnstone, D., additional, Kaufman, M. J., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, Marseille, M., additional, McCoey, C., additional, Melnick, G., additional, Neufeld, D., additional, Nisini, B., additional, Olberg, M., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Shipman, R., additional, Tafalla, M., additional, Tielens, A. G. G. M., additional, van der Tak, F., additional, Wyrowski, F., additional, Beintema, D., additional, de Jonge, A., additional, Dieleman, P., additional, Ossenkopf, V., additional, Roelfsema, P., additional, Stutzki, J., additional, and Whyborn, N., additional

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2010
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9. Sensitive limits on the abundance of cold water vapor in the DM Tauri protoplanetary disk

Author

Bergin, E. A., primary, Hogerheijde, M. R., additional, Brinch, C., additional, Fogel, J., additional, Yıldız, U. A., additional, Kristensen, L. E., additional, van Dishoeck, E. F., additional, Bell, T. A., additional, Blake, G. A., additional, Cernicharo, J., additional, Dominik, C., additional, Lis, D., additional, Melnick, G., additional, Neufeld, D., additional, Panić, O., additional, Pearson, J. C., additional, Bachiller, R., additional, Baudry, A., additional, Benedettini, M., additional, Benz, A. O., additional, Bjerkeli, P., additional, Bontemps, S., additional, Braine, J., additional, Bruderer, S., additional, Caselli, P., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Doty, S. D., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herczeg, G. J., additional, Herpin, F., additional, Jacq, T., additional, Johnstone, D., additional, Jørgensen, J. K., additional, Larsson, B., additional, Liseau, R., additional, Marseille, M., additional, Mc Coey, C., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Plume, R., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Shipman, R., additional, Tafalla, M., additional, van Kempen, T. A., additional, Visser, R., additional, Wampfler, S. F., additional, Wyrowski, F., additional, van der Tak, F., additional, Jellema, W., additional, Tielens, A. G. G. M., additional, Hartogh, P., additional, Stützki, J., additional, and Szczerba, R., additional

Published
2010
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10. Water in massive star-forming regions: HIFI observations of W3 IRS5

Author

Chavarría, L., primary, Herpin, F., additional, Jacq, T., additional, Braine, J., additional, Bontemps, S., additional, Baudry, A., additional, Marseille, M., additional, van der Tak, F., additional, Pietropaoli, B., additional, Wyrowski, F., additional, Shipman, R., additional, Frieswijk, W., additional, van Dishoeck, E. F., additional, Cernicharo, J., additional, Bachiller, R., additional, Benedettini, M., additional, Benz, A. O., additional, Bergin, E., additional, Bjerkeli, P., additional, Blake, G. A., additional, Bruderer, S., additional, Caselli, P., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Doty, S. D., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Hartogh, P., additional, Helmich, F., additional, Herczeg, G. J., additional, Hogerheijde, M. R., additional, Johnstone, D., additional, Jørgensen, J. K., additional, Kristensen, L. E., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, McCoey, C., additional, Melnick, G., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Stutzki, J., additional, Szczerba, R., additional, Tafalla, M., additional, Tielens, A., additional, van Kempen, T. A., additional, Visser, R., additional, Wampfler, S. F., additional, Willem, J., additional, and Yıldız, U. A., additional

Published
2010
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11. Water vapor toward starless cores: TheHerschelview

Author

Caselli, P., primary, Keto, E., additional, Pagani, L., additional, Aikawa, Y., additional, Yıldız, U. A., additional, van der Tak, F. F. S., additional, Tafalla, M., additional, Bergin, E. A., additional, Nisini, B., additional, Codella, C., additional, van Dishoeck, E. F., additional, Bachiller, R., additional, Baudry, A., additional, Benedettini, M., additional, Benz, A. O., additional, Bjerkeli, P., additional, Blake, G. A., additional, Bontemps, S., additional, Braine, J., additional, Bruderer, S., additional, Cernicharo, J., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Doty, S. D., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Gaier, T., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herczeg, G. J., additional, Herpin, F., additional, Hogerheijde, M. R., additional, Jackson, B., additional, Jacq, T., additional, Javadi, H., additional, Johnstone, D., additional, Jørgensen, J. K., additional, Kester, D., additional, Kristensen, L. E., additional, Laauwen, W., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, Luinge, W., additional, Marseille, M., additional, McCoey, C., additional, Megej, A., additional, Melnick, G., additional, Neufeld, D., additional, Olberg, M., additional, Parise, B., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Shipman, R., additional, Siegel, P., additional, van Kempen, T. A., additional, Visser, R., additional, Wampfler, S. F., additional, and Wyrowski, F., additional

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2010
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12. Herschel-PACS spectroscopy of the intermediate mass protostar NGC 7129 FIRS 2

Author

Fich, M., primary, Johnstone, D., additional, van Kempen, T. A., additional, McCoey, C., additional, Fuente, A., additional, Caselli, P., additional, Kristensen, L. E., additional, Plume, R., additional, Cernicharo, J., additional, Herczeg, G. J., additional, van Dishoeck, E. F., additional, Wampfler, S., additional, Gaufre, P., additional, Gill, J. J., additional, Javadi, H., additional, Justen, M., additional, Laauwen, W., additional, Luinge, W., additional, Ossenkopf, V., additional, Pearson, J., additional, Bachiller, R., additional, Baudry, A., additional, Benedettini, M., additional, Bergin, E., additional, Benz, A. O., additional, Bjerkeli, P., additional, Blake, G., additional, Bontemps, S., additional, Braine, J., additional, Bruderer, S., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Doty, S. D., additional, Encrenaz, P., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herpin, F., additional, Hogerheijde, M. R., additional, Jacq, T., additional, Jørgensen, J. K., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, Marseille, M., additional, Melnick, G., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Risacher, C., additional, Santiago, J., additional, Saraceno, P., additional, Shipman, R., additional, Tafalla, M., additional, van der Tak, F., additional, Visser, R., additional, Wyrowski, F., additional, and Yıldız, U. A., additional

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2010
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13. Water abundance variations around high-mass protostars: HIFI observations of the DR21 region

Author

van der Tak, F. F. S., primary, Marseille, M. G., additional, Herpin, F., additional, Wyrowski, F., additional, Baudry, A., additional, Bontemps, S., additional, Braine, J., additional, Doty, S., additional, Frieswijk, W., additional, Melnick, G., additional, Shipman, R., additional, van Dishoeck, E. F., additional, Benz, A. O., additional, Caselli, P., additional, Hogerheijde, M., additional, Johnstone, D., additional, Liseau, R., additional, Bachiller, R., additional, Benedettini, M., additional, Bergin, E., additional, Bjerkeli, P., additional, Blake, G., additional, Bruderer, S., additional, Cernicharo, J., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Giannini, T., additional, Goicoechea, J., additional, de Graauw, Th., additional, Helmich, F., additional, Herczeg, G., additional, Jørgensen, J., additional, Kristensen, L., additional, Larsson, B., additional, Lis, D., additional, McCoey, C., additional, Neufeld, D., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Pearson, J., additional, Plume, R., additional, Risacher, C., additional, Santiago, J., additional, Saraceno, P., additional, Tafalla, M., additional, van Kempen, T., additional, Visser, R., additional, Wampfler, S., additional, Yıldız, U., additional, Ravera, L., additional, Roelfsema, P., additional, Siebertz, O., additional, and Teyssier, D., additional

Published
2010
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14. Water cooling of shocks in protostellar outflows

Author

Nisini, B., primary, Benedettini, M., additional, Codella, C., additional, Giannini, T., additional, Liseau, R., additional, Neufeld, D., additional, Tafalla, M., additional, van Dishoeck, E. F., additional, Bachiller, R., additional, Baudry, A., additional, Benz, A. O., additional, Bergin, E., additional, Bjerkeli, P., additional, Blake, G., additional, Bontemps, S., additional, Braine, J., additional, Bruderer, S., additional, Caselli, P., additional, Cernicharo, J., additional, Daniel, F., additional, Encrenaz, P., additional, di Giorgio, A. M., additional, Dominik, C., additional, Doty, S., additional, Fich, M., additional, Fuente, A., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herczeg, G., additional, Herpin, F., additional, Hogerheijde, M., additional, Jacq, T., additional, Johnstone, D., additional, Jørgensen, J., additional, Kaufman, M., additional, Kristensen, L., additional, Larsson, B., additional, Lis, D., additional, Marseille, M., additional, McCoey, C., additional, Melnick, G., additional, Olberg, M., additional, Parise, B., additional, Pearson, J., additional, Plume, R., additional, Risacher, C., additional, Santiago, J., additional, Saraceno, P., additional, Shipman, R., additional, van Kempen, T. A., additional, Visser, R., additional, Viti, S., additional, Wampfler, S., additional, Wyrowski, F., additional, van der Tak, F., additional, Yıldız, U. A., additional, Delforge, B., additional, Desbat, J., additional, Hatch, W. A., additional, Péron, I., additional, Schieder, R., additional, Stern, J. A., additional, Teyssier, D., additional, and Whyborn, N., additional

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2010
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15. Origin of the hot gas in low-mass protostars

Author

van Kempen, T. A., primary, Kristensen, L. E., additional, Herczeg, G. J., additional, Visser, R., additional, van Dishoeck, E. F., additional, Wampfler, S. F., additional, Bruderer, S., additional, Benz, A. O., additional, Doty, S. D., additional, Brinch, C., additional, Hogerheijde, M. R., additional, Jørgensen, J. K., additional, Tafalla, M., additional, Neufeld, D., additional, Bachiller, R., additional, Baudry, A., additional, Benedettini, M., additional, Bergin, E. A., additional, Bjerkeli, P., additional, Blake, G. A., additional, Bontemps, S., additional, Braine, J., additional, Caselli, P., additional, Cernicharo, J., additional, Codella, C., additional, Daniel, F., additional, di Giorgio, A. M., additional, Dominik, C., additional, Encrenaz, P., additional, Fich, M., additional, Fuente, A., additional, Giannini, T., additional, Goicoechea, J. R., additional, de Graauw, Th., additional, Helmich, F., additional, Herpin, F., additional, Jacq, T., additional, Johnstone, D., additional, Kaufman, M. J., additional, Larsson, B., additional, Lis, D., additional, Liseau, R., additional, Marseille, M., additional, McCoey, C., additional, Melnick, G., additional, Nisini, B., additional, Olberg, M., additional, Parise, B., additional, Pearson, J. C., additional, Plume, R., additional, Risacher, C., additional, Santiago-García, J., additional, Saraceno, P., additional, Shipman, R., additional, van der Tak, F., additional, Wyrowski, F., additional, Yıldız, U. A., additional, Ciechanowicz, M., additional, Dubbeldam, L., additional, Glenz, S., additional, Huisman, R., additional, Lin, R. H., additional, Morris, P., additional, Murphy, J. A., additional, and Trappe, N., additional

Published
2010
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16. Evidence of warm and dense material along the outflow of a high-mass YSO*

Author

Bruderer, S., Benz, A. O., Bourke, T. L., Doty, S. D., Bruderer, S., Benz, A. O., Bourke, T. L., and Doty, S. D.

Abstract

Context. Outflow cavities in envelopes of young stellar objects (YSOs) have been predicted to allow far-UV (FUV) photons to escape far from the central source, with significant observable effects, especially if the protostar is a forming high-mass star suspected of emitting a copious amount of FUV radiation. Indirect evidence of this picture has been provided by models and unresolved single-dish observations, but direct high-resolution data are necessary for confirmation. Previous chemical modeling has suggested that CS and HCN are good probes of the local FUV field, so make good target species.

Published
2009
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17. The chemical history of molecules in circumstellar disks

Author

Visser, R., van Dishoeck, E. F., Doty, S. D., Dullemond, C. P., Visser, R., van Dishoeck, E. F., Doty, S. D., and Dullemond, C. P.

Abstract

Context. Many chemical changes occur during the collapse of a molecular cloud to form a low-mass star and the surrounding disk. One-dimensional models have been used so far to analyse these chemical processes, but they cannot properly describe the incorporation of material into disks.

Published
2009
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20. Water destruction by X-rays in young stellar objects

Author

Stäuber, P., Jørgensen, J. K., Dishoeck, E. F. van, Doty, S. D., Benz, A. O., Stäuber, P., Jørgensen, J. K., Dishoeck, E. F. van, Doty, S. D., and Benz, A. O.

Abstract

Aims.We study the H2O chemistry in star-forming environments under the influence of a central X-ray source and a central far ultraviolet (FUV) radiation field. The X-ray models are applied to envelopes around low-mass Class 0 and I young stellar objects (YSOs).

Published
2006
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21. The effect of a strong external radiation field on protostellar envelopes in Orion

Author

Jørgensen, J. K., Johnstone, D., van Dishoeck, E. F., Doty, S. D., Jørgensen, J. K., Johnstone, D., van Dishoeck, E. F., and Doty, S. D.

Abstract

We discuss the effects of an enhanced interstellar radiation field (ISRF) on the observables of protostellar cores in the Orion cloud region. Dust radiative transfer is used to constrain the envelope physical structure by reproducing SCUBA 850 μm emission. Previously reported 13CO, C17O and H2CO line observations are reproduced through detailed Monte Carlo line radiative transfer models. It is found that the 13CO line emission is marginally optically thick and sensitive to the physical conditions in the outer envelope. An increased temperature in this region is needed in order to reproduce the 13CO line strengths and it is suggested to be caused by a strong heating from the exterior, corresponding to an ISRF in Orion 103times stronger than the “standard” ISRF. The typical temperatures in the outer envelope are higher than the desorption temperature for CO. The C17O emission is less sensitive to this increased temperature but rather traces the bulk envelope material. The data are only fit by a model where CO is depleted, except in the inner and outermost regions where the temperature increases above 30–40 K. The fact that the temperatures do not drop below ≈25 K in any of the envelopes whereas a significant fraction of CO is frozen-out suggest that the interstellar radiation field has changed through the evolution of the cores. The H2CO lines are successfully reproduced in the model of an increased ISRF with constant abundances of 3–5 $\times$10-10.

Published
2006
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22. X-ray chemistry in the envelopes around young stellar objects

Author

Stäuber, P., Doty, S. D., van Dishoeck, E. F., Benz, A. O., Stäuber, P., Doty, S. D., van Dishoeck, E. F., and Benz, A. O.

Abstract

We present chemical models of the envelope of a young stellar object (YSO) exposed to a central X-ray source. The models are applied to the massive star-forming region AFGL 2591 for different X-ray fluxes. Model results for this region show that the X-ray ionization rate with and without the effects of Compton scattering differs by only a few percent and the influence of Compton scattering on the chemistry is negligible. The total X-ray ionization rate is dominated by the “secondary” ionization rate of H2resulting from fast electrons. The abundance profiles of several molecular and atomic species are shown to depend on the X-ray luminosity and on the distance from the source. The carbon, sulphur and nitrogen chemistries are discussed. It is found that He+and H$_3^+$are enhanced and trigger a peculiar chemistry. Several molecular X-ray tracers are found and compared to tracers of the far ultraviolet (FUV) field. Like ultraviolet radiation fields, X-rays enhance simple hydrides, ions and radicals. In contrast to ultraviolet photons, X-rays can penetrate deep into the envelope and affect the chemistry even at large distances from the source. Whereas the FUV enhanced species cover a region of $\approx $$200{-}300$AU, the region enhanced by X-rays is $\gtrsim $1000 AU. We find that N2O, HNO, SO, SO+, HCO+, CO+, OH+, N2H+, SH+and HSO+(among others) are more enhanced by X-rays than by FUV photons even for X-ray luminosities as low as $L_{{\rm X}} \approx 10^{30}$erg s-1. CO2abundances are reduced in the gas-phase through X-ray induced FUV photons. For temperatures $T \lesssim 230$K, H2O is destroyed by X-rays with luminosities $L_{{\rm X}} \gtrsim 10^{30}$erg s-1. Best-fit models for AFGL 2591 predict an X-ray luminosity $L_{{\rm X}} \gtrsim 10^{31}$erg s-1with a hard X-ray spectrum $T_{{\rm X}} \gtrsim 3 \times 10^7$K. This is the first time that the X-ray flux of a highly obscured source has been estimated by its envelope chemistry. Furthermore, we find $L_{{\rm X}}/L_{{\rm bol}} \approx 10^{-6}$. The chemistry of the bulk of the envelope mass is dominated by cosmic-ray induced reactions rather than by X-ray induced ionization for X-ray luminosities $L_{{\rm X}} \lesssim 10^{33}$erg s-1. The calculated line intensities of HCO+and HCS+show that high-Jlines are more affected than lower Jlines by the presence of X-rays due to their higher critical densities, and that such differences are detectable even with large aperture single-dish telescopes. Future instruments such as Herschel-HIFI or SOFIA will be able to observe X-ray enhanced hydrides whereas the sensitivity and spatial resolution of ALMA is well-suited to measure the size and geometry of the region affected by X-rays.

Published
2005
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23. Influence of UV radiation from a massive YSO on the chemistry of its envelope

Author

Stäuber, P., Doty, S. D., van Dishoeck, E. F., Jørgensen, J. K., Benz, A. O., Stäuber, P., Doty, S. D., van Dishoeck, E. F., Jørgensen, J. K., and Benz, A. O.

Abstract

We have studied the influence of far ultraviolet (UV) radiation ($6 < h\nu < 13.6$eV) from a massive young stellar object (YSO) on the chemistry of its own envelope by extending the models of Doty et al. ([CITE]) to include a central source of UV radiation. The models are applied to the massive star-forming region AFGL 2591 for different inner UV field strengths. Depth-dependent abundance profiles for several molecules are presented and discussed. We predict enhanced column densities for more than 30 species, especially radicals and ions. Comparison between observations and models is improved with a moderate UV field incident on the inner envelope, corresponding to an enhancement factor $G_{0} \approx 10$–100 at 200 AU from the star with an optical depth $\tau \approx 15$–17. The chemical networks of various species are explored. Subtle differences are found compared with traditional models of Photon Dominated Regions (PDRs) because of the higher temperatures and higher gas-phase H2O abundance caused by evaporation of ices in the inner region. In particular, the $\element{CN}$/$\element{HCN}$ratio is not a sensitive tracer of the inner UV field, in contrast with the situation for normal PDRs: for low UV fields, the extra CN reacts with H2in the inner dense and warm region and produces more HCN. It is found that the $\element{CH^+}$abundance is strongly enhanced and grows steadily with increasing UV field. In addition, the ratio $\element{CH^+}$/$\element{CH}$is increased by a factor of 103–105depending on the inner UV flux. High-Jlines of molecules like CN and HCN are most sensitive to the inner dense region where UV radiation plays a role. Thus, even though the total column density affected by UV photons is small, comparison of high-Jand low-Jlines can selectively trace and distinguish the inner UV field from the outer one. In addition, future Herschel-HIFI observations of hydrides can sensitively probe the inner UV field.

Published
2004
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24. Physical-chemical modeling of the low-mass protostar IRAS 16293-2422

Author

Doty, S. D., Schöier, F. L., van Dishoeck, E. F., Doty, S. D., Schöier, F. L., and van Dishoeck, E. F.

Abstract

We present detailed gas-phase chemical models for the envelope of the low-mass star-forming region IRAS 16293-2422. By considering both time- and space-dependent chemistry, these models are used to study both the physical structure proposed by Schöier et al. ([CITE]), as well as the chemical evolution of this region. A new feature of our study is the use of a detailed, self-consistent radiative transfer model to translate the model abundances into line strengths and compare them directly with observations of a total of 76 transitions for 18 chemical species, and their isotopes. The model can reproduce many of the line strengths observed within 50%. The best fit is for times in the range of $3\times 10^3{-}3\times 10^4$yrs and requires only minor modifications to our model for the high-mass star-forming region AFGL 2591. The ionization rate for the source may be higher than previously expected – either due to an enhanced cosmic-ray ionization rate, or, more probably, to the presence of X-ray induced ionization from the center. A significant fraction of the CO is found to desorb in the temperature range of 15-40 K; below this temperature ~90% or more of the CO is frozen out. The inability of the model to explain the HCS+, C2H, and OCS abundances suggests the importance of further laboratory studies of basic reaction rates. Finally, predictions of the abundances and spatial distributions of other species which could be observed by future facilities (e.g. Herschel-HIFI, SOFIA, millimeter arrays) are provided.

Published
2004
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25. Modeling gas-phase H2O between 5 $\mathsf{\mu}$m and 540 $\mathsf{\mu}$m toward massive protostars*

Author

Boonman, A. M. S., Doty, S. D., van Dishoeck, E. F., Bergin, E. A., Melnick, G. J., Wright, C. M., Stark, R., Boonman, A. M. S., Doty, S. D., van Dishoeck, E. F., Bergin, E. A., Melnick, G. J., Wright, C. M., and Stark, R.

Abstract

We present models and observations of gas-phase H2O lines between 5 and 540 μm toward deeply embedded massive protostars, involving both pure rotational and ro-vibrational transitions. The data have been obtained for 6 sources with both the Short and Long Wavelength Spectrometers (SWS and LWS) on board the Infrared Space Observatory (ISO) and with the Submillimeter Wave Astronomy Satellite (SWAS). For comparison, CO $J=7{-}6$spectra have been observed with the MPIfR/SRON 800 GHz heterodyne spectrometer at the James Clerk Maxwell Telescope (JCMT). A radiative transfer model in combination with different physical/chemical scenarios has been used to model these H2O lines for 4 sources to probe the chemical structure of these massive protostars. The results indicate that pure gas-phase production of H2O cannot explain the observed spectra. Ice evaporation in the warm inner envelope and freeze-out in the cold outer part are important for most of our sources and occur at $T\sim90$–110 K. The ISO-SWS data are particularly sensitive to ice evaporation in the inner part whereas the ISO-LWS data are good diagnostics of freeze-out in the outer region. The modeling suggests that the 557 GHz SWAS line includes contributions from both the cold and the warm H2O gas. The SWAS line profiles indicate that for some of the sources a fraction of up to 50% of the total flux may originate in the outflow. Shocks do not seem to contribute significantly to the observed emission in other H2O lines, however, in contrast with the case for Orion. The results show that three of the observed and modeled H2O lines, the $3_{03}{-}2_{12}, 2_{12}{-}1_{01}$, and $1_{10}{-}1_{01}$lines, are good candidates to observe with the Herschel Space Observatory in order to further investigate the physical and chemical conditions in massive star-forming regions.

Published
2003
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26. Numerical methods for non-LTE line radiative transfer: Performance and convergence characteristics

Author

van Zadelhoff, G.-J., Dullemond, C. P., van der Tak, F. F. S., Yates, J. A., Doty, S. D., Ossenkopf, V., Hogerheijde, M. R., Juvela, M., Wiesemeyer, H., Schöier, F. L., van Zadelhoff, G.-J., Dullemond, C. P., van der Tak, F. F. S., Yates, J. A., Doty, S. D., Ossenkopf, V., Hogerheijde, M. R., Juvela, M., Wiesemeyer, H., and Schöier, F. L.

Abstract

Comparison is made between a number of independent computer programs for radiative transfer in molecular rotational lines. The test models are spherically symmetric circumstellar envelopes with a given density and temperature profile. The first two test models have a simple power law density distribution, constant temperature and a fictive 2-level molecule, while the other two test models consist of an inside-out collapsing envelope observed in rotational transitions of HCO+. For the 2-level molecule test problems all codes agree well to within 0.2%, comparable to the accuracy of the individual codes, for low optical depth and up to 2% for high optical depths ($\tau=4800$). The problem of the collapsing cloud in HCO+has a larger spread in results, ranging up to 12% for the $J=4$population. The spread is largest at the radius where the transition from collisional to radiative excitation occurs. The resulting line profiles for the HCO+$J=4$–3 transition agree to within 10%, i.e., within the calibration accuracy of most current telescopes. The comparison project and the results described in this paper provide a benchmark for future code development, and give an indication of the typical accuracy of present day calculations of molecular line transfer.

Published
2002
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27. Chemistry as a probe of the structures and evolution of massive star-forming regions

Author

Doty, S. D., van Dishoeck, E. F., van der Tak, F. F. S., Boonman, A. M. S., Doty, S. D., van Dishoeck, E. F., van der Tak, F. F. S., and Boonman, A. M. S.

Abstract

We present detailed thermal and gas-phase chemical models for the envelope of the massive star-forming region AFGL 2591. By considering both time- and space-dependent chemistry, these models are used to study both the physical structure proposed by van der Tak et al. ([CITE], [CITE]), as well as the chemical evolution of this region. The model predictions are compared with observed abundances and column densities for 29 species. The observational data cover a wide range of physical conditions within the source, but significantly probe the inner regions where interesting high-temperature chemistry may be occurring. Taking appropriate care when comparing models with both emission and absorption measurements, we find that the majority of the chemical structure can be well-explained. In particular, we find that the nitrogen and hydrocarbon chemistry can be significantly affected by temperature, with the possibility of high-temperature pathways to HCN. While we cannot determine the sulphur reservoir, the observations can be explained by models with the majority of the sulphur in CS in the cold gas, SO2in the warm gas, and atomic sulphur in the warmest gas. Because the model overpredicts CO2by a factor of 40, various high-temperature destruction mechanisms are explored, including impulsive heating events. The observed abundances of ions such as HCO+and N2H+and the cold gas-phase production of HCN constrain the cosmic-ray ionization rate to ~$5.6 \times 10^{-17}$s-1, to within a factor of three. Finally, we find that the model and observations can simultaneously agree at a reasonable level and often to within a factor of three for $7 \times 10^{3} \leq t({\rm yrs}) \leq 5 \times 10^{4}$, with a strong preference for $t \sim 3 \times 10^{4}$yrs since the collapse and formation of the central luminosity source.

Published
2002
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28. Modeling water emission from low-mass protostellar envelopes

Author

van Kempen, T., Doty, S., van Dishoeck, E., Hogerheijde, M., and J?rgensen, J.

Abstract

Context. Within low-mass star formation, water vapor plays a key role in the chemistry and energy balance of the circumstellar material. The Herschel Space Observatory will open up the possibility to observe water lines originating from a wide range of excitation energies. Aims. Our aim is to simulate the emission of rotational water lines from envelopes characteristic of embedded low-mass protostars. A large number of parameters that influence the water line emission are explored: luminosity, density, density slope, and water abundances.Methods. Both dust and water emission are modeled using full radiative transfer in spherical symmetry. The temperature profile is calculated for a given density profile. The H2O level populations and emission profiles are in turn computed with a non-LTE line code. The results are analyzed to determine the diagnostic value of different lines, and are compared with existing observations. Results. Lines can be categorized in: (i) optically thick lines, including ground-state lines, mostly sensitive to the cold outer part; (ii)?highly excited (Eu>200?250?K) optically thin lines sensitive to the abundance in the hot inner part; and (iii)?lines which vary from optically thick to thin depending on the abundances.?Dust influences the emission of water significantly by becoming optically thick at the higher frequencies, and by pumping optically thin lines.Conclusions. A good physical model of a source, including the correct treatment of dust, is a prerequisite for inferring the water abundance structure and possible jumps at the evaporation temperature from observations. The inner warm (T>100?K) envelope can be probed by highly excited lines, while a combination of excited and spectrally resolved ground state lines probes the outer envelope. Observations of H218O lines, although weak, provide even stronger constraints on abundances.

Published
2008

29. The chemical history of molecules in circumstellar disks

Author

Visser, R., Doty, S. D., and van Dishoeck, E. F.

Abstract

Context.The chemical composition of a molecular cloud changes dramatically as it collapses to form a low-mass protostar and circumstellar disk. Two-dimensional (2D) chemodynamical models are required to properly study this process.

Published
2011
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30. First hyperfine resolved far-infrared OH spectrum from a star-forming region⋆⋆⋆

Author

Wampfler, S. F., Bruderer, S., Kristensen, L. E., Chavarría, L., Bergin, E. A., Benz, A. O., van Dishoeck, E. F., Herczeg, G. J., van der Tak, F. F. S., Goicoechea, J. R., Doty, S. D., and Herpin, F.

Abstract

OH is an important molecule in the H2O chemistry and the cooling budget of star-forming regions. The goal of the Herschel key program “Water In Star-forming regions with Herschel” (WISH) is to study H2O and related species during protostellar evolution. Our aim in this Letter is to assess the origin of the OH emission from star-forming regions and constrain the properties of the emitting gas. High-resolution observations of the OH \hbox{${}^2\Pi_{1/2}~J = 3/2{-}1/2 $}triplet at 1837.8   GHz (163.1   μm) towards the high-mass star-forming region W3 IRS 5 with the Heterodyne Instrument for the Far-Infrared (HIFI) on Herschel reveal the first hyperfine velocity-resolved OH far-infrared spectrum of a star-forming region. The line profile of the OH emission shows two components: a narrow component (FWHM≈  4−5   km   s-1) with partially resolved hyperfine structure resides on top of a broad (FWHM≈  30   km   s-1) component. The narrow emission agrees well with results from radiative transfer calculations of a spherical envelope model for W3 IRS 5 with a constant OH abundance of xOH≈ 8  ×  10-9. Comparison with H2O yields OH/H2O abundance ratios of around 10-3for T≳ 100   K and around unity for T≲ 100   K, consistent with the current picture of the dense cloud chemistry with freeze-out and photodesorption. The broad component is attributed to outflow emission. An abundance ratio of OH/H2O  ≳  0.028 in the outflow is derived from comparison with results of water line modeling. This ratio can be explained by a fast J-type shock or a slower UV-irradiated C-type shock.

Published
2011
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31. Water abundances in high-mass protostellar envelopes: Herschelobservations with HIFI ***

Author

Marseille, M. G., van der Tak, F. F. S., Herpin, F., Wyrowski, F., Chavarría, L., Pietropaoli, B., Baudry, A., Bontemps, S., Cernicharo, J., Jacq, T., Frieswijk, W., Shipman, R., van Dishoeck, E. F., Bachiller, R., Benedettini, M., Benz, A. O., Bergin, E., Bjerkeli, P., Blake, G. A., Braine, J., Bruderer, S., Caselli, P., Caux, E., Codella, C., Daniel, F., Dieleman, P., di Giorgio, A. M., Dominik, C., Doty, S. D., Encrenaz, P., Fich, M., Fuente, A., Gaier, T., Giannini, T., Goicoechea, J. R., de Graauw, Th., Helmich, F., Herczeg, G. J., Hogerheijde, M. R., Jackson, B., Javadi, H., Jellema, W., Johnstone, D., Jørgensen, J. K., Kester, D., Kristensen, L. E., Larsson, B., Laauwen, W., Lis, D., Liseau, R., Luinge, W., McCoey, C., Megej, A., Melnick, G., Neufeld, D., Nisini, B., Olberg, M., Parise, B., Pearson, J. C., Plume, R., Risacher, C., Roelfsema, P., Santiago-García, J., Saraceno, P., Siegel, P., Stutzki, J., Tafalla, M., van Kempen, T. A., Visser, R., Wampfler, S. F., and Yıldız, U. A.

Abstract

Aims. We derive the dense core structure and the water abundance in four massive star-forming regions in the hope of understanding the earliest stages of massive star formation.

Published
2010
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