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5 results on '"Maiwald, F.W."'

1. Detection of OH+ and H2O+ towards Orion KL

Author

Gupta, H., Rimmer, P., Pearson, J.C., Yu, S., Herbst, E., Harada, N., Bergin, E.A., Neufeld, D.A., Melnick, G.J., Bachiller, R., Bells, T.A., Blake, G.A., Caux, E., Ceccarelli, C., Cernicharo, J., Chattopadhyay, G., Comito, C., Cabrit, S., Crockett, N.R., Daniel, F., Falgarone, E., Diez-Gonzalez, M.C., Dubernet, M.-L., Erickson, N., Emprechtinger, M., Encrenaz, P., Gerin, M., Gill, J.J., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Joblin, C., Johnstone, D., Langer, W.D., Larsson, B., Latter, W.B., Lin, R.J., Lis, D.C., Liseau, R., Lord, S.D., Maiwald, F.W., Maret, S., Martin, P.G., Martin-Pintado, J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.A., Nordh, L.H., Olberg, M., Ossenkopf, V., Pagani, L., Perault, M., Phillips , T.G., Plume, R., Qin, S.-L., Salez, M., Samoska, L.A., Schilke, P., Schlecht, E., Schlemmer, S., Szczerba, R., Stutzki, J., Trappe, N., van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Zmuidzinas, J., Boogert, A., Gusten, R., Hartogh, P., Honigh, N., Karpov, A., Kooi, J., Krieg, J.-M., Schieder, R., and Zaal, P.

Subjects
Experimental Physics
Abstract

We report observations of the reactive molecular ions OH+, H2O+, and H3O+ towards Orion KL with Herschel/HIFI. All three N = 1−0 finestructure transitions of OH+ at 909, 971, and 1033 GHz and both fine-structure components of the doublet ortho-H2O+ 111−000 transition at 1115 and 1139 GHz were detected; an upper limit was obtained for H3O+. OH+ and H2O+ are observed purely in absorption, showing a narrow component at the source velocity of 9 km s−1, and a broad blueshifted absorption similar to that reported recently for HF and para-H18 2 O, and attributed to the low velocity outflow of Orion KL.We estimate column densities of OH+ and H2O+ for the 9 kms−1 component of 9±3×1012 cm−2 and 7±2×1012 cm−2, and those in the outflow of 1.9±0.7×1013 cm−2 and 1.0±0.3×1013 cm−2. Upper limits of 2.4×1012 cm−2 and 8.7×1012 cm−2 were derived for the column densities of ortho and para-H3O+ from transitions near 985 and 1657 GHz. The column densities of the three ions are up to an order of magnitude lower than those obtained from recent observations ofW31C and W49N. The comparatively low column densities may be explained by a higher gas density despite the assumption of a very high ionization rate.

Published
2010

2. The Herschel-Heterodyne Instrument for the Far-Infrared (HIFI)

Author

Graauw, T. de, Helmich, F.P., Phillips, T.G., Stutzki, J., Caux, E., Whyborn, N.D., Dieleman, P., Roelfsema, P.R., Aarts, H., Assendorp, R., Bachiller, R., Baechtold, W., Barcia, A., Beintema, D.A., Belitsky, V., Benz, A.O., Bieber, R., Boogert, A., Borys, C., Bumble, B., Caïs, P., Caris, M., Cerulli-Irelli, P., Chattopadhyay, G., Cherednichenko, S., Ciechanowicz, M., Coeur-Joly, O., Comito, C., Cros, A., Jonge, A. de, Lange, G. de, Delforges, B., Delorme, Y., Boggende, T. den, Desbat, J.M., Diez-González, C., Di Giorgio, A.M., Dubbeldam, L., Edwards, K., Eggens, M., Erickson, N., Evers, J., Fich, M., Finn, T., Franke, B., Gaier, T., Gal, C., Gao, J.R., Gallego, J.D., Gauffre, S., Gill, J.J., Glenz, S., Golstein, H., Goulooze, H., Gunsing, T., Güsten, R., Hartogh, P., Hatch, W.A., Higgins, R., Honingh, E.C., Huisman, R., Jackson, B.D., Jacobs, H., Jacobs, K., Jarchow, C., Javadi, H., Jellema, W., Justen, M., Karpov, A., Kasemann, C., Kawamura, J., Keizer, G., Kester, D., Klapwijk, T.M., Klein, T., Kollberg, E., Kooi, J., Kooiman, P.P., Kopf, B., Krause, M., Krieg, J.M., Kramer, C., Kruizenga, B., Kuhn, T., Laauwen, W., Lai, R., Larsson, B., Leduc, H.G., Leinz, C., Lin, R.H., Liseau, R., Liu, G.S., Loose, A., López-Fernandez, I., Lord, S., Luinge, W., Marston, A., Martín-Pintado, J., Maestrini, A., Maiwald, F.W., McCoey, C., Mehdi, I., Megej, A., Melchior, M., Meinsma, L., Merkel, H., Michalska, M., Monstein, C., Moratschke, D., Morris, P., Muller, H., Murphy, J.A., Naber, A., Natale, E., Nowosielski, W., Nuzzolo, F., Olberg, M., Olbrich, M., Orfei, R., Orleanski, P., Ossenkopf, V., Peacock, T., Pearson, J.C., Peron, I., Phillip-May, S., Piazzo, L., Planesas, P., Rataj, M., Ravera, L., Risacher, C., Salez, M., Samoska, L.A., Saraceno, P., Schieder, R., Schlecht, E., Schlöder, F., Schmülling, F., Schultz, M., Schuster, K., Siebertz, O., Smit, H., Szczerba, R., Shipman, R., Steinmetz, E., Stern, J.A., Stokroos, M., Teipen, R., Teyssier, D., Tils, T., Trappe, N., Baaren, C. van, Leeuwen, B.J. van, Stadt, H. van de, Visser, H., Wildeman, K.J., Wafelbakker, C.K., Ward, J.S., Wesselius, P., Wild, W., Wulff, S., Wunsch, H.J., Tielens, X., Zaal, P., Zirath, H., Zmuidzinas, J., Zwart, F., Graauw, T. de, Helmich, F.P., Phillips, T.G., Stutzki, J., Caux, E., Whyborn, N.D., Dieleman, P., Roelfsema, P.R., Aarts, H., Assendorp, R., Bachiller, R., Baechtold, W., Barcia, A., Beintema, D.A., Belitsky, V., Benz, A.O., Bieber, R., Boogert, A., Borys, C., Bumble, B., Caïs, P., Caris, M., Cerulli-Irelli, P., Chattopadhyay, G., Cherednichenko, S., Ciechanowicz, M., Coeur-Joly, O., Comito, C., Cros, A., Jonge, A. de, Lange, G. de, Delforges, B., Delorme, Y., Boggende, T. den, Desbat, J.M., Diez-González, C., Di Giorgio, A.M., Dubbeldam, L., Edwards, K., Eggens, M., Erickson, N., Evers, J., Fich, M., Finn, T., Franke, B., Gaier, T., Gal, C., Gao, J.R., Gallego, J.D., Gauffre, S., Gill, J.J., Glenz, S., Golstein, H., Goulooze, H., Gunsing, T., Güsten, R., Hartogh, P., Hatch, W.A., Higgins, R., Honingh, E.C., Huisman, R., Jackson, B.D., Jacobs, H., Jacobs, K., Jarchow, C., Javadi, H., Jellema, W., Justen, M., Karpov, A., Kasemann, C., Kawamura, J., Keizer, G., Kester, D., Klapwijk, T.M., Klein, T., Kollberg, E., Kooi, J., Kooiman, P.P., Kopf, B., Krause, M., Krieg, J.M., Kramer, C., Kruizenga, B., Kuhn, T., Laauwen, W., Lai, R., Larsson, B., Leduc, H.G., Leinz, C., Lin, R.H., Liseau, R., Liu, G.S., Loose, A., López-Fernandez, I., Lord, S., Luinge, W., Marston, A., Martín-Pintado, J., Maestrini, A., Maiwald, F.W., McCoey, C., Mehdi, I., Megej, A., Melchior, M., Meinsma, L., Merkel, H., Michalska, M., Monstein, C., Moratschke, D., Morris, P., Muller, H., Murphy, J.A., Naber, A., Natale, E., Nowosielski, W., Nuzzolo, F., Olberg, M., Olbrich, M., Orfei, R., Orleanski, P., Ossenkopf, V., Peacock, T., Pearson, J.C., Peron, I., Phillip-May, S., Piazzo, L., Planesas, P., Rataj, M., Ravera, L., Risacher, C., Salez, M., Samoska, L.A., Saraceno, P., Schieder, R., Schlecht, E., Schlöder, F., Schmülling, F., Schultz, M., Schuster, K., Siebertz, O., Smit, H., Szczerba, R., Shipman, R., Steinmetz, E., Stern, J.A., Stokroos, M., Teipen, R., Teyssier, D., Tils, T., Trappe, N., Baaren, C. van, Leeuwen, B.J. van, Stadt, H. van de, Visser, H., Wildeman, K.J., Wafelbakker, C.K., Ward, J.S., Wesselius, P., Wild, W., Wulff, S., Wunsch, H.J., Tielens, X., Zaal, P., Zirath, H., Zmuidzinas, J., and Zwart, F.

Abstract

Aims. This paper describes the Heterodyne Instrument for the Far-Infrared (HIFI) that was launched onboard ESA's Herschel Space Observatory in May 2009. Methods. The instrument is a set of 7 heterodyne receivers that are electronically tuneable, covering 480-1250 GHz with SIS mixers and the 1410-1910 GHz range with hot electron bolometer (HEB) mixers. The local oscillator (LO) subsystem comprises a Ka-band synthesizer followed by 14 chains of frequency multipliers and 2 chains for each frequency band. A pair of auto-correlators and a pair of acousto-optical spectrometers process the two IF signals from the dual-polarization, single-pixel front-ends to provide instantaneous frequency coverage of 2 × 4 GHz, with a set of resolutions (125 kHz to 1 MHz) that are better than 0.1 km s-1. Results. After a successful qualification and a pre-launch TB/TV test program, the flight instrument is now in-orbit and completed successfully the commissioning and performance verification phase. The in-orbit performance of the receivers matches the pre-launch sensitivities. We also report on the in-orbit performance of the receivers and some first results of HIFI's operations.

Published
2010

3. Herschel/HIFI measurements of the ortho/para ratio in water towards Sagittarius B2(M) and W31C

Author

Lis, D.C., Phillips, T.G., Goldsmith, P.F., Neufeld, D.A., Herbst, E., Comito, C., Schilke, P., Muller, H.S.P., Bergin, E.A., Gerin, M., Bell, T.A., Emprechtinger, M., Black, J., Blake, G.A., Boulanger, F., Caux, E., Ceccarelli, C., Cernicharo, J., Coutens, A., Crockett, N.R., Daniel, F., Dartois, E., De Luca, M., Dubernet, M.-L., Encrenaz, P., Falgarone, E., Geballe, T.R., Godard, B., Giesen, T.F., Goicoechea, J.R., Gry, C., Gupta, H., Hennebelle, P., Hily-Blant, P., Kolos, R., Krelowski, J., Joblin, C., Johnstone, D., Kazmierczak, M., Lord, S.D., Maret, S., Martin, P.G., Martin-Pintado, J., Melnick, G.J., Menten, K.M., Monjel, R., Mookerjea, B., Morris, P., Murphy, J.Anthony, Ossenkopf, V., Pearson, J.C., Perault, M., Persson, C., Plume, R., Qin, S.-L., Salez, M., Schlemmer, S., Schmidt, M., Sonnentrucker, P., Stutzki, J., Teyssier, D., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Zmuidzinas, J., Boogert, A., Erickson, N., Karpov, A., Kooi, J., Maiwald, F.W., Schieder, R., Zaal, P., Lis, D.C., Phillips, T.G., Goldsmith, P.F., Neufeld, D.A., Herbst, E., Comito, C., Schilke, P., Muller, H.S.P., Bergin, E.A., Gerin, M., Bell, T.A., Emprechtinger, M., Black, J., Blake, G.A., Boulanger, F., Caux, E., Ceccarelli, C., Cernicharo, J., Coutens, A., Crockett, N.R., Daniel, F., Dartois, E., De Luca, M., Dubernet, M.-L., Encrenaz, P., Falgarone, E., Geballe, T.R., Godard, B., Giesen, T.F., Goicoechea, J.R., Gry, C., Gupta, H., Hennebelle, P., Hily-Blant, P., Kolos, R., Krelowski, J., Joblin, C., Johnstone, D., Kazmierczak, M., Lord, S.D., Maret, S., Martin, P.G., Martin-Pintado, J., Melnick, G.J., Menten, K.M., Monjel, R., Mookerjea, B., Morris, P., Murphy, J.Anthony, Ossenkopf, V., Pearson, J.C., Perault, M., Persson, C., Plume, R., Qin, S.-L., Salez, M., Schlemmer, S., Schmidt, M., Sonnentrucker, P., Stutzki, J., Teyssier, D., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Zmuidzinas, J., Boogert, A., Erickson, N., Karpov, A., Kooi, J., Maiwald, F.W., Schieder, R., and Zaal, P.

Abstract

We present Herschel/HIFI observations of the fundamental rotational transitions of ortho- and para-H16 2 O and H18 2 O in absorption towards Sagittarius B2(M) and W31C. The ortho/para ratio in water in the foreground clouds on the line of sight towards these bright continuum sources is generally consistent with the statistical high-temperature ratio of 3, within the observational uncertainties. However, somewhat unexpectedly, we derive a low ortho/para ratio of 2.35±0.35, corresponding to a spin temperature of ∼27 K, towards Sagittarius B2(M) at velocities of the expanding molecular ring. Water molecules in this region appear to have formed with, or relaxed to, an ortho/para ratio close to the value corresponding to the local temperature of the gas and dust.

Published
2010

4. Herschel observations of ortho- and para-oxidaniumyl (H2O+) in spiral arm clouds toward Sagittarius B2(M)

Author

Schilke, P., Comito, C., Muller, H.S.P., Bergin, E.A., Herbst, E., Lis, D.C., Neufeld, D.A., Phillips , T.G., Bell, T.A., Blake, G.A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Crockett, N.R., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Murphy, J.Anthony, Ossenkopf, V., Pagini, L., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Salez, M., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Erickson, N., Maiwald, F.W., Kooi, J., Karpov, A., Zmuidzinas, J., Boogert, A., Schieder, R., Zaal, P., Schilke, P., Comito, C., Muller, H.S.P., Bergin, E.A., Herbst, E., Lis, D.C., Neufeld, D.A., Phillips , T.G., Bell, T.A., Blake, G.A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Crockett, N.R., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Murphy, J.Anthony, Ossenkopf, V., Pagini, L., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Salez, M., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Erickson, N., Maiwald, F.W., Kooi, J., Karpov, A., Zmuidzinas, J., Boogert, A., Schieder, R., and Zaal, P.

Abstract

H2O+ has been observed in its ortho- and para- states toward the massive star forming core Sgr B2(M), located close to the Galactic center. The observations show absorption in all spiral arm clouds between the Sun and Sgr B2. The average o/p ratio of H2O+ in most velocity intervals is 4.8, which corresponds to a nuclear spin temperature of 21 K. The relationship of this spin temperature to the formation temperature and current physical temperature of the gas hosting H2O+ is discussed, but no firm conclusion is reached. In the velocity interval 0–60 km s−1, an ortho/para ratio of below unity is found, but if this is due to an artifact of contamination by other species or real is not clear.

Published
2010

5. The Herschel-Heterodyne Instrument for the Far-Infrared (HIFI)

Author

de Graauw, Th., Helmich, F.P., Phillips , T.G., Stutzki, J., Caux, E., Whyborn, N.D., Dieleman, P., Roelfsema, P.R., Aarts, H., Assendorp, R., Bachiller, R., Baechtold, W., Barcia, A., Beintema, D.A., Belitsky, V., Benz, A.O., Bieber, R., Boogert, A., Borys, C., Bumble, B., Cais, P., Caris, M., Cerulli-Irelli, P., Chattopadhyay, G., Cherednichenko, S., Ciechanowicz, M., Coeur-Joly, O., Comito, C., Cros, A., de Jonge, A., de Lange, G., Delforges, B., Delorme, Y., den Boggende, T., Desbat, J.-M., Diez-Gonzalez, C., Di Giorgio, A.M., Dubbeldam, L., Edwards, K., Eggens, M., Erickson, N., Evers, J., Fich, M., Finn, T., Franke, B., Gaier, T., Gal, C., Gao, J.R., Gallego, J.-D., Gauffre, S., Gill, J.J., Glenz, S., Golstein, H., Goulooze, H., Gunsing, T., Gusten, R., Hartogh, P., Hatch, W.A., Higgins, R., Honingh, E.C., Huisman, R., Jackson, B.D., Jacobs, H., Jacobs, K., Jarchow, C., Javadi, H., Jellema, W., Justen, M., Karpov, A., Kasemann, C., Kawamura, J., Keizer, G., Kester, D., Klapwijk, T.M., Klein, Th., Kollberg, E., Kooi, J., Kooiman, P.-P., Kopf, B., Krause, M., Krieg, J.-M., Kramer, C., Kruizenga, B., Kuhn, T., Laauwen, W., Lai, R., Larsson, B., Leduc, H.G., Leinz, C., Lin, R.H., Liseau, R., Liu, G.S., Loose, A., Lopez-Fernandez, I., Lord, S., Luinge, W., Marston, A., Martin-Pintado, J., Maestrini, A., Maiwald, F.W., McCoey, C., Mehdi, I., Megej, A., Melchior, M., Meinsma, L., Merkel, H., Michalska, M., Monstein, C., Moratschke, D., Morris, P., Muller, H., Murphy, J.Anthony, Naber, A., Natale, E., Nowosielski, W., Nuzzolo, F., Olberg, M., Olbrich, M., Orfei, R., Orleanski, P., Ossenkopf, V., Peacock, T., Pearson, J.C., Peron, I., Phillip-May, S., Piazzo, L., Planesas, P., Rataj, M., Ravera, L., Risacher, C., Salez, M., Samoska, L.A., Saraceno, P., Schieder, R., Schlecht, E., Schloder, F., Schmulling, F., Schultz, M., Schuster, K., Siebertz, O., Smit, H., Szczerba, R., Shipman, R., Steinmetz, E., Stern, J.A., Stokroos, M., Teipen, R., Teyssier, D., Tils, T., Trappe, Neil, van Baaren, C., van Leeuwen, B.-J., van de Stadt, H., Visser, H., Wildeman, K.J., Wafelbakker, C.K., Ward, J.S., Wesselius, P., Wild, W., Wulff, S., Wunsch, H.-J., Tielens, X., Zaal, P., Zirath, H., Zmuidzinas, J., Zwart, F., de Graauw, Th., Helmich, F.P., Phillips , T.G., Stutzki, J., Caux, E., Whyborn, N.D., Dieleman, P., Roelfsema, P.R., Aarts, H., Assendorp, R., Bachiller, R., Baechtold, W., Barcia, A., Beintema, D.A., Belitsky, V., Benz, A.O., Bieber, R., Boogert, A., Borys, C., Bumble, B., Cais, P., Caris, M., Cerulli-Irelli, P., Chattopadhyay, G., Cherednichenko, S., Ciechanowicz, M., Coeur-Joly, O., Comito, C., Cros, A., de Jonge, A., de Lange, G., Delforges, B., Delorme, Y., den Boggende, T., Desbat, J.-M., Diez-Gonzalez, C., Di Giorgio, A.M., Dubbeldam, L., Edwards, K., Eggens, M., Erickson, N., Evers, J., Fich, M., Finn, T., Franke, B., Gaier, T., Gal, C., Gao, J.R., Gallego, J.-D., Gauffre, S., Gill, J.J., Glenz, S., Golstein, H., Goulooze, H., Gunsing, T., Gusten, R., Hartogh, P., Hatch, W.A., Higgins, R., Honingh, E.C., Huisman, R., Jackson, B.D., Jacobs, H., Jacobs, K., Jarchow, C., Javadi, H., Jellema, W., Justen, M., Karpov, A., Kasemann, C., Kawamura, J., Keizer, G., Kester, D., Klapwijk, T.M., Klein, Th., Kollberg, E., Kooi, J., Kooiman, P.-P., Kopf, B., Krause, M., Krieg, J.-M., Kramer, C., Kruizenga, B., Kuhn, T., Laauwen, W., Lai, R., Larsson, B., Leduc, H.G., Leinz, C., Lin, R.H., Liseau, R., Liu, G.S., Loose, A., Lopez-Fernandez, I., Lord, S., Luinge, W., Marston, A., Martin-Pintado, J., Maestrini, A., Maiwald, F.W., McCoey, C., Mehdi, I., Megej, A., Melchior, M., Meinsma, L., Merkel, H., Michalska, M., Monstein, C., Moratschke, D., Morris, P., Muller, H., Murphy, J.Anthony, Naber, A., Natale, E., Nowosielski, W., Nuzzolo, F., Olberg, M., Olbrich, M., Orfei, R., Orleanski, P., Ossenkopf, V., Peacock, T., Pearson, J.C., Peron, I., Phillip-May, S., Piazzo, L., Planesas, P., Rataj, M., Ravera, L., Risacher, C., Salez, M., Samoska, L.A., Saraceno, P., Schieder, R., Schlecht, E., Schloder, F., Schmulling, F., Schultz, M., Schuster, K., Siebertz, O., Smit, H., Szczerba, R., Shipman, R., Steinmetz, E., Stern, J.A., Stokroos, M., Teipen, R., Teyssier, D., Tils, T., Trappe, Neil, van Baaren, C., van Leeuwen, B.-J., van de Stadt, H., Visser, H., Wildeman, K.J., Wafelbakker, C.K., Ward, J.S., Wesselius, P., Wild, W., Wulff, S., Wunsch, H.-J., Tielens, X., Zaal, P., Zirath, H., Zmuidzinas, J., and Zwart, F.

Abstract

Aims. This paper describes the Heterodyne Instrument for the Far-Infrared (HIFI) that was launched onboard ESA’s Herschel Space Observatory in May 2009. Methods. The instrument is a set of 7 heterodyne receivers that are electronically tuneable, covering 480−1250 GHz with SIS mixers and the 1410−1910 GHz range with hot electron bolometer (HEB) mixers. The local oscillator (LO) subsystem comprises a Ka-band synthesizer followed by 14 chains of frequency multipliers and 2 chains for each frequency band. A pair of auto-correlators and a pair of acousto-optical spectrometers process the two IF signals from the dual-polarization, single-pixel front-ends to provide instantaneous frequency coverage of 2 × 4 GHz, with a set of resolutions (125 kHz to 1 MHz) that are better than 0.1 kms−1. Results. After a successful qualification and a pre-launch TB/TV test program, the flight instrument is now in-orbit and completed successfully the commissioning and performance verification phase. The in-orbit performance of the receivers matches the pre-launch sensitivities. We also report on the in-orbit performance of the receivers and some first results of HIFI’s operations.

Published
2010

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