889 results on '"Kemper, F."'
Search Results
152. Neuere Untersuchungen zur Beeinflussung des experimentellen Exophthalmus
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Kemper, F., Helmecke, K., and Schlegel, B., editor
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- 1965
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153. Beeinflussung der endokrinen Ophthalmopathie durch Pflanzenextrakte
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Kemper, F., Portheine, H., and Schlegel, Bernhard, editor
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- 1964
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154. Crystal Structure of Polyphosphate Kinase from Meiothermus ruber bound to ADP
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Gerhardt, S., primary, Einsle, O., additional, Kemper, F., additional, and Schwarzer, N., additional
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- 2017
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155. Structure of Polyphosphate Kinase from Meiothermus ruber Apo-form
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Kemper, F., primary, Einsle, O., additional, and Gerhardt, S., additional
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- 2017
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156. Structure of Polyphosphate Kinase from Meiothermus ruber bound to AMP
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Gerhardt, S., primary, Einsle, O., additional, Kemper, F., additional, and Schwarzer, N., additional
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- 2017
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157. The SAGE-Spec Spitzer Legacy program: the life-cycle of dust and gas in the Large Magellanic Cloud. Point source classification – III
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Jones, O. C., primary, Woods, P. M., additional, Kemper, F., additional, Kraemer, K. E., additional, Sloan, G. C., additional, Srinivasan, S., additional, Oliveira, J. M., additional, van Loon, J. Th., additional, Boyer, M. L., additional, Sargent, B. A., additional, McDonald, I., additional, Meixner, M., additional, Zijlstra, A. A., additional, Ruffle, P. M. E., additional, Lagadec, E., additional, Pauly, T., additional, Sewiło, M., additional, Clayton, G. C., additional, and Volk, K., additional
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- 2017
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158. Highly sensitive on-chip fluorescence sensor with integrated fully solution processed organic light sources and detectors
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Shu, Z., primary, Kemper, F., additional, Beckert, E., additional, Eberhardt, R., additional, and Tünnermann, A., additional
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- 2017
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159. Light filter tailoring – the impact of light emitting diode irradiation on the morphology and optical properties of silver nanoparticles within polyethylenimine thin films
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Kemper, F., primary, Beckert, E., additional, Eberhardt, R., additional, and Tünnermann, A., additional
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- 2017
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160. ITO-Free, Fully Solution Processed Transparent Organic Light-Emitting Electrochemical Cells on Thin Glass
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Shu, Z., primary, Kemper, F., additional, Beckert, E., additional, Eberhardt, R., additional, and Tünnermann, A., additional
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- 2017
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161. E/S/C/O/P Monographs. The Scientific Foundation for Herbal Medicinal Products
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Anton, R, Delaveau, P, Franz, G, Harvala, C, Kemper, F H, Kraft, K, Kubelka, W, Loew, D, Ollivier, E, Saller, R, Schilcher, H, Simmet, T, Sticher, O, Vincieri, F F, Vlietinck, A J, Anton, R ( R ), Delaveau, P ( P ), Franz, G ( G ), Harvala, C ( C ), Kemper, F H ( F H ), Kraft, K ( K ), Kubelka, W ( W ), Loew, D ( D ), Ollivier, E ( E ), Saller, R ( R ), Schilcher, H ( H ), Simmet, T ( T ), Sticher, O ( O ), Vincieri, F F ( F F ), Vlietinck, A J ( A J ), Anton, R, Delaveau, P, Franz, G, Harvala, C, Kemper, F H, Kraft, K, Kubelka, W, Loew, D, Ollivier, E, Saller, R, Schilcher, H, Simmet, T, Sticher, O, Vincieri, F F, Vlietinck, A J, Anton, R ( R ), Delaveau, P ( P ), Franz, G ( G ), Harvala, C ( C ), Kemper, F H ( F H ), Kraft, K ( K ), Kubelka, W ( W ), Loew, D ( D ), Ollivier, E ( E ), Saller, R ( R ), Schilcher, H ( H ), Simmet, T ( T ), Sticher, O ( O ), Vincieri, F F ( F F ), and Vlietinck, A J ( A J )
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- 2009
162. Differentielle Effekte der hochfrequenten rTMS zur Rehabilitation von Handfunktionsstörungen nach kortikalen und subkortikalen Schlaganfall
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Ameli, M, Grefkes, C, Kemper, F, Dafotakis, M, Tittgemeyer, M, Karbe, H, Fink, G.R, and Nowak, D.A
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- 2024
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163. Kinematische Bewegungsanalyse in Diagnostik und Therapie des Morbus Parkinson
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Dafotakis, M, Ameli, M, Kemper, F, Fink, G.R, and Nowak, D.A
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- 2024
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164. Hochfrequente rTMS zur Therapie von Handfunktionsstörungen nach Schlaganfall: differentielle Effekte in Abhängigkeit von der Lokalisation der Läsion
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Ameli, M, Dafotakis, M, Grefkes, C, Kemper, F, Fink, G.R, and Nowak, D.A
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- 2024
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165. Arbitrary sensory-motor mapping during object manipulation in healthy persons
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Kemper, F, Ameli, M, Dafotakis, M, Fink, G.R, and Nowak, D.A
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- 2024
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166. The infrared spectral properties of magellanic carbon stars
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Sloan, G C, Kraemer, K E, McDonald, I, Groenewegen, M. A. T., Wood, Peter R, Zijlstra, Albert A, Lagadec, E., Boyer, M.L, Kemper, F, Matsuura, M., Sahai, Ragvendra, Sargent, B. A., Srinivasan, S., van Loon, Jacco Th, Volk, Kevin M., Sloan, G C, Kraemer, K E, McDonald, I, Groenewegen, M. A. T., Wood, Peter R, Zijlstra, Albert A, Lagadec, E., Boyer, M.L, Kemper, F, Matsuura, M., Sahai, Ragvendra, Sargent, B. A., Srinivasan, S., van Loon, Jacco Th, and Volk, Kevin M.
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- 2016
167. Toxicity of Organotin Compounds in Chicken and Rats
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Renhof, M., Kretzer, U., Schürmeyer, T., Skopnik, H., Kemper, F. H., Chambers, Philip L., editor, and Klinger, Wolfgang, editor
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- 1980
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168. Spitzer Space Telescope spectra of post-AGB stars in the Large Magellanic Cloud - polycyclic aromatic hydrocarbons at low metallicities
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Peeters, Els, Szczerba, R., Wood, P., Zijlstra, Albert, Hony, S., Ita, Yoshifusa, Kamath, Devika, Lagadec, Eric, Parker, Quentin, Reid, Warren, Shimonishi, Takashi, Van Winckel, H., Woods, Paul, Kemper, F., Meixner, Margaret, Otsuka, M., Sahai, R., Sargent, B., Hora, J., Mcdonald, Iain, Matsuura, Mikako, Bernard-Salas, Jeronimo, Evans, T., Volk, Kevin, Hrivnak, Bruce, Sloan, G., Chu, You-Hua, Gruendl, Robert, Kraemer, Kathleen, and University of St Andrews. School of Physics and Astronomy
- Subjects
Metallicity ,FOS: Physical sciences ,Astrophysics ,circumstellar matter ,Spectral line ,Spitzer Space Telescope ,QB Astronomy ,Large Magellanic Cloud ,Solar and Stellar Astrophysics (astro-ph.SR) ,QC ,QB ,Physics ,stars [infrared] ,Astronomy ,Astronomy and Astrophysics ,Planetary nebula ,Astrophysics - Astrophysics of Galaxies ,AGB and post-AGB [stars] ,Galaxy ,Interstellar medium ,Stars ,QC Physics ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,individual: Large Magellanic Cloud [galaxies] - Abstract
This paper reports variations of polycyclic aromatic hydrocarbons (PAHs) features that were found in Spitzer Space Telescope spectra of carbon-rich post-asymptotic giant branch (post-AGB) stars in the Large Magellanic Cloud (LMC). The paper consists of two parts. The first part describes our Spitzer spectral observing programme of 24 stars including post-AGB candidates. The latter half of this paper presents the analysis of PAH features in 20 carbon-rich post-AGB stars in the LMC, assembled from the Spitzer archive as well as from our own programme. We found that five post-AGB stars showed a broad feature with a peak at 7.7 micron, that had not been classified before. Further, the 10--13 micron PAH spectra were classified into four classes, one of which has three broad peaks at 11.3, 12.3 and 13.3 micron rather than two distinct sharp peaks at 11.3 and 12.7 micron, as commonly found in HII regions. Our studies suggest that PAHs are gradually processed while the central stars evolve from post-AGB phase to PNe, changing their composition before PAHs are incorporated into the interstellar medium. Although some metallicity dependence of PAH spectra exists, the evolutionary state of an object is more significant than its metallicity in determining the spectral characteristics of PAHs for LMC and Galactic post-AGB stars., Accepted by MNRAS
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- 2014
169. Physical properties of fullerene-containing Galactic planetary nebulae
- Author
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Cami, J., Peeters, E., Kemper, F., Otsuka, Masaaki, and Bernard-Salas, J.
- Subjects
Physics ,Fullerene ,010504 meteorology & atmospheric sciences ,Metallicity ,Milky Way ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Effective temperature ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Planetary nebula ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Spitzer Space Telescope ,13. Climate action ,Space and Planetary Science ,Nucleosynthesis ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Asymptotic giant branch ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences - Abstract
We searched the Spitzer Space Telescope data archive for Galactic planetary nebulae (PNe), that show the characteristic 17.4 and um features due to C60, also known as buckminsterfullerene. Out of 338 objects with Spitzer/IRS data, we found eleven C60-containing PNe, six of which (Hen2-68, IC2501, K3-62, M1-6, M1-9, and SaSt2-3) are new detections. We analyzed the spectra, along with ancillary data, using the photo-ionization code CLOUDY to establish the atomic line fluxes, and determine the properties of the radiation field, as set by the effective temperature of the central star. In addition, we measured the infrared spectral features due to dust grains. We find that the Polycyclic Aromatic Hydrocarbon (PAH) profile over 6-9 um in these C60-bearing carbon-rich PNe is of the more chemically-processed class A. The intensity ratio of 3.3 um to 11.3 um PAH indicates that the number of C-atoms per PAH in C60-containing PNe is small compared to that in non-C60 PNe. The Spitzer spectra also show broad dust features around 11 and 30 um. Analysis of the 30-um feature shows that it is strongly correlated with the continuum, and we propose that a single carbon-based carrier is responsible for both the continuum and the feature. The strength of the 11-um feature is correlated to the temperature of the dust, suggesting that it is at least partially due to a solid-state carrier. The chemical abundances of C60-containing PNe can be explained by AGB nucleosynthesis models for initially 1.5-2.5 Msun stars with Z=0.004. We plotted the locations of C60-containing PNe on a face-on map of the Milky Way and we found that most of these PNe are outside the solar circle, consistent with low metallicity values. Their metallicity suggests that the progenitors are an older population., Comment: 18 pages, 13 figures, 13 tables, Accepted for publication by MNRAS
- Published
- 2014
170. THE INFRARED SPECTRAL PROPERTIES OF MAGELLANIC CARBON STARS
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Sloan, G. C., primary, Kraemer, K. E., additional, McDonald, I., additional, Groenewegen, M. A. T., additional, Wood, P. R., additional, Zijlstra, A. A., additional, Lagadec, E., additional, Boyer, M. L., additional, Kemper, F., additional, Matsuura, M., additional, Sahai, R., additional, Sargent, B. A., additional, Srinivasan, S., additional, van Loon, J. Th., additional, and Volk, K., additional
- Published
- 2016
- Full Text
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171. XSHOOTER spectroscopy of the enigmatic planetary nebula Lin49 in the Small Magellanic Cloud
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Otsuka, Masaaki, primary, Kemper, F., additional, Leal-Ferreira, M. L., additional, Aleman, I., additional, Bernard-Salas, J., additional, Cami, J., additional, Ochsendorf, B. B., additional, Peeters, E., additional, and Scicluna, P., additional
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- 2016
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172. Constraints on the circumstellar dust around KIC 8462852
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Thompson, M. A., primary, Scicluna, P., additional, Kemper, F., additional, Geach, J. E., additional, Dunham, M. M., additional, Morata, O., additional, Ertel, S., additional, Ho, P. T. P., additional, Dempsey, J., additional, Coulson, I., additional, Petitpas, G., additional, and Kristensen, L. E., additional
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- 2016
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173. The evolved-star dust budget of the Small Magellanic Cloud: the critical role of a few key players
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Srinivasan, S., primary, Boyer, M. L., additional, Kemper, F., additional, Meixner, M., additional, Sargent, B. A., additional, and Riebel, D., additional
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- 2016
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174. THE 2014 ALMA LONG BASELINE CAMPAIGN: AN OVERVIEW
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Fomalont, E. B., Vlahakis, C., Corder, S., Remijan, A., Barkats, D., Lucas, R., Hunter, T. R., Brogan, C. L., Asaki, Y., Matsushita, S., Dent, W. R. F., Hills, R. E., Phillips, N., Richards, A. M. S., Cox, P., Amestica, R., Broguiere, D., Cotton, W., Hales, A. S., Hiriart, R., Hirota, A., Hodge, J. A., Impellizzeri, C. M. V., Kern, J., Kneissl, R., Liuzzo, E., Marcelino, N., Marson, R., Mignano, A., Nakanishi, K., Nikolic, B., Perez, J. E., Perez, L. M., Toledo, I., Aladro, R., Butler, B., Cortes, J., Cortes, P., Dhawan, V., Di Francesco, J., Espada, D., Galarza, F., Garcia-Appadoo, D., Guzman-Ramirez, L., Humphreys, E. M., Jung, T., Kameno, S., Laing, R. A., Leon, S., Mangum, J., Marconi, G., Nagai, H., Nyman, L. -A., Radiszcz, M., Rodon, J. A., Sawada, T., Takahashi, S., Tilanus, R. P. J., van Kempen, T., Vila Vilaro, B., Watson, L. C., Wiklind, T., Gueth, F., Tatematsu, K., Wootten, A., Castro-Carrizo, A., Chapillon, E., Dumas, G., de Gregorio-Monsalvo, I., Francke, H., Gallardo, J., Garcia, J., Gonzalez, S., Hibbard, J. E., Hill, T., Kaminski, T., Karim, A., Krips, M., Kurono, Y., Lopez, C., Martin, S., Maud, L., Morales, F., Pietu, V., Plarre, K., Schieven, G., Testi, L., Videla, L., Villard, E., Whyborn, N., Zwaan, M. A., Alves, F., Andreani, P., Avison, A., Barta, M., Bedosti, F., Bendo, G. J., Bertoldi, F., Bethermin, M., Biggs, A., Boissier, J., Brand, J., Burkutean, S., Casasola, V., Conway, J., Cortese, L., Dabrowski, B., Davis, T. A., Trigo, M. Diaz, Fontani, F., Franco-Hernandez, R., Fuller, G., Galvan Madrid, R., Giannetti, A., Ginsburg, A., Graves, S. F., Hatziminaoglou, E., Hogerheijde, M., Jachym, P., Serra, I. Jimenez, Karlicky, M., Klaasen, P., Kraus, M., Kunneriath, D., Lagos, C., Longmore, S., Leurini, S., Maercker, M., Magnelli, B., Vidal, I. Marti, Massardi, M., Maury, A., Muehle, S., Muller, S., Muxlow, T., O'Gorman, E., Paladino, R., Petry, D., Pineda, J., Randall, S., Richer, J. S., Rossetti, A., Rushton, A., Rygl, K., Monge, A. Sanchez, Schaaf, R., Schilke, P., Stanke, T., Schmalzl, M., Stoehr, F., Urban, S., van Kampen, E., Vlemmings, W., Wang, K., Wild, W., Yang, Y., Iguchi, S., Hasegawa, T., Saito, M., Inatani, J., Mizuno, N., Asayama, S., Kosugi, G., Morita, K. -I., Chiba, K., Kawashima, S., Okumura, S. K., Ohashi, N., Ogasawara, R., Sakamoto, S., Noguchi, T., Huang, Y. -D., Liu, S. -Y., Kemper, F., Koch, P. M., Chen, M. -T., Chikada, Y., Hiramatsu, M., Iono, D., Shimojo, M., Komugi, S., Kim, J., Lyo, A. -R., Muller, E., Herrera, C., Miura, R. E., Ueda, J., Chibueze, J., Su, Y. -N., Trejo-Cruz, A., Wang, K. -S., Kiuchi, H., Ukita, N., Sugimoto, M., Kawabe, R., Hayashi, M., Miyama, S., Ho, P. T. P., Kaifu, N., Ishiguro, M., Beasley, A. J., Bhatnagar, S., Braatz, J. A., III, Brisbin, D. G., Brunetti, N., Carilli, C., Crossley, J. H., D'Addario, L., Meyer, J. L. Donovan, Emerson, D. T., Evans, A. S., Fisher, P., Golap, K., Griffith, D. M., Hale, A. E., Halstead, D., Hardy, E. J., Hatz, M. C., Holdaway, M., Indebetouw, R., Jewell, P. R., Kepley, A. A., Kim, D. -C., Lacy, M. D., Leroy, A. K., Liszt, H. S., Lonsdale, C. J., Matthews, B., McKinnon, M., Mason, B. S., Moellenbrock, G., Moullet, A., Myers, S. T., Ott, J., Peck, A. B., Pisano, J., Radford, S. J. E., Randolph, W. T., Venkata, U. Rao, Rawlings, M. G., Rosen, R., Schnee, S. L., Scott, K. S., Sharp, N. K., Sheth, K., Simon, R. S., Tsutsumi, T., Wood, S. J., Fomalont, E. B., Vlahakis, C., Corder, S., Remijan, A., Barkats, D., Lucas, R., Hunter, T. R., Brogan, C. L., Asaki, Y., Matsushita, S., Dent, W. R. F., Hills, R. E., Phillips, N., Richards, A. M. S., Cox, P., Amestica, R., Broguiere, D., Cotton, W., Hales, A. S., Hiriart, R., Hirota, A., Hodge, J. A., Impellizzeri, C. M. V., Kern, J., Kneissl, R., Liuzzo, E., Marcelino, N., Marson, R., Mignano, A., Nakanishi, K., Nikolic, B., Perez, J. E., Perez, L. M., Toledo, I., Aladro, R., Butler, B., Cortes, J., Cortes, P., Dhawan, V., Di Francesco, J., Espada, D., Galarza, F., Garcia-Appadoo, D., Guzman-Ramirez, L., Humphreys, E. M., Jung, T., Kameno, S., Laing, R. A., Leon, S., Mangum, J., Marconi, G., Nagai, H., Nyman, L. -A., Radiszcz, M., Rodon, J. A., Sawada, T., Takahashi, S., Tilanus, R. P. J., van Kempen, T., Vila Vilaro, B., Watson, L. C., Wiklind, T., Gueth, F., Tatematsu, K., Wootten, A., Castro-Carrizo, A., Chapillon, E., Dumas, G., de Gregorio-Monsalvo, I., Francke, H., Gallardo, J., Garcia, J., Gonzalez, S., Hibbard, J. E., Hill, T., Kaminski, T., Karim, A., Krips, M., Kurono, Y., Lopez, C., Martin, S., Maud, L., Morales, F., Pietu, V., Plarre, K., Schieven, G., Testi, L., Videla, L., Villard, E., Whyborn, N., Zwaan, M. A., Alves, F., Andreani, P., Avison, A., Barta, M., Bedosti, F., Bendo, G. J., Bertoldi, F., Bethermin, M., Biggs, A., Boissier, J., Brand, J., Burkutean, S., Casasola, V., Conway, J., Cortese, L., Dabrowski, B., Davis, T. A., Trigo, M. Diaz, Fontani, F., Franco-Hernandez, R., Fuller, G., Galvan Madrid, R., Giannetti, A., Ginsburg, A., Graves, S. F., Hatziminaoglou, E., Hogerheijde, M., Jachym, P., Serra, I. Jimenez, Karlicky, M., Klaasen, P., Kraus, M., Kunneriath, D., Lagos, C., Longmore, S., Leurini, S., Maercker, M., Magnelli, B., Vidal, I. Marti, Massardi, M., Maury, A., Muehle, S., Muller, S., Muxlow, T., O'Gorman, E., Paladino, R., Petry, D., Pineda, J., Randall, S., Richer, J. S., Rossetti, A., Rushton, A., Rygl, K., Monge, A. Sanchez, Schaaf, R., Schilke, P., Stanke, T., Schmalzl, M., Stoehr, F., Urban, S., van Kampen, E., Vlemmings, W., Wang, K., Wild, W., Yang, Y., Iguchi, S., Hasegawa, T., Saito, M., Inatani, J., Mizuno, N., Asayama, S., Kosugi, G., Morita, K. -I., Chiba, K., Kawashima, S., Okumura, S. K., Ohashi, N., Ogasawara, R., Sakamoto, S., Noguchi, T., Huang, Y. -D., Liu, S. -Y., Kemper, F., Koch, P. M., Chen, M. -T., Chikada, Y., Hiramatsu, M., Iono, D., Shimojo, M., Komugi, S., Kim, J., Lyo, A. -R., Muller, E., Herrera, C., Miura, R. E., Ueda, J., Chibueze, J., Su, Y. -N., Trejo-Cruz, A., Wang, K. -S., Kiuchi, H., Ukita, N., Sugimoto, M., Kawabe, R., Hayashi, M., Miyama, S., Ho, P. T. P., Kaifu, N., Ishiguro, M., Beasley, A. J., Bhatnagar, S., Braatz, J. A., III, Brisbin, D. G., Brunetti, N., Carilli, C., Crossley, J. H., D'Addario, L., Meyer, J. L. Donovan, Emerson, D. T., Evans, A. S., Fisher, P., Golap, K., Griffith, D. M., Hale, A. E., Halstead, D., Hardy, E. J., Hatz, M. C., Holdaway, M., Indebetouw, R., Jewell, P. R., Kepley, A. A., Kim, D. -C., Lacy, M. D., Leroy, A. K., Liszt, H. S., Lonsdale, C. J., Matthews, B., McKinnon, M., Mason, B. S., Moellenbrock, G., Moullet, A., Myers, S. T., Ott, J., Peck, A. B., Pisano, J., Radford, S. J. E., Randolph, W. T., Venkata, U. Rao, Rawlings, M. G., Rosen, R., Schnee, S. L., Scott, K. S., Sharp, N. K., Sheth, K., Simon, R. S., Tsutsumi, T., and Wood, S. J.
- Abstract
A major goal of the Atacama Large Millimeter/submillimeter Array (ALMA) is to make accurate images with resolutions of tens of milliarcseconds, which at submillimeter (submm) wavelengths requires baselines up to similar to 15 km. To develop and test this capability, a Long Baseline Campaign (LBC) was carried out from 2014 September to late November, culminating in end-to-end observations, calibrations, and imaging of selected Science Verification (SV) targets. This paper presents an overview of the campaign and its main results, including an investigation of the short-term coherence properties and systematic phase errors over the long baselines at the ALMA site, a summary of the SV targets and observations, and recommendations for science observing strategies at long baselines. Deep ALMA images of the quasar 3C 138 at 97 and 241 GHz are also compared to VLA 43 GHz results, demonstrating an agreement at a level of a few percent. As a result of the extensive program of LBC testing, the highly successful SV imaging at long baselines achieved angular resolutions as fine as 19 mas at similar to 350 GHz. Observing with ALMA on baselines of up to 15 km is now possible, and opens up new parameter space for submm astronomy.
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- 2015
175. Severely comminuted femoral shaft fractures: Treatment by bridging-plate osteosynthesis
- Author
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Heitemeyer, U., Kemper, F., Hierholzer, G., and Haines, J.
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- 1987
- Full Text
- View/download PDF
176. Abstracts
- Author
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Van den Brink, F. G., Vaccari, Andrea, Cugurra, Franco, Mazzanti, L., Crema, A., Frigo, G. M., Del Tacca, M., Lecchini, S., Beani, L., Bianchi, C., Gandini, A., Lualdi, P., Della Bella, D., Rossini, L., Sardi, A., Baldoli, E., Caravaggi, A. M., Kyncl, J., Mauz, G., Kreye, V. A. W., Tubaro, E., Bulgini, M. J., Biagi, G. L., Barbaro, A. M., Guerra, M. C., Hümpel, J. -E., Zetler, G., Stern, P., del Bianco, P. L., Fanciullacci, M., Franchi, G., Sicuteri, F., Rovati, A. L., Casula, P. L., Meldolesi, J., Angelucci, L., Linari, G., Soldani, G., Pacini, S., de Pascale, V., Mantovani, P., Fregnan, G. B., GlÄsser, A. H., Jahrreiss, R., Habermann, E., Breithaupt, H., Rübsamen, K., Walsch, P., Lankisch, P. G., Vogt, W., Rudinger, J., Krejčí, I., Pliška, V., Poláček, I., Möhring, J., Brekner, Hanna, Schömig, A., Möhring, BÄrbel, Philippu, A., Przuntek, H., Pecile, A., Felici, M., Müller, E. E., Muller, E. E., Cocchi, D., Scapagnini, U., van Look, G. R., Moberg, G. P., Preziosi, P., Ganong, W. F., Fraschini, F., Vargiu, L., Spano, P. F., Marquardt, H., Zedeck, M. S., Sternberg, S. S., Fleisher, M., Hamilton, L. D., Classen, H. -G., Marquardt, P., SpÄth, M., Schumacher, K. -A., Bernauer, W., Hahn, F., Wissler, J., Nimptsch, P., Filipowski, P., Gjuriš, V., Wolf, D., Moroni, F., Buiatti, E., Mannaioni, P. F., Periti, P., Lorenz, W., Schauer, A., Reimann, H. J., Guidotti, A., Meyer, R., Doenicke, A., Schmal, A., Hutzel, M., Werle, E., Bertaccini, G., Impicciatore, M., Mossini, F., Frontini, E., Giani, G., Nicolin, A., Olivani, P., Dietmann, K., Schieck, A., Kornalik, F., Chiarra, A., Piccinini, F., Villani, F., Caspary, W. F., Nell, G., Forth, W., Overhoff, H., Pfleger, K., Rummel, W., Agsten, M., Voth, D., Possner, R., Förschler, M. -L., KÄvenheim, W., Kurz, H., Wirth, K., Bodem, G., Dengler, H. J., Rietbrock, N., Plato, H. v., Bergmann, K. v., Abshagen, U., Kewitz, H., Hengstmann, J. H., Konen, W., Konen, C., Backmann, H., Haschemian, A., Kemper, F., Morgenroth, K., Winterhoff, H., Mascherpa, P., Strauer, B. E., Westberg, C., Tauchert, M., Juhran, W., Ledda, F., Giotti, A., Turnheim, K., Stühlinger, W., Kraupp, O., Trendelenburg, U., Haeusler, G., Brandt, W., Reiter, M., Nakamura, J., Gerold, M., Thoenen, H., Boksay, I., Bollmann, V., Kukovetz, W. R., Klein, W. W., Pöch, G., Lüdtke, A. H., Braga, P. C., Ferri, S., Magnoni, V., Romano, A., Bartsch, W., Heinz, N., Furlanello, F., Ferrari, M., Sava, C., Maragno, I., Bergamaschi, M., Fuccella, L. M., Mandelli, V., Tommasini, R., Turba, C., Usardi, M., Lehr, E., Gesmundo, F., Susanna, A., Paroli, E., Carpi, A., Cartoni, C., Del Basso, P., Giardini, V., Marmo, E., Brogi, M., Bossa, R., Fioroni, G., Galatulas, I., Pomarelli, P., Henderson, P. Th., Remmer, H., Casals, J., Petruch, F., Schüppel, R., Forti, G. Cantelli, Fracasso, M. E., Berti, T., Maccari, M., Gatti, M. T., Losert, W., Kraaz, W., Jahn, P., Rilke, A., Cascio, G., Mantia, G., Leone, F., Datz, B., Vetter, J., Brade, W., Schönhöfer, P. S., Skidmore, I. F., Bourne, H. R., Vapaatalo, H., Bieck, P., Westermann, E., Stork, H., Schmidt, F. H., Riemenschneider, H., Willig, F., May, B., Leinweber, W., Poser, W., Panten, U., Hasselblatt, A., Klissiunis, N., Mykoniatis, M., Lengsfeld, H., Gey, K. F., Bianchini, P., Mantovani, V., LoMarco, E., Bufalina, L., Guidi, G., Osima, B., Casetta, R., Casarini, A., Mann, E., Pepeu, G., Ruffi, A., Mulas, A., Pleul, O., Lipparini, F., Loizzo, A., de Carolis, Scotti, Marino, A., Girone, E., Battista, O., de Marino, V., Florio, V., Longo, V. G., Gogolák, G., Stumpf, Ch., Pavan, P., Dross, K., Bianchi, A., Caprio, F., Kuschinsky, K., Di Carlo, R., Mandel, P., Di Rosa, M., Willoughby, D. A., Sorrentino, L., Capasso, F., Sandow, J., Alpermann, H., Metzger, H., Vogel, H. G., Velo, G. P., Capelli, A., Martinelli, G., Bertoni, F., Karzel, K., Peters, H. D., Hack, G., Fleming, K., Kazda, S., Lamprecht, F., Miksche, L., Orth, H., Philippi, A., Schmidt, D., Schneider, D., Soell, G., Taugner, R., Hammersen, G., Rosenthal, J., Fülgraff, G., Meiforth, A., Sudhoff, D., Zimmermann, E., Knebel, L., Barzaghi, F., Riva, M., Mantegazza, P., Chiesara, E., Edwards, K. D. G., Morini, M., Bilone, F., Morini, M., Ortolani, L., de Barbieri, A., Bertelli, A., Cerrati, A., Bizzi, A., Codegoni, A. M., Medea, A., Tacconi, M. T., Garattini, S., Bonaccorsi, A., Cotillo, P., and Babulova, A.
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- 1971
- Full Text
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177. Der Einfluß von Psychopharmaka auf Schilddrüse und Geschlechtsorgane von Ratten
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Kemper, F.
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- 1964
- Full Text
- View/download PDF
178. Studien zur „Übertragung“ der Masuginephritis der Ratte: IV. Versuch der diaplacentaren „Übertragung“
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Schöffling, K., Kemper, F., Sandritter, W., and Pfeiffer, E. F.
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- 1960
- Full Text
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179. Sport en maatschappij in Nederland: contouren van een nieuw sporthistorisch onderzoeksprogramma
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Heerma van Voss, L., Kemper, F., Breuker, P., Wals, H., Politiek Institutionele Geschiedenis, and Huygens ING
- Published
- 2012
180. Naar een toekomstbestendig volmachtmodel
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Kerste, M., Risseeuw, P., Brandt, M., Kemper, F., Baarsma, B., and SEO Economisch Onderzoek
- Abstract
Gevolmachtigd agenten voeren namens verzekeraars diensten uit op het gebied van acceptatie, polisbeheer, portefeuillemanagement en schadeafhandeling. Ze fungeren als schakelpunt tussen verzekeraars en bemiddelaars, en combineren de slagkracht van de verzekeraars met de korte afstand tot de markt van bemiddelaars. Gevolmachtigd agenten worden voor hun diensten beloond met verschillende soorten commissies en vergoedingen. In de optiek van de Nederlandse Vereniging van Gevolmachtigde Assurantiebedrijven (NVGA) en het Verbond van Verzekeraars is het bestaande vergoedingstelsel aan herijking toe. De NVGA en het Verbond van Verzekeraars hebben SEO Economisch Onderzoek en SVC daarom gevraagd om in samenwerking een inventariserend onderzoek te doen naar de mogelijkheden van een eenduidige, passende volmachtbeloning die voldoet aan eisen van transparantie, passendheid en bruikbaarheid. Dit rapport geeft de bevindingen weer. De uitkomsten bieden marktpartijen een kader waarbinnen ze een nieuwe beloningssystematiek kunnen ontwikkelen.
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- 2011
181. Inleiding
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Boessenkool, J.H., Waardenburg, M., Lucassen, J., Boessenkool, J., Kemper, F., UU LEG Research USG Public Matters Managing Social Issues, LS Management van Cultuur en Zingeving, and UU LEG Research USG Public Matters
- Published
- 2011
182. Determining the Forsterite Abundance of the Dust around AGB Stars
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de Vries, B.L., Min, M., Waters, L.B.F.M., Blommaert, J.A.D.L., Kemper, F., Wing, R.F. Kerschbaum, F., Lebzelter, T., Astrophysics, Sub Experiment. Astrophysics begr 1/1/14, and Low Energy Astrophysics (API, FNWI)
- Subjects
International (English) ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We present a diagnostic tool to determine the forsterite abundance of the dust ejected by AGB stars. Our method is based on a comparison between the observed strength of spectral bands of forsterite and model calculations. We show that the 11.3 {\mu}m forsterite band is a robust indicator of the forsterite abundance of the current mass-loss period for AGB stars with an optically thick dust shell. The 33.6 {\mu}m band of forsterite is sensitive to changes in the density and the geometry of the emitting dust shell, and so a less robust indicator. We apply this method to six high mass-loss rate AGB stars, showing that AGB stars can have forsterite abundances of 12% by mass and higher, which is more than the previously found maximum abundance of 5%.
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- 2011
183. DUST PRODUCTION BY EVOLVED STARS IN THE MAGELLANIC CLOUDS
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KEMPER, F., primary
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- 2015
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184. Comparative Studies of the Dust around Red Supergiant and Oxygen-Rich Asymptotic Giant Branch Stars in the Local Universe
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Sargent, B. A., primary, Srinivasan, S., additional, Speck, A., additional, Volk, K., additional, Kemper, F., additional, Reach, W., additional, Lagadec, E., additional, Bernard, J.-P., additional, McDonald, I., additional, Meixner, M., additional, Sloan, G. C., additional, and Jones, O., additional
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- 2015
- Full Text
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185. THE 2014 ALMA LONG BASELINE CAMPAIGN: AN OVERVIEW
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Partnership, ALMA, primary, Fomalont, E. B., additional, Vlahakis, C., additional, Corder, S., additional, Remijan, A., additional, Barkats, D., additional, Lucas, R., additional, Hunter, T. R., additional, Brogan, C. L., additional, Asaki, Y., additional, Matsushita, S., additional, Dent, W. R. F., additional, Hills, R. E., additional, Phillips, N., additional, Richards, A. M. S., additional, Cox, P., additional, Amestica, R., additional, Broguiere, D., additional, Cotton, W., additional, Hales, A. S., additional, Hiriart, R., additional, Hirota, A., additional, Hodge, J. A., additional, Impellizzeri, C. M. V., additional, Kern, J., additional, Kneissl, R., additional, Liuzzo, E., additional, Marcelino, N., additional, Marson, R., additional, Mignano, A., additional, Nakanishi, K., additional, Nikolic, B., additional, Perez, J. E., additional, Pérez, L. M., additional, Toledo, I., additional, Aladro, R., additional, Butler, B., additional, Cortes, J., additional, Cortes, P., additional, Dhawan, V., additional, Francesco, J. Di, additional, Espada, D., additional, Galarza, F., additional, Garcia-Appadoo, D., additional, Guzman-Ramirez, L., additional, Humphreys, E. M., additional, Jung, T., additional, Kameno, S., additional, Laing, R. A., additional, Leon, S., additional, Mangum, J., additional, Marconi, G., additional, Nagai, H., additional, Nyman, L.-A., additional, Radiszcz, M., additional, Rodón, J. A., additional, Sawada, T., additional, Takahashi, S., additional, Tilanus, R. P. J., additional, Kempen, T. van, additional, Vilaro, B. Vila, additional, Watson, L. C., additional, Wiklind, T., additional, Gueth, F., additional, Tatematsu, K., additional, Wootten, A., additional, Castro-Carrizo, A., additional, Chapillon, E., additional, Dumas, G., additional, de Gregorio-Monsalvo, I., additional, Francke, H., additional, Gallardo, J., additional, Garcia, J., additional, Gonzalez, S., additional, Hibbard, J. E., additional, Hill, T., additional, Kaminski, T., additional, Karim, A., additional, Krips, M., additional, Kurono, Y., additional, Lopez, C., additional, Martin, S., additional, Maud, L., additional, Morales, F., additional, Pietu, V., additional, Plarre, K., additional, Schieven, G., additional, Testi, L., additional, Videla, L., additional, Villard, E., additional, Whyborn, N., additional, Zwaan, M. A., additional, Alves, F., additional, Andreani, P., additional, Avison, A., additional, Barta, M., additional, Bedosti, F., additional, Bendo, G. J., additional, Bertoldi, F., additional, Bethermin, M., additional, Biggs, A., additional, Boissier, J., additional, Brand, J., additional, Burkutean, S., additional, Casasola, V., additional, Conway, J., additional, Cortese, L., additional, Dabrowski, B., additional, Davis, T. A., additional, Trigo, M. Diaz, additional, Fontani, F., additional, Franco-Hernandez, R., additional, Fuller, G., additional, Madrid, R. Galvan, additional, Giannetti, A., additional, Ginsburg, A., additional, Graves, S. F., additional, Hatziminaoglou, E., additional, Hogerheijde, M., additional, Jachym, P., additional, Serra, I. Jimenez, additional, Karlicky, M., additional, Klaasen, P., additional, Kraus, M., additional, Kunneriath, D., additional, Lagos, C., additional, Longmore, S., additional, Leurini, S., additional, Maercker, M., additional, Magnelli, B., additional, Vidal, I. Marti, additional, Massardi, M., additional, Maury, A., additional, Muehle, S., additional, Muller, S., additional, Muxlow, T., additional, O’Gorman, E., additional, Paladino, R., additional, Petry, D., additional, Pineda, J., additional, Randall, S., additional, Richer, J. S., additional, Rossetti, A., additional, Rushton, A., additional, Rygl, K., additional, Monge, A. Sanchez, additional, Schaaf, R., additional, Schilke, P., additional, Stanke, T., additional, Schmalzl, M., additional, Stoehr, F., additional, Urban, S., additional, Kampen, E. van, additional, Vlemmings, W., additional, Wang, K., additional, Wild, W., additional, Yang, Y., additional, Iguchi, S., additional, Hasegawa, T., additional, Saito, M., additional, Inatani, J., additional, Mizuno, N., additional, Asayama, S., additional, Kosugi, G., additional, Morita, K.-I., additional, Chiba, K., additional, Kawashima, S., additional, Okumura, S. K., additional, Ohashi, N., additional, Ogasawara, R., additional, Sakamoto, S., additional, Noguchi, T., additional, Huang, Y.-D., additional, Liu, S.-Y., additional, Kemper, F., additional, Koch, P. M., additional, Chen, M.-T., additional, Chikada, Y., additional, Hiramatsu, M., additional, Iono, D., additional, Shimojo, M., additional, Komugi, S., additional, Kim, J., additional, Lyo, A.-R., additional, Muller, E., additional, Herrera, C., additional, Miura, R. E., additional, Ueda, J., additional, Chibueze, J., additional, Su, Y.-N., additional, Trejo-Cruz, A., additional, Wang, K.-S., additional, Kiuchi, H., additional, Ukita, N., additional, Sugimoto, M., additional, Kawabe, R., additional, Hayashi, M., additional, Miyama, S., additional, Ho, P. T. P., additional, Kaifu, N., additional, Ishiguro, M., additional, Beasley, A. J., additional, Bhatnagar, S., additional, III, J. A. Braatz, additional, Brisbin, D. G., additional, Brunetti, N., additional, Carilli, C., additional, Crossley, J. H., additional, D’Addario, L., additional, Meyer, J. L. Donovan, additional, Emerson, D. T., additional, Evans, A. S., additional, Fisher, P., additional, Golap, K., additional, Griffith, D. M., additional, Hale, A. E., additional, Halstead, D., additional, Hardy, E. J., additional, Hatz, M. C., additional, Holdaway, M., additional, Indebetouw, R., additional, Jewell, P. R., additional, Kepley, A. A., additional, Kim, D.-C., additional, Lacy, M. D., additional, Leroy, A. K., additional, Liszt, H. S., additional, Lonsdale, C. J., additional, Matthews, B., additional, McKinnon, M., additional, Mason, B. S., additional, Moellenbrock, G., additional, Moullet, A., additional, Myers, S. T., additional, Ott, J., additional, Peck, A. B., additional, Pisano, J., additional, Radford, S. J. E., additional, Randolph, W. T., additional, Venkata, U. Rao, additional, Rawlings, M. G., additional, Rosen, R., additional, Schnee, S. L., additional, Scott, K. S., additional, Sharp, N. K., additional, Sheth, K., additional, Simon, R. S., additional, Tsutsumi, T., additional, and Wood, S. J., additional
- Published
- 2015
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186. Spitzerinfrared spectrograph point source classification in the Small Magellanic Cloud
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Ruffle, Paul M. E., primary, Kemper, F., additional, Jones, O. C., additional, Sloan, G. C., additional, Kraemer, K. E., additional, Woods, Paul M., additional, Boyer, M. L., additional, Srinivasan, S., additional, Antoniou, V., additional, Lagadec, E., additional, Matsuura, M., additional, McDonald, I., additional, Oliveira, J. M., additional, Sargent, B. A., additional, Sewiło, M., additional, Szczerba, R., additional, van Loon, J. Th., additional, Volk, K., additional, and Zijlstra, A. A., additional
- Published
- 2015
- Full Text
- View/download PDF
187. ERRATUM: “SPITZER SAGE-SPEC: NEAR INFRARED SPECTROSCOPY, DUST SHELLS, AND COOL ENVELOPES IN EXTREME LARGE MAGELLANIC CLOUD ASYMPTOTIC GIANT BRANCH STARS” (2014, AJ, 148, 86)
- Author
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Blum, R. D., primary, Srinivasan, S., additional, Kemper, F., additional, Ling, B., additional, and Volk, K., additional
- Published
- 2015
- Full Text
- View/download PDF
188. ERRATUM: “THE HERSCHEL INVENTORY OF THE AGENTS OF GALAXY EVOLUTION (HERITAGE) IN THE MAGELLANIC CLOUDS, A HERSCHEL OPEN TIME KEY PROGRAM” (2013, AJ, 146, 62)
- Author
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Meixner, M., primary, Panuzzo, P., additional, Roman-Duval, J., additional, Engelbracht, C., additional, Babler, B., additional, Seale, J., additional, Hony, S., additional, Montiel, E., additional, Sauvage, M., additional, Gordon, K., additional, Misselt, K., additional, Okumura, K., additional, Chanial, P., additional, Beck, T., additional, Bernard, J.-P., additional, Bolatto, A., additional, Bot, C., additional, Boyer, M. L., additional, Carlson, L. R., additional, Clayton, G. C., additional, Chen, C.-H. R., additional, Cormier, D., additional, Fukui, Y., additional, Galametz, M., additional, Galliano, F., additional, Hora, J. L., additional, Hughes, A., additional, Indebetouw, R., additional, Israel, F. P., additional, Kawamura, A., additional, Kemper, F., additional, Kim, S., additional, Kwon, E., additional, Lebouteiller, V., additional, Li, A., additional, Long, K. S., additional, Madden, S. C., additional, Matsuura, M., additional, Muller, E., additional, Oliveira, J. M., additional, Onishi, T., additional, Otsuka, M., additional, Paradis, D., additional, Poglitsch, A., additional, Reach, W. T., additional, Robitaille, T. P., additional, Rubio, M., additional, Sargent, B., additional, Sewiło, M., additional, Skibba, R., additional, Smith, L. J., additional, Srinivasan, S., additional, Tielens, A. G. G. M., additional, van Loon, J. Th., additional, and Whitney, B., additional
- Published
- 2015
- Full Text
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189. Fast electrically assisted regeneration of on-chip SERS substrates
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Meier, T.-A., primary, Poehler, E., additional, Kemper, F., additional, Pabst, O., additional, Jahnke, H.-G., additional, Beckert, E., additional, Robitzki, A., additional, and Belder, D., additional
- Published
- 2015
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- View/download PDF
190. De mixfactor van sport: eenheid en verdeeldheid op het veld
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Veldboer, L., Boonstra, N., Krouwel, A., Duyvendak, J.W., Kemper, F., and IMES (FMG)
- Abstract
In dit hoofdstuk laten we zien dat sport zowel verenigt als verdeelt. Sport versterkt bestaande sociale netwerken, maar sluit ook bepaalde groepen uit. Bovendien vergroot sport onderlinge competitiegevoelens die op hun beurt kunnen leiden tot onsportief en zelfs agressief gedrag. Sportdeelname is ook niet kleurenblind of klasseloos, sportparticipatie verloopt veelal langs gevestigde sociale scheidslijnen. In prestatieverband krijgen ontmoetingen tussen verschillende sociale milieus gestalte doordat de besten, ongeacht sociale achtergrond, bij elkaar worden geplaatst. Bij recreanten liggen dergelijke ontmoetingen minder voor het oprapen, maar toch zijn er ook hier wel gelegenheden voor interetnische interactie. Dit leidt tot meer contact, ook al blijft dat contact vaak ppervlakkig. Het is eigen aan de aard van sport als vrijetijdsactiviteit dat het een belangrijke rol speelt bij het ontwikkelen en in stand houden van de eigen identiteit. De wens om onder elkaar te verkeren is vaak een positieve keus. Schaduwkant hiervan is dat de hieruit resulterende lichte gemengde contacten in de sport minder dan gehoopt de beeldvorming over en weer tussen sociale groepen veranderen. Bij intensievere omgang in een gemeenschappelijk verband is daar meer kans op (bijvoorbeeld bij prestatiesport). ‘Sport verbroedert’, maar we mogen het effect niet overschatten.
- Published
- 2010
191. De mixfactor van sport
- Author
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Krouwel, A.P.M., Veldboer, L., Boonstra, N., Duyvendak, J.W., Kemper, F., Political Science, Political Science and Public Administration, and Multi-layered governance in EUrope and beyond (MLG)
- Published
- 2010
192. Infrared spectroscopy of asymptotic giant branch stars in the Galactic bulge
- Author
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Golriz, S.S., Blommaert, J A D L, Vanhollebeke, E, Groenewegen, M. A. T., Habing, H.J., Kemper, F, Schultheis, M, Tielens, A.G.G.M., Waters, L B F M, Wood, Peter R, Cami, J, Golriz, S.S., Blommaert, J A D L, Vanhollebeke, E, Groenewegen, M. A. T., Habing, H.J., Kemper, F, Schultheis, M, Tielens, A.G.G.M., Waters, L B F M, Wood, Peter R, and Cami, J
- Abstract
We have selected a homogeneous sample of asymptotic giant branch (AGB) stars in theGalactic bulge population from the ISOGAL survey. Our target stars cover a wide range of mass-loss rates (~10-8-10-4 M⊙ yr-1) and differ primarily by their age on the AGB
- Published
- 2014
193. A Spitzer Space Telescope survey of extreme Asymptotic Giant Branch stars in M32
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Jones, O. C., McDonald, I., Rich, R. M., Kemper, F., Boyer, M. L., Zijlstra, A. A., Bendo, G. J., Jones, O. C., McDonald, I., Rich, R. M., Kemper, F., Boyer, M. L., Zijlstra, A. A., and Bendo, G. J.
- Abstract
We investigate the population of cool, evolved stars in the Local Group dwarf elliptical galaxy M32, using Infrared Array Camera observations from the Spitzer Space Telescope. We construct deep mid-infrared colour-magnitude diagrams for the resolved stellar populations within 3.5 arcmin of M32's centre, and identify those stars that exhibit infrared excess. Our data is dominated by a population of luminous, dust-producing stars on the asymptotic giant branch (AGB) and extend to approximately 3 mag below the AGB tip. We detect for the first time a sizeable population of `extreme' AGB stars, highly enshrouded by circumstellar dust and likely completely obscured at optical wavelengths. The total dust-injection rate from the extreme AGB candidates is measured to be $7.5 \times 10^{-7}$ ${\rm M}_{\odot} \, {\rm yr}^{-1}$, corresponding to a gas mass-loss rate of $1.5 \times 10^{-4}$ ${\rm M}_{\odot} \, {\rm yr}^{-1}$. These extreme stars may be indicative of an extended star-formation epoch between 0.2 and 5 Gyr ago., Comment: Accepted for publication in MNRAS, 14 pages, 12 figures, 3 tables
- Published
- 2014
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194. The Mass-Loss Return from Evolved Stars to the Large Magellanic Cloud II: Dust Properties for Oxygen-Rich Asymptotic Giant Branch Stars
- Author
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Sargent, Benjamin A., Srinivasan, S., Meixner, M., Kemper, F., Tielens, A. G. G. M., Speck, A. K., Matsuura, M., Bernard, J. -Ph., Hony, S., Gordon, Karl D., Indebetouw, R., Marengo, M., Sloan, G. C., Woods, Paul M., Sargent, Benjamin A., Srinivasan, S., Meixner, M., Kemper, F., Tielens, A. G. G. M., Speck, A. K., Matsuura, M., Bernard, J. -Ph., Hony, S., Gordon, Karl D., Indebetouw, R., Marengo, M., Sloan, G. C., and Woods, Paul M.
- Abstract
We model multi-wavelength broadband UBVIJHKs and Spitzer IRAC and MIPS photometry and IRS spectra from the SAGE and SAGE-Spec observing programs of two oxygen-rich asymptotic giant branch (O-rich AGB) stars in the Large Magellanic Cloud (LMC) using radiative transfer models of dust shells around stars. We chose a star from each of the bright and faint O-rich AGB populations found by earlier studies of the SAGE sample in order to derive a baseline set of dust properties to be used in the construction of an extensive grid of radiative transfer models of the O-rich AGB stars found in the SAGE surveys. From the bright O-rich AGB population we chose HV 5715, and from the faint O-rich AGB population we chose SSTISAGE1C J052206.92-715017.6 (SSTSAGE052206). We found the complex indices of refraction of oxygen-deficient silicates from Ossenkopf et al (1992) and a "KMH"-like grain size distribution with gamma of -3.5, a_min of 0.01 microns, and a_0 of 0.1 microns to be reasonable dust properties for these models. There is a slight indication that the dust around the faint O-rich AGB may be more silica-rich than that around the bright O-rich AGB. Simple models of gas emission suggest a relatively extended gas envelope for the faint O-rich AGB star modeled, consistent with the relatively large dust shell inner radius for the same model. The models compute the dust mass-loss rates for the two stars to be 2.0x10^-9 M_Sun/yr and 2.3x10^-9 M_Sun/yr, respectively. When a dust-to-gas mass ratio of 0.002 is assumed for SSTSAGE052206 and HV 5715, the dust mass-loss rates imply total mass-loss rates of 1.0x10^-6 M_Sun/yr and 1.2x10^-6 M_Sun/yr, respectively. These properties of the dust shells and stars, as inferred from our models of the two stars, are found to be consistent with properties observed or assumed by detailed studies of other O-rich AGB stars in the LMC and elsewhere., Comment: 37 pages, 3 figures, appeared in the 10 June 2010 issue of the Astrophysical Journal
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- 2014
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195. Spitzer SAGE-Spec: Near Infrared Spectroscopy, Dust Shells, and Cool Envelopes in Extreme Large Magellanic Cloud AGB Stars
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Blum, R. D., Srinivasan, S., Kemper, F., Ling, B., Volk, K., Blum, R. D., Srinivasan, S., Kemper, F., Ling, B., and Volk, K.
- Abstract
K-band spectra are presented for a sample of 39 Spitzer IRS SAGE-Spec sources in the Large Magellanic Cloud. The spectra exhibit characteristics in very good agreement with their positions in the near infrared - Spitzer color-magnitude diagrams and their properties as deduced from the Spitzer IRS spectra. Specifically, the near infrared spectra show strong atomic and molecular features representative of oxygen-rich and carbon-rich asymptotic giant branch stars, respectively. A small subset of stars were chosen from the luminous and red extreme "tip" of the color magnitude diagram. These objects have properties consistent with dusty envelopes but also cool, carbon-rich "stellar" cores. Modest amounts of dust mass loss combine with the stellar spectral energy distribution to make these objects appear extreme in their near infrared and mid infrared colors. One object in our sample, HV 915, a known post asymptotic giant branch star of the RV Tau type exhibits CO 2.3 micron band head emission consistent with previous work that demonstrates the object has a circumstellar disk., Comment: 32 pages, 12 figures (eps), accepted for publication in the AJ
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- 2014
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196. Carbon-rich dust past the asymptotic giant branch: aliphatics, aromatics, and fullerenes in the Magellanic Clouds
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Sloan, G. C., Lagadec, E., Zijlstra, A. A., Kraemer, K. E., Weis, A. P., Matsuura, M., Volk, K., Peeters, E., Duley, W. W., Cami, J., Bernard-Salas, J., Kemper, F., Sahai, R., Sloan, G. C., Lagadec, E., Zijlstra, A. A., Kraemer, K. E., Weis, A. P., Matsuura, M., Volk, K., Peeters, E., Duley, W. W., Cami, J., Bernard-Salas, J., Kemper, F., and Sahai, R.
- Abstract
Infrared spectra of carbon-rich objects which have evolved off the asymptotic giant branch reveal a range of dust properties, including fullerenes, polycyclic aromatic hydrocarbons (PAHs), aliphatic hydrocarbons, and several unidentified features, including the 21 um emission feature. To test for the presence of fullerenes, we used the position and width of the feature at 18.7-18.9 um and examined other features at 17.4 and 6-9 um. This method adds three new fullerene sources to the known sample, but it also calls into question three previous identifications. We confirm that the strong 11 um features seen in some sources arise primarily from SiC, which may exist as a coating around carbonaceous cores and result from photo-processing. Spectra showing the 21 um feature usually show the newly defined Class D PAH profile at 7-9 um. These spectra exhibit unusual PAH profiles at 11-14 um, with weak contributions at 12.7 um, which we define as Class D1, or show features shifted to ~11.4, 12.4, and 13.2 um, which we define as Class D2. Alkyne hydrocarbons match the 15.8 um feature associated with 21 um emission. Sources showing fullerene emission but no PAHs have blue colors in the optical, suggesting a clear line of sight to the central source. Spectra with 21 um features and Class D2 PAH emission also show photometric evidence for a relatively clear line of sight to the central source. The multiple associations of the 21 um feature to aliphatic hydrocarbons suggest that the carrier is related to this material in some way., Comment: 30 pages, 30 figures, ApJ, in press
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- 2014
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197. Interstellar and circumstellar fullerenes
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Bernard-Salas, J., Cami, J., Jones, A. P., Peeters, E., Micelotta, E. R., Otsuka, M., Sloan, G. C., Kemper, F., Groenewegen, M., Bernard-Salas, J., Cami, J., Jones, A. P., Peeters, E., Micelotta, E. R., Otsuka, M., Sloan, G. C., Kemper, F., and Groenewegen, M.
- Abstract
Fullerenes are a particularly stable class of carbon molecules in the shape of a hollow sphere or ellipsoid that might be formed in the outflows of carbon stars. Once injected into the interstellar medium (ISM), these stable species survive and are thus likely to be widespread in the Galaxy where they contribute to interstellar extinction, heating processes, and complex chemical reactions. In recent years, the fullerene species C60 (and to a lesser extent C70) have been detected in a wide variety of circumstellar and interstellar environments showing that when conditions are favourable, fullerenes are formed efficiently. Fullerenes are the first and only large aromatics firmly identified in space. The detection of fullerenes is thus crucial to provide clues as to the key chemical pathways leading to the formation of large complex organic molecules in space, and offers a great diagnostic tool to describe the environment in which they reside. Since fullerenes share many physical properties with PAHs, understanding how fullerenes form, evolve and respond to their physical environment will yield important insights into one of the largest reservoirs of organic material in space. In spite of all these detections, many questions remain about precisely which members of the fullerene family are present in space, how they form and evolve, and what their excitation mechanism is. We present here an overview of what we know from astronomical observations of fullerenes in these different environments, and discuss current thinking about the excitation process. We highlight the various formation mechanisms that have been proposed, discuss the physical conditions conducive to the formation and/or detection of fullerenes in carbon stars, and their possible connection to PAHs, HACs and other dust features., Comment: 6 pages, 2 figures. Proceedings of "The Life Cycle of Dust in the Universe: Observations, Theory, and laboratory Experiments". Taipei, Taiwan 18-22 November 2013. Editors: A. Andersen, M. Baes, H. Gomez, C. Kemper, D. Watson
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- 2014
198. Modelling the alumina abundance of oxygen-rich evolved stars in the Large Magellanic Cloud
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Jones, O. C., Kemper, F., Srinivasan, S., McDonald, I., Sloan, G. C., Zijlstra, A. A., Jones, O. C., Kemper, F., Srinivasan, S., McDonald, I., Sloan, G. C., and Zijlstra, A. A.
- Abstract
In order to determine the composition of the dust in the circumstellar envelopes of oxygen-rich asymptotic giant branch (AGB) stars we have computed a grid of modust radiative-transfer models for a range of dust compositions, mass-loss rates, dust shell inner radii and stellar parameters. We compare the resulting colours with the observed oxygen-rich AGB stars from the SAGE-Spec Large Magellanic Cloud (LMC) sample, finding good overall agreement for stars with a mid-infrared excess. We use these models to fit a sample of 37 O-rich AGB stars in the LMC with optically thin circumstellar envelopes, for which 5$-$35-$\mu$m Spitzer infrared spectrograph (IRS) spectra and broadband photometry from the optical to the mid-infrared are available. From the modelling, we find mass-loss rates in the range $\sim 8\times10^{-8}$ to $5\times10^{-6}$ M$_{\odot}\ \mathrm{yr}^{-1}$, and we show that a grain mixture consisting primarily of amorphous silicates, with contributions from amorphous alumina and metallic iron provides a good fit to the observed spectra. Furthermore, we show from dust models that the AKARI [11]$-$[15] versus [3.2]$-$[7] colour-colour diagram, is able to determine the fractional abundance of alumina in O-rich AGB stars., Comment: 22 pages, 17 figures, accepted MNRAS
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- 2014
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199. Spitzer Space Telescope spectra of post-AGB stars in the Large Magellanic Cloud ---polycyclic aromatic hydrocarbons at low metallicities
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Matsuura, Mikako, Bernard-Salas, Jeronimo, Evans, T. Lloyd, Volk, Kevin M., Hrivnak, Bruce J., Sloan, G. C., Chu, You-Hua, Gruendl, Robert, Kraemer, Kathleen E., Peeters, Els, Szczerba, R., Wood, P. R., Zijlstra, Albert A., Hony, S., Ita, Yoshifusa, Kamath, Devika, Lagadec, Eric, Parker, Quentin A, Reid, Warren A., Shimonishi, Takashi, Van Winckel, H., Woods, Paul M., Kemper, F., Meixner, Margaret, Otsuka, M., Sahai, R., Sargent, B. A., Hora, J. L., McDonald, Iain, Matsuura, Mikako, Bernard-Salas, Jeronimo, Evans, T. Lloyd, Volk, Kevin M., Hrivnak, Bruce J., Sloan, G. C., Chu, You-Hua, Gruendl, Robert, Kraemer, Kathleen E., Peeters, Els, Szczerba, R., Wood, P. R., Zijlstra, Albert A., Hony, S., Ita, Yoshifusa, Kamath, Devika, Lagadec, Eric, Parker, Quentin A, Reid, Warren A., Shimonishi, Takashi, Van Winckel, H., Woods, Paul M., Kemper, F., Meixner, Margaret, Otsuka, M., Sahai, R., Sargent, B. A., Hora, J. L., and McDonald, Iain
- Abstract
This paper reports variations of polycyclic aromatic hydrocarbons (PAHs) features that were found in Spitzer Space Telescope spectra of carbon-rich post-asymptotic giant branch (post-AGB) stars in the Large Magellanic Cloud (LMC). The paper consists of two parts. The first part describes our Spitzer spectral observing programme of 24 stars including post-AGB candidates. The latter half of this paper presents the analysis of PAH features in 20 carbon-rich post-AGB stars in the LMC, assembled from the Spitzer archive as well as from our own programme. We found that five post-AGB stars showed a broad feature with a peak at 7.7 micron, that had not been classified before. Further, the 10--13 micron PAH spectra were classified into four classes, one of which has three broad peaks at 11.3, 12.3 and 13.3 micron rather than two distinct sharp peaks at 11.3 and 12.7 micron, as commonly found in HII regions. Our studies suggest that PAHs are gradually processed while the central stars evolve from post-AGB phase to PNe, changing their composition before PAHs are incorporated into the interstellar medium. Although some metallicity dependence of PAH spectra exists, the evolutionary state of an object is more significant than its metallicity in determining the spectral characteristics of PAHs for LMC and Galactic post-AGB stars., Comment: Accepted by MNRAS
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- 2014
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200. Molecular hydrogen emission in the interstellar medium of the Large Magellanic Cloud
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Naslim, N., primary, Kemper, F., additional, Madden, S. C., additional, Hony, S., additional, Chu, Y.- H., additional, Galliano, F., additional, Bot, C., additional, Yang, Y., additional, Seok, J., additional, Oliveira, J. M., additional, van Loon, J. T., additional, Meixner, M., additional, Li, A., additional, Hughes, A., additional, Gordon, K. D., additional, Otsuka, M., additional, Hirashita, H., additional, Morata, O., additional, Lebouteiller, V., additional, Indebetouw, R., additional, Srinivasan, S., additional, Bernard, J.- P., additional, and Reach, W. T., additional
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- 2014
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