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Your search keyword '"Schilke, P."' showing total 12 results
Start Over Author "Schilke, P." Publication Year Range Last 3 years Publisher edp sciences
12 results on '"Schilke, P."'

5. HyGAL: Characterizing the Galactic ISM with observations of hydrides and other small molecules

Author

Kim, W.-J., primary, Schilke, P., additional, Neufeld, D. A., additional, Jacob, A. M., additional, Sánchez-Monge, Á., additional, Seifried, D., additional, Godard, B., additional, Menten, K. M., additional, Walch, S., additional, Falgarone, E., additional, Veena, V. S., additional, Bialy, S., additional, Möller, T., additional, and Wyrowski, F., additional

Published
2023
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6. A Survey of SiO J = 1 – 0 emission toward massive star-forming regions

Author

Kim, W.-J., Urquhart, J.S., Veena, V.S., Fuller, G.A., Schilke, P., Kim, K-T, Kim, W.-J., Urquhart, J.S., Veena, V.S., Fuller, G.A., Schilke, P., and Kim, K-T

Abstract

Aims. The application of silicon monoxide (SiO) as a shock tracer arises from its propensity to occur in the gas phase as a result of shock-induced phenomena, including outflow activity and interactions between molecular clouds and expanding Hii regions or supernova remnants. Here we search for indications of shocks toward 366 massive star-forming regions by observing the ground rotational transition of SiO (v = 0, J = 1 − 0) at 43 GHz with the Korean VLBI Network (KVN) 21 m telescopes to extend our understanding on the origins of SiO in star-forming regions. Methods. We analyze the thermal SiO 1 – 0 emission and compare the properties of SiO emission with the physical parameters of associated massive dense clumps as well as 22 GHz H2O and Class I 44 GHz CH3OH maser emission. Results. We detect SiO emission toward 104 regions which consist of 57 IRDCs, 21 HMPOs, and 26 UCHiis. Out of 104 sources, 71 and 80 sources have 22 GHz H2O and 44 GHz Class I CH3OH maser counterparts, respectively. The determined median SiO column density, N(SiO), and abundance, X(SiO), relative to N(H2) are 8.12 × 1012 cm−2 and 1.28 × 10−10, respectively. These values are similar to those obtained toward other star-forming regions and also consistent with predicted values from shock models with low-velocity shocks (≲10 – 15 km s−1). For sources with dust temperatures (Tdust) ≲ 20 K, we find that N(SiO) and X(SiO) derived with the J = 1 − 0 transition are a factor ∼ 3 larger than those from the previous studies obtained with SiO 2 – 1. While the X(SiO) does not exhibit any strong correlation with the evolutionary stages of their host clumps, LSiO is highly correlated with dust clump mass, and LSiO/Lbol also has a strong negative correlation with Tdust. This shows that colder and younger clumps have high LSiO/Lbol suggestive of an evolutionary trend. This trend is not due to excess emission at higher velocities, such as SiO wing features, as the colder sources with high LSiO/Lbol ratios lack wi

Published
2023

7. N-bearing complex organics toward high-mass protostars

Author

Nazari, P., primary, Meijerhof, J. D., additional, van Gelder, M. L., additional, Ahmadi, A., additional, van Dishoeck, E. F., additional, Tabone, B., additional, Langeroodi, D., additional, Ligterink, N. F. W., additional, Jaspers, J., additional, Beltrán, M. T., additional, Fuller, G. A., additional, Sánchez-Monge, Á., additional, and Schilke, P., additional

Published
2022
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8. Methanol deuteration in high-mass protostars

Author

van Gelder, M. L., primary, Jaspers, J., additional, Nazari, P., additional, Ahmadi, A., additional, van Dishoeck, E. F., additional, Beltrán, M. T., additional, Fuller, G. A., additional, Sánchez-Monge, Á., additional, and Schilke, P., additional

Published
2022
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9. The physical and chemical structure of Sagittarius B2

Author

Meng, F., primary, Sánchez-Monge, Á., additional, Schilke, P., additional, Ginsburg, A., additional, DePree, C., additional, Budaiev, N., additional, Jeff, D., additional, Schmiedeke, A., additional, Schwörer, A., additional, Veena, V. S., additional, and Möller, Th., additional

Published
2022
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10. Importance of source structure on complex organics emission

Author

van Gelder, M. L., primary, Nazari, P., additional, Tabone, B., additional, Ahmadi, A., additional, van Dishoeck, E. F., additional, Beltrán, M. T., additional, Fuller, G. A., additional, Sakai, N., additional, Sánchez-Monge, Á., additional, Schilke, P., additional, Yang, Y.-L., additional, and Zhang, Y., additional

Published
2022
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11. The sharp ALMA view of infall and outflow in the massive protocluster G31.41+0.31

Author

Beltrán, M. T., primary, Rivilla, V. M., additional, Cesaroni, R., additional, Galli, D., additional, Moscadelli, L., additional, Ahmadi, A., additional, Beuther, H., additional, Etoka, S., additional, Goddi, C., additional, Klaassen, P. D., additional, Kuiper, R., additional, Kumar, M. S. N., additional, Lorenzani, A., additional, Peters, T., additional, Sánchez-Monge, Á., additional, Schilke, P., additional, van der Tak, F., additional, and Vig, S., additional

Published
2022
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12. Disk fragmentation in high-mass star formation

Author

Suri, S., primary, Beuther, H., additional, Gieser, C., additional, Ahmadi, A., additional, Sánchez-Monge, Á., additional, Winters, J. M., additional, Linz, H., additional, Henning, Th., additional, Beltrán, M. T., additional, Bosco, F., additional, Cesaroni, R., additional, Csengeri, T., additional, Feng, S., additional, Hoare, M. G., additional, Johnston, K. G., additional, Klaassen, P., additional, Kuiper, R., additional, Leurini, S., additional, Longmore, S., additional, Lumsden, S., additional, Maud, L., additional, Moscadelli, L., additional, Möller, T., additional, Palau, A., additional, Peters, T., additional, Pudritz, R. E., additional, Ragan, S. E., additional, Semenov, D., additional, Schilke, P., additional, Urquhart, J. S., additional, Wyrowski, F., additional, and Zinnecker, H., additional

Published
2021
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