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Imaging the water masers toward the H2O-PN IRAS 18061–2505

Published online by Cambridge University Press:  24 July 2012

Yolanda Gómez ,
Daniel Tafoya ,
Olga Suárez ,
Jose F. Gómez ,
Luis F. Miranda ,
Guillem Anglada ,
Jóse M. Torrelles  and
Roberto Vázquez
Yolanda Gómez
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAMAntigua Carretera a Pátzcuaro # 8701 Ex-Hda. San José de la Huerta Morelia, Michoacán. México. C.P.58089 Apartado Postal 3-72 (Xangari).
Daniel Tafoya
Affiliation:
Department of Physics and Astronomy, Kagoshima University, Japan. email: [email protected]
Olga Suárez
Affiliation:
Université de Nice Sophia Antipolis, France.
Jose F. Gómez
Affiliation:
Instituto de Astrofísica de Andalucía, Spain.
Luis F. Miranda
Affiliation:
Departmento de Física Aplicada, Universidade de Vigo, Spain.
Guillem Anglada
Affiliation:
Instituto de Astrofísica de Andalucía, Spain.
Jóse M. Torrelles
Affiliation:
Facultat de Fisica, Instituto de Ciencias del Espacio, Spain.
Roberto Vázquez
Affiliation:
Observatorio Astronómico Nacional, UNAM, México.
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Abstract

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It has been suggested that the presence of disks or tori around the central stars of pre Planetary Nebulae and Planetary Nebulae is related to the collimation of the jet that are frequently observed in these sources. These disks or tori can be traced by the maser emission of some molecules such as water. In this work we present Very Large Array (VLA) observations of the water maser emission at 22 GHz toward the PN IRAS 18061–2505, for which the masers appear located on one side of the central star. For comparison with the observations, we present a simple kinematical model of a disk rotating and expanding around the central star. The model matches qualitatively the observations. However, since the masers appear only on one side of the disk, these results are not conclusive.

Keywords

(ISM:) planetary nebulae: individual (IRAS 18061–2505)ISM: jets and outflowsmasers
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S287: Cosmic Masers - from OH to H0 , January 2012 , pp. 258 - 259
Copyright
Copyright © International Astronomical Union 2012

References

de Gregorio-Monsalvo, I., Gómez, Y., Anglada, G., Cesaroni, R., Miranda, L. F., Gómez, J. F., & Torrelles, J. M. 2003, ApJ, 601, 921CrossRefGoogle Scholar
Gómez, J. F., Suárez, O., Gómez, Y., Miranda, L. F., Torrelles, J. M., Anglada, G., & Morata, O. 2008, AJ, 135, 2074CrossRefGoogle Scholar
Miranda, L. F., Gómez, Y., Anglada, G., & Torrelles, J. M. 2001, Nature 414, 284CrossRefGoogle Scholar
Reyes-Ruiz, M. & López, J. A. 1999, ApJ, 524, 952Google Scholar
Tafoya, D., Gómez, Y., Patel, N. A., Torrelles, J. M., Gómez, J. F., Anglada, G., Miranda, L. F., & de Gregorio-Monsalvo, I. 2009, ApJ 691, 611CrossRefGoogle Scholar
Uscanga, L., Gómez, Y., Raga, A. C., Cantó, J., Anglada, G., Gómez, J. F., Torrelles, J. M., & Miranda, L. F. 2008, MNRAS, 390, 1127CrossRefGoogle Scholar