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HCO+ emission possibly related with a shielding mechanism that protects water molecules in the young PN K 3-35

Published online by Cambridge University Press:  01 February 2008

Y. Gómez ,
D. Tafoya ,
G. Anglada ,
L. Loinard ,
J. M. Torrelles ,
L. F. Miranda ,
M. Osorio ,
R. Franco-Hernández ,
L. Nyman  and
J. Nakashima
...Show all authors
Y. Gómez
Affiliation:
Centro de Radioastronomía y astrofísica, UNAM, México email: [email protected]
D. Tafoya
Affiliation:
Centro de Radioastronomía y astrofísica, UNAM, México email: [email protected] Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
G. Anglada
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Granada, Spain
L. Loinard
Affiliation:
Centro de Radioastronomía y astrofísica, UNAM, México email: [email protected]
J. M. Torrelles
Affiliation:
Instituto de Ciencias del Espacio, and IEE de Catalunya, Barcelona, Spain
L. F. Miranda
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Granada, Spain
M. Osorio
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Granada, Spain
R. Franco-Hernández
Affiliation:
Centro de Radioastronomía y astrofísica, UNAM, México email: [email protected] Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
L. Nyman
Affiliation:
European Southern Observatory, Santiago, Chile
J. Nakashima
Affiliation:
Department of Physics, University of Hong Kong, Hong Kong
S. Deguchi
Affiliation:
Nobeyama Radio Observatory, NAO, Nagano, Japan
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Abstract

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Water maser emission has been detected only toward three planetary nebulae (PNe). In particular, in K3-35, the first PN where water vapor maser emission was detected, the components are located in a torus-like structure with a radius of 85 AU and also at the surprisingly large distance of 5000 AU from the star, in the tips of the bipolar lobes. The existence of these water molecules in PNe is puzzling, probably related to some unknown mechanism shielding them against the ionizing radiation. We report the detection of HCO+ (J = 1 − 0) emission toward K 3-35, that not only suggests that dense molecular gas (~105 cm−3) is present in this PN, but also that this kind of PN can enrich their surroundings with organic molecules.

Keywords

Planetary Nebulastars: individual (K 3-35)radio lines: moleculesstars: circumstellar matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S251: Organic Matter in Space , February 2008 , pp. 173 - 174
Copyright
Copyright © International Astronomical Union 2008

References

de Gregorio-Monsalvo, I., Gómez, Y., Anglada, G., Cesaroni, R., Miranda, L. F., Gómez, J. F., & Torrelles, J. M. 2004, ApJ 601, 921CrossRefGoogle Scholar
Gómez, Y. 2007, Astrophysical masers and their environments, IAU Proceedings 242, 292Google Scholar
Gómez, J. F., Suárez, O., Gómez, Y., Miranda, L. F., Torrelles, J. M., Anglada, G., & Morata, O. 2008, AJ in press.Google Scholar
Miranda, L. F., Gómez, Y., Anglada, G., & Torrelles, J. M. 2001, Nature 414, 284CrossRefGoogle Scholar
Tafoya, D., et al. 2007, ApJ 133, 364CrossRefGoogle Scholar
Velázquez, P. F., Gómez, Y., Esquivel, A., & Raga, A. C. 2007, MNRAS 382, 1965CrossRefGoogle Scholar