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Planetary nebulae and determination of the bulge–disk boundary

Published online by Cambridge University Press:  26 February 2013

Roberto D. D. Costa ,
Oscar Cavichia  and
Walter J. Maciel
Roberto D. D. Costa
Affiliation:
Departamento de Astronomia, IAG, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo/SP, Brazil email: [email protected], [email protected], [email protected]
Oscar Cavichia
Affiliation:
Departamento de Astronomia, IAG, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo/SP, Brazil email: [email protected], [email protected], [email protected]
Walter J. Maciel
Affiliation:
Departamento de Astronomia, IAG, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo/SP, Brazil email: [email protected], [email protected], [email protected]
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Abstract

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In this paper, a sample of planetary nebulae in the Galaxy's inner-disk and bulge is used to find the galactocentric distance that optimally separates these two populations in terms of their abundances. Statistical distance scales were used to investigate the distribution of abundances across the disk–bulge interface, while a Kolmogorov–Smirnov test was used to find the distance at which the chemical properties of these regions separate optimally. The statistical analysis indicates that, on average, the inner population is characterized by lower abundances than the outer component. Additionally, for the α-element abundances, the inner population does not follow the disk's radial gradient toward the Galactic Center. Based on our results, we suggest a bulge–disk interface at 1.5 kpc, marking the transition between the bulge and the inner disk of the Galaxy as defined by the intermediate-mass population.

Keywords

techniques: spectroscopicmethods: numericalplanetary nebulae: generalGalaxy: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S289: Advancing the Physics of Cosmic Distances , August 2012 , pp. 375 - 378
Copyright
Copyright © International Astronomical Union 2013

References

Alexander, J. & Balick, B. 1997, AJ, 114, 713Google Scholar
Cavichia, O., Costa, R. D. D., & Maciel, W. J. 2010, Rev. Mex. A&A, 46, 159Google Scholar
Cavichia, O., Costa, R. D. D., & Maciel, W. J. 2011, Rev. Mex. A&A, 47, 49Google Scholar
Escudero, A. V., Costa, R. D. D., & Maciel, W. J. 2004, A&A, 414, 211Google Scholar
Górny, S. K., Stasińska, G., Escudero, A. V., & Costa, R. D. D. 2004, A&A, 427, 231Google Scholar
Gutenkunst, S., Bernard-Salas, J., Pottasch, S., Sloan, G., & Houck, J. R. 2008, ApJ, 680, 1206CrossRefGoogle Scholar
Maciel, W. J., Lago, L., & Costa, R. D. D. 2006, A&A, 453, 587Google Scholar
Stanghellini, L., Shaw, R. A., & Villaver, E. 2008, ApJ, 689, 194 (SSV08)Google Scholar
Zhang, C. Y. 1995, ApJS 98 659 (Z95)Google Scholar