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Dust & Abundances of Metal-Poor Planetary Nebulae in the Galactic Anti-Center

Published online by Cambridge University Press:  08 August 2017

George J. S. Pagomenos Open the ORCID record for George J. S. Pagomenos [Opens in a new window] ,
Jeronimo Bernard-Salas  and
G. C. Sloan Open the ORCID record for G. C. Sloan [Opens in a new window]
George J. S. Pagomenos
Affiliation:
School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, Bucks, MK7 6AA, UK email: george.pagomenos@open.ac.uk
Jeronimo Bernard-Salas
Affiliation:
School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, Bucks, MK7 6AA, UK email: george.pagomenos@open.ac.uk
G. C. Sloan
Affiliation:
Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA Cornell Center for Astrophysics & Planetary Science, Cornell Univ., Ithaca, NY 14853-6801, USA
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Abstract

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Much of the new dust in the local ISM is produced in the last phases of stellar evolution of low- and intermediate-mass stars on the Asymptotic Giant Branch (AGB). Despite its importance, our knowledge of how dust properties depend on metallicity is limited. Studies of planetary nebulae in irregular galaxies in the Local Group (mostly focused on the LMC and SMC) have revealed a diverse spectral zoo and shown that low metallicity favours carbon-rich dust production by AGB stars. However, at ~1/3 and ~1/5 times the solar metallicity respectively, they provide two snapshots of dust composition at low metallicity, emphasising the need to investigate a region with a range of metallicity values. With its abundance gradient, the Milky Way fits this criterion and provides a good opportunity to observe the dust composition over a large metallicity range. In particular the Galactic anti-center, which is largely unexplored beyond galactocentric distances of 10 kpc, allows us to study the AGB dust a priori assumed to be metal-poor as well as exploring the extent of the Galactic abundance gradient. We analyse a Spitzer spectroscopic sample of 23 planetary nebulae towards the anti-center in order to understand how the metallicity gradient extends beyond 10 kpc from the Galactic center and to observe the dust composition in this region of our Galaxy. We find that the abundance gradients of Ne, S and Ar continue to distances of around 20 kpc (albeit with a large scatter) and the dust emission shows a carbon-rich chemistry similar to that in the Magellanic Clouds.

Keywords

planetary nebulaedustabundancesmetallicity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 341 - 342
Copyright
Copyright © International Astronomical Union 2017 

References

Bernard-Salas, J., Peeters, E., Sloan, G. C., et al. 2009, ApJ, 699, 1541 CrossRefGoogle Scholar
Costa, R. D. D., Uchida, M. M. M., & Maciel, W. J., 2004, A&A, 423, 199 Google Scholar
Frew, D. J., Parker, Q. A., & Bojičić, I. S., 2016, MNRAS, 455, 1459 CrossRefGoogle Scholar
Gutenkunst, S., Bernard-Salas, J., Pottasch, et al., 2008, ApJ, 680, 1206 CrossRefGoogle Scholar
Henry, R. B. C, Kwitter, K. B., Jaskot, A. E., et al. 2010, ApJ, 724, 748 CrossRefGoogle Scholar
Martín-Hernández, N. L., Peeters, E., Morisset, C., et al. 2002, A&A, 381, 606 Google Scholar
Otsuka, M., Kemper, F., Cami, J., et al. 2014, MNRAS, 437, 2577 CrossRefGoogle Scholar
Pottasch, S. R. & Bernard-Salas, J., 2006, A&A, 457, 189 Google Scholar
Sloan, G. C., Lagadec, E., Zijlstra, A. A., et al. 2014, ApJ, 791, 28 CrossRefGoogle Scholar