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Probing Galactic Chemical Evolution with J-PLUS Photometry

Published online by Cambridge University Press:  02 August 2018

Devin D. Whitten ,
Vinicius M. Placco ,
Timothy C. Beers ,
Spencer Clark ,
Alessandro Ederoclite  and
Cláudia Mendes de Oliveira
Devin D. Whitten
Affiliation:
University of Notre Dame, Notre Dame, IN, USA, email: [email protected] JINA-CEE, Notre Dame, IN, USA
Vinicius M. Placco
Affiliation:
University of Notre Dame, Notre Dame, IN, USA, email: [email protected] JINA-CEE, Notre Dame, IN, USA
Timothy C. Beers
Affiliation:
University of Notre Dame, Notre Dame, IN, USA, email: [email protected] JINA-CEE, Notre Dame, IN, USA
Spencer Clark
Affiliation:
University of Notre Dame, Notre Dame, IN, USA, email: [email protected]
Alessandro Ederoclite
Affiliation:
Centro de Estudios de Física del Cosmos de Aragón, Teruel, Spain
Cláudia Mendes de Oliveira
Affiliation:
Universidade de São Paulo, Brazil
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Abstract

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Narrow-band photometric surveys, such as the Javalambre Photometric Local Universe Survey (J-PLUS), provide not only a means of pre-selection for high-resolution follow-up, but open a new era of precision photometric stellar parameter determination. Using a family of machine learning algorithms known as Artificial Neural Networks (ANNs), we have obtained photometric estimates of effective temperature (Teff) and metallicity ([Fe/H]) across a wide parameter range of temperature and metallicity (4000 < Teff <7000 K; −3.5 <[Fe/H]<0.0) for a number of stars in the J-PLUS Early Data Release. With this methodology, we expect to increase the number of known Carbon-enhanced Metal-poor (CEMP; [C/Fe]>+0.7) stars by several orders of magnitude, as well as constrain the metallicity distribution function of the Milky Way Halo system.

Keywords

General: stellar parametersGalaxy: halostars: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 383 - 384
Copyright
Copyright © International Astronomical Union 2018 

References

Lee, Y. S., Beers, T. C., Sivarani, T., et al., 2008, AJ, 136, 2022Google Scholar
Placco, V. M., Frebel, A., Lee, Y. S., et al., 2014, ApJ, 809, 136Google Scholar
Starkenburg, E., Martin, N., Youakim, K., et al., 2017, MNRAS, 471, 2587Google Scholar
Reidmiller, V., 2002, Computer Standards & Interfaces, 16, 265Google Scholar