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Estimation of Contaminants for Direct Imaging of Exoplanets: Constraint on the Stellar Distribution Model with both NIR and Deep Imaging Data

Published online by Cambridge University Press:  06 January 2014

Mihoko Konishi ,
Hiroshi Shibai ,
Taro Matsuo ,
Kodai Yamamoto ,
Jun Sudo ,
Matthias S. Samland ,
Misato Fukagawa ,
Takahiro Sumi  and
SEEDS team
Mihoko Konishi
Affiliation:
Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan email: [email protected]
Hiroshi Shibai
Affiliation:
Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan email: [email protected]
Taro Matsuo
Affiliation:
Department of Astronomy, Faculty of Science, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606-8502, Japan
Kodai Yamamoto
Affiliation:
Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan email: [email protected]
Jun Sudo
Affiliation:
Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan email: [email protected]
Matthias S. Samland
Affiliation:
Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan email: [email protected]
Misato Fukagawa
Affiliation:
Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan email: [email protected]
Takahiro Sumi
Affiliation:
Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan email: [email protected]
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Abstract

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There are faint contaminants near primary stars in the direct imaging of exoplanets. Our goal is to estimate statistically the ratio of exoplanets in the detected batch of point sources by calculating the fraction of contamination. In this study, we compared the detected number of stars with the number of contaminants predicted by our model. We found that the observed number of faint stars were fewer than the predicted results towards the Pleiades and GOODS-South field when the parameters of the conventional stellar distribution models were employed. We thus estimated new model parameters in correspondence to the results of the observations.

Keywords

infrared: stars - Galaxy: stellar content - Galaxy: fundamental parameters - stars: low-massbrown dwarfs - stars: luminosity functionmass function
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 42 - 43
Copyright
Copyright © International Astronomical Union 2013 

References

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