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Title:
Estimation of Contaminants for Direct Imaging of Exoplanets: Constraint on the Stellar Distribution Model with both NIR and Deep Imaging Data
Authors:
Konishi, Mihoko; Shibai, Hiroshi; Matsuo, Taro; Yamamoto, Kodai; Sudo, Jun; Samland, Matthias S.; Fukagawa, Misato; Sumi, Takahiro
Affiliation:
AA(Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan ), AB(Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan), AC(Department of Astronomy, Faculty of Science, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606-8502, Japan), AD(Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan), AE(Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan), AF(Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan), AG(Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan), AH(Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka, 560-0043, Japan)
Publication:
Exploring the Formation and Evolution of Planetary Systems, Proceedings of the International Astronomical Union, IAU Symposium, Volume 299, pp. 42-43
Publication Date:
01/2014
Origin:
CUP
Keywords:
infrared: stars, Galaxy: stellar content, Galaxy: fundamental parameters, stars: low-mass, brown dwarfs, stars: luminosity function, mass function,
Abstract Copyright:
(c) 2014: Copyright © International Astronomical Union 2013
DOI:
10.1017/S1743921313007783
Bibliographic Code:
2014IAUS..299...42K

Abstract

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.

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