Hostname: page-component-5c6d5d7d68-wp2c8 Total loading time: 0 Render date: 2024-08-16T14:27:39.801Z Has data issue: false hasContentIssue false
  • English
  • Français

Challenges in Timeseries Analysis from Microlensing

Published online by Cambridge University Press:  30 May 2017

R. A. Street
R. A. Street*
Affiliation:
6740 Cortona Drive, Suite 102, Goleta, CA 93117, USA email: rstreet@lco.global
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Despite a flood of discoveries over the last ~ 20 years, our knowledge of the exoplanet population is incomplete owing to a gap between the sensitivities of different detection techniques. However, a census of exoplanets at all separations from their host stars is essential to fully understand planet formation mechanisms. Microlensing offers an effective way to bridge the gap around 1–10 AU and is therefore one of the major science goals of the Wide Field Infrared Survey Telescope (WFIRST) mission. WFIRST’s survey of the Galactic Bulge is expected to discover ~ 20,000 microlensing events, including ~ 3000 planets, which represents a substantial data analysis challenge with the modeling software currently available. This paper highlights areas where further work is needed. The community is encouraged to join new software development efforts aimed at making the modeling of microlensing events both more accessible and rigorous.

Keywords

gravitational lensingmethods: data analysisstars: planetary systems
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S325: Astroinformatics , October 2016 , pp. 253 - 258
Copyright
Copyright © International Astronomical Union 2017 

References

Bachelet, E. 2015, ApJ, 812, 136.CrossRefGoogle Scholar
Bachelet, E., 2016, in prep.Google Scholar
Bozza, V. 2010, MNRAS, 408, 2188.CrossRefGoogle Scholar
Dong, S. et al. 2007, ApJ, 664, 862.CrossRefGoogle Scholar
Gaudi, B. S. 2010, Microlensing by Exoplanets in Exoplanets, ed. Seager, S., p. 79.Google Scholar
Gaudi, B. S. & Gould, A. 1997, ApJ, 486, 85.Google Scholar
Gould, A. et al. 2009, ApJ, 698, 147.CrossRefGoogle Scholar
Han, C. et al. 2016, ApJ, 825, id.8.CrossRefGoogle Scholar
Ida, S., Lin, D. N. C., & Nagasawa, M. 2013, ApJ, 775, 42.Google Scholar
Penny, M. et al. 2016, in prep.Google Scholar
Poleski, R. 2016, MNRAS, 455, 3656.Google Scholar
Refsdal, S. 1964, MNRAS, 128, 29.Google Scholar
Street, R. A. et al. 2016, ApJ, 819, 93.Google Scholar
Sumi, T. et al. 2011, Nature, 473, 349.Google Scholar
Sumi, T. & Penny, M. 2016, ApJ, 827, id.139.CrossRefGoogle Scholar
Udalski, A. et al. 2015, ApJ, 799, id.237.Google Scholar
Udalski, A. et al. 2015, ApJ, 812, id.47.CrossRefGoogle Scholar
Yoo, J. et al. 2004, ApJ, 603, 139.CrossRefGoogle Scholar