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Direct Imaging of Faint Companions

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Book cover Methods of Detecting Exoplanets

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 428))

Abstract

The exoplanets around stars in the solar neighborhood are expected to be bright enough for us to characterize them with direct imaging; however, they are much fainter than their parent stars, and separated by very small angles, so conventional imaging techniques are totally inadequate, and new methods are needed. The direct imaging of exoplanets is extremely challenging. Jupiter is 109 times fainter than our Sun in reflected visible light. A direct imaging instrument for exoplanets must suppress (1) the bright star image and diffraction pattern and (2) the stellar scattered light from imperfections in the telescope. The main goal of high-contrast imaging is primarily to discover and characterize extrasolar planetary systems. High-contrast observations, in optical and infrared astronomy, are defined as any observation requiring a technique to reveal a low mass companion that is so close to the primary, brighter by a factor of at least 105, that optical effects hinder or prevent the collection of photons directly from the target of observation. To overcome this, astronomers combined large telescopes (to reduce the impact of diffraction), adaptive optics (to correct for phase errors induced by atmospheric turbulence), and sophisticated image processing.

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Notes

  1. 1.

    The first light of Project1640 was taken in 2010 (Hinkley et al. 2011).

  2. 2.

    This is what is called a warm start. Not all agree with this vision of the evolution of the planets just after the formation. For example, (Marley et al. 2007) consider instead a cold start with planets that become brighter during the gravitational focus event when the gas is accreted from the disk.

  3. 3.

    US military started to invest in AO in the 1970s and had commissioned the first adaptive optical system in 1982 (Davies and Kasper 2012).

  4. 4.

    Apodization is the technique that allows reduction of the sharp discontinuity in the transmitted wavefront at the edge of the pupil reducing the amplitude of the secondary maxima of the diffraction figure.

  5. 5.

    Before combining the images they should be reduced in the usual way: normalization of flat field and bad-pixel correction.

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Acknowledgements

The author acknowledges support from the “Progetti Premiali” WOW funding scheme of the Italian Ministry of Education, University, and Research. Furthermore I would like to thank Anthony Boccaletti and Raffaele Gratton for the useful discussion and material for the front lectures. Besides I would like to thank also all those unaware colleagues from who I took some help for preparing the lectures and these lecture notes. A particular thanks goes to the organizers of the school (V. Bozza, L. Mancini, and A. Sozzetti) and also to the patient young colleagues and students without who these lecture notes could not exist.

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  1. INAF – Osservatorio Astronomico di Padova, Vicolo Osservatorio, 5, 35122, Padova, Italy

    Riccardo Claudi

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Editors and Affiliations

  1. Department of Physics, University of Salerno, Fisciano, Italy

    Valerio Bozza

  2. Planet and Star Formation, Max Planck Institute for Astronomy, Heidelberg, Germany

    Luigi Mancini

  3. INAF–Osservatorio Astrofisico di Torino, Pino Torinese (TO), Italy

    Alessandro Sozzetti

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Claudi, R. (2016). Direct Imaging of Faint Companions. In: Bozza, V., Mancini, L., Sozzetti, A. (eds) Methods of Detecting Exoplanets. Astrophysics and Space Science Library, vol 428. Springer, Cham. https://doi.org/10.1007/978-3-319-27458-4_4

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