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Light Pollution as a Risk for Astronomical Research and How to Manage It

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Risk Management in Outer Space Activities

Part of the book series: Space Law and Policy ((SLP))

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Abstract

Astronomers undertake research by observing the universe to collect relevant data, which they analyse to deduce a model for the physical state of the objects observed. This enables them to make informed deductions about the origin and future evolution of planets, stars, galaxies and other astronomical bodies. Historically, these observations were made by ground-based astronomers using optical telescopes. Indeed, this has been the case for four centuries since Galileo Galilei first used a telescope for astronomy in 1609.

The views of the author are the authors’ alone and are intended to provide commentary and general information, and do not represent the views of any organisation. This chapter should not be relied upon as a substitute for professional legal advice or for any other purpose.

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Notes

  1. 1.

    The brightness of stars as seen by an observer on Earth is specified by their apparent magnitude. The brightest stars in the sky are about magnitude zero (a few have negative magnitudes), while the faintest just visible to the naked eye on a clear moonless night are at about magnitude 6–6.5. The fainter the star, the larger the magnitude will be.

  2. 2.

    These two parameters are closely related.

  3. 3.

    The numbers in Table 7.1’s final column are approximate.

  4. 4.

    It is important to note that the limiting magnitude depends on many factors in addition to light pollution. These include sky transparency, phase and position of the Moon, time since sunset or before sunrise, age of the observer and whether complete eye dark adaptation has occurred. All these factors combined make star counts, or estimating the limiting magnitude, a very crude indicator of light pollution.

  5. 5.

    This might be several times greater for a higher power rating.

  6. 6.

    These conditions are optimal for astronomers working in the darkest of observing sites.

  7. 7.

    Where mV stands for the apparent magnitude in the V-filter band.

  8. 8.

    For more information see, the IAU website (IAU, 2020a) as well as the detailed history of the IAU as articulated by Andersen et al. (2019) and Sterken et al. (2019).

  9. 9.

    The story of the founding of IDA can be found in Hunter (2013). An article by Crawford and Hunter (1990), soon after the founding of the organization, outlines some of their early work.

  10. 10.

    The coordinates of the centre of the reserve are about 44 degrees south and 170.3 degrees east (AMIDSR, 2020).

  11. 11.

    Having the legal status of a charity, and the tax exemptions that come with this, assists with the running of many events and activities.

  12. 12.

    These figures do not apply to the coronavirus pandemic year of 2020.

  13. 13.

    The telescope was formerly at the University of Pennsylvania before coming to New Zealand in 1963.

  14. 14.

    The correlated colour temperature (CCT) of a light source is the temperature of a radiating black body that presents the same apparent colour to the human eye as the light source.

  15. 15.

    In Spanish it is known as la Fundación Starlight.

  16. 16.

    A useful list is found at Wikipedia (2020c).

  17. 17.

    The diffraction rings and Airy disk of a point-like star are an artefact of the wave nature of light on entering an aperture such as a telescope. In turbulent air at low altitude observatories these fine features are normally washed out in a blurred image.

  18. 18.

    It is important to note that the analysis presented in this chapter has been simplified. This is because the so-called photon noise is not the only source of noise present in astronomical observations. A modern digital camera (often a charge-coupled device) will also have readout noise (when the stored image is readout and digitized to a computer) and thermal noise (arising from the thermal accumulation of a spurious signal within the camera chip itself). The analysis of these additional noise sources is beyond the scope of this chapter, except to note that for long exposures on faint objects, photon noise normally dominates.

  19. 19.

    Details can be found on the IDA website (IDA, 2020a, b, c) and at Ministère de la Transition Écologique et Solidaire (2018).

  20. 20.

    This corresponds to bn of 8.61 × 107 visual photons cm−2 s−1 sr−1, or 252 μcd m−2.

  21. 21.

    The standard reference on the ecological effects of light pollution is compiled in a book by Rich and Longcore (2006), with comprehensive sections on mammals, birds, reptiles, fish, invertebrates and plants.

  22. 22.

    In 2013 the Israeli scientists Abrahim Haim and Boris Portnov wrote a book with the title Light Pollution as a new Risk Factor for Human Breast and Prostate Cancers (Haim & Portnov, 2013).

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Correspondence to John Hearnshaw .

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Hearnshaw, J. (2022). Light Pollution as a Risk for Astronomical Research and How to Manage It. In: Pozza, M.A., Dennerley, J.A. (eds) Risk Management in Outer Space Activities. Space Law and Policy. Springer, Singapore. https://doi.org/10.1007/978-981-16-4756-7_7

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