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Light Phenomena Over the ESO Observatories I: Airglow

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Light Phenomena Over the ESO Observatories I: Airglow Astronomical News Light Phenomena over the ESO Observatories I: Airglow Lars Lindberg Christensen1 Earth’s atmosphere with ultraviolet light, fainter reddish tint of luminescent atmos­ Stefan Noll 2 which photodissociates molecular oxygen phere resides above the green layer, at 1 Petr Horálek (O2) into individual atoms during the altitudes between 150 and 350 kilometres. daytime and triggers a chain of complex Both layers are related to atomic oxygen, chemical reactions after sunset. Atomic but their different altitudes cause the 1 ESO oxygen (O) cannot efficiently recombine green emission to peak much closer to 2 Institute for Astro­ and Particle Physics, and therefore has a long lifetime in the the horizon (Noll et al., 2012). University of Innsbruck, Austria upper atmosphere. It represents a store of chemical energy that is also available The extent, colour and brightness of at night. O2, O, sodium (Na), and the airglow is influenced by many different Airglow, the faint light emitted by the hydroxyl radical OH can then be produced factors, including the time and location Earth’s atmosphere, has in recent years and excited by further reactions and col­ of the observation (Roach & Gordon, been frequently photographed in large lisions, causing them to emit radiation 1973; Khomich et al., 2008; Patat, 2008; field images taken at ESO’s observa­ by chemiluminescence (Roach & Gordon, Noll et al., 2012). The red oxygen glow, tories. The nature of the airglow is 1973; Khomich et al., 2008; Noll et al., for example, tends to be brightest at the briefly described and example images 2012, 2015a, 2015b). start of the night, but after midnight, it are shown, capturing the variety of the can be very weak. However sporadic displays. Astronomers are used to subtracting bursts of airglow emission can occur at airglow emission lines from ground­ any time. based spectra. The airglow lines extend On a moonless night at the La Silla from the near­ultraviolet to the near­ Airglow can also appear in formations Observatory, in the Atacama Desert of infrared regime (Rousselot et al., 2000; called gravity waves (Taylor et al., 1997; northern Chile, it should be very dark, Hanuschik, 2003; Noll et al., 2012), and Khomich et al., 2008), as illustrated by but at times, strange green and red col­ are characterised by clusters of numerous Figure 1, lower right. These propagating ours can be seen shimmering in the night narrow emission lines. This structure air pressure oscillations are mainly sky. Although visible, albeit faintly, to is especially common in the near­infrared, formed in the lower atmosphere (e.g., by the unaided eye, these unusual lights are where the strongest airglow lines are air flows over mountains) and can then very prominent in long exposures cap­ found (OH bands) and give rise to back­ rise to high altitudes. Here, their ampli­ tured by commercial digital single­lens ground patterns that present interesting tudes can increase to widths greater than reflex (SLR) cameras. An example is challenges if they have to be removed those of the airglow layers due to very shown in Figure 1. To the untrained eye, (Noll et al., 2014). An example is pre­ low air pressure and the conservation of these lights may appear to be some kind sented by exposures from the VLT Infra­ wave energy and momentum. In turn, this of peculiar low­latitude auroral phenome­ red Survey Telescope for Astronomy affects the intensity of the airglow and non, but they are actually the emission (VISTA), in which the OH airglow struc­ characteristic moving ripples in the air­ of airglow — light emitted by the Earth’s tures move between the dithered glow can be formed (Figure 1). atmosphere. This optical phenomenon exposures of the widely spaced array of prevents the night sky from ever becom­ CCD chips. This effect is especially visible ing completely dark (Roach & Gordon, until about two hours after twilight1. Airglow increase 1973; Patat, 2004, 2008; Noll et al., 2012), even in the absence of astronomi­ The origin of the airglow is now fairly cal sources. Observations of airglow well understood, but why are we seeing it more often in images taken at ESO Airglow is very faint, but the strongest sites in Chile over the past five years (see The formation of airglow appearances of the phenomenon can be Figures 3, 4 and 5)? Has airglow become visible to the naked eye as an unexpected more common? Could it be caused by The first airglow emission line was iden- faint structure on the stellar background. global changes in weather patterns? The tified in 1868 by the Swedish scientist To the naked eye, the colours of this air­ answer is not yet clear, but the recent Anders Ångström, but it took until the glow are invisible, but sensitive wide­ rapid development of digital cameras 1920s to understand that airglow differs angle photographs reveal the fine green seems to play an important role as they from aurorae (Mc Lennan, 1928; Roach and reddish shades of the phenomenon. allow for fainter details to be picked up & Gordon, 1973). Since the 1950s airglow Sometimes airglow presents itself as in the night sky more frequently. has been extensively studied by ground­ just a faint tinge of colour on the horizon, based instruments (photometric and but it can also appear as a melange of Identical cameras, however, have been spectroscopic), by instruments aboard changing colourful shapes (Figure 1). found to capture dramatically different rockets and satellites and by laboratory skies just weeks apart. Airglow changes experiments (Khomich et al., 2008). The green layer of airglow lies about with solar activity, so the 11­year solar 100 kilometres above the ground and cycle can have an impact on the bright­ These research efforts have revealed can easily be observed from the Interna­ ness of the airglow. The current solar that the Sun is constantly showering the tional Space Station (Figure 2). A much cycle (Cycle 24) peaked in 2014, although 40 The Messenger 163 – March 2016 N N P. Horálek/ESOP. E W E W 2:29 UTC5:40 UTC View from the Swedish-ESO View from the platform of S 15-metre Submillimetre Telescope the ESO 3.6-metre telescope S N View from the NE path to the View from the path nearby N Danish 1.54-metre telescope the ESO 1-metre telescope 6:51 UTC 8:44 UTC E W E W S Colours of airglow radiation S O2 O Na O OOH radicals 400 nm 500 nm 600 nm 700 nm Figure 1. One night at the La Silla Observatory (20 January 2015) exhibiting different displays of green and red airglow seen in deep fisheye images spanning 360 degrees azimuth and 120 degrees alti­ tude. In the lower right image, gravity waves can be seen forming ripples in the greenish layer of airglow. The Messenger 163 – March 2016 41 Astronomical News Christensen L. L. et al., Light Phenomena over the ESO Observatories I: Airglow ISS/NASA Y. BeletskyY. (LCO)/ESO Figure 2. This unique photograph, taken from the Figure 3. Red and green airglow dances above International Space Station, shows the airglow layers ESO Photo Ambassador Babak Tafreshi as he above the city lights of Brisbane, Australia. prepares his camera to capture the night sky. Y. Beletsky/ESOY. Y. BeletskyY. (LCO)/ESO Figure 4. An example of airglow display at Figure 5. Flaming red airglow photographed over the Cerro Paranal with the VLT in the foreground. Paranal Observatory. The three 1.8­metre Auxiliary Telescopes, part of the Very Large Telescope Inter­ ferometer, can be seen in the foreground. it was amongst the weakest maxima One way or another, airglow has become Khomich, V. Y. et al. 2008, Airglow as an Indicator of on record (Hathaway, 2015). It seems that a regular feature in the magnificent celes­ Upper Atmospheric Structure and Dynamics, (Berlin: Springer) the solar maximum could be partly tial displays witnessed over the ESO McLennan, 1928, Bakerian Lecture. The Aurora and responsible for the increase in airglow sites. Even at one of the darkest places Its Spectrum, Royal Society Proc. A, 120, 785 captured in images from ESO’s observa­ on the planet, the sky never becomes Noll, S. et al. 2012, A&A, 543, A92 tories in recent years (Noll et al., 2012). completely dark. Noll, S. et al. 2014, A&A, 567, A25 Noll, S. et al. 2015a, Atmospheric Chemistry and Physics, 15, 3647 It is also worth mentioning that ESO’s Noll, S. et al. 2015b, ACPD, 15, 30793 observatories in Chile are located below Acknowledgements Patat, F. 2004, The Messenger, 115, 18 the South Atlantic Anomaly (Heirtzler, Patat, F. 2008, A&A, 481, 575 The authors acknowledge interesting conversations Roach, F. E. & Gordon, J. L. 1973, The Light of the 2002). Here, the Earth’s magnetic field — with Bob Fosbury. Night Sky, (Dordrecht: Reidel) which prevents charged particles from Rousselot, P. et al. 2000, A&A, 354, 1134 reaching the surface — is reduced and Taylor, M. J. et al. 1997, JGR, 102, 26283 thus more particles from the Sun pene­ References trate the atmosphere. This anomaly can Hanuschik, R. W. 2003, A&A, 407, 1157 Links affect the red airglow, which originates Hathaway, D. H. 2015, Living Rev. Solar Phys., 12, 4 in the Earth’s ionosphere (see Figure 5), Heirtzler, J. R. 2002, JASTP, 64, 1701 1 Sky brightness record from VISTA VIRCAM imag­ although the geomagnetic latitude is ing: http://casu.ast.cam.ac.uk/surveys-projects/ vista/technical/sky-brightness-variation more crucial for the observed variability. 42 The Messenger 163 – March 2016.
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