For the more information about natural sounds and night skies in the National Park Service, please visit http://www.nature.nps.gov/sound_night/.
Science of Light
Learning more about the science of light and human vision will help us understand the value and fragility of natural lightscapes. During the day, the surface of the planet is bathed in light from the sun. The energy in sunlight drives weather, the water cycle, and ecosystems. But at night, in the absence of bright light, our atmosphere turns transparent and allows us to see beyond our planet into the vastness of the cosmos.
Light visible to the human eye is a portion of the electromagnetic spectrum, which encompasses radiant energy over the entire range of propagating mechanisms. Radiant energy may be seen (visible light), felt (infrared radiation or heat transferred from warm objects), or it can actually penetrate (x-rays) and do physical damage to the cells of the human body (gamma rays or nuclear radiation). Very low energy radiation is used by human technology as a carrier for communications (microwaves and radio waves). What we call visible light forms the visible spectrum, or colors of the rainbow, and represents a very narrow band in entire electromagnetic spectrum. Blue and violet light contain more energy and have a shorter wavelength than orange and red light.
The response of the human eye over the visible light spectrum defines the so-called luminosity function or photopic curve. The peak of this curve is in the yellow-green, at a wavelength of 555 nano-meters (nm). The curve shifts toward the blue under very dark conditions (called scotopic or dark-adapted) because of differences in the chemistry of the rod and cone cells in the human retina. Scotopic vision is more blue-sensitive, but it is perceived as a black-and-white image by the human brain, since the rods do not have a means to differentiate color. While scotopic vision is important in observing the night sky and the landscape at night, light measurement (or photometry) is based upon daytime vision or the photopic curve. Light meters are designed with a filter in the optical system which appears green and mimics the photopic response of the human eye.
The manner in which the human eye-brain combination perceives light is important to the aesthetic appreciation of night sky quality. The eye (and other human sensory devices) natural measures in a logarithmic scale, hence the original stellar magnitude scale was logarithmic. That is, objects are seen relative to each other, so if four objects were seen side by side with an actual brightness of 2, 4, 8, and 16, they would be perceived by the eye as 1, 2, 3, and 4 in brightness. This logarithmic response allows the eye to see faint objects without “bottoming out.” Visual contrast, as well, is seen in a non-linear manner. Contrast is also dependent on the angular size of the object.
Radiant energy behaves both as waves, with measurable wavelengths and frequencies, and as particles, or as discrete "packages" of energy, called photons for visible light. Light cannot be propagated, transmitted, or received in quantities smaller than 1 photon, and a photon of a particular wavelength contains a discrete amount of radiant energy. Light travels at a constant speed of 3 x 108 meters per second, or 186,000 miles per second, in a vacuum.
Light is usually measured as photon flux, proportional to the number of photons per second striking the human eye or a light meter. Photon flux is called illuminance, and its engineering units are lux (metric) or footcandles (English); both are linear scales. The human eye is capable of observing an extremely wide range of photon flux, from about 6 photons per second of blue light (about 10-9 lux) to brilliant sunlight reflecting off snow (about 104 lux), a range of nearly 10 trillion to one.
In astronomy, illuminance is measured in visual magnitudes, a logarithmic scale similar to decibels for measuring sound, except that the magnitude scale is inverse, where smaller numbers mean brighter objects. The sun has a visual magnitude of -26.7 (producing an illuminance of 108,000 lux) at the top Earth’s atmosphere, while the faintest stars visible to the human eye without optical aid are about magnitude 7.2 (0.000000003 lux). Individual light sources can therefore be measured in terms of the illuminance they produce at the observer's location. Photons leaving the source are subject to the inverse square law for radiant energy. This law states that the energy reaching the observer varies at one over the square of the distance to the source.
Energy = Intensity / Distance from the obsever2
Therefore, doubling the distance will result in one-quarter the illuminance from the same source. Astronomical objects such as the stars are so far away that their illuminance does not change measurably even as Earth moves around the sun. The planets, however, vary in brightness primarily because of the inverse square law. The sun and moon are also subject to small but measurable variations in apparent brightness because of variations in distance from Earth.
Light sources on Earth, however, such as street lamps, obviously produce much more illuminance as an observer gets closer to them. When outdoor light at night escapes from its intended use, and is observed directly, it creates light trespass, a form of light pollution, especially in a natural landscape like a national park. These bright objects are very noticeable, even at a great distance. For example, a typical streetlamp produces about 5 lux of illuminance immediately beneath it (let’s say 5 meters away), in the area intended for its use. If the lamp is unshielded and emits light equally in all directions, an observer on the landscape 100 times more distant (500 meters or ¼ mile) away will be illuminated by the lamp according to the inverse square law:
Energy = 5 lux / 1002 = 0.0005 lux
This seems like a small amount, but the crescent moon produces only 0.01 lux, and the planet Venus at its brightest produces 0.0001 lux of illuminance. Therefore, this single unshielded street lamp seen from 500 meters away would be brighter than any natural object in the night sky other than the moon. Also, a small, bright source of light will impair dark adaptation of the human eye, further restricting the observer’s ability to enjoy the natural night environment.
While illuminance is total photon flux striking a surface or the human eye, luminance refers to the apparent surface brightness of objects that have a visible size or viewing angle from the point of view of the observer. Computer monitors and flat-screen televisions are often advertised with a value for maximum surface brightness in nits, or candela per meter squared (cd/m2). Values of 500-1,000 cd/m2 are common for these devices. The brightness of the landscape from the reflected light of the sun, moon, or the night sky depends on its reflectance (snow vs. black lava rock, for example) and ranges from about 8,000 cd/m2 in bright sunlight to 0.000001 cd/m2 on a moonless night.
The sun's surface as seen from earth measures an apparent 0.5 degrees in diameter and has a luminance of about 1,600,000,000 cd/m2. It cannot be observed directly with the human eye without damaging the retina. Conversely, the darkest part of the natural night sky on a moonless night is not "pitch black," but in fact can be measured at about 0.00017 cd/m2. It is easily seen as luminous to the dark-adapted human eye, especially if objects like trees are silhouetted against it.
In astronomy, luminance may be expressed as visual magnitudes per square arc second, and 0.00017 cd/m2 is equivalent to 22.0 magnitudes per square arc second (MSA). Remember that the magnitude scale is inverse and logarithmic: 17.0 magnitudes per square arc second is 100 times brighter than 22.0; 12.0 MSA is 10,000 times brighter than 22.0 MSA.
Atmospheric Scattering and Light Pollution
The sky may also appear luminous at night because of light scattered by the atmosphere. When light passes through any medium other than a vacuum, it is subject to reflection, refraction, diffraction, and absorption. The combined effect of these processes is scattering of the original light beam. The atmosphere includes molecules of gases (such as nitrogen, oxygen, water vapor, and carbon dioxide) and suspended solid particles (such as dust, soot, salts, and chemical precipitates, collectively called aerosols). The amount and type of aerosols present, the amount of moisture in the air, and the altitude above sea level are the primary variables determining the scattering that will occur. Even perfectly clear air at high altitude will scatter light to some degree. Scattering of sunlight by air molecules gives the daytime sky its blue color. We describe the air as "hazy" when there is high water vapor or aerosol content; the deep blue color is replaced with a milky white hue, especially near the sun.
At night, luminance to the air is called skyglow. There are natural sources of skyglow, such as the aurorae (northern lights); the greenish airglow (a faint glow from the upper atmosphere present most nights); scattering of the light of the moon, planets, and stars; and the Zodical Light (a band of light along the Zodiac that is part of our solar system). These natural sources tend to be faint. However, if the light source is human caused, like a large city with thousands of street lamps, the skyglow produced by scattering of this light is a form of light pollution that degrades the view of the night sky by reducing the contrast between faint extraterrestrial objects and the background, the luminous atmosphere.
Even if the area of the sky near the Zenith is relatively free of scattered anthropogenic (human-caused) light, areas near the horizon may appear bright or individual light domes from distant cities may be seen. In a natural protected area like a national park, these bright areas produce a measurable impairment or deviation from the natural condition. Models and measurements of the brightness of city light domes have revealed a relationship between them, the city's population, and the distance from the center of the city to the observer, known as Walker's Law. Primarily derived from actual observations, this formula may predict the anthropogenic skyglow at a given point in the sky above the city:
L = C x Population x (Distance)-2.5
The constant C is dependent on the units of luminance used and the per capita "escaped light" of the city. Measurements have shown that certain cities produce much less escaped light per capita than others. This is an important concern in protection of natural night skies.
For the visual observer, there are certain characteristics of the appearance of the night sky that may be used to determine its quality. The number of stars visible or more properly the "visual limiting magnitude at the Zenith," or ZLM, is one of the most frequently quoted. Faint stars are difficult to see, and require proper dark adaptation and the use of averted vision to maximize the sensitivity of the human eye. Stars of magnitude 6.0–6.3 are often used as a test of a dark sky, but experience has shown that stars 2–3 times fainter at magnitude 7.0–7.5 can be seen by skilled observers under the best of conditions. Therefore, this method has a large margin of error at dark sites. In areas with significant amounts of sky glow at the Zenith, however, it is much easier to use, as brighter stars are few in number and much easier to spot.
An attempt to synthesize a number of sky quality indicators is made in the Bortle Dark Sky Scale which rates sky quality in intervals from 1 to 9, where 1 is pristine and 9 represents a sky dominated by anthropogenic (human-caused) light in which only the very brightest dozen or so stars and planets may be seen. Only a few areas in the conterminous 48 United States display class 1 or 2 skies. The sky quality in many western national parks has degraded to class 3 or 4. Class 5 and higher skies are observed in or near large metropolitan areas.
An exceptional view of the night sky (Bortle Class 1 or 2) may be achieved on nights when the weather, atmospheric clarity, and absence of anthropogenic light combine to produce favorable observing conditions. Certain locations in the world that have these qualities have been sought out by professional astronomers. In the early 1900s, the coastal mountains of California became home to three major observatories: Lick Observatory near San Jose, Mt Wilson Observatory near Los Angeles, and Palomar Observatory near San Diego. Not only was there an abundance of cloud-free nights, but the high altitude air was free of pollutants and had exceptional "seeing" (the view of the stars is crisp and without distortion).
As the population of California grew rapidly, so did light pollution, vastly degrading the usefulness of these observatories. Astronomers retreated to the remote high mountains of Chile and the summit of Mauna Kea, on the island of Hawaii. Mauna Kea is at an altitude of 13,796' (4175 meters), placing these telescopes far above the majority of atmospheric aerosols (a small suspended particle in the air). Also, it possesses some of the finest atmospheric seeing of any location, though while instruments work fine at such high altitudes, the lack of oxygen decreases the ability of human observers to see faint objects at night.
Last Updated: April 23, 2012