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La Palma Night-Sky Brightness
Chris R. Benn1 & Sara L. Ellison2
1Isaac Newton Group of Telescopes, Apartado 321, E-38700 Santa Cruz de La Palma,
Last Updated: 2007 Apr 12.
The brightness of the moonless night sky above La Palma was measured on 427 CCD images taken with the Isaac Newton and Jacobus Kapteyn Telescopes on 63 nights during 1987 - 1996. The median sky brightness, in units of mag arcsec-2, at high elevation, high galactic latitude and high ecliptic latitude, at sunspot minimum, is B = 22.7, V = 21.9, R = 21.0, similar to that at other dark sites. The sky brightness in U and I is less well-determined, U ~ 22.0 (few data), I ~ 20.0 mag arcsec-2 (variable). As at other dark sites, the main contributions to sky brightness are airglow and zodiacal light, in the ratio 2.5:1 at high ecliptic latitude.
The sky is brighter at low ecliptic latitude (by 0.4 mag); at solar maximum (by 0.4 mag); and at high airmass (0.25 mag brighter at airmass 1.5).
The mean brightness of the sky varies by < 0.1 mag with time after astronomical twilight.
Light pollution is visible to the naked eye at certain azimuths on the horizon, but its contribution to the continuum brightness at the zenith is < 0.03 mag in all bands, meeting one of the IAU's two recommendations for a dark site. The IAU's second recommendation, that NaD 5890/6-A emission should not exceed in intensity the natural airglow NaD, is not met during the summer, but few spectroscopic observing programmes are likely to be significantly affected. The NaD emission brightens the sky in both V and R broad bands by about 0.07 mag. Total contamination (line + continuum) at the zenith is < 0.03 mag in U, ~ 0.02 mag in B, ~ 0.10 mag in V, ~ 0.10 mag in R.
The brightness of the sky shows no dependence on atmospheric extinction Av, for Av < 0.25 mag (as is the case on 80% of nights). The sample includes two nights with Av > 0.25 mag. With Av = 0.4 mag, the sky was brighter by ~ 0.3 mag, and with Av = 0.8 mag by ~ 1.4 mag, probably because of enhanced back-scattering of streetlighting by the dust layer.
The glow of the night sky comprises contributions from a number of sources, summarised in Table 2 (and reviewed by Leinert et al (1998) for 0.1 < lambda < 10 micron). Between the stars, the brightness of the sky is dominated by airglow and zodiacal light, and the night sky is darkest at high ecliptic latitude and low zenith distance, at solar minimum. Typical spectra of the night and twilight skies are reproduced in Figs. 1 and 2.
Fig. 1 - Typical spectrum of the La Palma sky on a moonless night, taken with the faint-object spectrograph of the William Herschel Telescope in March 1991. Most of the distinctive features of the night-sky spectrum are due to airglow. Airglow also contributes a pseudo-continuum in the blue from overlapping O2 (forbidden Herzberg) bands (2600 - 3800 A) and in the green from NO2 bands (5000 - 6500 A). The NaD emission at 5890/6 A is partly from streetlighting, the mercury emission at 4358, 5461 A wholly so. With the exception of the 8645-A O2 line, the features dominating the spectrum redward of 6500 A are the Meinel rotation-vibration bands of OH. An atlas of the airglow 3100 - 10000 A was presented by Broadfoot & Kendall (1968) (see also Ingham 1962). More recently, a low-resolution spectrum of the night sky was given by Louistisserand et al (1987) and high-resolution (0.2 A) spectra of the wavelength range 5200 - 10600 A were presented by Osterbrock et al (1996, 1997), and for > 3100 A by Vlasyuk & Spiridovna (1993). Spectra of the infrared airglow were presented by Ramsay et al (1992), Oliva & Origlia (1992) and Maihara et al (1993). The relative strengths of the lines do not reflect relative concentrations of the emitting species (NaD is bright in part because of the very short lifetime ~ 10-8 sec of the high-energy state, so that many transitions are possible per unit time).
Fig. 2 - Typical spectrum of the La Palma sky during twilight, taken with the faint-object spectrograph of the William Herschel Telescope in March 1991. The Fraunhofer A and B bands at 7594 and 6867 A are due to absorption by molecular oxygen in the earth's atmosphere.
In the remainder of this section, we introduce the individual contributions to the brightness of the night sky. In Section 2, we report measurements of sky brightness made on La Palma. In Section 3, we compare the median dark-of-moon sky brightness at the observatory on La Palma with measurements made elsewhere; estimate the amount of light pollution; and report how sky brightness varies with time during the night, solar activity, ecliptic latitude, airmass and extinction. Conversion factors between different units commonly used for measuring sky brightness (mag arcsec-2, microJy arcsec-2, Rayleighs A-1, cd m-2, nLamberts) are given in the Appendix.
Sky brightness Place Nts Year S10.7 U B V R I Reference MJy mag arcsec^-2 McDonald 5 1960 22.8 21.7 Kalinowski et al (1975) Junipero Serra 1 1966 23.0 21.9 Walker (1970) San Pedro Martir 2 1970 1.5 22.9 21.9 Walker (1971) Junipero Serra 1 1971 1.2 22.9 21.9 Walker (1973) McDonald 6 1973 1.0 22.7 21.7 Kalinowski et al (1975) San Benito 1 1976 0.7 22.9 21.9 Walker (1988) La Silla 1 1978 1.5 22.8 21.7 20.8 19.5 Mattila et al (1996) Sacramento Peak 12 1978 1.5 21.9 Schneeberger et al (1979) Kottamia 1 1980 2.0 22.9 21.9 20.1 Nawar et al (1995) San Benito 7 1981 2.0 22.6 21.6 Walker (1988) Kitt Peak 7 1987 0.9 22.9 21.9 Pilachowski et al (1988,9) Cerro Tololo 2 1987 0.9 22.9 22.0 Geisler (1987) San Benito 6 1985-7 0.9 22.9 21.9 Walker (1988) La Palma 4 1987 0.9 21.8 This paper Cerro Tololo 1 1988 1.6 22.5 21.6 Geisler (1988) Siding Spring 1989 2.1 22.7 Savage (1989) Mauna Kea 16 1989-91 2.0 22.7 21.9 Krisciunas (1997) Calar Alto 3 1990 2.0 22.2 22.6 21.5 20.6 18.7 Leinert et al (1995) La Palma 9 1990-2 2.0 22.5 21.5 This paper Cerro Tololo 1 1991 2.0 22.4 Pettini (private comm.) Mauna Kea 8 1995-6 0.8 22.8 21.9 Krisciunas (1997) La Palma 43 1994-6 0.8 22.0 22.7 21.9 21.0 20.0 This paper
Table 1 - Near-zenith dark-of-moon broad-band sky brightness measured at various observatories. Nts is the number of nights on which data were taken. S10.7cm is the solar 10.7-cm radio flux density, an indicator of solar activity, measured at Ottawa (Penticton). The last five solar minima occured in 1954.5 (start of cycle 19, largest maximum on record), 1965.0 (cycle 20), 1976.8 (cycle 21), 1986.8 (cycle 22) and 1996.5 (cycle 23). Cycles 21 and 22 were of similar amplitude. As far as can be ascertained from the original references, the quoted solar-minimum sky brightnesses were measured at ecliptic latitude > 40o, ecliptic longitude > 120o from that of the sun, so that variations in the zodiacal-light contribution should affect the total by < 0.1 mag. The San Benito data include faint stars (V > 10). The Mauna Kea data were taken with a photometer with 6.5-arcmin aperure, and may be 0.2 mag too bright due to inclusion in the beam of stars V > 13. The above median values for La Palma (3 ranges of dates) are based on 56 nights of data. The other 7 nights in the sample were not close to either solar minimum or maximum. The table omits any sites where light pollution is believed a priori (e.g. from the models of Garstang 1989a) to raise the sky brightness by >~ 0.1 mag. Calar Alto, Lick, Lowell, Mt Wilson and Palomar are such sites.
Contribution Surface brightness V Typical Vzen (S10 units) (sunspot min) Airglow ~ 145 + 130(S_sun - 0.8)/1.2 145 Aurora negligible at |latitude| < 40 deg 0 Zodiacal light ~ 140 - 90 sin(|beta|) (|beta| < 60 deg) 60 ~ 60 (|beta| > 60o) (when > 90o from the sun) Stars < 55 (V > 20, integ light) Starlight scattered by ~ 100 exp(-(|b|/10 deg)) 10 interstellar dust Extragalactic light ~ 1 Light pollution < 20 at a `dark' site (Smith 1979) ---- Total 220
Table 2 - Typical contributions to the V brightness of the moonless night sky. The unit of surface brightness S10 corresponds to one 10th-mag star per square degree (i.e. 27.78 mag arcsec-2); 220 S10 corresponds to V = 21.9 mag arcsec-2, a typical sky brightness at high ecliptic latitudes beta (Table 1) (for beta > 40o the changes are small) during solar minimum, at a site with low geomagnetic latitude. b is galactic latitude. The formula for zodiacal light is an approximate fit to the ground-based results of Levasseur-Regourd & Dumont (1980), for ecliptic longitude > 90o different from that of the sun. The formula for starlight scattered by interstellar dust is an approximate fit to the data presented by Roach & Gordon (1973). Airglow is presumed to contribute the rest of the light, and its variation with solar cycle was deduced from the ~ 0.5 mag brightening at solar maximum (see Section 1.1). Ssun is the solar 10.7-cm radio flux density in MJy; it varies between 0.8 and 2.0 MJy (Section 1.1). The (small) auroral contribution peaks ~ 2 years after the peak of the solar cycle (Roach & Gordon 1973). The zodiacal-light spectrum is approximately solar. That of the airglow is redder than solar for wavelengths > 4500 A, i.e. the fractional contribution of zodiacal light peaks around this wavelength. The integrated light from the airglow over the whole sky corresponds to V ~ -6 (cf Venus -4, full moon -13).
The airglow is emitted by atoms and molecules in the upper atmosphere which are excited by solar UV radiation during the day (Ingham 1972). Airglow is the brightest component of the light of the night sky and it contributes the main spectral features to the night-sky spectrum (Fig. 1), including the 5577- and 6300-A lines from OI (both also prominent in the spectrum of the aurora), the ubiquitous 5890/6-A NaD doublet (the Na may be from sea salt carried to high altitude) and the bright OH rotation/vibration (Meinel) bands in the red and IR. The atoms and molecules responsible for individual features lie in well-defined layers of the atmosphere e.g. the O2 Herzberg bands, OI 5577 A, NaD 5890/6 A and the OH bands arise at an altitude of 90 - 100 km (mesopause, D layer) while OI 6300, 6364 A and O2 8645 A arise at ~ 300 km (F2 layer of ionosphere). The airglow lines are ~ 1000 times brighter during the day.
The brightness of the airglow correlates with solar activity, e.g. with the 10.7-cm radio flux density S10.7cm, which in turn correlates with the intensity of solar EUV radiation (100 - 600 A) striking the upper atmosphere (Chatterjee & Das 1995). S10.7cm varies approximately sinusoidally during the solar cycle, from ~ 0.8 MJy at solar minimum, to ~ 2.0 MJy at solar maximum (typical values; the amplitude of the solar cycle, and presumably the effect on sky brightness, varies). The sky is ~ 0.5 mag brighter at solar maximum, judging from monitoring carried out at three sites: Hawaii 1985-96 (Krisciunas 1990, 1996, 1997); San Benito 1976-87 (Walker 1988); and La Silla 1989-93 (Leinert et al 1995). The La Silla data are omitted from Table 1; they were taken through a narrow-band filter.
Some dimming of the airglow might be expected after astronomical twilight, which is approximately the time at which sunset is seen from an altitude of 100 km. The 6300-A OI emission line decays rapidly after twilight, the 5577-A line does not. Walker (1988) reported that the B and V sky brightness at San Benito decreased by 0.4 mag during the first half of the night, with no change after midnight. Krisciunas (1990, 1997) found evidence for a small decrease during the night in the brightness of the sky over Hawaii, but using few data. Pilachowski et al (1989), Leinert et al (1995) and Mattila et al (1996) detected no systematic variations with time during the night at Kitt Peak, Calar Alto and La Silla respectively.
The brightness of the airglow can vary randomly, by up to a few 10s of %, with position on the sky and with time during the night (Shefov 1972, Roach & Gordon 1973, Turnrose 1974, Kalinowski et al 1975, Pilachowski et al 1989, Krisciunas 1997, Leinert et al 1998). Some of the variations at different wavelengths are correlated (Chamberlain 1961, Leinert et al 1995), e.g. the strength of the 5577-A line correlates with that of the green/blue pseudo-continuum. The variations in intensity of the 5577-A emission with time and position are suggestive of clouds of emitting material drifting across the line of sight at air speeds typical of the 100-km altitude. The brightness of the OH Meinel bands in the red and infrared can vary by a factor of 2 during the night, and during the year, and can show quasi-periodic variations with time (probably atmospheric oscillations, Leinert et al 1998). The strength of at least the NaD line varies with season; ~ 30 Rayleighs in local summer vs ~ 180 Rayleighs in winter (Allen 1973). Other complex variations with time are known. For example in winter the 6300-A line can brighten abruptly sometime before midnight, when the ionosphere at the `conjugate point' on the other side of the globe sees sunrise, releasing a flood of charged particles along the earth's magnetic-field lines (Ingham 1972).
The airglow is about twice as bright at geomagnetic latitude 70o as at latitude 20o (Allen 1973). The intensity of the 6300-A line shows a complex dependence on geomagnetic coordinates. Roach & Gordon (1973) give a map based on measurements from a few satellite passes; the strengths in Rayleighs above different observatory locations were: La Palma 100 (the strength of the line in Fig. 1 is about 160 Rayleighs); Hawaii 400; Chile < 50; and Siding Spring < 50.
Variations in the brightness of the airglow triggered by lunar and solar tides in the atmosphere have been reported, but a recent study at La Silla found none (Mattila et al 1996 and references therein).
The spectrum of zodiacial light is very similar to that of the sun over the UV - IR range (Weinberg & Sparrow 1978), and its fractional contribution to the brightness of the night sky peaks at a wavelength of 4500 A (O'Connell 1987) (~ 0.5 of total for ecliptic latitude beta = 30o). By 8000 A, the brightness of the OH airglow bands has reduced the zodiacal light's fractional contribution to ~ 0.1. In the UV, the fractional contribution falls off dramatically with decreasing wavelength, and shortward of 2500 A, the non-airglow contribution is dominated by starlight scattered by interstellar dust. From space, the sky at 2000 and 10000 A is a factor ~ 40 fainter than from the ground, compared with a factor ~ 2 in the optical (O'Connell 1987).
It is important to take the contribution of zodiacal light into account when studying diurnal or seasonal variations of zenith sky brightness. For example, at typical geographical observing latitudes 20 - 40o, the midnight sky brightness at the zenith is lowest during local summer (ecliptic low), highest during local winter (ecliptic high), mimicking a seasonal variation.
(approximate fit to the data of Roach & Gordon 1973, b = galactic latitude). If all the starlight were scattered uniformly over the sky, it would produce a background of ~ 100 S10 units. However, most of this light is from stars with 6 < V < 16 and published measurements of sky brightness usually now refer to the sky between the stars. Stars fainter than V = 20 (easily detected in a 10-minute CCD exposure with a 1-m telescope) contribute insignificantly to the total brightness of the night sky. Starlight scattered by interstellar dust produces a diffuse glow concentrated along the galactic plane, analagous to the zodiacal light along the ecliptic (see Table 2). As noted above, for wavelengths shorter than 2000 A, this dominates the brightness of the sky as seen from outside the earth's atmosphere (Paresce & Jakobsen 1980).
Although extragalactic light contributes only ~ 1% of the total sky brightness, its distribution on the sky is uneven (see e.g. Cole, Treyer & Silk 1992) and it may have a disproportionate effect on the signal-to-noise of observations of faint objects (e.g. Davies et al 1994). When photon noise from a smooth sky background is the limiting factor, signal-to-noise rises with integration time tau as tau0.5. However, a discrete object within the photometry aperture will produce an error in the measurement of intensity which is independent of tau. Since apertures are typically a few arcsec in diameter (to be > seeing), the effect becomes important for objects with a density on the sky ~ (few arcsec)-2, i.e. V > 21. At this level, and fainter, the object counts are dominated by galaxies rather than stars. E.g. the galaxy counts from Longair (1993) indicate that there is a probability ~ 20% of including a galaxy with B < 24 within a randomly-positioned aperture of size 5 x 5 arcsec2. This will cause an error in the measured flux of a B = 23 target object of 40%, much greater than that due to airglow/zodiacal-light photon noise during a short dark-of-moon exposure with a 1-m telescope.
Typical street-lamp spectra were presented by Osterbrock et al (1976). The 4358-A Hg line can be a hazard for observers wanting to compare the intensities of the 4363 and 5007-A OIII lines (for measuring the temperature of astrophysical plasmas). The 5460-A Hg line lies in the centre of the y band of the ubvy system. The NaD 5890/6-A line typically contaminates both the V and R passbands. Models of the contribution of city lighting to dark-sky brightness were presented by Treanor (1973), Walker (1973), Yocke et al (1986) and Garstang (1984, 1986, 1989, 1991a,b,c). Walker (1977, 1991) and Garstang (1989) estimate the increase in brightness at zenith distance 45o, in the direction of a conurbation of population P at distance D km to be ~ PD-2.5/70 mag. The sky near the horizon is brightened in directions both towards and away from a source of light pollution (Berry 1976). The IAU recommendations for a dark site are continuum Delta mag < 0.1 for 3000 < lambda < 10000 A, and intensity of NaD light pollution < that from airglow, at ZD = 45o towards any city (Smith 1979, appendix 4.1 of McNally 1994).
where a is the radius of the earth (van Rhijn 1921). (The dependence on zenith distance of the intensity of a given emission line can be used to determine the height of the airglow species responsible.) For XD < 70 deg, I(ZD) ~ airmass ~ sec(ZD). If a fraction f of the sky brightness is due to airglow, one expects the sky to be
Mattila et al (1996) observed the 1978 La Silla sky brightness to be about 0.05 mag brighter at ZD = 30o than at the zenith, while Leinert et al (1995) reported that at Calar Alto in 1990, the sky was 0.1 mag brighter at ZD = 40o. These two measurements are broadly consistent with the prediction of the second equation above.
Fig. 3 - Variation of extinction, as revealed by nightly measures made at the Carlsberg Automatic Meridian Circle during 1984-96 (CAMC 1997). Saharan dust is responsible for the high values of extinction measured during the summer (July to September). The summer peaks in extinction seen at La Silla have a different cause (Burki et al 1995). The ~ 0.1 mag rise in extinction in 1991 - 93 is due to dust injected into the atmosphere by the eruption of Mt. Pinatubo in the Philippines (noted also at other observatories e.g. by Burki et al 1995, Forbes et al 1995).
Fig. 4 - Recent (> 1995) decline in the fraction of dusty nights at the observatory, a night being considered dusty if the extinction Av measured at the Carlsberg Automatic Meridian Circle is greater than (running median + 0.05) mag, the median being that of the current month plus 3 months either side, but excluding July, August, September.
Dark-of-moon sky brightness was measured from images in the electronic data archive of the Isaac Newton Group of telescopes. This archive includes all digital (mainly CCD) data taken with the 4.2-m William Herschel, 2.5-m Isaac Newton and 1.0-m Jacobus Kapteyn Telescopes. It currently (1997) comprises ~ 430000 CCD exposures, ~ 50% of which are direct images. Most of the direct images are taken through broad-band U, B, V, R or I filters (very few in Z) with the 2.5-m or 1.0-m telescopes. The 4.2-m telescope is used mainly for spectroscopic work. For this study, only images taken with the moon below the horizon and during astronomical night (sun at least 18o below the horizon) were used. We concentrated on nights when several observations had also been made of photometric standard stars, and avoided periods when poor observing conditions were logged. Nights on which the Carlsberg Automatic Meridian Circle did not record a measure of extinction (usually because the night was not photometric) were excluded. Most of the data are drawn from the solar-minimum years 1994-6, but we also sampled the other years (> 1987) covered by the archive. In all, we measured the background brightness on 397 images taken on 58 nights with the Isaac Newton Telescope and 30 images on 5 nights with the Jacobus Kapteyn Telescope.
Sky brightness was measured in areas
apparently free of nebulosity, stars, cosmic-ray events or CCD defects.
Photometric calibration was obtained from the archived observations of
standard stars (usually from the list of Landolt 1992)
on the same night.
Sky brightness was calculated for each band, as follows:
Zeropoint (apparent mag for 1 count/sec):
Counts sec-1 pixel-1 from sky:
Sky brightness in mag arcsec-2:
where sky is the sky-background level on the exposures of standards; bias is the CCD bias level; counts and bias are within an aperture for the standard, and per pixel for sky; tauST and tauSK are the exposure times on standards (typically a few seconds) and sky (typically 200 - 1000 seconds); mapp is the catalogue apparent magnitude of the standard star in the relevant band; ext is the atmospheric extinction in magnitudes for the standard star (airmass x zenith extinction); and scale is the angular scale at the CCD (between 0.3 and 0.6 arcsec/pixel). In the equation for ZST, the mean zeropoint ZST for the given band for the night was used. Note that the standard-star magnitudes have been corrected for extinction, the sky brightnesses have not, following the convention adopted in most of the recent studies of sky brightness (e.g. by Walker 1988, Krisciunas 1990, Lockwood et al 1990, Leinert et al 1995, and Mattila et al 1996). Correcting the sky brightness for extinction would be appropriate only if the extinguishing layer were known to be below all sources of sky brightness, which is not the case; and would be feasible only if the relative amounts of extinction due to absorption (affecting light from stars and sky) and scattering (affecting only light from stars) were known.
To minimise the amount of data-reduction required, the CCD images were not flat-fielded. On the EEV and TEK CCDs in use during this period, the rms sensitivity variations are about 5% pixel to pixel and over larger areas. Since the sky brightness measurements were averaged over many pixels, and the counts from the standard stars were typically spread over ~ 10 pixels, omission of flat-fielding introduces errors <~ 5% into the measurements of sky brightness. To exclude non-photometric nights, data were discarded if the rms on the zeropoints for the standard stars was > 0.2 mag in any band, or, in a few cases, if the measured zeropoint was grossly different from that obtained with the same instrument/detector combination on other nights. The zeropoint for a given CCD is stable to < 10% from night to night.
The analyses reported in the following sections are based on 427 sky-brightness measurements and 451 observations of standard stars, made during 63 nights at the Isaac Newton and Jacobus Kapteyn Telescopes.
Fig. 5 - Stars represent data satisfying the following criteria: ecliptic latitude > 40 deg; galactic latitude > 10 deg; airmass < 1.4; mean V extinction during the night < 0.2 mag; at least one photometric standard observed that night; rms on standards < 0.15 mag; Tektronix or EEV CCD. Circles represent data satisfying similar criteria but with ecliptic latitude beta < 40o (i.e. contaminated by zodiacal light). The plotted points have been given a small random scatter along the abcissa to reduce overlap. On this and succeeding figures, points falling outside the graphed area are plotted at the appropriate edge (or corner). The dashed line indicates typical solar-minimum sky brightness measured at other observatories (from Table 1).
Fig. 6 - La Palma V sky brightness vs date. Symbols are as for Fig. 5.
Fig. 7 - La Palma R sky brightness vs date. Symbols are as for Fig. 5.
Fig. 8 - La Palma combined B-0.8, V sky brightness (i.e. data from Figs. 5 and 6) vs date. In this and succeeding figures, the measured sky brightnesses have been corrected for zodiacal light in order to reduce the scatter: the formula given in Table 2 has been used to normalise the sky brightnesses to ecliptic latitude beta = 40o (the size of the corrections applied is < 0.2 mag). The curve indicates the variation of sky brightness expected with solar activity, using the S10.7cm flux density as an indicator of solar activity, and assuming a total range of 0.4 mag. Symbols are as for Fig. 5.
Although these data sample only sparsely the period of solar maximum ~ 1990, an enhancement of sky brightness at that time is evident in Fig. 8, which includes both the B and V data, corrected for the contribution from zodiacal light. The sky was 0.4 +- 0.1 mag brighter in 1990 than in 1995. In R, the large variations in airglow intensity mask any changes with solar cycle, but assuming that the relative contributions of airglow and zodiacal light in V given in Table 2, that the brightness of the R airglow is proportional to that in V, and that the zodiacal light has the spectrum of a 6000-K blackbody, the predicted variation in total R sky brightness with solar cycle is ~ 0.5 mag. No measurements were made close to the time of the Pinatubo (1993.5) volcanic eruption, but the sky probably brightened then by a few tenths of a mag (Krisciunas 1996).
There are fewer measurements in U and I bands; the median sky brightnesses are U ~ 22.0, I ~ 20.0 mag arcsec-2, broadly consistent with the few values measured elsewhere (Table 1). The I brightness is dominated by OH (Meinel) emission bands (Fig. 1) and varies by up to a factor ~ 2 during the night.
Fig. 9 - La Palma sky brightness vs time after astronomical twilight. Stars: data taken after 1994.0, ecliptic latitude > 30o and satisfying the other criteria given in the caption of Fig. 5. Circles: data satisfying similar criteria but with ecliptic latitude beta > 30o. A correction has been made for the varying contribution of zodiacal light (see caption of Fig. 8).
The difference between the sky brightnesses at the beginning and end of the night is 0.03 +- 0.07 mag, consistent with zero. A similar plot against hours before dawn astronomical twilight provides no support for the idea that the sky is darkest before dawn. These results contrast with the finding by Walker (1988) that the sky brightness at San Benito dimmed by ~ 0.4 mag in B and V during the first half of the night. However, some of the variation he saw might be due to the diminishing contribution of zodiacal light at the zenith. This effect is particularly pronounced in the spring, when Walker observed, because at zenith both ecliptic latitude and helioecliptic longitude increase after astronomical twilight, and the zenith brightness will diminish by ~ 0.25 mag during the first half of the night (assuming the zodiacal-light distribution measured by Levasseur-Regourd & Dumont 1980). Walker noted this possibility but thought the intensity of the zodiacal-light varaiations too small to account for the effect he observed.
After astronomical twilight, the prominent 6300-A line diminishes rapidly in intensity, e.g. on 24 June 1995 from 150 A to 30 A equivalent width. This implies a small (<~ 0.1 mag) diminution in the broad-band R sky brightness. No variation > 0.1 mag is visible in a plot of R sky brightness against time after twilight.
Fig. 10 - La Palma sky brightness vs |ecliptic latitude beta|. Stars: measurements made after 1994.0, and satisfying the other criteria given in the caption of Fig. 5, except that relating to ecliptic latitude. The solid curve indicates the brightness variation predicted by the formula given in Table 2.
10 measurements were made at |beta| < 5 deg. One of these lies in the expected region of the gegenschein between 170 and 190o in longitude from the sun. It is 0.3 mag brighter than the median of the other 9, consistent within the errors with the 0.2 mag brightening expected in the antisun direction (Section 1.2).
Fig. 11 - La Palma sky brightness vs airmass. Stars: measurements made after 1994.0, ecliptic latitude > 30o, and satisfying the other criteria given in the caption of Fig. 5, except that relating to airmass. Circles: data satisfying similar criteria but with beta > 30o. A correction has been made for the varying contribution of zodiacal light (see caption to Fig. 8). The solid curve indicates the variation in sky brightness predicted by the second equation in Section 1.7, with f = 0.7.
Place Azimuth Population Distance Delta mag_G (deg) (1986) km Barlovento 50 3000 10 0.06 Los Sauces / San Andres 110 6000 12 0.08 Tenerife 115 600000 130 0.02 Santa Cruz 125 18000 15 0.18 Brena Alta/Baja 140 8000 15 0.08 La Gomera 140 17000 90 <0.01 El Paso 180 7000 12 0.10 El Hierro 190 7000 110 <0.01 Los Llanos / Tazacorte 200 23000 12 0.32Table 3 - Possible sources of light pollution at the observatory on La Palma. The estimated changes in zenith sky brightness given in the last column are from the model of Garstang (1989a). They are likely to be overestimates (see text) but give a rough idea of the relative contributions to be expected from different sources.
Orange glows are visible to the naked eye at azimuths ~ 50, 120, 190. The most luminous contributor is the island of Tenerife, but visual inspection of the horizon confirms what Table 3 suggests, that the glow in this direction is not particularly bright, and that lighting on Tenerife does not threaten the quality of the La Palma sky. Most of the contaminating light is from La Palma's 14000 streetlamps, which consume ~ 2 MW of electrical power and emit ~ 120 Mlumens, ~ 180 kW, of visible light (see Appendix for conversion factors). Approximately half of the light generated emerges from the lamp housing, and ~ 10% of the emerging light is reflected from the ground, so ~ 9 kW, or ~ 10 Wkm-2 (island area = 700 km2) escapes to the sky. This is comparable with the inbound light of the night sky, ~ 10 W km-2 (see Table 5), so that significant back-scattering by the atmosphere constitutes a light-pollution hazard. The fractional illumination provided by each type of lamp is given in Table 4.
Contamination of sky brightness (mag) Type of lamp Philips Flux U B V R brand % Sodium low-pressure SOX 49 0 0 0.05 0.04 Sodium high-pressure SON-T 21 0 <0.01 0.03 0.02 Mercury HPL-N 13 <0.03 0.02 0.01 0.02 Incandescent 15 <0.01 <0.01 0.01 0.02 Total <0.03 0.02 0.10 0.10Table 4 - Contamination of the sky above the observatory by streetlamps on La Palma. The first 3 columns give the lamp type, commonest Philips' serial and fraction of total lumens illumination on La Palma (information supplied by Javier Diaz of the Oficina Tecnica para la Proteccion de la Calidad del Cielo). Fluorescent lamps contribute a negligible fraction of the total illumination, ~ 2%. Columns 4 - 7 give the brightening of the sky above the observatory in mag for line plus continuum emission from the lamps, as estimated in Section 3.6 (U = 3200 - 3800 A, B = 3800 - 5000 A, V = 5000 - 5900 A, R = 5900 - 7200 A). The effect of NaD emission on the brightness of the sky in V and R is less than it otherwise might be because the line enters near the edge of the passbands in both cases (typically ~ 0.6 x maximum in V, ~ 0.75 * maximum in R for the passbands used for the observations described in this paper).
A royal decree of 1992 (La Ley del Cielo, reproduced in appendix 6 of McNally 1994) strictly limits outdoor night-time illumination on La Palma. Low-pressure sodium lamps must be used except in urban areas; the fraction of ultraviolet light emitted by lamps is limited; discharge-tube illumination, and most high-pressure sodium lamps, must be extinguished after midnight. Lamps must not emit light above the horizontal, so only the ~ 10% of the light reflected from the ground (snow does not fall on the streetlit parts of the island) escapes into the sky. Between 1992 and 1997, the estimated amount of light escaping into the sky has decreased by 20% as a consequence of an ongoing programme to improve the efficiency and shielding of public lighting (Javier Diaz, private communication).
The V-band zenith sky brightness on La Palma is similar to that at other dark sites (Table 1), which suggests that light pollution must contribute <~ 0.1 mag to the total. Sky brightness is plotted against azimuth in Fig. 12. The raw data show considerable brightening in the south, but as can be seen from Fig. 12, this brightening disappears after the measuerments are corrected for the contribution of zodiacal light, and there is no discernible peak in sky brightness at any particular azimuth.
Fig. 12 - La Palma sky brightness vs azimuth. Stars: measurements made after 1994.0, ecliptic latitude > 30o, and satisfying the other criteria given in the caption of Fig. 5. Circles: data satisfying similar criteria but with beta > 30o. A correction has been made for the varying contribution of zodiacal light (see caption to Fig. 8); without this correction, the sky appears brighter in the south because of the lower mean ecliptic latitude (reflected in the preponderance of data represented by circles). A similar plot for airmass > 1.4 is sparsely populated (see Fig. 11) but shows no dependence of sky brightness on azimuth.
A much stronger limit on the contribution of light pollution to the brightness of the sky may be obtained from the equivalent widths of the NaD and Hg lines in the spectrum of the zenith night sky. These yield directly the contribution to sky brightness from emission lines, while that from broad and continuum features can be inferred from the strengths of the emission lines, the known shapes of the lamp spectra (given e.g. by Osterbrock 1976, and in the Philips Catalogue of Lamps), and the relative numbers of lamps of different kinds. The median equivalent widths of the NaD 5890/6, Hg 5460 and Hg 4358 A lines at solar minimum (when the continuum is faintest) during summer (when the airglow NaD is dimmest) are 100, 7 and 9 A respectively, although they vary by a factor of ~ 1.5, probably due to changing cloud cover below the observatory (as found at Palomar, see Turnrose 1974), which often blots streetlighting from view. The equivalent width shows no significant variation with zenith distance for ZD < 45o. Below are derived estimates of contamination in each of the bands U, B, V and R (negligible in I, where sky brightness is dominated by the OH airglow). The results are summarised in Table 4.
Low-presure sodium lamps
An opportunity to separate the airglow and light-pollution NaD contributions arose on the night of 24/25 June 1995, when the Instituto de Astrofisica de Canarias arranged for most of the ~ 100000 street lamps on the four western Canary islands (La Palma, Tenerife, La Gomera and El Hierro) to be switched off for 1 hour starting at local midnight, to celebrate the 10th anniversary of the inauguration of the observatories. The observer at the William Herschel Telescope that night (Ian Waddington) happened to be taking near-zenith low-resolution spectra covering most of the visible range. From these it was possible to extract spectra of the moonless sky before, during and after the blackout (Fig. 13).
The equivalent widths of the NaD line before and during the blackout were 75 and 30 A respectively. At this wavelength, with the zenith sky brightness given in Table 2, an equivalent width of 30 A corresponds to 30 Rayleighs (see Appendix), in agreement with the 30 Rayleighs given by Allen (1973) for the summer strength of the NaD line. Thus, of the 100-A median observed equivalent width of the NaD line during the summer, ~ 70 A (70 Rayleighs) is due to street lighting, corresponding to an increase in sky brightness of ~ 0.04 mag in both V and R bands (equivalent width / bandwidth x relative filter transmission at 5893 A).
High-pressure sodium lamps
In summary, light pollution contributes < 0.03 mag to the zenith continuum sky brightness in all bands (Table 4), well below the IAU recommendation of < 0.1 mag at ZD = 45o, (see Section 1.5) for a dark observing site. The strength of the typical NaD 5890/6-A light pollution, ~ 70 Rayleighs, exceeds that due to natural airglow radiation (the limit recommended by the IAU for a dark site) during the summer. However, few spectroscopic observing programmes are likely to be adversely affected by this contamination. Streetlamp emissions in the Hg and NaD lines raise the broad-band V and R sky brightnesses by 0.09 and 0.08 mag respectively. The total contamination is < 0.03 mag in U, ~ 0.02 mag in B, ~ 0.10 mag in V, ~ 0.10 mag in R.
This degree of light pollution is comparable to that at Kitt Peak, ~ 0.02 mag in B, 0.05 mag in V in 1988 (Massey et al 1990) from Tucson (275000 inhabitants, 65 km distant). It is less than that at Calar Alto, ~ 0.2 mag in V (Leinert et al 1995) from Almeria (160000 inhabitants, 45 km distant). It is more than that at La Silla, probably <~ 0.02 mag (Mattila et al 1996) from Vallemar (38000 inhabitants, 65 km away) and La Serena (160000 inhabitants, 150 km away).
The change in sky brightness due to backscattering of streetlighting depends in a complex way on the size, space density and vertical distributions of the scattering species, on the distribution of streetlamps and on local topography (e.g. obscuring mountains) (Garstang 1989a,b, 1991a,b,c). However, a rough order-of-magnitude upper limit can be placed on the possible brightening of the sky due to this backscattering. We noted above that the intensities of eartbound light from the night sky, and of spacebound light escaping from street lamps, are similar, ~ 10 Wkm-2, so that if a large fraction of the streetlighting is back-scattered, the brightness of the sky could increase by a factor ~ 2, i.e. by ~ 1 mag.
The relationship between extinction Av and brightening of the sky Delta may be predicted on the basis of an approximate model. About 0.1 mag of the total extinction on La Palma is due to atoms and molecules (King 1985), the rest (Av - 0.1) to dust. The dust is lower lying and is probably responsible for scattering back most of the street illumination which reaches the observatory. The intensity of the scattered light (proportional to 10Delta/2.5 -1) should be proportional to the fraction of starlight extinguished by dust (1-10-(Av-0.1)/2.5). Thus:
Measured sky brightness is plotted against extinction Av (as recorded for the night by the Carlsberg Automatic Meridian Circle) in Figs. 14, 15. For Av < 0.25 mag, there is no significant variation (< 0.1 mag) of sky brightness with Av. Approximately 20% of nights on La Palma have Av > 0.25 mag, but our sample includes none satisfying the criteria given in the caption to Fig. 14, and when B, V measurements were made. Measurements were made from images taken at low ecliptic and galactic latitude on 21 August 1990 (INT, Av = 0.44 mag) and 13 June 1996 (JKT, Av = 0.76 mag), and the sky was markedly bright on both nights (Fig. 15). In part, this brightening is due to the lower ecliptic and galactic latitudes of the observations (Table 2), but the contributions from these effects are much smaller than the observed changes, and in the case of the 1996 data, similar measurements were obtained from the sky background on observations of high-latitude standard stars. On both nights, a similar number of measurements was made in both B and V bands, and the increases in sky brightness Delta B,V mag in the two bands are similar within the errors, Delta B,V ~ 0.3 mag (after correcting for the variation due to the solar cycle) at extinction 0.44 mag, Delta B,V ~ 1.4 mag at extinction 0.76 mag. Data are available in R band for June 1996, and the brightening is again ~ 1.4 mag.
The brightening by 0.3 mag when Av = 0.44 mag implies that in the equation above, const = 1.0. This then predicts that for Av = 0.15 mag (median non-summer value), Delta ~ 0.06 mag, consistent with the observed value (0.10 mag) given in the last row of Table 4. For Av = 0.76 mag, on the other hand, the predicted brightening is only Delta = 0.5 mag, compared with an observed 1.4 mag. Clearly the model is naive for very large extinctions, possibly because the amount of dust close to the observatory does not vary in a simple way with the measured extinction of starlight.
The similarity in Delta V and Delta R is consistent with the predictions of Table 4, since the contribution in both bands is determined mainly by the scattering properties of the dust at 5890/6 A. The similarity Delta B and Delta V is less easily explained, but the ratio is hard to predict, given the possible wavelength-dependence of the fraction scattered, and a probably changing mix of streetlamp types in the light scattered when the extinction is unusually high (the contribution from some towns may be blotted out). More detailed investigation of the effects of dust on sky brightness will be the subject of future work (maybe).
Fig. 14 - La Palma sky brightness vs mean extinction Av during the night, as measured by Carlsberg Automatic Meridian Circle. Stars: measurements made after 1994.0, ecliptic latitude > 30o, and satisfying the other criteria given in the caption of Fig. 5, except that relating to extinction. Circles: data satisfying similar criteria but with beta > 30o.
A correction has been made for the varying contribution of zodiacal light (see caption to Fig. 8).
Fig. 15 - As Fig. 14, but relaxing the selection criteria so that data with lower ecliptic and galactic latitudes from the INT (21 Aug 1990, extinction = 0.44) and JKT (13 June 1996, extinction = 0.76) are included.
Because of the significant equivalent widths of the emission lines in the airglow spectrum, the pseudo-continuum sky brightness in V,R seen by spectroscopists is ~ 0.2 mag fainter than the broad-band sky brightness seen by imaging observers.
Band wavel log10 Jy mag S_10 microJy ph R/A W/km^2 mic Hz mag0 "^-2 arcsec^-2 rate /ster U 0.36 14.92 1810 22.0 205 2.87 0.012 0.64 1.02 B 0.44 14.83 4260 22.7 107 3.54 0.012 0.65 1.03 V 0.55 14.74 3640 21.9 224 6.33 0.017 0.93 1.47 R 0.64 14.67 3080 21.0 515 12.26 0.029 1.55 2.45 I 0.79 14.58 2550 20.0 1294 25.50 0.049 2.61 4.13 J 1.22 14.39 1570 16.6 29648 359.67 0.445 23.80 37.68 H 1.63 14.26 1020 14.4 224905 1772.56 1.640 87.80 138.98 K 2.19 14.14 640 12.0 2051163 10143.32 6.986 373.97 591.92Table 5 - La Palma dark-of-moon sky brightness is given in columns 5 - 10, in various units (see Appendix for details of the conversions). The V sky brightness corresponds to ~ 59 nLamberts. Approximate measurements in J,H, and K, from WHIRCAM on the William Herschel Telescope, are included for convenience. The K value includes an unknown thermal contribution from the telescope; at UKIRT on Mauna Kea the measured K brightness is about 1.5 mag dimmer. Columns 1, 2, 3 and 4 give the band name, wavelength in microns, log10(frequency/Hz) and the equivalent intensity in Jy for apparent mag = 0 (this last from Bessell 1979, Bessell & Brett J.M., 1988). The units of column 8 (ph) are photons s-1m-2A-1arcsec-2. The last column gives nu snu in Wkm-2ster-1. The total sky brightnesses in the optical, in microwave-background photons and in cosmic rays, are remarkably similar, a few Wkm-2 each. Some of the energy of the cosmic-rays is converted to optical (Cerenkov) photons, but they contribute only ~ 10-4 of the total sky brightnes (Jelley 1958).
The sky brightness in V, R is similar to that at other dark sites.
In B the sky is measured to
be about 0.2 mag brighter than at other sites, but this may be because most
of the B data are drawn from 1995 when the B sky brightness was still
declining (Krisciunas 1997).
The V sky brightness on La Palma (and probably at other sites)
is given approximately (+- 0.1 mag) by the following formula
(reflecting the contributions listed in Table 2):
with a small contribution (<~ 0.1 mag) from light pollution, much enhanced in the presence of extinction > 0.25 mag. The symbols are as given in Table 2. airmass approximates the van Rhijn factor given by the first equation in Section 1.7. The colour of the La Palma sky at solar minimum is B-V ~ 0.8, V-R ~ 0.9.
For sky-limited exposures, an uncertainty of 0.4 mag in the surface brightness of the night sky translates into an uncertainty of a factor of 2 in the exposure time required to reach a given signal-to-noise, with potential wastage of half that time. The measurements reported here of the absolute level of sky brightness, and of the ways in which it varies, allow more efficient use to be made of telescope time.
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Physical units of surface brightness:
The lumen, used by lighting engineers, is a measure of luminous flux as perceived by the eye. An isotropic source of luminous flux 4pi lumens has a luminous intensity of 1 candela = 1 lumen ster-1, and this illuminates a surface 1 m away with illuminance E = 1 lux = 1 lumen m-2 = 10-4 phot.
Luminance L measures light emitted or reflected by a surface, in lumens ster-1 m-2 (= cd m-2 = nit) (1 stilb = 1 cd cm-2, 1 lambert = 1/pi cd cm-2). Crawford (1997) gives a useful summary of these units and their interconversions.
V = 21.9 mag arcsec-2 corresponds to 0.00019 cd m-2 equivalent to 59 nLamberts.
Typical luminance values from Crawford (1997) and Holmes (1997):
Surface L (cd m^-2) Dark night sky 0.0002 Sky at full moon 0.03 Lit road surface at night 0.5 Zenith at sunset 100 Surface of full moon 2500 Candle 10000 Surface of sun 1.6 x 10^9
A surface of luminance L cd m-2, subtending solid angle omega ster, yields an illuminance E = L omega lm m-2, e.g. for the sun, L = 1.6 x 109 cd m-2, omega = 7.7 x 10-5 ster, E = 1.2 x 105 lum m-2. Note that the values of L, whose units are lm ster-1 m-2, can be interpreted in two equivalent ways: as the number of lumens emitted into each steradian by each m2 of a luminous surface, or as the number of lumens received by each m2 of a surface from each steradian subtended by an emitter.
At 5550 A, 1 W ~ 680 lumens (Kaye & Laby 1973). On La Palma, the streetlamps (typically emitting a few thousand lumens each) produce an average of 63 lumens per W of electrical power supplied by the lamp control gear. Approximately half the lumens emitted escape from the lamp housing, and about 10% of the latter are reflected upwards by the ground.
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