Page updated: April 12, 2020
Author: Curtis Mobley
View PDF

# The Atmospheric Correction Problem

An instrument viewing the ocean from a satellite or aircraft measures upwelling radiances that include contributions by the atmosphere, the water surface, and the water column. The atmospheric contribution ${L}_{a}$ comes from solar radiance that is scattered one or more times by atmospheric gases and aerosols into the direction of the sensor. The surface-reﬂected radiance (sun and sky glint) ${L}_{r}$ is downwelling solar radiance that is reﬂected toward the sensor by the water surface. The water-leaving radiance ${L}_{w}$ comes from light that is transmitted through the surface into the ocean, ${L}_{t}$, where it is changed by the absorbing and scattering components in the water, and is then scattered into an upward direction, ${L}_{u}$, and eventually leaves the sea surface in the sensor direction. Figure 1 shows this conceptually.

Radiance reﬂected by the sea surface contains information about the wave state of the surface, which may be of interest in itself or which, for example, may be useful for detection of surface oil slicks. Radiance scattered by the atmosphere along the path between the sea surface and the sensor contains information about atmospheric aerosols and other atmospheric parameters. However, only the water-leaving radiance carries information about the water column and bottom conditions. A sensor looking downward measures the total radiance ${L}_{u}={L}_{a}+{L}_{r}+{L}_{w}$ and cannot separate the various contributions to the total. Atmospheric correction refers to the process of removing the contributions by surface glint and atmospheric scattering from the measured total to obtain the water-leaving radiance.

Figure 2 shows examples of at-sensor total radiances ${L}_{u}$ for diﬀerent sensor altitudes. The inputs to MODTRAN were for

• cloudless mid-latitude summer atmosphere
• marine aerosols
• relative humidity of 76% at sea level
• solar zenith angle of 50 deg
• surface wind speed of $6\phantom{\rule{1em}{0ex}}m\phantom{\rule{0.3em}{0ex}}\phantom{\rule{0.3em}{0ex}}{s}^{-1}$

These atmospheric conditions gave excellent remote-sensing conditions with a horizontal visibility of 63 km at sea level. The HydroLight inputs were for

• homogeneous water
• Case 1 water with a chlorophyll concentration of $1\phantom{\rule{1em}{0ex}}mg\phantom{\rule{0.3em}{0ex}}\phantom{\rule{0.3em}{0ex}}{m}^{-3}$
• inﬁnitely deep water

The runs were from 300 to 1000 nm with 10 nm bandwidths. The sun and viewing geometry gives almost no sun glint radiance. However, there is always surface-reﬂected sky radiance, which shows up in the surface (zero altitude) spectrum (black curve) as non-zero ${L}_{u}$ radiance beyond 750 nm, where the water-leaving radiance is very close to zero. The diﬀerences in these curves are due solely to atmospheric contributions along the diﬀerent path lengths from the sea surface to the sensor because all other conditions were the same for each curve. This ﬁgure shows that there is a noticeable atmospheric contribution to the total radiance even for sensors just a few hundred meters above the surface in very clear atmospheres. Airborne sensors typically ﬂy at altitudes from 3,000 to 10,000 m, and even at lower altitudes the atmospheric contribution is greater than the water-leaving radiance. At 30,000 m, a sensor is eﬀectively above the top of the atmosphere (TOA) and atmospheric path radiance is typically 90-95% of the total.

Figure 3 shows the Fig. 2 at-sensor radiance at 3,000 m partitioned into the contributions by water-leaving, surface-reﬂected, and atmospheric path radiances; the individual contributions can be separated in the numerical models. This altitude is typical for aircraft acquiring high spatial resolution hyperspectral imagery.

The atmospheric correction problem becomes even more intimidating when eﬀects of sun and sensor viewing directions, atmospheric conditions, and surface wave state are considered. The following ﬁgures show a few examples of simulations performed in support of the design of the proposed NASA HyspIRI (Hyperspectral InfraRed Imager) mission. That sensor will measure radiances at the top of the atmosphere at 10 nm resolution from 380 to 2500 nm with 60 m ground resolution. The simulations shown below all have a chlorophyll value of $0.05\phantom{\rule{1em}{0ex}}mg\phantom{\rule{1em}{0ex}}{m}^{-3}$ characteristic of the very clear Case 1 ocean water near the Hawaiian Islands. The atmospheric conditions are for either a very clear tropical atmosphere (horizontal visibility of 100 km at sea level) or one with considerable haze (horizontal visibility of 10 km). The wind speed was 0 (a level sea surface) or $10\phantom{\rule{1em}{0ex}}m\phantom{\rule{1em}{0ex}}{s}^{-1}$. The sensor viewing direction was 30 deg east of nadir, nadir, or 30 deg west of nadir. The sun zenith angle was 18 deg, which corresponds to the time of the satellite overpass on 21 June at Station Aloha, near Hawaii.

Figure 4 shows the TOA radiances computed for the clear atmosphere, wind speed of $U=10\phantom{\rule{1em}{0ex}}m\phantom{\rule{1em}{0ex}}{s}^{-1}$, and a viewing direction of 30 deg east of the satellite nadir direction. The blue curves are the total radiance ${L}_{u}$, orange is atmospheric path radiance ${L}_{a}$, green is water-leaving radiance ${L}_{w}$, and red is sun and sky glint ${L}_{g}$. The solid lines are the radiances measured at the TOA and the dashed lines are radiances at the sea surface. Thus the dashed green curve is the true water-leaving radiance just above the sea surface. The solid green curve is how much of ${L}_{w}$ at the surface makes it to the TOA; the rest is lost to absorption and scattering along the path from the sea surface to the TOA. The TOA ${L}_{u}$ curve is the sum of the TOA atmospheric, water-leaving, and glint radiances. The surface (SFC) ${L}_{u}$ curve is the sum of the corresponding surface contributions; note that there is no atmospheric contribution at the surface. The atmospheric correction problem is to measure the solid blue spectrum and then extract the dashed green spectrum.

Figure 4 also shows the plane irradiance ${E}_{d}$ at the TOA and sea surface. Water-vapor and $C{O}_{2}$ absorption bands centered near 1400 and 1900 nm reduce the sea-level ${E}_{d}$ to essentially zero in those spectral regions.

Most remote-sensing retrieval algorithms use the remote-sensing reﬂectance ${R}_{rs}={L}_{w}∕{E}_{d}$ or an equivalent nondimensional reﬂectance $\rho =\pi {L}_{w}∕{E}_{d}$. (If ${L}_{w}$ were directionally isotropic, ${R}_{rs}=1∕\pi$, so $\rho$ is the ratio of the actual ${R}_{rs}$ to an idealized isotropic remote-sensing reﬂectance. The $\pi$ carries units of steradian.) The use of an apparent optical property like ${R}_{rs}$ or $\rho$ minimizes the eﬀects of external environmental conditions like sun angle on the magnitude of the spectra.

Figure 5 plots the same information as Fig. 4 but in terms of $\rho$. The TOA $\rho$ spectra were computed from the TOA radiances divided by the TOA ${E}_{d}$; the surface $\rho$ spectra were computed from surface radiances divided by the surface ${E}_{d}$. The surface sun and sky glint ${\rho }_{g}$ spectrum was not plotted near 1900 nm because the ${E}_{d}$ values at the sea surface were too small for accurate numerical computation (a small eﬀect of numerical inaccuracy in ${\rho }_{g}\left(SFC\right)$ is also seen near 1350 nm). Note that the surface glint reﬂectance spectrum ${\rho }_{g}$ (red dashed curve) is nearly independent of wavelength because the glint radiance spectrum has almost the same wavelength dependence as the surface irradiance that is being reﬂected by the sea surface.

Figure 6 compares the $\rho$ spectra for viewing directions of 30 deg east of nadir, nadir, and 30 deg west of nadir. The sky was clear and the wind speed was $10\phantom{\rule{1em}{0ex}}m\phantom{\rule{1em}{0ex}}{s}^{-1}$. The ${\rho }_{g}$ spectra are much diﬀerent for the diﬀerent viewing directions. The sun is almost due east and high in the sky, so the 30 deg east viewing direction sees a lot of sun glint and has a high-magnitude ${\rho }_{g}$. The 30 deg west viewing direction sees very little sun glint and has a ${\rho }_{g}$ that is mostly sky reﬂectance. The atmospheric path radiances are noticeably diﬀerent for the three viewing directions because of the diﬀerent scattering angles between the sun’s direct beam and the viewing direction, and because of the diﬀerences in path length through the atmosphere for the east and west vs nadir directions. The water-leaving reﬂectances ${\rho }_{w}$ are almost independent of viewing direction. The almost unnoticeable (in this ﬁgure) diﬀerences in the three ${\rho }_{w}$ curves are due to diﬀerences in the in-water scattering angles and path lengths.

Figure 7 shows the $\rho$ spectra for clear vs. hazy sky conditions. The wind speed was $10\phantom{\rule{1em}{0ex}}m\phantom{\rule{1em}{0ex}}{s}^{-1}$ and the viewing direction was 30 deg west. The diﬀerences in atmospheric path radiance are most pronounced in the infrared. There is some diﬀerence in the surface glint spectra because the glint for the hazy atmosphere contains more sky reﬂectance and less direct sun glint than for the clear sky case. The water-leaving radiances are indistinguishable in the plot.

Figure 8 shows the eﬀect of wind speed for a clear sky and a nadir viewing direction. The large diﬀerence in the surface reﬂectance spectra ${\rho }_{g}$ is due to the large amount of direct sun glint in the $10\phantom{\rule{1em}{0ex}}m\phantom{\rule{1em}{0ex}}{s}^{-1}$ case. There is only sky glint when the surface is level. The atmospheric path reﬂectances are diﬀerent because the diﬀerent wind speeds result in diﬀerent concentrations of aerosols in the marine boundary layer.

Figure 9 summarizes Figs. 5-8 by showing the 12 ${\rho }_{u}$ spectra at the TOA for the two winds speeds of 0 and $10\phantom{\rule{1em}{0ex}}m\phantom{\rule{1em}{0ex}}{s}^{-1}$, the two sky conditions of clear and hazy, and the three viewing directions of 30 deg east, nadir, and 30 deg west. As before, the green spectrum at the bottom is ${\rho }_{w}$, which is almost the same for each of the 12 ${\rho }_{u}$ spectra. Given any of the ${\rho }_{u}$ spectra measured at the TOA, one must some way extract the surface ${\rho }_{w}$ spectrum. This is clearly a diﬃcult task owing to the non-unique relation between TOA and water-leaving radiances, and it is only partially solved.

Atmospheric correction is the central problem of ocean color remote sensing. However, the problem is not intractable–if it were, we could not do ocean color remote sensing! There are many inversion algorithms that can retrieve ocean properties such as chlorophyll, mineral, or CDOM concentrations, or bottom depth and reﬂectance, IF an accurate ${\rho }_{w}$ is available. The hard part of the game is to get from ${\rho }_{u}$ measured at the TOA to ${\rho }_{w}$ at the sea surface. The process of atmospheric correction is considered in detail in the Atmospheric Correction chapter.