Limb Geometry Overview and Setup

A typical limb-viewing geometry is shown in the figure below where a satellite is orbiting the Earth at locations P1, P2 and P3. At each location an instrument looks towards the atmospheric limb in directions L1, L2, L3 observing tangent points T1, T2 and T3.

_images/limbgeometry_basic.png

The HR engine is used to calculate the vector or scalar radiance observed by the instrument at each location. There is a huge computational saving if we assume all measurements are sufficiently close together that they essentially occur at the same instant with the same solar illumination conditions. If we can make this assumption then we only have to solve the diffuse radiative field once and can quickly integrate through the field for each line of sight. If the assumption is not valid then the calculation must be broken down into smaller subsets and the HR engine re-configured for each separate illumination condition.

We generally use 2 minutes as a reasonable period to consider measurements instantaneous. This period is the time taken for the Sun to move one solar disk, or 0.5 degrees, across the sky (assuming 15 degrees/hour). This seems a reasonable limit given that the 0.5 degree, finite size of the Sun is not generally accounted for in the HR engine.

Lines of Sight

All sasktranif engines assume you can define each line of sight with:

  1. the position (P1, P2, P3) of the observer as (X,Y,Z )vectors from the center of the oblate Earth.
  2. the look direction (L1, L2, L3) away from the observer as unit vectors.
  3. the time of the measurements as a modified julian date. This condition is relaxed if you know the direction of the Sun and all climatologies are time independent.

X is a horizontal unit vector in the equatorial plane of the oblate Earth from the centre of the Earth towards 0 degrees longitude, Z is a unit vector parallel to the Earth’s spin axis and Y forms the third vector of a right-handed system. This system works well for many observational data sets but if you have a different way of specifying the same information then class ISKGeodetic has been written to help you convert to the required system. Let us know if ISKGeodetic is lacking the functionality you need.

Sun Direction

You will normally not specify the unit vector of the Sun as the HR engine by default will calculate the Sun’s position using the average of the modified julian dates (mjd) of the lines of sight. You must override the default setting if you are creating test lines of sight and/or want to explicitly set the position of the sun. The sun position is specified as a unit vector from the centre of the Earth toward the Sun using the same X,Y,Z corodinate system as the observer coordinates.

Reference Point and Osculating Sphere

The HR model approximates the shape of the Earth to be a sphere. The radius of the sphere is chosen so it matches the radius of curvature of the Earth at a Reference Point. This sphere is called the osculating sphere as it kisses the true oblate Earth at the reference point, see figure below. The Reference Point is normally chosen from the average of the tangent point or ground intersection of each line of sight.

_images/limbgeometry_osculating.png

The centre of the osculating sphere is offset from the centre of the true oblate Earth and the HR engine creates an internal coordinate transformation that maps positions from one system to the other and vice-versa. The transformation from true oblate Earth to osculating sphere coordinates generates a small height registration difference for locations not directly above the reference point. This is important as lines of sight not tangent at the reference point will have a tangent height slightly higher in the osculating system than in the oblate system. By default the HR engine adjusts the look vector of lines of sight which are tangential within the true oblate atmosphere so they look at the same tangent height in the osculating system.

Surface Height and TOA

By default the HR engine will assume the surface of the Earth is at 0 meters above mean sea-level and the top of the atmosphere is at 100 kilometers (100,000 m). Both the lower and upper altitudes can be set to other values using properties TOAHeight and SurfaceHeight. Lowering the upper altitude can have a significant positive impact upon performance as it reduces the size of the diffuse field.

Polarization

The HR engine supports calculation of either scalar radiances or full stokes vectors, see property SetPolarizationMode(). The polarization calculation is done through an approximation–for low orders of scatter the full calculation is performed, while higher orders of scatter are assumed to have a specific polarization state. The level of approximation used is controlled through calling SetPolarizationMode().

There are two functions that perform the radiative transfer calculation, CalculateRadiance() and CalculateStokesVector(). These do not determine whether or not a polarized calculation is performed, they only determine the final return type: CalculateRadiance() returns a two dimensional array of scalar values representing \(I\) while CalculateStokesVector() returns a two dimensional array of ISKStokesVector objects. Whether or not a polarization calculation is done or not is determined entirely by SetPolarizationMode().

Number of Scatter Orders

The successive orders algorithm successively calculates higher orders of scatter using the previous order of scatter. The maximum number of scatter orders calculated is set through:

ok = engine.SetProperty('numordersofscatter', n)

where n is the number of scatter orders. The default value is n=50.

Caching is done in the HR engine which makes the second order of scatter take the longest time to run. All orders after the second are relatively quick. Furthermore, convergence checking is done internally in the engine which stops the calculation when rays stop contributing to the final answer. For these reasons it is recommended to use either n=1 (for a quick not-accurate calculation) or n=50 (for the full calculation).

Diffuse Profiles

The primary option that controls the accuracy of the HR radiative transfer calculation is the number of diffuse profiles. Each diffuse profile represents a single solar zenith angle where the multiple scattering source function is calculated. By default, only one diffuse profile is used in the calculation and is placed at the solar zenith angle of the average tangent point. Whether or not this is appropriate is heavily dependant on a variety of factors

  • Wavelength – Wavelengths where the atmosphere is thick and there is little absorption (e.g. around 350 nm) have a large amount of multiple scatter and are more sensitive to the number of diffuse profiles.
  • Solar zenith angle span – Since the multiple scattering source function varies with solar zenith angle, lines of sight which have a large solar zenith angle span will be sensitive to the number of diffuse profiles. Solar scattering angle is a rough proxy of this effect. Forward and backward scatter geometries will be most sensitive to the number of diffuse profiles, while scattering angles near \(90^\circ\) will see no effect.
  • Solar zenith angle – The absolute solar zenith angle also effects the optimal number of diffuse profiles. The multiple scattering source function is slowly varying for low solar zenith angles (sun high in the sky) and varies rapidly at high solar zenith angles near the solar terminator. Generally, more diffuse profiles are required the closer you get to the terminator.
  • What the radiance is being used for – Often times the absolute radiance is not the quantity of interest. For example, in many retrievals radiances are normalized by high altitude measurements. This normalization process removes a lot of the dependence on the number of diffuse profiles.

The number of diffuse profiles can be changed in the HR option through:

ok = engine.SetProperty('numdiffuseprofilesinplane', n)

where n is the number of diffuse profiles. Calculation time scales roughly linearly with the number of diffuse profiles; a calculation with 5 diffuse profiles will take approximately 5 times as long as a calculation with 1 diffuse profile. RAM usage scales the same way.

Figuring out the optimal number of diffuse profiles for a specific situation is an important and difficult problem. As a first step, we recommend switching between n=1 and n=5 and seeing how the results change. As an additional tool, radiances can be benchmarked against the MC engine to verify that the number of diffuse profiles used is sufficient.

Weighting Functions

The HR engine supports analytical computation of weighting functions for absorbing and scattering species. The theoretical basis for the method is described in [Zawada2015]. Prior to calculating weighting functions it is necessary to both tell the engine to calculate weighting functions, and specify the species we are calculating weighting functions for.

Example:

import sasktranif.sasktranif as skif
engine = skif.ISKEngine('HR')

# Set up lines of sight/wavelengths/atmosphere

optprop_o3 = skif.ISKOpticalProperty('O3_DBM')
ok = engine.SetProperty('WFSpecies', optprop_o3)
ok = engine.SetProperty('calcwf', 2)
ok, rad = engine.CalculateRadiance()
ok, wf = engine.GetWeightingFunctions()

The wf object that is returned is a three dimensional numpy.ndarray with dimensions corresponding to [wavelength, line of sight, volume],

\[\texttt{wf[i, j, k]} = \frac{\partial I(\lambda_i, \text{LOS}_j)}{\partial x_k},\]

and has units of [radiance/cm^{-3}]. In our example, the quantity \(x_k\) is the ozone number density over a finite volume. Since we set calcwf = 2 the finite volumes are uniform spherical shells spaced 1 km apart evenly from 0.5 km to 99.5 km. Therefore, the quantity wf[i, j, 10] can be thought of as the derivative of the radiance (for wavelength i and line of sight j) with respect to changing ozone number density in the 10.5 km shell.

Notes

Currently the model is limited to calculating weighting functions for one species at a time. This is normally not an issue, since typically wavelengths used for retrievals are sensitive to only one species.

The weighting function species does not have to be a species that was added to the model.

Weighting functions are not calculated by assuming a constant perturbation within the specified finite volume. Rather, the returned quantity should be thought of as the derivative of radiance with respect to how HR responds to changes in that volume. For example, when the finite volume is spherical shells, linear interpolation is done between the shell directly above and below the specified shell to better represent how the radiative transfer calculation is done.

Standard Mode

This is the recommended mode for weighting function calculations using a one dimensional (spherically symmetric) atmosphere, and is set through:

ok = engine.SetProperty('calcwf', 2)

Weighting functions are calculated on a grid of spherical shells. By default this is an evenly spaced grid from 0.5 km to 99.5 km in steps of 1 km; i.e. the returned wf object will have dimensions (len(wavel), len(lineofsight), 100), and the quantity wf[i, j, 10] can be thought of as the derivative of the radiance (for wavelength i and line of sight j) with respect to changing number density in the 10.5 km shell.

The shell locations and widths can be changed through the properties wfheights and wfwidths:

wfwidths = [2000, 2000, 2000, 2000]
wfheights = [10000, 20000, 30000, 40000]

engine.SetProperty('wfwidths', wfwidths)
engine.SetProperty('wfheights', wfheights)

Weighting functions will now be calculated for spherical shells centred at [10 km, 20 km, 30 km, 40 km] with widths of 2 km.

Line of Sight Mode

The line of sight weighting function mode is a special mode where weighting functions are calculated on the tangent altitude grid of the lines of sight. This can be useful for some retrieval algorithms and is set through:

ok = engine.SetProperty('calcwf', 1)

The weighting functions returned has dimensions (len(wavel), len(linesofsight), len(linesofsight)) and are centred on the line of sight tangent altitudes. The widths are chosen such that the spherical shell extends between the line of sight directly below and the line of sight directly above.

Two Dimensional Mode

Not yet written.

Other Options

While the computation time of weighting functions for a standard multiple scatter calculation is negligible compared to the actual calculation, for some situations (e.g. single scatter in the IR region) the majority of time could be spent calculating weighting functions. For this reason we have added the option wfprecision.

By default, weighting functions are calculated considering three effects:

  • Line of sight
  • Solar
  • Higher Order

By setting:

ok = engine.SetProperty('wfprecision', 1)

The solar and higher order effects are turned off, thus only line of sight contributions are accounted for. This degrades the quality of the weighting functions, but often they are still usable for retrieval purposes.

Three Dimensional Atmospheres

The HR model supports calculations where atmospheric constituents are allowed to vary three dimensionally.