Optical (UV/visible) Remote Sensing Remote Sensing I Lecture 8 Summer 2006 B.-M. Sinnhuber

Material for this lecture by courtesy of Christian von Savigny and Andreas Richter

The optical (UV-visible-NIR) spectral range 1 nm 10 nm 100 nm200 nm 400 nm 700 nm 5  m VisibleVacuum UV Near UV NIRIR EUVX-rays  100 nm400 nm320 nm280 nm UV AUV CUV B

The sun as a light source the solar spectrum can be approximated by a black body at temperature 5780K absorption in the solar atmosphere leads to Fraunhofer lines in the atmosphere, the solar radiation is attenuated by scattering and absorption strong absorption by O 3, O 2, H 2 O und CO 2 there are some atmospheric windows where absorption is small multitude of Fraunhofer lines 11 year solar cycle, particularly relevant at short wavelengths < 300 nm spectrum varies over the solar disk Doppler shift resulting from rotation of sun variation of intensity due to changes in distance sun - earth => sun is not an ideal light source!

Instrumentation for remote sensing measurements Atmospheric remote sensing methods usually require spectrally resolved radiation measurements  spectrally dispersing elements required The standard radiation-dispersing devices are: Prisms Gratings Michelson Interferometers Fabry-Perot Interferometers

Prism spectrometer The prisms exploits refraction in media with different refractive indices n for spectral dispersion:  ’’ n prism > n medium Refraction is described by Snell’s law: n = c 0 / c is the refractive index c 0 is the speed of light in vaccum

For constructive interference, the path difference between two neighboring grating rules has to be a multiple of the wavelength: Diffraction by a grating Gratings are the most common dispersing elements used in remote sensing instruments: g    m g  g distance between grating grooves m diffraction order wavelength

Fourier Transform Spectrometers (FTS of FTIR) Michelson interferometer Measured is the intensity of the two interfering light beams as a function of the position x of the movable mirror: I(x) is called interferogram The spectrum S( ) is the Fourier-transform of I(x) x Movable mirror Fixed mirror Source Beam splitter Detector L 1 /2 L 2 /2 I(x) FTS = Fourier Transform Spectrometer / FTIR = Fourier Transform Infra-Red Spectrometer

Monochromators and spectrometers Monochromators are single color, tunable optical band pass filters Spectrometers measure a continuous spectral range simultaneously Note: Depending on the type of detector, a prism or grating instrument can be a monochromator or a spectrometer

Principle of wavelength pairs (online - off-line) Cross secton  1 2 Note: Absorption cross section typically also dependent on x Complication: Light path dependent on Known from measurements of solar spectrum Absorber column amount along effective light path

Dobson’s spectrophotometer I Quartz plates Adjustable wedge Fixed slits Prisms Detector: photomultiplier Org. photographic plate

Dobson’s spectrophotometer II NameWL 1 [nm]WL 2 [nm] A B C D C’ Longest existing ozone time series Used wavelength pairs

Overview of satellite observations geometries Measured signal: Reflected and scattered sunlight Measured signal: Directly transmitted solar radiation Measured signal: Scattered solar radiation

Backscatter UV Ozone measurements I Solar UV radiation reflected from the surface and backscattered by atmosphere or clouds is absorbed by ozone in the Hartley-Huggins bands (< 350 nm) Note:  most ozone lies in the stratosphere  most of the backscattered UV radiation comes from the troposphere  little absorption by ozone occurs in the troposphere  little scattering occurs in the stratosphere  radiation reaching the satellite passes through the ozone layer twice Backscatter UV measurements allow retrieval of total O 3 columns and also vertical profiles, but with poor vertical resolution (7 – 10 km) Measure O 3 slant column and use Radiative transfer model to convert to vertical column

Examples: BUV (Backscatter Ultraviolet) instrument on Nimbus 4, SBUV (Solar Backscatter Ultraviolet) instrument on Nimbus 7, operated from 1978 to 1990 SBUV/2 (Solar Backscatter Ultraviolet 2) instrument on the NOAA polar orbiter satellites: NOAA-11 ( ), NOAA-14 (in orbit)can measure ozone profiles as well as columns TOMS (Total Ozone Mapping Spectrometer) first on Nimbus 7, operated from 1978 to Then three subsequent versions: Meteor 3 ( ), ADEOS (1997), Earth Probe (1996-). Measures total ozone columns. GOME (Global Ozone Monitoring Experiment) launched on ESA's ERS-2 satellite in 1995 employs a nadir-viewing BUV technique that measures radiances from 240 to 793 nm. Measures O 3 columns and profiles, as well as columns of NO 2, H 2 O, SO 2, BrO, OClO. Backscatter UV Ozone measurements II

Solar occultation measurements I I 0 ( )spectrum at the highest tangent altitude with negligible atmospheric extinction I(,z i )spectrum at tangent altitude z i within the atmosphere LoS: line of sight With α ext, being the total extinction coefficient at position s along the line of sight LoS. Extinction is usually due to Rayleigh-scattering, aerosol scattering and absorption by minor constituents:

Disadvantage of solar occultation measurements: The occultation condition has to be met: Measurements only possible during orbital sunrises/sunsets For typical Low Earth Orbits there are 14–15 orbital sunrises and sunsets per day  poor geographical coverage Solar occultation measurements II If we assume that the cross-section does not depend on x, i.e., not on temperature and/or pressure, then With the column density c(z i ) The measurement provides a set of column densities integrated along the line of sight for different tangent altitudes z i.  Inversion to get vertical O 3 profile Due to the different spectral characteristics of the different absorbers and scatterers the optical depth due to, e.g., O 3 can be extracted. Absorption cross-section O 3 Number density

Solar occultation measurements III Examples: SAGE (Stratospheric Aerosol and Gas Experiment) Series provided constinuous observations since 1984 to date Latest instrument is SAGE III on a Russian Meteor-3M spacecraft HALOE (Halogen Occultation Experiment) on UARS (Upper Atmosphere Research Satellite) operated from 1991 until end of 2005, employing IR wavelengths POAM (Polar Ozone and Aerosol Measurement) series use UV-visible solar occultation to measure profiles of ozone, H 2 O, NO 2, aerosols GOMOS (Global Ozone Monitoring by Occultation of Stars) on Envisatwill performs UV-visible occultation using stars SCIAMACHY (Scanning Imaging Absorption spectroMeter for Atmospheric CHartographY) on Envisat performs solar and lunar occultation measurements providing e.g., O 3, NO 2, and (nighttime) NO 3 profiles.

Limb scatter measurements I Radiation is detected which is scattered into the field of view of the instrument along the line of sight and also transmitted from the scattering point to the instrument Solar radiation pickts up absorption signatures along the way Also: Light path can be modified by atmospheric absorption Vertical profiles of several trace constituents can be retrieved fom limb-scattered spectra emplying a radiative transfer model (RTM) to simulate the measurements  Retrieval without forward model not possible “Knee” Optically thin regime Optically thick regime At 280 nm Modelled limb-radiance profiles

Examples: SME (Solar Mesosphere Explorer) launched in 1981, carried the first ever limb scatter satellite instruments. Mesospheric O 3 profiles were retrieved using the Ultraviolet Spectrometer and stratospheric NO 2 profiles were retrieved using the Visible Spectrometer MSX satellite – launched in 1996, carried a suite of UV/visible sensors (UVISI) SOLSE (Shuttle Ozone Limb Sounding Experiment) flown on the Space Shuttle flight in Provided good ozone profiles with high vertical resolution down to the tropopause OSIRIS (Optical Spectrograph and Infrared Imager System) launched in 2001 on Odin satellite. Retrieval of vertical profiles of O 3, NO 2, OClO, BrO SCIAMACHY (Scanning Imaging Absorption SpectroMeter for Atmospheric CHartographY), launched on Envisat in Retrieval of vertical profiles of O 3, NO2, OClO, BrO and aerosols Limb scatter measurements II

TECHNIQUE ADVANTAGES DISADVANTAGES Emission doesn’t require sunlight slightly less accurate than long time series backscatter UV simple retrieval technique long horizontal path for limb obs. provides global maps twice a day (good spatial coverage) Backscatter UV accurate requires sunlight, so can’t be long time series used at night or over winter poles good horizontal resolution poor vertical resolution below the due to nadir viewing ozone peak (~30 km) due to the effects of multiple scattering and reduced sensitivity to the profile shape Occultation simple equipment can only be made at satellite simple retrieval technique sunrise and sunset, which limits good vertical resolution number and location of meas. self-calibrating long horizontal path Limb Scattering excellent spatial coverage complex viewing geometry good vertical resolution data can be taken nearly poor horizontal resolution continuously Advantages and disadvantages of measurement techniques:

Example: Onion peel inversion of occultation observations Earth x1x1 x2x2 x3x3 x4x4 x5x5  (TH 1 )  (TH 2 )  (TH 3 )  (TH 4 )  (TH 5 ) x i : O 3 concentration at altitude z i y j : O 3 column density at tangent height TH j a 11 a 21 /2 a 22 a 32 /2 The matrix elements a ij correspond to geometrical path lengths through the layers Sun

Inverse of A exists if the determinant of A is not zero Standard approach: least squares solution (assume N=M) Minimize: by: This leads to: Unconstrained least squares solution

Constrained least squares solution Add additional condition to constrain the solution, e.g.:  is a smoothing or constraint coefficient coefficient

Differential Optical Absorption Spectroscopy (DOAS) remote sensing measurement of atmospheric trace gases in the atmosphere measurement is based on absorption spectroscopy in the UV and visible wavelength range to avoid problems with extinction by scattering or changes in the instrument throughput, only signals that vary rapidly with wavelength are analysed (thus the differential in DOAS) measurements are taken at moderate spectral resolution to identify and separate different species when using the sun or the moon as light source, very long light paths can be realised in the atmosphere which leads to very high sensitivity even longer light paths are obtained at twilight when using scattered light scattered light observations can be taken at all weather conditions without significant loss in accuracy for stratospheric measurements use of simple, automated instruments for continuous operation

Multiple light paths SZA  Offset for clarity only! In practice, many light paths through the atmosphere contribute to the measured signal. Intensity measured at the surface consist of light scattered in the atmosphere from different altitudes For each altitude, we have to consider extinction on the way from the top of the atmosphere scattering probability extinction on the way to the surface in first approximation, the observed absorption is then the absorption along the individual light paths weighted with the respective intensity.

Airmass factors The airmass factor (AMF) is the ratio of the measured slant column (SC) to the vertical column (VC) in the atmosphere: The AMF depends on a variety of parameters such as wavelength geometry vertical distribution of the species clouds aerosol loading surface albedo The basic idea is that the sensitivity of the measurement depends on many parameters but if they are known, signal and column are proportional VC SC

Airmass factors: dependence on solar zenith angle (SZA) For a stratospheric absorber, the AMF strongly increases with solar zenith angle (SZA) for ground-based, airborne and satellite measurements. Reason: increasing light path in the upper atmosphere (geometry) For an absorber close to the surface, the AMF is small, depends weakly on SZA but at large SZA rapidly decreases. Reason: light path in the lowest atmosphere is short as it is after the scattering point for zenith observation. => stratospheric sensitivity is highest at large SZA (twilight) => tropospheric sensitivity is largest at high sun (noon) => diurnal variation of slant column carries information on vertical profile

Airmass factors: dependence on absorber altitude The AMF depends on the vertical profile of the absorber. The shape of the vertical dependence depends on wavelength, viewing geometry and surface albedo. For zenith-viewing measurements, the sensitivity increases with altitude (geometry). For satellite nadir observations, the sensitivity is low close to the surface over dark surfaces (photons don’t reach the surface) but large over bright surfaces (multiple scattering). => the vertical profile must be known for the calculation of AMF

Airmass factors: dependence on wavelength the AMF depends on wavelength as Rayleigh scattering is a strong function of wavelength and also the absorption varies with wavelength at low sun, the AMF is smaller in the UV than in the visible as more light is scattered before travelling the long distance in the atmosphere. at high sun, the opposite is true as a result of multiple scattering UV measurements are more adequate for large absorption in the case of large absorptions, the nice separation of fit and radiative transfer is not valid anymore as AMF and absorption are correlated different wavelengths “see” different parts of the atmosphere which can be used for profile retrieval

DOAS equation I The intensity measured at the instrument is the extraterrestrial intensity weakened by absorption, Rayleigh scattering and Mie scattering along the light path: absorption by all trace gases j extinction by Mie scattering extinction by Rayleigh scattering unattenuated intensity integral over light path scattering efficiency exponential from Lambert Beer’s law

DOAS equation II if the absorption cross-sections do not vary along the light path, we can simplify the equation by introducing the slant column SC, which is the total amount of the absorber per unit area integrated along the light path through the atmosphere:

DOAS equation III As Rayleigh and Mie scattering efficiency vary smoothly with wavelength, they can be approximated by low order polynomials. Also, the absorption cross-sections can be separated into a high (“differential”) and a low frequency part, the later of which can also be included in the polynomial: polynomial differential cross-section slant column

DOAS equation IV Finally, the logarithm is taken and the scattering efficiency included in the polynomial. The result is a linear equation between the optical depth, a polynomial and the slant columns of the absorbers. by solving it at many wavelengths (least squares approximation), the slant columns of several absorbers can be determined simultaneously. polynomial (b p * are fitted) slant columns SC j are fitted absorption cross-sections (measured in the lab) intensity with absorption (the measurement result) intensity without or with less absorption (reference measurement)

Example of DOAS data analysis measurementoptical depth differential optical depth O3O3 H2OH2O NO 2 residual Ring

Example for satellite DOAS measurements Nitrogen dioxide (NO 2 ) and NO are key species in tropospheric ozone formation they also contribute to acid rain sources are mainly anthropogenic (combustion of fossil fuels) but biomass burning, soil emissions and lightning also contribute GOME and SCIAMACHY are satellite borne DOAS instruments observing the atmosphere in nadir data can be analysed for tropospheric NO 2 providing the first global maps of NO x pollution after 10 years of measurements, trends can also be observed GOME annual changes in tropospheric NO 2 A. Richter et al., Increase in tropospheric nitrogen dioxide over China observed from space, Nature,