MIPAS Overview

MIPAS Applications

MIPAS

MIPAS was a high-resolution Fourier Transform Infrared spectrometer which was designed to measure concentration profiles of various atmospheric constituents on a global scale. Designed as a high-resolution limb sounder, it provided detailed insights into the chemistry of the atmosphere by observing emission spectra in the near to mid-infrared. This information enhanced studies of the composition, dynamics and radiation balance of the middle atmosphere (stratosphere+mesosphere) and the upper part of the troposphere.

The atmosphere at the Earth's limb was observed by MIPAS covering a possible altitude range from 5 km to 150 km with a vertical resolution of about 3 km. MIPAS was enabled to retrieve vertical trace gas profiles of over 20 species day and night. Global coverage was obtained within 3 days. As one of the atmospheric instruments on Envisat, MIPAS complemented information obtained by SCIAMACHY, GOMOS and MERIS.

These data contributed to the development of a better understanding in the following research areas:

  • Stratospheric Chemistry: Global ozone problem, polar stratospheric chemistry
  • Global Climatology: Global distribution of climate relevant constituents
  • Atmospheric Dynamics: transport exchange between troposphere and stratosphere
  • Upper Tropospheric Chemistry: Correlation of gas distribution with human activities

Design

MIPAS flight paths

The MIPAS instrument was designed to allow the simultaneous measurement of more than 20 relevant trace gases, including the complete NOy family and several CFCs. The atmospheric temperature as well as the distribution of aerosol particles, tropospheric cirrus clouds and stratospheric ice clouds (including Polar Stratospheric Clouds) are further important parameters which were derived from MIPAS observations.

The data was obtained with complete global coverage, for all seasons and independent of illumination conditions, allowing measurement of the diurnal variation of trace species.

The atmospheric emissions were measured at the horizon of the Earth (limb) over a height range of 5 to 150 km. This observation geometry allowed the maximum measurement sensitivity and a good profiling capability to be achieved.

The MIPAS data products are calibrated high-resolution spectra which were derived on ground from the transmitted interferograms. From these spectra, geophysical parameters such as trace gas concentrations, temperature profiles, mixing ratios, were retrieved, enabling the creation of global maps of atmospheric constituents in geophysical coordinates.

MIPAS performed measurements in either of two pointing regimes: rearwards within a 35° wide viewing range in the anti-flight direction and sideways within a 30° wide range on the anti-sun side. The rearward viewing range was used for most measurements, since it provided a good Earth coverage including the polar regions.

The sideways range was important for observations of special events, like volcano eruptions, trace gas concentrations above major traffic routes or concentration gradients across the dawn/dusk border. In nominal measurement mode, MIPAS performed some series of measurements at different tangent heights by performing elevation scan sequences with a duration of 75 seconds in the rearward viewing range. Such an elevation scan sequence comprised typically 16 interferometers sweeps.

MIPAS functional block diagram

For special event observations, viewing elevation scans sequences in the sideways range were commanded. Radiometric calibration was performed using two measurements:

  • gain calibration approximately once per week, applying a two-point calibration method, where radiances from deep space and an internal blackbody were recorded in sequence
  • offset calibration, prior to every elevation scan sequence, in order to correct for the instrument self-emission

Another calibration was required for the inflight determination of the line of-sight pointing direction, which was based on the observation of stars crossing the instrument field of view and subsequent correlation of the actual with the predicted time of star crossing.

The MIPAS blockdiagram depicted the functional elements and their relationship. The radiation emitted from the observed scene entered MIPAS through the Front-End Optics comprising an azimuth scan mirror, an elevation scan mirror and a telescope. The radiation propagated through a dual slide, dual port Michelson-type interferometer, which was designed to provide an unapodized spectral resolution of better than 0.035 cm-1 throughout the observed spectral range.

The input signals were divided at the beamsplitter inside the interferometer and directed to cube corners moving at a constant velocity of 25 mm/s along a path of 100 mm. Hence one spectrum was typically recorded within 4 seconds. From the cube corners the IR beam is reflected to the beam recombiner and then directed to the output ports.

Depending on the optical path difference in the two interferometer arms, the recombined signal was an intensity modulated interferogram. The optical path difference signal for the interferogram sampling was derived from a reference laser the interferogram. The output signal entered the Focal Plane Subsystem where beam size matching, beam splitting and optical filtering was performed.

After optical filtering the input spectrum was separated into eight narrow spectral bands for detection by eight Hg:Cd:Te-detectors operating at about 70K.

After pre-amplification, the eight signals were amplified, lowpass filtered and digitized by the analogue processing part of the Signal Processing Electronics. Its digital part separated the spectral range of interest by complex filtering, under sampled the input sequences individually and equalized channels combined.

Word length truncation was then performed to reduce the data rate for downlink budget reasons. In a final processing step, measurement data was multiplexed and formatted to source packets. On ground, the incoming source packets were sorted according to measurement/calibration data and the interferograms are converted into calibrated spectra.

 

Technical Characteristics

  • Accuracy: Radiometric precision: 685-970 cm-1: 1%, 2410 cm-1: 3%
  • Spatial Resolution: Vertical resolution: 3 km, vertical scan range 5 km -150 km, Horizontal: 3 km x 30 km, Spectral resolution: 0.035 lines/cm 
  • Swath Width: 3 km x 30 km 
  • Waveband: MWIR-TIR: between 4.15 and 14.6µm 

Sensor Modes

The MIPAS acquisition baseline was defined by a Science Team in the MIPAS Mission Plan Rationale, and was regularly revised during the mission in order to adapt the measuring scenario to scientific requirements, such as special operations in support to calibration/validation campaigns or special events. Different measurements modes were thus implemented.

In addition, the Interferometer Drive Unit major anomaly in 2004, required the acquisition scenarios and the mission target itself to be modified. Download the MIPAS Mission Plan document for more information.

Observation modes during Full Resolution (FR) mission
Download the full details of each of the FR modes
ID Description
NOM Stratospheric chemistry and dynamics – Applications in climatology – Applications in medium range forecasts
S1 Polar chemistry and dynamics
S2 Tropospheric / stratospheric exchange processes – Tropospheric chemistry
S3 Impact of aircraft emissions
S4 Stratospheric dynamics – Transport processes
S5 Diurnal changes
S6 Upper troposphere / lower stratosphere
UA1 Validation (confirmation of predicted non-LTE effects on the retrieval of p-T and target species)
UA2 Upper polar vortex dynamics – Stratosphere-mesosphere exchange and dynamics
UA3 Radiative energy budget of the mesosphere and lower thermosphere – Hydrogen, nitrogen and carbon budgets in the upper atmosphere – mesospheric dynamic – Non-LTE studies
UA4 Non-LTE studies of NO – Radiative cooling of the thermosphere

 

Observation modes during Optimised Resolution (OR) mission
Download the full details of each of the OR modes
ID Description
NOM Nominal mode using floating altitudes
UTLS-1 Upper Troposphere Lower Stratosphere
UTLS-2 Upper Troposphere Lower Stratosphere (for 2-D retrievals)
MA Middle Atmosphere
NLC Middle/Upper Atmosphere – Noctilucent Clouds
UA Upper Atmosphere
AE Aircraft Emissions - sideways observation mode
UA1 Validation (confirmation of predicted non-LTE effects on the retrieval of p-T and target species)

Mission Planning

Mission Operations

The MIPAS instrument was operational for ten years, from 1 March 2002 until 8 April 2012. In 2004, it suffered a major anomaly affecting the Interferometer Drive Unit (IDU), which had a serious impact on performance. To avoid problems, ESA took the decision to interrupt MIPAS regular operations on 26 March 2004. Different tests with different slide configurations, and spectral resolutions were carried out to identify the source of the trouble and to try to recover and restore MIPAS to full operational capacity. Despite such a serious problem, ESA succeeded in recovering the instrument in January 2005, after only a few months of tests.

MIPAS was operated at 100% from July 2002 to March 2004. Due to the instrument anomaly, it was operated at a reduced capacity (about 30% at the beginning of 2005 and progressively increased) until December 2007, when it was successfully recovered back to 100%, three and a half years since the first failure. The reduced operational capacity had a direct consequence on the overall number of acquisitions acquired by MIPAS in the different periods. The acquisition scenarios had to be modified and the instrument was completely re-characterised.

Different phases can be therefore identified for the MIPAS mission, characterised by a different spectral resolution and a different limb scanning pattern with different vertical and horizontal sampling:

  • Commissioning Phase: 1 March – July 2002: Envisat launch, SODAP and MIPAS cal/val phase
     
  • Full Resolution (FR) phase: 1 July 2002 – 26 March 2004: MIPAS original measurement mode acquiring full spectral resolution measurements (0.025 cm-1). During this phase, MIPAS measurements were mainly acquired in Nominal Mode with 17 sweeps per scan; only a few orbits were commanded in the Special observation Mode and in the Upper Atmosphere observational scenario for scientific purposes.
     
  • Mission suspended: 26 March 2004 – 9 August 2004
     
  • Reduced Resolution (RR) phase: 9 August 2004 – 17 September 2004: MIPAS was tested for acquiring 41% reduced spectral resolution measurements (0.0625 cm-1) and asymmetric transitory sweeps (3.3 mm asymmetry). For this phase, Nominal Mode operations had 17 sweeps per scan.
     
  • Mission suspended: 17 September 2004 – 10 January 2005
     
  • Optimised Resolution (OR) phase: 10 January 2005 – 21 October 2010: MIPAS was operated in double slides configuration for acquiring 41% reduced spectral resolution measurements (0.0625 cm-1) and asymmetric transitory sweeps (3.3 mm asymmetry). Operations were based on an "event driven scenario" with priority to validation campaigns and special observations. The instrument duty cycle increased from 30% up to 100% i.e. continuous operations since 1 December 2007. During this phase, beside the most frequent Nominal Mode, several measurements have been acquired in UTLS-1 (Upper Troposphere-Lower Stratosphere), MA (Middle Atmosphere) and UA (Upper Atmosphere) modes. The new Nominal Mode had 27 sweeps per scan. The other observation modes were updated for the new instrument configuration and optimised with regards to vertical and horizontal spacing.
     
  • Envisat extended mission: 21 October 2010 – 8 April 2012: MIPAS was still operated in Optimized Resolution (OR) but the Envisat platform was moved to a lower altitude with a drifting orbit. 

Download the list of events affecting the MIPAS mission during the Envisat lifetime.

MIPAS Resources