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Trace Gas Orbiter

April 24, 2023

The ExoMars Trace Gas Orbiter (TGO or ExoMars Orbiter) is a collaborative project between the European Space Agency (ESA) and the Russian Roscosmos agency that sent an atmospheric research orbiter and the Schiaparelli demonstration lander to Mars in 2016 as part of the European-led ExoMars programme.[7][8][9]

Trace Gas Orbiter
Artist's illustration of ExoMars 2016
Mission typeMars orbiter
OperatorESA · Roscosmos
COSPAR ID2016-017A
SATCAT no.41388
Websitehttp://exploration.esa.int/jump.cfm?oid=46475
Mission durationPlanned: 7 years[1][2]
Elapsed: 7 years, 1 month, 7 days
Spacecraft properties
ManufacturerThales Alenia Space
Launch mass4,332 kg[3]
Payload massInstruments: 113.8 kg (251 lb)[4]
Schiaparelli: 577 kg (1,272 lb)[4]
Dimensions3.2 × 2 × 2 m (10.5 × 6.6 × 6.6 ft)[4]
Power~2000 W[4]
Start of mission
Launch date14 March 2016, 09:31 (2016-03-14UTC09:31) UTC[5]
RocketProton-M/Briz-M
Launch siteBaikonur 200/39
ContractorKhrunichev
Orbital parameters
Reference systemAreocentric
RegimeCircular
Eccentricity0
Periareion altitude400 km (250 mi)
Apoareion altitude400 km (250 mi)
Inclination74 degrees
Period2 hours
EpochPlanned
Mars orbiter
Orbital insertion19 October 2016, 15:24 UTC[6]
Transponders
BandX band
UHF band
Frequency390–450 MHz
TWTA power65 W
Instruments
NOMADNadir and Occultation for Mars Discovery
ACSAtmospheric Chemistry Suite
CaSSISColour and Stereo Surface Imaging System
FRENDFine-Resolution Epithermal Neutron Detector

ESA mission insignia for the ExoMars 2016 launch, featuring the Trace Gas Orbiter (left) and Schiaparelli (right).
ExoMars programme
 

The Trace Gas Orbiter delivered the Schiaparelli lander on 16 October 2016, which crashed on the surface due to a premature release of the parachute.[10]

The orbiter began aerobraking in March 2017 to lower its initial orbit of 200 by 98,000 km (120 by 60,890 mi). Aerobraking concluded on 20 February 2018 when a final thruster firing resulted in an orbit of 200 by 1,050 km (120 by 650 mi).[11] Additional thruster firings every few days raised the orbiter to a circular "science" orbit of 400 km (250 mi), which was achieved on 9 April 2018.[12]

A key goal is to gain a better understanding of methane (CH4) and other trace gases present in the Martian atmosphere that could be evidence for possible biological activity. The programme will follow with the Kazachok lander and the Rosalind Franklin rover in 2022,[13][14] which will search for biomolecules and biosignatures; the TGO will operate as the communication link for the ExoMars lander and rover and provide communication for other Mars surface probes with Earth.

History

Investigations with space and Earth-based observatories have demonstrated the presence of a small amount of methane on the atmosphere of Mars that seems to vary with location and time.[15][16][17] This may indicate the presence of microbial life on Mars, or a geochemical process such as volcanism or hydrothermal activity.[18][19][20][21]

The challenge to discern the source of methane in the atmosphere of Mars prompted the independent planning by ESA and NASA of one orbiter each that would carry instruments in order to determine if its formation is of biological or geological origin,[22][23] as well as its decomposition products such as formaldehyde and methanol.

Origins

ExoMars Trace Gas Orbiter was born out of the nexus of ESA's Aurora programme ExoMars flagship and NASA's 2013 and 2016 Mars Science Orbiter (MSO) concepts.[24][25] It became a flexible collaborative proposal within NASA and ESA to send a new orbiter-carrier to Mars in 2016 as part of the European-led ExoMars mission.[9] On the ExoMars side, ESA authorised about half a billion Euros in 2005 for a rover and mini-station; eventually this evolved into being delivered by an orbiter rather than a cruise stage.[26]

Attempted collaboration with NASA

NASA's Mars Science Orbiter (MSO) was originally envisioned in 2008 as an all-NASA endeavour aiming for a late 2013 launch.[24][25] NASA and ESA officials agreed to pool resources and technical expertise and collaborate to launch only one orbiter.[27] The agreement, called the Mars Exploration Joint Initiative, was signed in July 2009 and proposed to use an Atlas rocket launcher instead of a Soyuz rocket, which significantly altered the technical and financial setting of the European ExoMars mission. Since the rover was originally planned to be launched along with the TGO, a prospective agreement would require that the rover lose enough weight to fit aboard the Atlas launch vehicle with NASA's orbiter.[28] Instead of reducing the rover's mass, it was nearly doubled when the mission was combined with other projects to a multi-spacecraft programme divided over two Atlas V launches:[27][29] the ExoMars Trace Gas Orbiter (TGO) was merged into the project, carrying a meteorological lander planned for launch in 2016. The European orbiter would carry several instruments originally meant for NASA's MSO, so NASA scaled down the objectives and focused on atmospheric trace gases detection instruments for their incorporation in ESA's ExoMars Trace Gas Orbiter.[4][9][25]

Under the FY2013 budget President Barack Obama released on 13 February 2012, NASA terminated its participation in ExoMars due to budgetary cuts in order to pay for the cost overruns of the James Webb Space Telescope.[30] With NASA's funding for this project cancelled, most of ExoMars' plans had to be restructured.[31]

Collaboration with Russia

On 15 March 2012, the ESA's ruling council announced it would press ahead with its ExoMars program in partnership with the Russian space agency Roscosmos, which planned to contribute two heavy-lift Proton launch vehicles and an additional entry, descent and landing system to the 2020 rover mission.[32][33][34][35][36]

Under the collaboration proposal with Roscosmos, the ExoMars mission was split into two parts: the orbiter/lander mission in March 2016 that includes the TGO and a 2.4 m (7 ft 10 in) diameter stationary lander built by ESA named Schiaparelli,[37] and the Rosalind Franklin rover mission in 2020[13] (postponed to 2022 [38]). Both missions are using a Proton-M rocket.

Launch

 
Launch of the Proton carrier rocket
 
Animation of ExoMars Trace Gas Orbiter's trajectory
   Sun ·    Earth ·    Mars ·    ExoMars Trace Gas Orbiter
 
Animation of ExoMars Trace Gas Orbiter's trajectory around Mars
   Mars ·    ExoMars Trace Gas Orbiter

The Trace Gas Orbiter and descent module Schiaparelli completed testing and were integrated to a Proton rocket at the Baikonur Cosmodrome in Kazakhstan in mid-January 2016.[39] The launch occurred at 09:31 UTC on 14 March 2016.[5] Four rocket burns occurred in the following 10 hours before the descent module and orbiter were released.[40] A signal from the spacecraft was received at 21:29 UTC that day, confirming that the launch was successful and the spacecraft were functioning properly.[41]

Shortly after separation from the probes, a Brazilian ground telescope recorded small objects in the vicinity of the Briz-M upper booster stage, suggesting that the Briz-M stage exploded a few kilometres away, without damaging the orbiter or lander.[42] Briefing reporters in Moscow, the head of Roscosmos denied any anomaly and made all launch data available for inspection.[43]

Status

The Schiaparelli lander separated from the TGO orbiter on 16 October 2016,[44] three days before it arrived on Mars, and entered the atmosphere at 21,000 km/h (13,000 mph; 5.8 km/s).[45] Schiaparelli transmitted about 600 megabytes of telemetry during its landing attempt,[46][47] before it impacted the surface at 540 km/h (340 mph).[48]

The TGO was injected into Mars orbit on 19 October 2016 and underwent 11 months of aerobraking (March 2017 to February 2018), reducing its orbital speed by 3,600 km/h (2,200 mph) and its orbit from an initial 98,000 by 200 km (60,890 by 120 mi) down to 1,050 by 200 km (650 by 120 mi). Additional thruster firings through mid-April circularised the spacecraft's orbit to 400 km (250 mi), and full science activities began on 21 April 2018.[49][50]

Specifications

 
Size of the Trace Gas Orbiter (left) with the Schiaparelli EDM attached, compared to Mars Express (right) and an average human
Dimensions
The central bus is 3.2 m × 2 m × 2 m (10.5 ft × 6.6 ft × 6.6 ft)[4]
Propulsion
424 N (95 lbf) bi-propellant main engine, used for Mars orbit insertion and manoeuvres[4]
Power
20 m2 (220 sq ft) solar arrays spanning 17.5 m (57 ft) tip-to-tip, and capable of rotating in one axis;[51] generates about 2,000 W of power at Mars[4]
Batteries
2 modules of lithium-ion batteries with approximately 5100 watt hours total capacity to provide power during eclipses over the prime mission[4]
Communication
2.2 m (7 ft 3 in) X band high-gain antenna with a two-axis pointing mechanism and 65 W RF travelling-wave tube amplifier to communicate with Earth[4]
Two Electra UHF band transceivers with a single helical antenna to communicate with spacecraft at Mars[4]
Thermal control
Spacecraft yaw axis control to ensure the three faces containing the science payload remain cold
Mass
3,755 kg (8,278 lb), wet mass of the orbiter[4]
4,332 kg (9,550 lb), wet mass of the orbiter plus Schiaparelli lander[4]
Payload
113.8 kg (251 lb) of science instruments[4]

Science

 
Scale model of the ExoMars Trace Gas Orbiter displayed during the Paris Air Show, 2015

The TGO separated from the ExoMars Schiaparelli demonstration lander and would have provided it with telecommunication relay for 8 Martian solar days (sols) after landing. Then the TGO gradually underwent aerobraking for seven months into a more circular orbit for science observations and will provide communications relay for the Rosalind Franklin rover to be launched in 2022, and will continue serving as a relay satellite for future landed missions.[2]

The FREND instrument is currently mapping hydrogen levels to a maximum depth of 1 m (3 ft 3 in) beneath the Martian surface.[52][53] Locations where hydrogen is found may indicate water-ice deposits, which could be useful for future crewed missions.

Particularly, the mission is in the process of characterising spatial, temporal variation, and localisation of sources for a broad list of atmospheric trace gases. If methane (CH4) is found in the presence of propane (C3H8) or ethane (C2H6), that would be a strong indication that biological processes are involved.[54] However, if methane is found in the presence of gases such as sulfur dioxide (SO2), that would be an indication that the methane is a byproduct of geological processes.[55]

Detection
 
Visualisation of a methane plume found in Mars' atmosphere during the northern summer season

The nature of the methane source requires measurements of a suite of trace gases in order to characterise potential biochemical and geochemical processes at work. The orbiter has very high sensitivity to (at least) the following molecules and their isotopomers: water (H2O), hydroperoxyl (HO2), nitrogen dioxide (NO2), nitrous oxide (N2O), methane (CH4), acetylene (C2H2), ethylene (C2H4), ethane (C2H6), formaldehyde (H2CO), hydrogen cyanide (HCN), hydrogen sulfide (H2S), carbonyl sulfide (OCS), sulfur dioxide (SO2), hydrogen chloride (HCl), carbon monoxide (CO) and ozone (O3). Detection sensitivities are at levels of 100 parts per trillion, improved to 10 parts per trillion or better by averaging spectra which could be taken at several spectra per second.[56]

Characterisation
  • Spatial and temporal variability: latitude–longitude coverage multiple times in a Mars year to determine regional sources and seasonal variations (reported to be large, but still controversial with present understanding of Mars gas-phase photochemistry)
  • Correlation of concentration observations with environmental parameters of temperature, dust and ice aerosols (potential sites for heterogeneous chemistry)[4]
Localisation
  • Mapping of multiple tracers (e.g., aerosols, water vapour, CO, CH4) with different photochemical lifetimes and correlations helps constrain model simulations and points to source/sink regions
  • To achieve the spatial resolution required to localise sources might require tracing molecules at parts-per-billion concentrations

Instruments

 
Colour and Stereo Surface Imaging System (CaSSIS)

Like the Mars Reconnaissance Orbiter, the Trace Gas Orbiter is a hybrid science and telecom orbiter.[57] Its scientific payload mass is about 113.8 kg (251 lb) and consists of:[4][58]

NOMAD and ACS are providing the most extensive spectral coverage of Martian atmospheric processes so far.[57][62] Twice per orbit, at local sunrise and sunset, they are able to observe the Sun as it shines through the atmosphere. Detection of atmospheric trace species at the parts-per-billion (ppb) level are possible.
  • The Colour and Stereo Surface Imaging System (CaSSIS) is a high-resolution, 4.5 m per pixel (15 ft/pixel), colour stereo camera for building accurate digital elevation models of the Martian surface. It will also be an important tool for characterising candidate landing site locations for future missions. Developed by Switzerland.
  • The Fine-Resolution Epithermal Neutron Detector (FREND) is a neutron detector that can provide information on the presence of hydrogen, in the form of water or hydrated minerals, in the top 1 m (3 ft 3 in) of the Martian surface.[61] Developed by Russia.

Relay telecommunications

 
An Electra radio, in this case the one for the MAVEN probe. Electra radios were also deployed on the Trace Gas Orbiter and on other Mars telecommunications assets.

Due to the challenges of entry, descent and landing, Mars landers are highly constrained in mass, volume and power. For landed missions, this places severe constraints on antenna size and transmission power, which in turn greatly reduce direct-to-Earth communication capability in comparison to orbital spacecraft. As an example, the capability downlinks on Spirit and Opportunity rovers had only 1⁄600 the capability of the Mars Reconnaissance Orbiter downlink. Relay communication addresses this problem by allowing Mars surface spacecraft to communicate using higher data rates over short-range links to nearby Mars orbiters, while the orbiter takes on the task of communicating over the long-distance link back to Earth. This relay strategy offers a variety of key benefits to Mars landers: increased data return volume, reduced energy requirements, reduced communications system mass, increased communications opportunities, robust critical event communications and in situ navigation aid.[63] NASA provided an Electra telecommunications relay and navigation instrument to assure communications between probes and rovers on the surface of Mars and controllers on Earth.[64] The TGO will provide the 2022 Rosalind Franklin rover with telecommunications relay; it will also serve as a relay satellite for future landed missions.[2]

Results

 
Image of the edge of Planum Australe, Mars' south polar ice cap, taken by CaSSIS. The dusty ice layers that compose the South Polar Layered Deposits (SPLD) are exposed and visible in the image.

The spacecraft took its first photos of the surface of Mars on 15 April 2018.[65] The first year of science operations[66] yielded a wealth of new data and scientific discoveries, including: new observations of the atmospheric composition and structure,[67][68] water-ice cloud enhancement during a global dust storm,[69] new measurements of the atmospheric thermal structure and density,[70] estimations of the timespan of the climate record of the south polar ice sheet,[71] confirmation of dry-processes being responsible for Recurring Slope Lineae in Gale crater,[72] and high-resolution maps of shallow subsurface Hydrogen, increasing the known amounts of probably near-surface buried water ice.[73]

In April 2019, the science team reported their first methane results: TGO had detected no methane whatsoever, even though their data were more sensitive than the methane concentrations found using Curiosity, Mars Express, and ground-based observations.[74][75]

See also

References

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  75. ^ Trokhimovskiy, A.; Perevalov, V.; Korablev, O.; Fedorova, A. A.; Olsen, K. S.; Bertaux, J.-L.; Patrakeev, A.; Shakun, A.; Montmessin, F.; Lefèvre, F.; Lukashevskaya, A. (2020). "First observation of the magnetic dipole CO2absorption band at 3.3μm in the atmosphere of Mars by the Exo Mars Trace Gas Orbiter ACS instrument". Astronomy & Astrophysics. 639: A142. Bibcode:2020A&A...639A.142T. doi:10.1051/0004-6361/202038134. S2CID 225600219.

External links

  • ExoMars Trace Gas Orbiter at ESA.int
  • ESA ExoMars on Flickr

April 24, 2023
trace, orbiter, this, article, needs, updated, please, help, update, this, article, reflect, recent, events, newly, available, information, march, 2020, exomars, exomars, orbiter, collaborative, project, between, european, space, agency, russian, roscosmos, ag. This article needs to be updated Please help update this article to reflect recent events or newly available information March 2020 The ExoMars Trace Gas Orbiter TGO or ExoMars Orbiter is a collaborative project between the European Space Agency ESA and the Russian Roscosmos agency that sent an atmospheric research orbiter and the Schiaparelli demonstration lander to Mars in 2016 as part of the European led ExoMars programme 7 8 9 Trace Gas OrbiterArtist s illustration of ExoMars 2016Mission typeMars orbiterOperatorESA RoscosmosCOSPAR ID2016 017ASATCAT no 41388Websitehttp exploration esa int jump cfm oid 46475Mission durationPlanned 7 years 1 2 Elapsed 7 years 1 month 7 daysSpacecraft propertiesManufacturerThales Alenia SpaceLaunch mass4 332 kg 3 Payload massInstruments 113 8 kg 251 lb 4 Schiaparelli 577 kg 1 272 lb 4 Dimensions3 2 2 2 m 10 5 6 6 6 6 ft 4 Power 2000 W 4 Start of missionLaunch date14 March 2016 09 31 2016 03 14UTC09 31 UTC 5 RocketProton M Briz MLaunch siteBaikonur 200 39ContractorKhrunichevOrbital parametersReference systemAreocentricRegimeCircularEccentricity0Periareion altitude400 km 250 mi Apoareion altitude400 km 250 mi Inclination74 degreesPeriod2 hoursEpochPlannedMars orbiterOrbital insertion19 October 2016 15 24 UTC 6 TranspondersBandX bandUHF bandFrequency390 450 MHzTWTA power65 WInstrumentsNOMADNadir and Occultation for Mars DiscoveryACSAtmospheric Chemistry SuiteCaSSISColour and Stereo Surface Imaging SystemFRENDFine Resolution Epithermal Neutron DetectorESA mission insignia for the ExoMars 2016 launch featuring the Trace Gas Orbiter left and Schiaparelli right ExoMars programmeRosalind Franklin rover and Kazachok lander The Trace Gas Orbiter delivered the Schiaparelli lander on 16 October 2016 which crashed on the surface due to a premature release of the parachute 10 The orbiter began aerobraking in March 2017 to lower its initial orbit of 200 by 98 000 km 120 by 60 890 mi Aerobraking concluded on 20 February 2018 when a final thruster firing resulted in an orbit of 200 by 1 050 km 120 by 650 mi 11 Additional thruster firings every few days raised the orbiter to a circular science orbit of 400 km 250 mi which was achieved on 9 April 2018 12 A key goal is to gain a better understanding of methane CH4 and other trace gases present in the Martian atmosphere that could be evidence for possible biological activity The programme will follow with the Kazachok lander and the Rosalind Franklin rover in 2022 13 14 which will search for biomolecules and biosignatures the TGO will operate as the communication link for the ExoMars lander and rover and provide communication for other Mars surface probes with Earth Contents 1 History 1 1 Origins 1 2 Attempted collaboration with NASA 1 3 Collaboration with Russia 1 4 Launch 1 5 Status 2 Specifications 3 Science 4 Instruments 4 1 Relay telecommunications 5 Results 6 See also 7 References 8 External linksHistory EditInvestigations with space and Earth based observatories have demonstrated the presence of a small amount of methane on the atmosphere of Mars that seems to vary with location and time 15 16 17 This may indicate the presence of microbial life on Mars or a geochemical process such as volcanism or hydrothermal activity 18 19 20 21 The challenge to discern the source of methane in the atmosphere of Mars prompted the independent planning by ESA and NASA of one orbiter each that would carry instruments in order to determine if its formation is of biological or geological origin 22 23 as well as its decomposition products such as formaldehyde and methanol Origins Edit ExoMars Trace Gas Orbiter was born out of the nexus of ESA s Aurora programme ExoMars flagship and NASA s 2013 and 2016 Mars Science Orbiter MSO concepts 24 25 It became a flexible collaborative proposal within NASA and ESA to send a new orbiter carrier to Mars in 2016 as part of the European led ExoMars mission 9 On the ExoMars side ESA authorised about half a billion Euros in 2005 for a rover and mini station eventually this evolved into being delivered by an orbiter rather than a cruise stage 26 Attempted collaboration with NASA Edit NASA s Mars Science Orbiter MSO was originally envisioned in 2008 as an all NASA endeavour aiming for a late 2013 launch 24 25 NASA and ESA officials agreed to pool resources and technical expertise and collaborate to launch only one orbiter 27 The agreement called the Mars Exploration Joint Initiative was signed in July 2009 and proposed to use an Atlas rocket launcher instead of a Soyuz rocket which significantly altered the technical and financial setting of the European ExoMars mission Since the rover was originally planned to be launched along with the TGO a prospective agreement would require that the rover lose enough weight to fit aboard the Atlas launch vehicle with NASA s orbiter 28 Instead of reducing the rover s mass it was nearly doubled when the mission was combined with other projects to a multi spacecraft programme divided over two Atlas V launches 27 29 the ExoMars Trace Gas Orbiter TGO was merged into the project carrying a meteorological lander planned for launch in 2016 The European orbiter would carry several instruments originally meant for NASA s MSO so NASA scaled down the objectives and focused on atmospheric trace gases detection instruments for their incorporation in ESA s ExoMars Trace Gas Orbiter 4 9 25 Under the FY2013 budget President Barack Obama released on 13 February 2012 NASA terminated its participation in ExoMars due to budgetary cuts in order to pay for the cost overruns of the James Webb Space Telescope 30 With NASA s funding for this project cancelled most of ExoMars plans had to be restructured 31 Collaboration with Russia Edit On 15 March 2012 the ESA s ruling council announced it would press ahead with its ExoMars program in partnership with the Russian space agency Roscosmos which planned to contribute two heavy lift Proton launch vehicles and an additional entry descent and landing system to the 2020 rover mission 32 33 34 35 36 Under the collaboration proposal with Roscosmos the ExoMars mission was split into two parts the orbiter lander mission in March 2016 that includes the TGO and a 2 4 m 7 ft 10 in diameter stationary lander built by ESA named Schiaparelli 37 and the Rosalind Franklin rover mission in 2020 13 postponed to 2022 38 Both missions are using a Proton M rocket Launch Edit Launch of the Proton carrier rocket Animation of ExoMars Trace Gas Orbiter s trajectory Sun Earth Mars ExoMars Trace Gas Orbiter Animation of ExoMars Trace Gas Orbiter s trajectory around Mars Mars ExoMars Trace Gas Orbiter The Trace Gas Orbiter and descent module Schiaparelli completed testing and were integrated to a Proton rocket at the Baikonur Cosmodrome in Kazakhstan in mid January 2016 39 The launch occurred at 09 31 UTC on 14 March 2016 5 Four rocket burns occurred in the following 10 hours before the descent module and orbiter were released 40 A signal from the spacecraft was received at 21 29 UTC that day confirming that the launch was successful and the spacecraft were functioning properly 41 Shortly after separation from the probes a Brazilian ground telescope recorded small objects in the vicinity of the Briz M upper booster stage suggesting that the Briz M stage exploded a few kilometres away without damaging the orbiter or lander 42 Briefing reporters in Moscow the head of Roscosmos denied any anomaly and made all launch data available for inspection 43 Status Edit The Schiaparelli lander separated from the TGO orbiter on 16 October 2016 44 three days before it arrived on Mars and entered the atmosphere at 21 000 km h 13 000 mph 5 8 km s 45 Schiaparelli transmitted about 600 megabytes of telemetry during its landing attempt 46 47 before it impacted the surface at 540 km h 340 mph 48 The TGO was injected into Mars orbit on 19 October 2016 and underwent 11 months of aerobraking March 2017 to February 2018 reducing its orbital speed by 3 600 km h 2 200 mph and its orbit from an initial 98 000 by 200 km 60 890 by 120 mi down to 1 050 by 200 km 650 by 120 mi Additional thruster firings through mid April circularised the spacecraft s orbit to 400 km 250 mi and full science activities began on 21 April 2018 49 50 Specifications Edit Size of the Trace Gas Orbiter left with the Schiaparelli EDM attached compared to Mars Express right and an average human Dimensions The central bus is 3 2 m 2 m 2 m 10 5 ft 6 6 ft 6 6 ft 4 Propulsion 424 N 95 lbf bi propellant main engine used for Mars orbit insertion and manoeuvres 4 Power 20 m2 220 sq ft solar arrays spanning 17 5 m 57 ft tip to tip and capable of rotating in one axis 51 generates about 2 000 W of power at Mars 4 Batteries 2 modules of lithium ion batteries with approximately 5100 watt hours total capacity to provide power during eclipses over the prime mission 4 Communication 2 2 m 7 ft 3 in X band high gain antenna with a two axis pointing mechanism and 65 W RF travelling wave tube amplifier to communicate with Earth 4 Two Electra UHF band transceivers with a single helical antenna to communicate with spacecraft at Mars 4 Thermal control Spacecraft yaw axis control to ensure the three faces containing the science payload remain cold Mass 3 755 kg 8 278 lb wet mass of the orbiter 4 4 332 kg 9 550 lb wet mass of the orbiter plus Schiaparelli lander 4 Payload 113 8 kg 251 lb of science instruments 4 Science Edit Scale model of the ExoMars Trace Gas Orbiter displayed during the Paris Air Show 2015 The TGO separated from the ExoMars Schiaparelli demonstration lander and would have provided it with telecommunication relay for 8 Martian solar days sols after landing Then the TGO gradually underwent aerobraking for seven months into a more circular orbit for science observations and will provide communications relay for the Rosalind Franklin rover to be launched in 2022 and will continue serving as a relay satellite for future landed missions 2 The FREND instrument is currently mapping hydrogen levels to a maximum depth of 1 m 3 ft 3 in beneath the Martian surface 52 53 Locations where hydrogen is found may indicate water ice deposits which could be useful for future crewed missions Particularly the mission is in the process of characterising spatial temporal variation and localisation of sources for a broad list of atmospheric trace gases If methane CH4 is found in the presence of propane C3H8 or ethane C2H6 that would be a strong indication that biological processes are involved 54 However if methane is found in the presence of gases such as sulfur dioxide SO2 that would be an indication that the methane is a byproduct of geological processes 55 Detection Visualisation of a methane plume found in Mars atmosphere during the northern summer season The nature of the methane source requires measurements of a suite of trace gases in order to characterise potential biochemical and geochemical processes at work The orbiter has very high sensitivity to at least the following molecules and their isotopomers water H2O hydroperoxyl HO2 nitrogen dioxide NO2 nitrous oxide N2O methane CH4 acetylene C2H2 ethylene C2H4 ethane C2H6 formaldehyde H2CO hydrogen cyanide HCN hydrogen sulfide H2S carbonyl sulfide OCS sulfur dioxide SO2 hydrogen chloride HCl carbon monoxide CO and ozone O3 Detection sensitivities are at levels of 100 parts per trillion improved to 10 parts per trillion or better by averaging spectra which could be taken at several spectra per second 56 CharacterisationSpatial and temporal variability latitude longitude coverage multiple times in a Mars year to determine regional sources and seasonal variations reported to be large but still controversial with present understanding of Mars gas phase photochemistry Correlation of concentration observations with environmental parameters of temperature dust and ice aerosols potential sites for heterogeneous chemistry 4 LocalisationMapping of multiple tracers e g aerosols water vapour CO CH4 with different photochemical lifetimes and correlations helps constrain model simulations and points to source sink regions To achieve the spatial resolution required to localise sources might require tracing molecules at parts per billion concentrationsInstruments Edit Colour and Stereo Surface Imaging System CaSSIS Like the Mars Reconnaissance Orbiter the Trace Gas Orbiter is a hybrid science and telecom orbiter 57 Its scientific payload mass is about 113 8 kg 251 lb and consists of 4 58 The Nadir and Occultation for Mars Discovery NOMAD has two infrared and one ultraviolet spectrometer channels 59 Developed by Belgium The Atmospheric Chemistry Suite ACS has three infrared spectrometer channels 60 61 Developed by Russia NOMAD and ACS are providing the most extensive spectral coverage of Martian atmospheric processes so far 57 62 Twice per orbit at local sunrise and sunset they are able to observe the Sun as it shines through the atmosphere Detection of atmospheric trace species at the parts per billion ppb level are possible The Colour and Stereo Surface Imaging System CaSSIS is a high resolution 4 5 m per pixel 15 ft pixel colour stereo camera for building accurate digital elevation models of the Martian surface It will also be an important tool for characterising candidate landing site locations for future missions Developed by Switzerland The Fine Resolution Epithermal Neutron Detector FREND is a neutron detector that can provide information on the presence of hydrogen in the form of water or hydrated minerals in the top 1 m 3 ft 3 in of the Martian surface 61 Developed by Russia Relay telecommunications Edit An Electra radio in this case the one for the MAVEN probe Electra radios were also deployed on the Trace Gas Orbiter and on other Mars telecommunications assets Due to the challenges of entry descent and landing Mars landers are highly constrained in mass volume and power For landed missions this places severe constraints on antenna size and transmission power which in turn greatly reduce direct to Earth communication capability in comparison to orbital spacecraft As an example the capability downlinks on Spirit and Opportunity rovers had only 1 600 the capability of the Mars Reconnaissance Orbiter downlink Relay communication addresses this problem by allowing Mars surface spacecraft to communicate using higher data rates over short range links to nearby Mars orbiters while the orbiter takes on the task of communicating over the long distance link back to Earth This relay strategy offers a variety of key benefits to Mars landers increased data return volume reduced energy requirements reduced communications system mass increased communications opportunities robust critical event communications and in situ navigation aid 63 NASA provided an Electra telecommunications relay and navigation instrument to assure communications between probes and rovers on the surface of Mars and controllers on Earth 64 The TGO will provide the 2022 Rosalind Franklin rover with telecommunications relay it will also serve as a relay satellite for future landed missions 2 Results Edit Image of the edge of Planum Australe Mars south polar ice cap taken by CaSSIS The dusty ice layers that compose the South Polar Layered Deposits SPLD are exposed and visible in the image The spacecraft took its first photos of the surface of Mars on 15 April 2018 65 The first year of science operations 66 yielded a wealth of new data and scientific discoveries including new observations of the atmospheric composition and structure 67 68 water ice cloud enhancement during a global dust storm 69 new measurements of the atmospheric thermal structure and density 70 estimations of the timespan of the climate record of the south polar ice sheet 71 confirmation of dry processes being responsible for Recurring Slope Lineae in Gale crater 72 and high resolution maps of shallow subsurface Hydrogen increasing the known amounts of probably near surface buried water ice 73 In April 2019 the science team reported their first methane results TGO had detected no methane whatsoever even though their data were more sensitive than the methane concentrations found using Curiosity Mars Express and ground based observations 74 75 See also Edit Astronomy portal Biology portal Solar System portal Spaceflight portalCuriosity rover NASA robotic rover exploring the crater Gale on Mars List of missions to Mars Mars 2020 Astrobiology Mars rover mission by NASA Mars Exploration Joint Initiative international space agencies agreement about mars explorationPages displaying wikidata descriptions as a fallback Mars Express European Mars orbiter Mars Global Surveyor NASA Mars orbiter launched in 1996 Mars Orbiter Mission Indian Mars orbiter launched in 2013 MAVEN NASA Mars orbiterReferences Edit ExoMars Trace Gas Orbiter and Schiaparelli Mission 2016 European Space Agency 16 October 2016 Retrieved 24 October 2016 a b c Allen Mark A Witasse Olivier 2011 2016 ESA NASA ExoMARS Trace Gas Orbiter Mars Exploration Program Assessment Group 15 16 June 2011 Lisbon Portugal hdl 2014 42148 ExoMars 2016 NASA Space Science Data Coordinated Archive Retrieved 30 November 2022 a b c d e f g h i j k l m n o p ExoMars Trace Gas Orbiter TGO European Space Agency 12 July 2012 Retrieved 8 March 2014 a b Amos Jonathan 14 March 2016 Mars methane mission lifts off BBC Retrieved 14 March 2016 Nowakowski Tomasz 20 October 2016 Lost on Mars Schiaparelli lander falls silent shortly before touchdown Spaceflight Insider Retrieved 24 October 2016 Chang Kenneth 19 October 2016 ExoMars Mission to Join Crowd of Spacecraft at Mars The New York Times Retrieved 19 October 2016 Vago J L 10 September 2009 Mars Panel Meeting PDF Planetary Science Decadal Survey Arizona State University Tempe US European Space Agency a b c Mustard Jack 9 July 2009 MEPAG Report to the Planetary Science Subcommittee PDF Mars Exploration Program Analysis Group p 3 Amos Jonathan 19 October 2016 Fears grow for European Schiaparelli Mars lander BBC News Retrieved 20 October 2016 Surfing complete European Space Agency 21 February 2018 Archived from the original on 22 February 2018 Retrieved 1 May 2018 Mitschdoerfer Pia et al 9 April 2018 ExoMars poised to start science mission European Space Agency Retrieved 18 June 2018 a b Second ExoMars mission moves to next launch opportunity in 2020 Press release European Space Agency 2 May 2016 Retrieved 2 May 2016 The way forward to Mars ESA 1 October 2020 Retrieved 5 October 2020 Mars Trace Gas Mission MEPAG 10 September 2009 Archived from the original on 21 July 2011 Mumma Michael J Villanueva Geronimo L Novak Robert E Hewagama Tilak Bonev Boncho P Disanti Michael A Mandell Avi M Smith Michael D 20 February 2009 Strong Release of Methane on Mars in Northern Summer 2003 PDF Science 323 5917 1041 1045 Bibcode 2009Sci 323 1041M doi 10 1126 science 1165243 PMID 19150811 S2CID 25083438 Hand Eric 21 October 2008 Plumes of methane 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Whewell Megan 15 February 2012 Have Europe s Martian exploration plans been derailed by America MSN News Archived from the original on 11 May 2012 Retrieved 15 February 2012 Svitak Amy 16 March 2012 Europe Joins Russia on Robotic ExoMars Aviation Week Retrieved 16 March 2012 Amos Jonathan 15 March 2012 Europe still keen on Mars missions BBC News Archived from the original on 7 November 2022 Retrieved 8 March 2023 NASA drops ExoMars missions in 2013 budget Optics 15 February 2012 Retrieved 15 February 2012 Spacewatch Uncertainties for ExoMars The Guardian 16 March 2012 Amos Jonathan 15 March 2012 Europe still keen on Mars missions BBC News Retrieved 16 March 2012 ExoMars Russian Space Web Retrieved 22 October 2013 N 6 2020 ExoMars to take off for the Red Planet in 2022 Press release ESA 12 March 2020 Retrieved 12 March 2020 ExoMars 2016 Schiaparelli Module in Baikonur ESA SpaceRef 6 January 2016 Retrieved 6 January 2016 Gibney Elizabeth 11 March 2016 Mars launch to test collaboration between Europe and Russia Nature 531 7594 288 299 Bibcode 2016Natur 531 288G doi 10 1038 nature 2016 19547 PMID 26983519 ExoMars on its way to solve the Red Planet s mysteries ESA 14 March 2016 Archived from the original on 26 October 2016 Retrieved 15 March 2016 King Bob 24 March 2016 ExoMars Mission Narrowly Avoids Exploding Booster Universe Today Retrieved 25 March 2016 de Selding Peter B 5 April 2016 Roscosmos gives detailed rebuttal to reports of Proton ExoMars launch anomaly Space News Retrieved 5 April 2016 Malik Tariq 16 October 2016 European Mars Lander Separates From Mothership Takes Aim at Red Planet Space com Retrieved 16 October 2016 Aron Jacob 7 March 2016 ExoMars probe set to sniff out signs of life on the Red Planet New Scientist Retrieved 7 March 2016 de Selding Peter B 20 October 2016 Europe s ExoMars enters Mars orbit but lander feared lost SpaceNews Retrieved 21 October 2016 Gebhardt Chris 19 October 2016 ExoMars completes crucial orbit insertion hope lost for lander NASASpaceflight com Archived from the original on 25 October 2022 Retrieved 8 March 2023 Mars lander smashed into ground at 540km h after misjudging its altitude The Guardian Agence France Presse 24 November 2016 Retrieved 1 January 2017 Wall Mike 23 February 2018 Methane Sniffing Orbiter Finishes Aerobraking Dives Through Mars Atmosphere Space com Retrieved 24 February 2018 Svedhem Hakan Vago Jorge L Bruinsma Sean Muller Wodarg Ingo et al 2017 ExoMars Trace Gas Orbiter provides atmospheric data during Aerobraking into its final orbit 49th Annual Division for Planetary Sciences Meeting 15 20 October 2017 Provo Utah Bibcode 2017DPS 4941801S 418 01 Trace Gas Orbiter TGO Spacecraft Frames Kernel 26 September 2016 Retrieved 6 October 2018 ExoMars 2016 National Space Science Data Center NASA Retrieved 15 March 2016 Gannon Megan 14 March 2016 The Science of ExoMars New Mission to Hunt for Mars Life Space com Retrieved 16 March 2016 Montmessin F Atmospheric Chemistry Suite Science Overview PDF LATMOS CNRS France p 44 Archived from the original PDF on 15 March 2016 Retrieved 14 March 2016 Determining the origin of methane on Mars can only be addressed by looking at methane isotopologues and at higher alkanes ethane propane McKie Robin 20 February 2016 Giant nose in the sky ready for lift off in mission to sniff out traces of life on Mars The Guardian Retrieved 21 February 2016 Vandaele A C et al NOMAD a spectrometer suite for nadir and solar occultation observations on the ExoMars Trace Gas Orbiter PDF Institut des NanoSciences de Paris Retrieved 4 September 2015 a b Vago J et al August 2013 ExoMars ESA s next step in Mars exploration PDF ESA Bulletin No 155 pp 12 23 ExoMars Trace Gas Orbiter Instruments ESA 20 February 2014 Archived from the original on 19 February 2016 Retrieved 8 March 2014 Thomas I R Vandaele A C Neefs E et al 2017 The NOMAD Spectrometer Suite on the ExoMars 2016 Orbiter Current Status PDF The Sixth International Workshop on the Mars Atmosphere Modelling and Observation 17 20 January 2017 Granada Spain 4401 Bibcode 2017mamo conf 4401T Zakutnyaya Olga 25 November 2012 Europe to invest 12 bln euros in a new space Odyssey Space Daily a b Russia to Construct Landing Pad for Russian European ExoMars 2018 Space Mission RIA Novosti Russia 4 August 2014 Retrieved 5 August 2014 Amos Jonathan 18 June 2013 Europe BBC News Retrieved 18 June 2013 Edwards Charles D Jr Banerdt William B Beaty David W Tamppari Leslie K Zurek Richard W 15 September 2009 Relay Orbiters for Enhancing and Enabling Mars In Situ Exploration PDF Report Mars Exploration Program Analysis Group De Selding Peter B 26 September 2012 U S Europe Won t Go It Alone in Mars Exploration Space News Retrieved 27 September 2012 Thomas Nicolas et al 26 April 2018 ExoMars returns first images from new orbit European Space Agency Retrieved 18 June 2018 Svedhem H Vago J L Rodionov D 1 December 2019 The ExoMars Trace Gas Orbiter New Results and Future Plans AGU Fall Meeting Abstracts 23 Bibcode 2019AGUFM P23B3482S Trokhimovskiy A Perevalov V Korablev O Fedorova A A Olsen K S Bertaux J L Patrakeev A Shakun A Montmessin F Lefevre F Lukashevskaya A 1 July 2020 First observation of the magnetic dipole CO2 absorption band at 3 3 mm in the atmosphere of Mars by the ExoMars Trace Gas Orbiter ACS instrument Astronomy amp Astrophysics 639 A142 Bibcode 2020A amp A 639A 142T doi 10 1051 0004 6361 202038134 ISSN 0004 6361 Olsen K S Lefevre F Montmessin F Fedorova A A Trokhimovskiy A Baggio L Korablev O Alday J Wilson C F Forget F Belyaev D A 18 January 2021 The vertical structure of CO in the Martian atmosphere from the ExoMars Trace Gas Orbiter Nature Geoscience 14 2 67 71 Bibcode 2021NatGe 14 67O doi 10 1038 s41561 020 00678 w ISSN 1752 0908 Stcherbinine A Vincendon M Montmessin F Wolff M J Korablev O Fedorova A Trokhimovskiy A Patrakeev A Lacombe G Baggio L Shakun A 2020 Martian Water Ice Clouds During the 2018 Global Dust Storm as Observed by the ACS MIR Channel Onboard the Trace Gas Orbiter Journal of Geophysical Research Planets 125 3 e2019JE006300 arXiv 1912 08018 Bibcode 2020JGRE 12506300S doi 10 1029 2019JE006300 ISSN 2169 9100 S2CID 209386623 Siddle A G Mueller Wodarg I C F Bruinsma S Marty J C 23 October 2020 Density structures in the martian lower thermosphere as inferred by Trace Gas Orbiter accelerometer measurements Icarus 357 114109 doi 10 1016 j icarus 2020 114109 ISSN 0019 1035 S2CID 226339347 Becerra Patricio Sori Michael M Thomas Nicolas Pommerol Antoine Simioni Emanuele Sutton Sarah S Tulyakov Stepan Cremonese Gabriele 2019 Timescales of the Climate Record in the South Polar Ice Cap of Mars Geophysical Research Letters 46 13 7268 7277 Bibcode 2019GeoRL 46 7268B doi 10 1029 2019GL083588 hdl 10150 634664 ISSN 1944 8007 S2CID 198424636 Munaretto G Pajola M Cremonese G Re C Lucchetti A Simioni E McEwen A S Pommerol A Becerra P Conway S J Thomas N 1 August 2020 Implications for the origin and evolution of Martian Recurring Slope Lineae at Hale crater from CaSSIS observations Planetary and Space Science 187 104947 Bibcode 2020P amp SS 18704947M doi 10 1016 j pss 2020 104947 ISSN 0032 0633 S2CID 218929279 Malakhov Alexey Mitrofanov Igor Golovin Dmitry Sanin Anton Litvak Maxim Mokrousov Maxim Kozyrev Alexander Tretyakov Vladislav Djachkova Maya Nikiforov Sergey Lisov Denis 1 April 2019 Mars subsurface hydrogen as seen by FREND onboard TGO EGU General Assembly Conference Abstracts 21 16504 Bibcode 2019EGUGA 2116504M Korablev Oleg et al 2019 No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations PDF Nature 568 7753 517 520 Bibcode 2019Natur 568 517K doi 10 1038 s41586 019 1096 4 PMID 30971829 S2CID 106411228 Trokhimovskiy A Perevalov V Korablev O Fedorova A A Olsen K S Bertaux J L Patrakeev A Shakun A Montmessin F Lefevre F Lukashevskaya A 2020 First observation of the magnetic dipole CO2absorption band at 3 3mm in the atmosphere of Mars by the Exo Mars Trace Gas Orbiter ACS instrument Astronomy amp Astrophysics 639 A142 Bibcode 2020A amp A 639A 142T doi 10 1051 0004 6361 202038134 S2CID 225600219 External links EditExoMars Trace Gas Orbiter at ESA int ESA ExoMars on Flickr Retrieved from https en wikipedia org w index php title Trace Gas Orbiter amp oldid 1150303903, wikipedia, wiki, book, books, library,

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