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Space Variable Objects Monitor

January 01, 1970

The Space Variable Objects Monitor (SVOM) is a planned small X-ray telescope satellite under development by China National Space Administration (CNSA), Chinese Academy of Sciences (CAS) and the French Space Agency (CNES),[3] to be launched on 24 June 2024.[1]

Space Variable Objects Monitor
SVOM artist impression
NamesSpaceborne multiband astronomical Variable Objects Monitor mission
Mission typeGamma-ray burst observatory
OperatorCNES / CNSA
Websitehttp://www.svom.fr/en/
Mission duration3 years (planned)
Spacecraft properties
SpacecraftSVOM
Launch mass950 kg (2,090 lb)
Dimensions2.5 × 2.8 m (8 ft 2 in × 9 ft 2 in)
Power800 watts
Start of mission
Launch date24 June 2024 (planned)[1]
RocketLong March 2C[2]
Launch siteXichang Satellite Launch Center
ContractorChina Aerospace Science and Technology Corporation (CASC)
Orbital parameters
Reference systemGeocentric orbit
RegimeLow Earth orbit
Perigee altitude625 km (388 mi)
Apogee altitude625 km (388 mi)
Inclination30°
Period90.0 minutes
Instruments
ECLAIRsWide-field camera
GRMGamma-ray Burst Monitor
MXTMicrochannel X-ray Telescope
VTVisible Telescope
 

SVOM will study the explosions of massive stars by analysing the resulting gamma-ray bursts. The light-weight X-ray mirror for SVOM weighs just 1 kg (2.2 lb).[3] SVOM will add new capabilities to the work of finding gamma-ray bursts currently being done by the multinational satellite Swift Gamma-Ray Burst Mission.[3] Its anti-solar pointing strategy makes the Earth cross the field of view of its payload every orbit.[4]

Objectives edit

Using synergy between space and ground instruments, the mission has these scientific objectives:[5]

  • Permit the detection of all known types of Gamma-ray bursts (GRB)
  • Provide fast, reliable GRB positions
  • Measure the broadband spectral shape of the prompt emission (from visible to MeV)
  • Measure the temporal properties of the prompt emission (from visible to MeV)
  • Quickly identify the afterglows of detected GRBs at X-ray and optical wavelengths, including those which are highly redshifted (z>6)
  • Measure the broadband spectral shape of the early and late afterglow (from visible to X-rays)
  • Measure the temporal evolution of the early and late afterglow (from visible to X-rays)

Scientific instruments edit

The selected orbit is circular with an altitude of 600 km (370 mi) and an inclination angle of 30° with a precession period of 60 days.[6] The payload is composed of the following four main instruments:[6][7]

 
ECLAIRs coded mask
ECLAIRs
ECLAIRs is a wide-field (~2 sr) coded mask camera with a mask transparency of 40% and a 1,024 cm2 (158.7 sq in) detection plane coupled to a data processing unit, so-called UGTS, which is in charge of locating GRBs in near real time image and rate triggers.[8] The trigger system of the coded-mask telescope ECLAIRs onboard SVOM images the sky in the 4-120 keV energy range, in order to detect and localize GRB in its 2 sr-wide field of view. The low-energy threshold of ECLAIRs is well suited for the detection of highly red-shifted GRB.[9] ECLAIRs is expected to detect ~200 GRBs of all types during the nominal 3 year mission lifetime. To reach a 4 keV low-energy threshold, the ECLAIRs detection plane is paved with 6400 4×4 mm2 and 1 mm-thick Schottky CdTe detectors. The detectors are grouped by 32, in 8x4 matrices read by a low-noise ASIC, forming elementary modules called XRDPIX.[8]
Gamma-ray Burst Monitor (GRM)
A gamma-ray non-imaging spectrometer (GRM), sensitive in the 50 keV to 5 MeV domain, will extend the prompt emission energy coverage. GRB alerts are sent in real-time to the ground observers community.
Microchannel X-ray Telescope (MXT)
A spacecraft slew is performed in order to place the GRB within the narrow fields of view of two instruments - a soft X-ray telescope (MXT) and a visible-band telescope (VT), to refine the GRB position and study the early phases of the GRB afterglow.[10] MXT uses lobster-eye optics that will give it a wide field of view.[11]
Visible Telescope (VT)
A 45 cm (18 in) visible telescope operating from 400 to 950 nm, with a FOV of 21 × 21 arcminutes. It will reach a sensitivity of about 23 magnitudes, in the R band, in a 300 seconds exposure time, at 5 seconds.

Ground segment edit

The ground segment includes a set of three ground-based dedicated instruments – two robotic Ground Follow-up Telescopes (GFT) and an optical monitor, Ground Wide Angle Camera (GWAC) – which will complement the space borne instruments. A large fraction of GRB will have redshift determinations, an observing strategy optimized to facilitate follow-up observations by large ground-based spectroscopic telescopes.

A key elements of the SVOM mission are the Ground Wide Angle Cameras (GWACs) and the Ground Follow-up Telescopes (GFTs).[12][13] The GWACs, an array of wide FoV optical cameras operating in the optical domain, will permit a systematic study of the visible emission during and before the prompt high-energy emission. It will cover a field of view of about 8000 deg², with a sensitivity of about 15 magnitudes at 5 seconds (under the full Moon condition), in the V band and with a 15 seconds exposure time. It will monitor continuously the field covered by ECLAIRs in order to observe the visible emissions of more than 20% of the events, at least 5 minutes before and 15 minutes after the GRB trigger.

The GFTs, two robotic 1-meter class telescopes (one managed by France, another one by China), will point automatically their field-of view towards the space-given error box within tens of seconds after the alert reception and will provide panchromatic follow-up (visible to near-infrared). They will contribute to the improvement of the link between the scientific payload and the largest telescopes by measuring the celestial coordinates with an accuracy better than 0.5″, and by providing an estimate of its photometric redshift in less than 5 minutes after the beginning of the observations. This data will be available to the scientific community through an alert message. Evenly placed on the Earth (one in South America in a place to be defined, the other one in China), they will be in a position to start the research of the GRB optical emission immediately after the alert reception in more than 40% of the cases.

See also edit

References edit

  1. ^ a b "Svom". Retrieved 14 January 2024.
  2. ^ "SVOM (Spaceborne multiband astronomical Variable Objects Monitor) mission". ESA Earth Observation Portal. 20 May 2021. Retrieved 20 May 2021.
  3. ^ a b c . University of Leicester. 26 October 2015. Archived from the original on 28 January 2021. Retrieved 20 May 2021.
  4. ^ Zhao, Donghua; Cordier, Bertrand; Sizun, Patrick; Wu, Bobing; Dong, Yongwei; et al. (November 2012). "Influence of the Earth on the background and the sensitivity of the GRM and ECLAIRs instruments aboard the Chinese-French mission SVOM". Experimental Astronomy. 34 (3): 705–728. arXiv:1208.2493. Bibcode:2012ExA....34..705Z. doi:10.1007/s10686-012-9313-2. S2CID 54647027.
  5. ^ "The SVOM mission, a new generation GRB mission". Commissariat à l'énergie atomique et aux énergies alternatives. Retrieved 26 October 2015.
  6. ^ a b "SVOM: The scientific payload". Commissariat à l'énergie atomique et aux énergies alternatives. Retrieved 26 October 2015.
  7. ^ "SVOM Satellite". CNES. 2014. Retrieved 26 October 2015.
  8. ^ a b Godet, O.; Nasser, G.; Atteia, Jonathan; Cordier, B.; Mandrou, P.; et al. (July 2014). Takahashi, Tadayuki; Den Herder, Jan-Willem A.; Bautz, Mark (eds.). "The x-/gamma-ray camera ECLAIRs for the gamma-ray burst mission SVOM". Proceedings of the SPIE. Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray. 9144: 914424. arXiv:1406.7759. Bibcode:2014SPIE.9144E..24G. doi:10.1117/12.2055507. S2CID 119248306.
  9. ^ Schanne, S.; Paul, J.; Wei, J.; Zhang, S.-N.; Basa, S.; et al. (13–17 October 2009). The future Gamma-Ray Burst Mission SVOM. The Extreme Sky: Sampling the Universe Above 10 keV. Otranto, Italy. arXiv:1005.5008. Bibcode:2010arXiv1005.5008S.
  10. ^ Gotz, D.; Paul, J.; Basa, S.; Wei, J.; Zhang, S. N.; et al. (20–23 October 2008). SVOM: A new mission for Gamma-Ray Burst Studies. Gamma-ray Burst: 6th Huntsville Symposium. Huntsville, Alabama. arXiv:0906.4195. Bibcode:2009AIPC.1133...25G. doi:10.1063/1.3155898.
  11. ^ "Delivery of the MXT telescope optics – Svom".
  12. ^ "SVOM: The ground segment". Commissariat à l'énergie atomique et aux énergies alternatives. Retrieved 26 October 2015.
  13. ^ "Ground Segment". CNES. 24 April 2015. Retrieved 26 October 2015.

External links edit

January 01, 1970
space, variable, objects, monitor, svom, planned, small, telescope, satellite, under, development, china, national, space, administration, cnsa, chinese, academy, sciences, french, space, agency, cnes, launched, june, 2024, svom, artist, impressionnamesspacebo. The Space Variable Objects Monitor SVOM is a planned small X ray telescope satellite under development by China National Space Administration CNSA Chinese Academy of Sciences CAS and the French Space Agency CNES 3 to be launched on 24 June 2024 1 Space Variable Objects MonitorSVOM artist impressionNamesSpaceborne multiband astronomical Variable Objects Monitor missionMission typeGamma ray burst observatoryOperatorCNES CNSAWebsitehttp www svom fr en Mission duration3 years planned Spacecraft propertiesSpacecraftSVOMLaunch mass950 kg 2 090 lb Dimensions2 5 2 8 m 8 ft 2 in 9 ft 2 in Power800 wattsStart of missionLaunch date24 June 2024 planned 1 RocketLong March 2C 2 Launch siteXichang Satellite Launch CenterContractorChina Aerospace Science and Technology Corporation CASC Orbital parametersReference systemGeocentric orbitRegimeLow Earth orbitPerigee altitude625 km 388 mi Apogee altitude625 km 388 mi Inclination30 Period90 0 minutesInstrumentsECLAIRsWide field cameraGRMGamma ray Burst MonitorMXTMicrochannel X ray TelescopeVTVisible Telescope SVOM will study the explosions of massive stars by analysing the resulting gamma ray bursts The light weight X ray mirror for SVOM weighs just 1 kg 2 2 lb 3 SVOM will add new capabilities to the work of finding gamma ray bursts currently being done by the multinational satellite Swift Gamma Ray Burst Mission 3 Its anti solar pointing strategy makes the Earth cross the field of view of its payload every orbit 4 Contents 1 Objectives 2 Scientific instruments 3 Ground segment 4 See also 5 References 6 External linksObjectives editUsing synergy between space and ground instruments the mission has these scientific objectives 5 Permit the detection of all known types of Gamma ray bursts GRB Provide fast reliable GRB positions Measure the broadband spectral shape of the prompt emission from visible to MeV Measure the temporal properties of the prompt emission from visible to MeV Quickly identify the afterglows of detected GRBs at X ray and optical wavelengths including those which are highly redshifted z gt 6 Measure the broadband spectral shape of the early and late afterglow from visible to X rays Measure the temporal evolution of the early and late afterglow from visible to X rays Scientific instruments editThe selected orbit is circular with an altitude of 600 km 370 mi and an inclination angle of 30 with a precession period of 60 days 6 The payload is composed of the following four main instruments 6 7 nbsp ECLAIRs coded mask ECLAIRs ECLAIRs is a wide field 2 sr coded mask camera with a mask transparency of 40 and a 1 024 cm2 158 7 sq in detection plane coupled to a data processing unit so called UGTS which is in charge of locating GRBs in near real time image and rate triggers 8 The trigger system of the coded mask telescope ECLAIRs onboard SVOM images the sky in the 4 120 keV energy range in order to detect and localize GRB in its 2 sr wide field of view The low energy threshold of ECLAIRs is well suited for the detection of highly red shifted GRB 9 ECLAIRs is expected to detect 200 GRBs of all types during the nominal 3 year mission lifetime To reach a 4 keV low energy threshold the ECLAIRs detection plane is paved with 6400 4 4 mm2 and 1 mm thick Schottky CdTe detectors The detectors are grouped by 32 in 8x4 matrices read by a low noise ASIC forming elementary modules called XRDPIX 8 Gamma ray Burst Monitor GRM A gamma ray non imaging spectrometer GRM sensitive in the 50 keV to 5 MeV domain will extend the prompt emission energy coverage GRB alerts are sent in real time to the ground observers community Microchannel X ray Telescope MXT A spacecraft slew is performed in order to place the GRB within the narrow fields of view of two instruments a soft X ray telescope MXT and a visible band telescope VT to refine the GRB position and study the early phases of the GRB afterglow 10 MXT uses lobster eye optics that will give it a wide field of view 11 Visible Telescope VT A 45 cm 18 in visible telescope operating from 400 to 950 nm with a FOV of 21 21 arcminutes It will reach a sensitivity of about 23 magnitudes in the R band in a 300 seconds exposure time at 5 seconds Ground segment editThe ground segment includes a set of three ground based dedicated instruments two robotic Ground Follow up Telescopes GFT and an optical monitor Ground Wide Angle Camera GWAC which will complement the space borne instruments A large fraction of GRB will have redshift determinations an observing strategy optimized to facilitate follow up observations by large ground based spectroscopic telescopes A key elements of the SVOM mission are the Ground Wide Angle Cameras GWACs and the Ground Follow up Telescopes GFTs 12 13 The GWACs an array of wide FoV optical cameras operating in the optical domain will permit a systematic study of the visible emission during and before the prompt high energy emission It will cover a field of view of about 8000 deg with a sensitivity of about 15 magnitudes at 5 seconds under the full Moon condition in the V band and with a 15 seconds exposure time It will monitor continuously the field covered by ECLAIRs in order to observe the visible emissions of more than 20 of the events at least 5 minutes before and 15 minutes after the GRB trigger The GFTs two robotic 1 meter class telescopes one managed by France another one by China will point automatically their field of view towards the space given error box within tens of seconds after the alert reception and will provide panchromatic follow up visible to near infrared They will contribute to the improvement of the link between the scientific payload and the largest telescopes by measuring the celestial coordinates with an accuracy better than 0 5 and by providing an estimate of its photometric redshift in less than 5 minutes after the beginning of the observations This data will be available to the scientific community through an alert message Evenly placed on the Earth one in South America in a place to be defined the other one in China they will be in a position to start the research of the GRB optical emission immediately after the alert reception in more than 40 of the cases See also edit nbsp Astronomy portal nbsp Spaceflight portal List of gamma ray bursts List of X ray space telescopesReferences edit a b Svom Retrieved 14 January 2024 SVOM Spaceborne multiband astronomical Variable Objects Monitor mission ESA Earth Observation Portal 20 May 2021 Retrieved 20 May 2021 a b c Lobster inspired 3 8m super lightweight mirror chosen for Chinese French space mission University of Leicester 26 October 2015 Archived from the original on 28 January 2021 Retrieved 20 May 2021 Zhao Donghua Cordier Bertrand Sizun Patrick Wu Bobing Dong Yongwei et al November 2012 Influence of the Earth on the background and the sensitivity of the GRM and ECLAIRs instruments aboard the Chinese French mission SVOM Experimental Astronomy 34 3 705 728 arXiv 1208 2493 Bibcode 2012ExA 34 705Z doi 10 1007 s10686 012 9313 2 S2CID 54647027 The SVOM mission a new generation GRB mission Commissariat a l energie atomique et aux energies alternatives Retrieved 26 October 2015 a b SVOM The scientific payload Commissariat a l energie atomique et aux energies alternatives Retrieved 26 October 2015 SVOM Satellite CNES 2014 Retrieved 26 October 2015 a b Godet O Nasser G Atteia Jonathan Cordier B Mandrou P et al July 2014 Takahashi Tadayuki Den Herder Jan Willem A Bautz Mark eds The x gamma ray camera ECLAIRs for the gamma ray burst mission SVOM Proceedings of the SPIE Space Telescopes and Instrumentation 2014 Ultraviolet to Gamma Ray 9144 914424 arXiv 1406 7759 Bibcode 2014SPIE 9144E 24G doi 10 1117 12 2055507 S2CID 119248306 Schanne S Paul J Wei J Zhang S N Basa S et al 13 17 October 2009 The future Gamma Ray Burst Mission SVOM The Extreme Sky Sampling the Universe Above 10 keV Otranto Italy arXiv 1005 5008 Bibcode 2010arXiv1005 5008S Gotz D Paul J Basa S Wei J Zhang S N et al 20 23 October 2008 SVOM A new mission for Gamma Ray Burst Studies Gamma ray Burst 6th Huntsville Symposium Huntsville Alabama arXiv 0906 4195 Bibcode 2009AIPC 1133 25G doi 10 1063 1 3155898 Delivery of the MXT telescope optics Svom SVOM The ground segment Commissariat a l energie atomique et aux energies alternatives Retrieved 26 October 2015 Ground Segment CNES 24 April 2015 Retrieved 26 October 2015 External links editSVOM website by Commissariat a l energie atomique et aux energies alternatives CEA SVOM website by CNES Retrieved from https en wikipedia org w index php title Space Variable Objects Monitor amp oldid 1199458487, wikipedia, wiki, book, books, library,

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