next space vlbi mission, astro-g (vsop-2) and its spectrum management astro-g project (jaxa) y....
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NEXT SPACE VLBI MISSION, ASTRO-G (VSOP-2)
ANDITS SPECTRUM MANAGEMENT
ASTRO-G Project (JAXA)
Y. Murata ( JAXA)
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HALCA and VSOP (1997-2005)Highly Advanced Laboratory for Communications and Astronomy
VLBI Space Observatory Programme
3C345
VLBA VSOP
Launch: Feb. 12, 1997 Apogee 21,000km Perigee 560 km 380 minutes period
Observing bands:
1.6, 5.0 GHz
(22 GHz)
Phase Link & Data Transmission:
Downlink 128 Mbps QPSK
@ 14.2 GHz
Uplink CW @ 15.3 GHz
TT&C: S-band with LGA
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Plasma torus
VSOP with HALCA
• The first space VLBI imaging mission
• Studied AGN environment and jet physics– Structure and kinematics of jet
in AGN– Absorption near the core and
study of torus structure– Existence of high brightness
temperature sources
Also Pulsars, X-ray binaries, OH masers
Beamwidth 100 Rs at 5 GHz for M87
Plasma Torus in absorption
4-years jet monitoring
3C273
Jet Structure
1928+738
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ASTRO-G (VSOP-2) – VLBI Space Observatory Programme – 2
10 times higher sensitivity
10 times higher frequency observation
10 times higher resolution with ~ 40 arcseconds
Observing bands 8, 22, 43 GHz
Dual polarization
Phase-referencing capability
The next generation Space VLBI (SVLBI) mission following the VSOP mission
9.26 m Antenna for
Radio Astronomy
Mass 1200kg (Nominal)
1 Gbps Data Downlink
Compared to VSOP:
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Astrophysics with ASTRO-G (VSOP-2)
Generate VLBI array with Ground Radio Telescopes.
Magnetic fields of galaxies
Jets from the accretion disks around black holes
Radio galaxies
Quasars
Observe astronomical objects with the highest resolution.
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Lobanov, A.P. 2003, SKA Memo 38
Comparison of Telescope Resolutions
VSOP
CurrentTelescopes
VERA
Radio IROptical
UV X γ
1mas
1SKA
ASTRO-G(VSOP-2)
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Comparison ofASTRO-G/VSOP-2 and HALCA/VSOP
• More information on fine structure and magnetic field from AGN jets and cores– Higher resolution with polarization capability
• Higher sensitivity– With 2 polarization, 8 times wider bandwidth (only continuum sources)
• High agility attitude control system using control moment gyros– Improved calibration capability (ASTRO-G can observe calibrators, HALCA could not)– Phase-referencing observations enabled
Allows weaker source detection by extending integration time and astrometry observations
• High accuracy navigation using onboard GPSR and SLRRequired for phase-referencing
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ASTRO-G Satellite Configuration• 9.3-m offset Cassegrain antenna with module structures
– Light weight– gimbal adjuster– focusing system
– Mass (wet) 1200Kg– Power 2000W
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第22号科学衛星 SOLAR-B ASTRO-G Configuration
Orbit Apogee Height 25,000 km Perogee Height 1,000 km Inclination 31° Orbit Period 7.5 h
Solar Paddle
rSolar Paddle天体方向
副鏡
主鏡
9.6 m
Ka Ant for VLBI Link
Satelite Size Mass 1,200 kg Power 2,000 W
Observation Target Satellite For VLBI• 9 meter Deployable Antenna for 43GHz• Cooled LNA ( 30 K )• 1 Gbps Down Link• Phase Compensation Observation Target Switching (3deg manoeuvre in 15 sec) Orbit Determnation with 10 cm Accuracy
Solar Paddle
Sub Reflector
Main Reflector
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Rocket & Orbit
• Launch Rocket is H2A – Launch epoch; FY 2012– Single or Shared Launch is not decided now.
• ASTRO-G Orbit (HALCA)– Apogee Height: 25,000 km (21,300 km)– Perigee Height: 1,000 km (560 km)– Inclination 31°(31 °)– Orbit Period 7.5 hours (6.3 h)
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Key Technology: Large Deployable Antenna
Module-type offset-Cassegrain antenna(use ETS-VIII deployment mechanism)
Mesh + Tension Truss
Need higher accuracy moduleOffset-cassegrain antenna
HALCA ( 1997 )
ETS-VIII ( Dec. 2006 )
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Large Deployable Antennas (2/2)
Seven Modules (Stow / Deployment)
Azimuthal Hoop Cable & Radial Rib. Cable Network
XY
Development Module (2003)
Improve Surface accuracy (0.4mmrms)ETS-VIII 2GHz, ASTRO-G 43GHz
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ASTRO-G Observing System
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ASTRO-G tracking station
H Maser
Data Storage
VLBI Data DownlinkFrequency 37-38 GHzBit Rate 1 GbpsModulation QPSKTX-Power 25 W
High Gain AntennaDiameter: 80cm
Data StorageCapacity 4 TB / 8 hours
Phase Transfer UplinkFrequency 40 GHzNo ModulationTX-Power 100mW
Phase Comparison
Ground Link Station Diameter >10mOver 3 stations
ASTRO-G
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Precision Oribt Determination
GPS
Precision LaserReflectors
Postioning Accuracy<10 cm
Ground Laser Stations
ASTRO-G25,000x1,000km
GPS20,000km
1,2 GPS Sats @ Apogee.Many GPS Sats @ Perigee
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Astro-G Operation and Data flow
Ground telescopes
Tracking
Station
Satellite Operation
Correlator
Data Analysis
SchedulingScheduling
• Note: very similar to HALCA operation and data flow
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Current Status of ASTRO-G
System Definition Review 19 Mar. 2007PROJECT Official START 1 Jul, 2007Basic Design of the satellite system (April 2007 – March 2008) Structure and Thermal model analysis is on going. Thermal deformation, Fix of the interfaces.Preliminary Design Review #1 (February – June 2008) 3 month delay For instruments need to start detailed design earlier. Main Reflector, Structures, Cryostat, Ka-HGA Preliminary Design Review #2 (March 2009) Other instrumentsCritical Design Review (March 2010) 6 month delay to the last schedule
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Basic DesignSub-reflector
Antenna Tower
Bus System Solar ArrayPaddle
Ka HGA
Main Reflector
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International Matters
• Meetings– Tracking station meetings
• #4 @ Greenbank, Aug. 2007• #5 @ Sagamihara, Dec. 2007
– VSOP-2 symposium (Dec 3-7, 2007 @ Sagamihara) • 135 participants. Half from outside of Japan (13 countries)
– VSOP-2 Science Meeting (14-16, 2008 @ Bonn)
• Proposals– SAMURAI proposal (submitted in Jan. 2008)
• Proposal to NASA Mission of opportunity for US VSOP-2 supports (Tracking station, VLBA, JPL project office and navigation. See. NRAO report)
– European Proposals FP7 SPIRIT • ESA Nationally Led proposal (Tracking station, SVLBI use of GRT, Correlat
ors).
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International Matters (2)• VISC-2 Formation
– VISC-2(VSOP-2 International Science Council) We form VISC-2 to make consensus related to scientific operations of VSOP-2. Possible VISC-2 fu
nctions are selection of KSPs, scientific scheduling, decisions of international relations, scientific operations. (Finally decided in the first VISC-2 meeting in Bonn in May, 2008)
– pre-meeting • Dec. 2007 @ Sagamihara• April, 2009 @Telecon• May, 2009 First F-F Meeting in Bonn
– Members: • Ex-officio(ISAS/JAXA): H.Saito, M.Tsuboi • Institutional members (12):ISAS(1): Y.Murata (co-chair), NAOJ(1): M.Inoue, JVN(1): K.Fujisawa EAVN (1): H.Kobayashi, KVN/KASI (1): S.-H.Cho, NRAO(1): J.Ulvestad( JPL(1): D.Murphy ), JIVE(1): L.Gurvits, EVN(1): A.Zensus (co-chair)OAN(1): R.Bachiller, ATNF(1): P.Edwards, GVWG(1): J.Romney (NRAO)• At-large members (3): D. Gabuzda (Univ. Collage Cork, Ireland), S.Kameno (Kagoshima Univ.), + Astrome
try person (TBD)• VISC2 adviser (2): D.Jauncey, H.Hirabayashi• Liaison (1): R.Schilizzi (ISPO (International SKA Project Office))• Secretary(1): Y.Hagiwara (NAOJ)
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ASTRO-G radio frequency usage
Ground Radio Telescopes Ground Tracking StationsCommanding
Station
40 GHz 37-38 GHz
3-4 stations in the world.10-20 radio telescopes around the world.
JAXA commanding
station
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Frequency Management Activities
1. Frequency Selection:• Observing bands, Space VLBI (Up/downlink data), TT&C
2. SFCG (Space Frequency Coordination Group)• Coordination among space agencies• Information for ASTRO-G was submitted in September, 2007
3. ITU-R SG7• General SVLBI (Space VLBI) coordination have already done by US (JPL)
group at WP7B. Recommendation ITU-R SA.1344 : SVLBI system description “Preferred frequency bands and bandwidths for Space VLBI” Up 40-40.5 GHz, Down 37-38 GHz• Sharing studies in 37-38 GHz band are going now.• Observing band protection in radio astronomy bands in 22/43 GHz is not cl
ear now.
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ASTRO-G frequency SelectionObserving band:
8.0 – 8.8 GHz, 20.6 – 22.6 GHz, 41.0 – 43.0 GHz
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ASTRO-G (VSOP-2) Specifications (1/2)
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Status of the frequency sharing study for ASTRO-G in 37-38 GHz downlink
•Space VLBI (SVLBI) system : Recommendation ITU-R SA.1344.
•Drafting Group 3 in ITU-R SG-7 Working Party 7B (WP7B)
•Sharing study to Lunar systems (SRS) and FSS.
•WP7B chairman's report (Document 7B/168-E) was released last February
•VSOP-2/ASTRO-G parameters are in Table 3.1 in Annex 8 to document 7B/168-E. But some of the parameters in this table have already updated. Difference of the table is as follows:
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ASTRO-G (VSOP-2) – VLBI Space Observatory Programme – 2
10 times higher sensitivity
10 times higher frequency observation
10 times higher resolution with ~ 40 arcseconds
Observing bands 8, 22, 43 GHz
Dual polarization
Phase-referencing capability
The next generation Space VLBI (SVLBI) mission following the VSOP mission
9.26 m Antenna for
Radio Astronomy
Mass 1200kg (Nominal)
1 Gbps Data Downlink
Compared to VSOP: