vlbi activities in china an update · kashi 13m sanya 13m jilin13m legacy cvn newly built big dish...
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VLBI Activities in China:an update
Zhi-Qiang Shen
Shanghai Astronomical ObservatoryChinese Academy of Sciences
11th East Asia VLBI Workshop 20184-7 September 2018, PyeongChang, Korea
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Major Facilities for RA in China
Kashi 13m
Sanya 13m
Jilin13m
Legacy CVN
Newly built big dish
VGOS
CDSN
Current VLBI facilities in China
Luonan 40m
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Activities at each site FAST
Kunming
Urumqi
VGOS
Shanghai
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FAST - VLBI system installed
Test observations in planning
• L band with Sh, Ur
• Drift scan mode
• Tracking mode
• First light in 2019?
H-maser ROACH-2 Mark 6
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Kunming - VLBI system updated
Updated to CDAS2
DBBC2+MARK6
New H-maser
FlexBuff coming soon!
S X C(new)
Frequency range
2150~2450MHz
8200~9000MHz
4000~8000MHz
Polarization
L&R L&R L&R
LO 2000MHz 8100MHz optional
Tsys 50K(Room TEMP.)
70K(Cooled)
45K
Efficiency ~60% ~45% ~50%
Good EM env (4040—7500 MHz)
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Urumqi – updated to 26m
Dish 25m -> 26m
New Q-band Rx
30 GHz~50 GHz
Tsys < 65K
DBBC2 backend
Test observations in late of 2018
Tsys measurements LCP & RCP
Q-band receiver installing
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25 m
VGOS – NTSC+SHAO
13m diameter antennaVery high slew rates
12° /s in azimuth 6° /s in elevation
Frequency range 1.2 ~ 9 GHzEfficiency > 50%Bandwidth: 1GHz *4Commissioning since 2017
Sheshan VGOS
Fringes Dec. 2017
Tianma VGOS
Sh
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Shanghai – update
FlexBuff installed 240 TB e-VLBI & local disk
e-VLBI up to 2Gbps under testing
EAVN 2018B open useCE-4 VLBI trackingrelay-sat in orbit
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Shanghai – VLBI Sci & Tech workshop
(18-19 May, 2018)
More than 100 participants from 20+ institutes and universities.
40+ presentations: covering VLBI facilities, astrophysics, astrometry, geodesy, deep space applications and technical development.
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Related scientific outputs AGN studies
Pulsar astrometry, Survey
Lunar missions
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Study the compact structure in M81*
Tm
Ur
Sh
6.1km
~3250km
VLBI detected jet component of M81* with CVN at X-band (Kawaguchi et al. 2015)
0.1 mas
The first VLBI Image of M81* at 3.4 mm with VLBA. (Jiang et al. 2018)
Peak=45.3 mJy/beamRMS=0.34 mJy/beamDynamic range ~ 130
s ∝ λ0.88
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Among 3321 sources (red+green) in the ecliptic plane, 556 sources detected (green).
VLBI Ecliptic Plane Survey (VEPS)
(Shu et al. 2017 )
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澳大利亚LBA干涉阵+昆明40米望远镜
~13 arcsec, ~45 arcsec ~1 mJy, compact and flat spectrum calibrators
LBA+KM40:@2.3GHz;
Li et al, 2018
Improve the parallax of J0437-4715 Measure Gdot combined with timing results
Detection of nearby calibrators for MSP
J0437-4715 with LBA+KM 40m
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Pulsar Astrometry with VLBA+TM
NAME PSRJ P0 DM S1400B0458+46 J0502+4654 0.638565 s 42.19 cm^-3 pc 2.50 mJyB2334+61 J2337+6151 0.495370 s 58.41 cm^-3 pc 1.40 mJy
(Yan et al. )
pulsar parallaxes via relative astrometry (differential
astrometry) to get distances and transverse velocities
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VLBI astrometry of white dwarf binary
system AR Sco with EVN and CVN
PM_ra = 11.44 ± 0.33 mas/yrparallax=8.37 ± 0.19 mas
(Jiang, Cui, et al. )
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In collaborations with HartRAO, SHAO, UTAS etc.
Fringe test on April 18, 2017 (Hart26m-TMRT).
The first 24 h session already done on August 28, 2017!
K band Astrometry
Corr. @ SHAO
2Gbps K-band fringe Hh-T6!
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Phase-reference results of CE-3 Rover
Target: Rover using the Lander as the Calibrator.
The accuracy of the relative position between Lander and Rover is ~1m (0.5mas).
Rover
Lander
AB
C
D
EE17
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Future QTT110m
A 40-m RT at YBJ(Tibet)
Space VLBI
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QTT110m
150 MHz – 115 GHz (1st phase upto 30 GHz)
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Major Facilities for RA in China
Kashi 13m
Sanya 13m
Jilin13m
Legacy CVN
Newly built big dish
VGOS
CDSN
Current VLBI facilities in China
Luonan 40m
YBJ 40m
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Space Millimeter VLBI Array
Main Scientific Objectives:• High-resolution imaging of emission structure surrounding super-massive
black hole (SMBH) to study
• SMBH Shadow (e.g. M87)
• Disk structure & dynamics, SMBH mass (water mega-masers)
• Astrophysical Jet in Active Galactic Nuclei (AGN)
Specifications:
• Two 10-m (in diameter) space antennas
• Three frequency bands (8, 22 & 43 GHz)
• Dual polarization (LCP/RCP)
• Date rate (1.2 Gbps , or 2.4 Gbps)
• Angular resolution: 20 micro-arc-second
• Optimized orbits for a better (u,v) coverage
• Apogee: 60,000 km
• Perigee: 1,200 km
• Inclination: 28.5 deg
• Life time: 3 year
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Review Mtg in June 2016
@ CAST (China Academy of Space Technology)
High precision reflector: 10m diameter with a surface accuracy better than 0.4mm (RMS)
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Lunar orbit VLBI experiment(LOVE)
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• Relay satellite antenna diameter: 4.2m (?)
• Band: X (8-9 GHz), Cooled receiver, bandwidth: 512MHz
• Orbit: 200 km x 8,500 km
• Baseline: ~400,000km, unprecedented longest baseline
• Ground telescope: Big Dishes of Ground VLBI Network,e.g. Tianma 65m、GBT 110m,Effelsberg 100m,SRT 64m, et el.
conception of lunar orbit VLBI experiment
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• Space antennas: 2 x 30 m
• Orbit :
– Apogee (60-)90,000 km
– Perigee 2,000 km
– Inclination angle 28.5o
• Frequency Bands:
– 30MHz, 74MHz, 330MHz, 1.7GHz
• Weight: 1.5 Ton/satellite
• Resolution :
– 20mas (30MHz), 8mas (74MHz), 2mas (300MHz),
0.36 mas (1.7GHz)
• Sensitivity:
– BL sensitivity: sub-mJy (int. time =10min)
– image sensitivity: 1 microJy/beam (1h, 1.7GHz)
• Onboard Clocks : H maser or Rb standard
Space VLBI in FAST & SKA era -‘microscope’ probing the Universe from nearby exoplanets to SMBHs in Cosmic Dawn
Low Frequency Twin VLBI Stations in Space
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Operation modes
1. Space-ground VLBI
• Unprecedented Super VLBI network consists of
Twin space-based VLBI Stations + ground large telescopes (SKA1, FAST, Arecibo, Effelsberg, GBT, GMRT, QTT......)
• new electromagnetic spectrum window (30 - 300MHz) for space VLBI
2. Space-space VLBI (single baseline)
• Unique space-based VLBI, long integration time, fast response of super-burst of OH masers, auroral radiation from extrasolar systems
3. Space-based single dish
• EoR total power spectrum, pulsar timing array, planets......
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Scientific objectives
• EoR and Cosmic Dawn
• Discovery of Jupiter-type exoplanets, Solar flares in nearby stellar systems
• Search for Dual AGN and SMBH binariesin nearby massive galactic centers as remnants of mergers – nano Hz GW sources
• BH (AGN, XRB; Galactic transients) physics: jet launching, collimation, acceleration; GRB, FRB
• Pulsar : accurate astrometry, parallax distance, radiation mechanism; giant pulse
• Planets radio emission
• …
30MHz
74MHz
330MHz
1670MHz
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Thank you for your attention!
Welcome collaboration from
all of you!