Current status of OCTAVE
Yusuke Kono1, Tomoaki Oyama1, Noriyuki Kawaguchi1, Kotaro Niinuma2, Kenta Fujisawa2, Hiroshi Takaba3, Kazuhiro Sorai4, Mamoru Sekido5, Shinobu Kurihara6, Yasuhiro Murata7
National Astronomical Observatory of Japan1, Yamaguchi university2,Gifu university3, Hokkaido university4 NICT5, GSI6, JAXA7
OCTAVE Array OCTAVE Family EHT application
Contents
eVLBI network in Japan High sensitivity, on-the-fly result and low cost
operation
OCTAVE : Optically ConnecTed Array for Vlbi Exploration
Hokkaido univ.11m
NICTKashima 34m*
GSI Tsukuba 32m
Gifu univ.11m
Yamaguchi univ.32m
JAXAUsuda 64m*
NAOJNRO 45m*
Ibaraki Univ.*32m x 2
The longest baseline is 1
,300km
Supplied by academic network (SINET4) and Test bed network (JGN-X)
10GbE to nodes 2x10GbE to Correlator at HQ of NAOJ in Tokyo
Kashima and Ibaraki are offline now. Trying to connect.
Usuda and NRO are offline now
Communication lines
Network configuration (Plan)
Local Recorders, OCTADISK and K5, are installed into Usuda, NRO, Ibaraki and Tomakomai for a while.
X-band Usuda64, Kashima34*, Yamaguchi32,
Ibaraki32 8192-8704MHz, BW512MHz x 1/2pols
K-band NRO45, Kashima34*, Yamaguchi,
Ibaraki32, Gifu11, Tomakomai11m 21.5-23.8GHz, BW512MHz x 1/2pols
Observation capability
Kashima34* will be available if the network is connected.
Image of 4C32.44 X-band, BW512 MHz, 4stations software: AIPS
VLBI Detections of Parsec-Scale Nonthermal Jets in Radio-Loud Broad Absorption Line Quasars,
Doi et al., 2009
VLBI Observation of Fermi/LAT Un-associated Gamma-ray Sources, Niinuma et al.,2013
Science Obs. proposals are selected and operated by JVN(Japanese VLBI Network)
Data processing and results
Recording and copying function at NAOJ/Tokyo Fringe test with EAVN (East Asia VLBI
Network) September 2013, 14 stations
Fringe test with Noto April 2013
International Observation
K5(NiCT)
Mark5B+(Haystack)
OCTADISK(NAOJ)
DF
We have developed several instruments for OCTAVE. We call them Octave family.
OCTAVIA OCTAVe optIcal Adapter
OCTADISK OCTAve Recorder
OCTACOR OCTAve Correlator
OCTAD OCTave ADc
OCTADIV OCTAve DIVider
Octave family
Many non-OCTAVE family instruments are also used in the array, such as ASD1000/3000, K5(NICT) and Mark5B(Haystack).
Converter between VSI and 10GbE Electrical I/O
VSI-H 4 Ports Total 8 Gbps
Optical I/O 10GbE Protocol
VDIF/UDP/IP/10GbE
OCTAVIA (OCTAVe optIcal Adapter)
Work by Dr Oyama (NAOJ)
VSIOCTAVIA 10Gb
EADC etc Network etc
DISK Recorder I/O
10GbE (up to 4Gbps) Use with OCTAVIA
Portable module 12 HDDs /module dedicated format.
Under Operation at the VERA stations.
OCTADISK
Work by Dr Oyama (NAOJ)
OCTADISK2 is under development Parts discontinuance of OCTADISK COTS base, except Chassis
OS:Linux, Linux file system Portable module
same to OCTADISK
OCTADISK2
Work by Mr Suzuki and Dr Oyama (NAOJ)
Prototype
“Perfect COTS”
NAOJ supplied Raw VLBI Data Buffer to KJCC
OCTAVIA/DISK in KJCC
Origin of OCTAVIA and OCTADISK
http://kvn-web.kasi.re.kr/en/en_under_correlator.php
VSI Inputfrom variousterminals
Storage on HDD
outputSynchronizeddata to VCS
Real time correlator FPGA correlator
FX and XF type 2Gbps/station
Post processing correlator Software correlator
Engine(GICO3) by NICT Integration by NAOJ with NICT
Correlators for OCTAVE
Soft Correlators Hard CorrelatorsWork by Dr Oyama (NAOJ)
Direct RF sampling 22GHz (43GHz, under test)
Wide bandwidth 8.192Gsps-3bit
use with a RF band pass filter For next generation VERA system
Wideband observation enable us to use weaker and closer reference sources of dVLBI astrometry
OCTAD (ADC)
Lab. test of sampling jitter 0.17 psec (Lc<1% @43GHz)
Fringe test observation Mizusawa 10m x 20m BL=60m 16Gbps x 2 OCTAD
OCTAD
Jitter 0.17psecLc <1%
15 PI: Dr Oyama (NAOJ)
We add two functions DBBC
Backward compatibility BW:16MHz~2048MHz/ch
External AD module up to 50GHz V-connector Direct receiving
Upgraded OCTAD
50GHzModule
Event Horizon Telescope Japanese contribution
Data transfer from AOS to OFS
AOS: Telescope site OSF: Operations Support
Facility 64Gbps(8Gbps x8ch) A single dark fiber Design started at 2011.
EHT / ALMA Phasing
Optical link 30km
VLBI Recorder
Storage Transfer and Correlation
Telescopes and Phasing
PI: Prof. Honma (NAOJ)
EHT / ALMA Phasing WDM of 16 wavelengths by 10GbE-ZR
XFP
XFP –ZRlambda3
AWG2
XFP
XFP
XFP
XFP
XFP
XFP
XFP
XFP –ZRlambda1
XFP –ZRlambda7
XFP –ZRlambda5
XFP –ZRlambda11
XFP –ZRlambda9
XFP –ZRlambda15
XFP –ZRlambda13
AWG4
AWG6
AWG8
AWG10
AWG12
AWG14
AWG16
AWG1
AWG3
AWG5
AWG7
AWG9
AWG11
AWG13
AWG15
AWG2
AWG4
AWG6
AWG8
AWG10
AWG12
AWG14
AWG16
AWG1
AWG3
AWG5
AWG7
AWG9
AWG11
AWG13
AWG15
XFP –ZRlambda4
XFP –ZRlambda2
XFP –ZRlambda8
XFP –ZRlambda6
XFP –ZRlambda12
XFP –ZRlambda10
XFP –ZRlambda16
XFP –ZRlambda14
XFP
XFP
XFP
XFP
XFP
XFP
XFP
XFP
PIC
PIC
PIC
PIC
PIC
PIC
PIC
PIC
REC
REC
REC
REC
REC
REC
REC
REC
Monitor Power Power Monito
r Power PowerMoni.(Ethernet)
AOS OFS
18
XFP
OFL (Opical Fiber Link) NAOJ/Elecs corp. High Cost performance “Error Free” is confirmed
EHT / ALMA Phasing
optical attenuator
Expected Attenuation between AOS and OFSOFL at Haystack
OFLs for AOS and OSF
Introduction of Octave and Octave family
Application of OCTAVE technology to EHT/WDM
Summary
backup
Jitter measurement
Synchronized SG input Phase are extracted by FFT
SG CLKDIST
AD storageinputGOD SG
22
・・・FFT FFT FFT
Phase fluctuations 18.424GHz
14.328GHz
10.232GHz
6.136GHz
2.040GHz
Time (sec)
Phase rms and jitter Linear fitting
Φrms=2πf δT+σ
JitterδT 0.17psec
Allan standard deviation
VSOP- 2 SPEC.ASD 9E-13@1sec( WPM - 45GHz Lc 1% )