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% ）