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Current status of OCTAVE Current status of OCTAVE

Current status of OCTAVE - PowerPoint Presentation

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Current status of OCTAVE - PPT Presentation

Yusuke Kono 1 Tomoaki Oyama 1 Noriyuki Kawaguchi 1 Kotaro Niinuma 2 Kenta Fujisawa 2 Hiroshi Takaba 3 Kazuhiro Sorai 4 Mamoru Sekido 5 Shinobu Kurihara 6 Yasuhiro Murata ID: 799789

octave xfp rec naoj xfp octave naoj rec pic network vlbi octavia test octadisk oyama correlator observation nict aos

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Slide1

Current status of OCTAVE

Yusuke Kono

1

,

Tomoaki

Oyama

1

, Noriyuki Kawaguchi

1

, Kotaro Niinuma

2

,

Kenta Fujisawa

2

, Hiroshi Takaba

3

, Kazuhiro Sorai

4

, Mamoru Sekido

5

,

Shinobu

Kurihara

6

, Yasuhiro Murata

7

National Astronomical Observatory of Japan

1

,

Yamaguchi university

2

,Gifu university

3

, Hokkaido university

4

NICT

5

, GSI

6

, JAXA

7

Slide2

OCTAVE ArrayOCTAVE FamilyEHT application

Contents

Slide3

eVLBI

network in Japan

High sensitivity, on-the-fly result and

low cost operation

OCTAVE :

Optically

ConnecTed

Array for Vlbi Exploration

Hokkaido univ.

11m

NICT

Kashima 34m*

GSI Tsukuba

32m

Gifu univ.

11m

Yamaguchi univ.

32m

JAXA

Usuda

64m*

NAOJNRO 45m*

Ibaraki Univ.*32m x 2

The longest baseline is 1,300km

Slide4

Supplied by academic network

(SINET4)

and Test

bed

network

(JGN-X)

10GbE to nodes2x10GbE to Correlator at HQ of NAOJ in TokyoKashima and Ibaraki are offline now. Trying to connect.

Usuda and NRO are offline nowCommunication lines

Network configuration (Plan)

Local Recorders, OCTADISK and K5,

are installed into Usuda, NRO, Ibaraki and Tomakomai for a while.

Slide5

X-bandUsuda64, Kashima34*, Yamaguchi32, Ibaraki328192-8704MHz, 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.

Slide6

Image of 4C32.44X-band, BW512 MHz, 4stationssoftware: 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.,2013Science Obs. proposals are selected and operated by JVN(Japanese VLBI Network)Data processing and results

Slide7

Recording and copying function at NAOJ/TokyoFringe 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

Slide8

We have developed several instruments for OCTAVE. We call them Octave family.

OCTAVIA

OCTAVe

optIcal

Adapter

OCTADISK

OCTAve RecorderOCTACOR

OCTAve Correlator

OCTADOCTave

ADc

OCTADIVOCTAve

DIVider

Octave family

Many non-OCTAVE family instruments are also used in the array,

such as ASD1000/3000, K5(NICT

) and Mark5B(Haystack).

Slide9

Converter between VSI and 10GbEElectrical I/OVSI-H 4 Ports Total 8

Gbps

Optical I/O

10GbE

Protocol

VDIF/UDP/IP/10GbE

OCTAVIA (OCTAVe optIcal

Adapter)Work by Dr Oyama (NAOJ)

VSI

OCTAVIA

10GbE

ADC etc

Network

etc

Slide10

DISK RecorderI/O10GbE (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)

Slide11

OCTADISK2 is under developmentParts discontinuance of OCTADISKCOTS 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”

Slide12

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 Input

from various

terminals

Storage

on HDD

output

Synchronized

data to VCS

Slide13

Real time correlatorFPGA correlator

FX and XF type

2Gbps/station

Post processing

correlator

Software

correlatorEngine(GICO3) by NICTIntegration by NAOJ with NICT

Correlators for OCTAVESoft Correlators

Hard CorrelatorsWork by Dr Oyama

(NAOJ)

Slide14

Direct RF sampling22GHz (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)

Slide15

Lab. test of sampling jitter

0.17

psec

(

Lc

<

1% @43GHz)Fringe test observation Mizusawa 10m x 20m BL=60m

16Gbps x 2 OCTADOCTAD

Jitter

 0.17psecLc <1%

15

PI: Dr Oyama (NAOJ)

Slide16

We add two functions DBBCBackward compatibilityBW:16MHz~2048MHz/

ch

External

AD module up to 50GHz

V-connector

Direct receivingUpgraded OCTAD

50GHzModule

Slide17

Event Horizon TelescopeJapanese contributionData 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)

Slide18

EHT / ALMA Phasing

WDM

of 16 wavelengths by 10GbE-ZR

XFP

XFP

–ZR

lambda3

AWG2

XFP

XFP

XFP

XFP

XFP

XFP

XFP

XFP

–ZR

lambda1

XFP

–ZR

lambda7

XFP –ZRlambda5

XFP –ZRlambda11

XFP –ZRlambda9

XFP

–ZR

lambda15

XFP

–ZR

lambda13

AWG4

AWG6

AWG8

AWG10

AWG12

AWG14

AWG16

AWG

1

AWG3

AWG5

AWG7

AWG9

AWG11

AWG13

AWG15

AWG2

AWG4

AWG6

AWG8

AWG10

AWG12

AWG14

AWG16

AWG

1

AWG3

AWG5

AWG7

AWG9

AWG11

AWG13

AWG15

XFP

–ZR

lambda4

XFP

–ZR

lambda2

XFP

–ZR

lambda8

XFP

–ZR

lambda6

XFP

–ZR

lambda12

XFP

–ZR

lambda10

XFP

–ZR

lambda16

XFP

–ZR

lambda14

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

Monitor

Power

Power

Moni

.

(Ethernet)

AOS

OFS

18

XFP

Slide19

OFL (Opical Fiber Link) NAOJ/

Elecs

corp.

High Cost performance

“Error Free” is

confirmed

EHT / ALMA Phasing

optical attenuator

Expected

Attenuation between AOS and OFS

OFL at Haystack

OFLs for AOS and OSF

Slide20

Introduction of Octave and Octave familyApplication of OCTAVE technology to EHT/WDM

Summary

Slide21

backup

Slide22

Jitter measurement

Synchronized SG input

Phase are extracted by FFT

SG

CLK

DIST

AD

storage

input

GOD

SG

22

・・・

FFT

FFT

FFT

Slide23

Phase fluctuations

18.424GHz

14.328GHz

10.232GHz

6.136GHz

2.040GHz

Time (sec)

Slide24

Phase

rms

and jitter

Linear fitting

Φ

rms

=2πf

δT+σJitterδT 0.17psec

Slide25

Allan standard deviation

VSOP- 2 SPEC.

ASD 9E-13@1sec

WPM

45GHz

Lc

1% )