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
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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
Slide2OCTAVE ArrayOCTAVE FamilyEHT application
Contents
Slide3eVLBI
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
Slide4Supplied 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.
Slide5X-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.
Slide6Image 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
Slide7Recording 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
Slide8We 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).
Slide9Converter 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
Slide10DISK 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)
Slide11OCTADISK2 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”
Slide12NAOJ 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
Slide13Real 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)
Slide14Direct 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)
Slide15Lab. 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)
Slide16We add two functions DBBCBackward compatibilityBW:16MHz~2048MHz/
ch
External
AD module up to 50GHz
V-connector
Direct receivingUpgraded OCTAD
50GHzModule
Slide17Event 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)
Slide18EHT / 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
Slide19OFL (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
Slide20Introduction of Octave and Octave familyApplication of OCTAVE technology to EHT/WDM
Summary
Slide21backup
Slide22Jitter measurement
Synchronized SG input
Phase are extracted by FFT
SG
CLK
DIST
AD
storage
input
GOD
SG
22
・・・
FFT
FFT
FFT
Slide23Phase fluctuations
18.424GHz
14.328GHz
10.232GHz
6.136GHz
2.040GHz
Time (sec)
Slide24Phase
rms
and jitter
Linear fitting
Φ
rms
=2πf
δT+σJitterδT 0.17psec
Slide25Allan standard deviation
VSOP- 2 SPEC.
ASD 9E-13@1sec
(
WPM
-
45GHz
Lc
1% )