Current status of OCTAVE Yusuke Kono 1 Tomoaki

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

Contents ¥ OCTAVE Array ¥ OCTAVE Family ¥ EHT application

OCTAVE : Optically Connec. Ted Array for Vlbi Exploration ¥ ¥ e. VLBI network in Japan High sensitivity, on-the-fly result and low cost operation on el ge Th Yamaguchi univ. 32 m km ei n eli as b st 00 3 , s 1 Hokkaido univ. 11 m JAXA Usuda 64 m* NAOJ NRO 45 m* Gifu univ. 11 m GSI Tsukuba 32 m Ibaraki Univ. * 32 m x 2 NICT Kashima 34 m*

Communication lines ¥ Supplied by academic network (SINET 4) and Test bed network (JGN-X) ¥ ¥ 10 Gb. E to nodes 2 x 10 Gb. E to Correlator at HQ of NAOJ in Tokyo Kashima and Ibaraki are offline now. Trying to connect. Usuda and NRO are offline now Network configuration (Plan) Local Recorders, OCTADISK and K 5, are installed into Usuda, NRO, Ibaraki and Tomakomai for a while.

Observation capability ¥ X-band Usuda 64, Kashima 34*, Yamaguchi 32, Ibaraki 32 ¥ 8192 -8704 MHz, BW 512 MHz x 1/2 pols ¥ ¥ K-band NRO 45, Kashima 34*, Yamaguchi, Ibaraki 32, Gifu 11, Tomakomai 11 m ¥ 21. 5 -23. 8 GHz, BW 512 MHz x 1/2 pols ¥ Kashima 34* will be available if the network is connect

Data processing and results ¥ Image of 4 C 32. 44 ¥ ¥ ¥ X-band, BW 512 MHz, 4 stations 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 Unassociated Gamma-ray Sources, Niinuma et al. , 2013 ¥ Science Obs. proposals are selected and operated by JVN(Japanese VLBI Network)

International Observation ¥ Recording and copying function at NAOJ/Tokyo ¥ Fringe test with EAVN (East Asia VLBI Network) ¥ ¥ September 2013, 14 stations Fringe test with Noto ¥ K 5 (Ni. CT) April 2013 Mark 5 B+ (Haystack) OCTADISK (NAOJ) DF

Octave family ¥ ¥ ¥ We have developed several instruments for OCTAVE. We call them Octave family. OCTAVIA ¥ OCTAVe opt. Ical Adapter ¥ OCTAve Recorder ¥ OCTAve Correlator ¥ OCTave ADc ¥ OCTAve DIVider OCTADISK OCTACOR OCTADIV Many non-OCTAVE family instruments are also used in the array, such as ASD 1000/3000, K 5(NICT) and Mark 5 B(Haystack).

OCTAVIA (OCTAVe opt. Ical Adapter) ¥ Converter between VSI and 10 Gb. E ¥ Electrical I/O VSI-H 4 Ports ¥ Total 8 Gbps ADC etc ¥ ¥ Optical OCTAVIA 10 Gb Network E etc I/O 10 Gb. E ¥ Protocol ¥ ¥ VDIF/UDP/IP/10 Gb. E Work by Dr Oyama (NAOJ

OCTADISK ¥ Recorder I/O ¥ 10 Gb. E (up to 4 Gbps) ¥ ¥ Use with OCTAVIA Portable module 12 HDDs /module ¥ dedicated format. ¥ ¥ Under Operation at the VERA stations. Work by Dr Oyama (NAOJ

OCTADISK 2 ¥ OCTADISK 2 is under development Parts discontinuance of OCTADISK ¥ COTS base, except Chassis ¥ OS: Linux, Linux file system ¥ Portable module ¥ ¥ Prototype same to OCTADISK “Perfect COTS” Work by Mr Suzuki and Dr Oyama (NAOJ

OCTAVIA/DISK in KJCC ¥ NAOJ supplied Raw VLBI Data Buffer to KJCC VSI Input Storage from various on HDD terminals output Synchronize d data to VCS Origin of OCTAVIA and OCTADISK http: //kvn-web. kasi. re. kr/en/en_under_correlator. php

Correlators for OCTAVE ¥ Real ¥ time correlator FPGA correlator ¥ ¥ ¥ Post ¥ FX and XF type 2 Gbps/station processing correlator Software correlator Engine(GICO 3) by NICT ¥ Integration by NAOJ with NICT ¥ Work by Dr Oyama (NAOJ) Soft Correlators Hard Correlators

OCTAD (ADC) ¥ Direct ¥ 22 GHz (43 GHz, under test) ¥ Wide ¥ bandwidth 8. 192 Gsps-3 bit ¥ ¥ For ¥ RF sampling use with a RF band pass filter next generation VERA system Wideband observation enable us to use weaker and closer reference sources of d. VLBI astrometry

OCTAD ¥ Lab. test of sampling jitter ¥ ¥ 15 0. 17 psec (Lc<1% @43 GHz) Fringe test observation ¥ Mizusawa 10 m x 20 m BL=60 m ¥ 16 Gbps x 2 OCTAD Jitter　0. 17 psec Lc <1% PI: Dr Oyama (NAOJ)

Upgraded OCTAD ¥ We ¥ add two functions DBBC ¥ Backward compatibility ¥ ¥ BW: 16 MHz~2048 MHz/ch External AD module up to 50 GHz V-connector ¥ Direct receiving ¥ 50 GHz. Module

EHT / ALMA Phasing ¥ Event Horizon Telescope ¥ Japanese contribution ¥ Telescopes and Phasing Data transfer from AOS to OFS AOS: Telescope site ¥ OSF: Operations Support Facility ¥ 64 Gbps(8 Gbps x 8 ch) ¥ A single dark fiber ¥ Design started at 2011. ¥ PI: Prof. Honma (NAOJ) Optical link 30 km VLBI Recorder Storage Transfer and Correlati

EHT / ALMA Phasing XFP ¥ WDM of 16 wavelengths by 10 Gb. E-ZR OFS AOS PIC XFP –ZR lambda 1 PIC XFP –ZR lambda 3 PIC XFP –ZR lambda 5 PIC XFP –ZR lambda 7 PIC XFP –ZR lambda 9 PIC XFP –ZR lambda 11 PIC XFP –ZR lambda 13 PIC XFP –ZR lambda 15 Monitor 18 AWG 1 AWG 2 AWG 3 AWG 4 AWG 5 AWG 6 AWG 7 AWG 8 AWG 9 AWG 10 AWG 11 AWG 12 AWG 13 AWG 14 AWG 15 AWG 16 Power Monitor Moni. (Ethernet) XFP –ZR lambda 2 XFP REC XFP –ZR lambda 4 XFP REC XFP –ZR lambda 6 XFP REC XFP –ZR lambda 8 XFP REC XFP –ZR lambda 10 XFP REC XFP –ZR lambda 12 XFP REC XFP –ZR lambda 14 XFP REC XFP –ZR lambda 16 XFP REC Power

EHT / ALMA Phasing ¥ OFL (Opical Fiber Link) NAOJ/Elecs corp. ¥ High Cost performance ¥ “Error Free” is confirmed ¥ OFLs for AOS and OSF optical attenuator Expected Attenuation between AOS and OFS OFL at Haystack

Summary ¥ Introduction of Octave and Octave family ¥ Application of OCTAVE technology to EHT/WDM

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Jitter measurement GOD SG input SG AD storage CLK DIST ¥ Synchronized SG input ¥ Phase are extracted by FFT 22 FFT FFT ・・・

Phase fluctuations ¥ 18. 424 GHz ¥ 14. 328 GHz ¥ 10. 232 GHz ¥ 6. 136 GHz ¥ 2. 040 GHz Time (sec)

Phase rms and jitter ¥ Linear ¥ fitting Φrms=2πｆδT+σ ¥ JitterδT ¥ 0. 17 psec

Allan standard deviation VSOP- 2 SPEC. ASD 9 E-13@1 sec （WPM－45 GHz Lc 1% ）