AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Development of
NRO 3mm VLBI system

Toward EA 3mm VLBI Network
K. Niinuma (Yamaguchi U.)
M. Kino (Kogakuin U./NAOJ), K. Hada (NAOJ/VLBI)
S. Sawada-Satoh, R. Amari, T. Tsutsumi, T. Aoki (Yamaguchi U.)
H. Ogawa, A. Nishimura (Osaka Pref. U.), Y. Kono (NAOJ/VLBI)AndHINOTORI Project led by H. Imai (Kagoshima U.)
This work was supported by JSPS KAKENHI Grant Number 18H03721

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Contents
pMotivation
pDevelopment of Nobeyama 3mm (w/ Quasi-optics) VLBI
systempSummary and prospect (EA @ 86GHz)
pOther activities (higher frequency / lower frequency)

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Our observational exploration on M87
w/ KaVA-EAVN
pHada et al. 2017, PASJ

- The first KaVA-LP result

pPark et al. 2019, ApJ- Velocity field > ~100 Rs

pRo et al. in prep.

- Transverse structure

pCui et al. in prep.

- High cadence EAVN monitor

What’s next?

Park et al. (2019)

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Measuring velocity field:<100Rs – 10000Rs
by truly simultaneous observation

Park et al. (2019)

For direct comparison withthe result derived fromtheoretical works andnumerical simulations

How?

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

KVN/KaVA+Nobeyama (NRO45)
at 22/43/86GHz with quasi-optics
pHINOTORI (Hybrid Installation Project in Nobeyama, Tripleband Oriented) led by Imai-san (Kagoshima U.)- 22/43/86GHz simultaneous receiving system for VLBI
- Development of Quasi-optics, new VLBI backend

pScience targets of HINOTORI Project:- Jet acceleration mechanisms at the innermost AGN jet- Process of shock propagation and stellar wind acceleration incircumstellar envelopes proved by H2O and SiO masers- Mass accretion process inside the AGN molecular torus→Regular (Weekly/Monthly) monitor is required

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Nobeyama 45m Radio TelescopepRegular operation (common-use):since 1982 (start construction in 1980)- Mainly for single-dish use

pOne of the largest telescopes at~100GHz in the EA
pAlso powerful telescope for mmVLBI- Quasi-optics and wide-band VLBI
Backend are preparedAGN JET WS@Tohoku Univ., 2020 Jan 20-22

Quasi-Optics (22/43/86GHz) / Receivers
pFilter 2 and 3: Developed!
pReceivers: K/Q/W- K/Q band (circular pol.) simultaneousreceiving system via Filter 3 iscompleted and under thecommissioning to open for common
use in next season- TZ100 (SIS-HEMT) receiver for Wband• Decommissioned for the purpose of
single-dish-use at NRO45 in 2017

Fixed mirror

NRO 45 m
first generation
beam
transmission
block

䐠

3mm
13mm(TZ)(H22)
LCP/RCPLCP/RCP→VLP/HLP(?)

Chopper wheelfor power calibratoin

䐟 High band-pass filter
HPFs 䐠 and 䐡
developped䐡

in FY2016 ―2017

7mm7mm(Z45)(H40)
VLP/HLPLCP/RCP→Z45 (???) →1䇷2mm (???)

VLBI use
HINOTORI quasi-optics

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

NRO 45m Receiver Roomon November 9-10, 2018
First generation optics system
in NRO 45 m telescope

D/C (V)

Z45

(V/H)

K/Q-banddichroic plate

D/C (H)

0.1―2.0 GHz

4―8GHzWidebandconverter

OCTAD(V1&V2)(FY2017
commissioned)

H40(R/L)

mirrorD/C (L)D/C (R)

5―7GHz#9#7

H22(R/L)#8KQ/W-band
dichroicplate
1/4λ plate(in VLBI only)

D/C (L)D/C (R)

5―7GHz3➡5➡6 IFs
2 GHz/IF
12➡16➡24BBCs

ADS3000+
Reference
distributer
VDIF
10GbE
format switch
BEARS E/O-O/E
for H22 L/R
H40 L(/R), Z45 V/H
TZ LSB R/L (or V/H)

IF selector

4―8GHzNew IFsystemV/H→R/L PC(PolariH)
OCTADISK

Data storage

OCTADISK2Coaxis IFswitch

TZ
(V/H)

OCTAVIA2SAM45

Data server(single dishpolarimetry)

Down convert to

2―4 GHz(2.2―3.8 GHz)LSB (V)

10 MHz
1 PPS

USB (V)HINOTORI
FY2018-2019

Present pathwill be replaced
Present pathdefinitely developed

LSB (H)
USB (H)

H-maser

Reference distributer

Future plan
In feasibility checkfor development

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Quasi-Optics (22/43/86GHz) / Receivers
pTZ100 (3mm) receiver for QO- Development of receiver control system
ü Done (by Aug 2019)- Re-installed in NRO45 for VLBI-use
ü Done (the end of Aug 2019)

Fixed mirror

NRO 45 m
first generation
beamtransmission
block䐠

Chopper wheel
for power calibratoin

䐟 High band-pass filter
HPFs 䐠 and 䐡
developped䐡

in FY2016 ―2017- First light: simultaneous 3-bands obs.
ü Done (Nov 2019, single dish)- Adjustment/Measurement of beam-squint,
beam-pattern, efficiency
ü Done (Dec 2019)by Amari-san, Tsutsumi-san, Sawada-Satoh-san, Aoki-san, Nishimurasan, Ogawa-san, and OPU-students

3mm13mm(TZ)(H22)
LCP/RCPLCP/RCP→VLP/HLP(?)

7mm7mm(Z45)(H40)
VLP/HLPLCP/RCP→Z45 (???) →1䇷2mm (???)

VLBI use
HINOTORI quasi-opticsAGN JET WS@Tohoku Univ., 2020 Jan 20-22

First light with QO (22/43/86 GHz)

NRO staffs (especially, Miyazawa-san, Torii-san, Kaneko-san) gave us huge supports!

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Beam-Squint / Beam pattern

Tsys_3mm (H) = 250K
Tsys_3mm (V) = 450K
Tsys_7mm (L) = 170K

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Beam-Squint / Beam pattern
Our measurement in 2019 Dec

36 arcsec

1st null

Tsys_3mm (H) = 250K
Tsys_3mm (V) = 420K
HPBW3mm ~ 18.5”

Status report in 2016 (before decommission)

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

VLBI Backend
pΔB = 2GHz x 6 IFs INPUT at maximum are availableüSamplers: total of 6 IFs input are now available• OCTAD-V1 (input: 8Gsps x 3 IFs, DBBC): ready• OCTAD-V2 (input: 16Gsps x 3 IFs, DBBC): ready (installed on Aug 2019)üRecorder• OCTADISK2 (32Gbps recording): ready (installed on Aug 2019)• Two 8Gbps recorders have already been installed (by HINOTORI/NAOJ)-> Total of 48Gbps recording※Because of the rack of disk packages, OCTADISK2 can record with 16 Gbps atmaximum now (i.e., total of 32Gbps recording)AGN JET WS@Tohoku Univ., 2020 Jan 20-22

A few concerns
pNot yet- Measurement of Image Rejection Ratio (after re-installed)- Tuning bias for SIS/HEMT to reduce Tsys
• There is a room to improve Tsys of both H/V (Tsys of 150 – 300 K are described inNakajima et al. 2013)• The value of V is almost double of the one of H
※ Current SEFD (H-pol) ~ 1000 Jy (with Tsys of ~ 250K)

pImprovement of some scripts for setting obs. mode automatically- Preparing by Imai-san- It is possible to set manually (ready)AGN JET WS@Tohoku Univ., 2020 Jan 20-22

3mm-VLBI commissioning will start
p1st VLBI test with QO (22/43/86GHz) & new VLBI backend
system will be performed on Jan 27 together with KVN(Thanks Jung-san, Byun-san, and KASI colleagues !)Stay tunes!

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

KVN/KaVA+NRO45

with Quasi-Optics (@22/43/86GHz )Measuring velocity field of AGN jet with QO & new VLBI-BE

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Merits of K/Q/W truly simultaneous obs.
w/ quasi-optics
pVLBI observation time with NRO45 is quite limited, i.e.,~72hrs-cap per year from this season- “Quasi-optics” + “simultaneous recording” significantly save time-> Regular VLBI monitor at 22 – 86 GHz

pVariability matters at a jet base. Assumptions are needed.
- “Quasi-optics” + “simultaneous recording” does not require suchassumptions.

pCalibration / Source Frequency Phase Reference technique

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

GMVA@3mm Antenna Sensitivities
GMVA status report

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Sensitivity: KVN/KaVA + NRO45
SEFD (Jy)

KVN

VERA

NRO45

23 GHz1300 (L/R)

2300 (L/R)

280 (L/R)

43 GHz2000 (L/R)

4800 (L/R)

490 (L)86 GHz3200 (L/R)-~1000 (H/V)

VLBA

GBT

3000 - 6000 (L/R)~130 (???)(NRAO status report)

Baseline Sens. (mJy @ 1σ)

KaVA

KVN+NRO45

KaVA+NRO45

23 GHzw 2Gbps, 2min

4-7-

2-7

43 GHzw 2Gbps, 1min

6 - 16-5 - 1686 GHzw 2Gbps, 0.5min

-12-

VLBA

VLBA+GBT

23 - 38

5-6

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Array: KVN + NRO45@86 GHz
uv-coverage by KVN+NRO45
Red: KVN onlyBlack and red: KVN+NRO45

Baseline length will be 3 times longer than KVN along M87 jet direction!

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

M87 jet with KVN+NRO45@86GHz

M87 with VLBA+GBT@86GHz(Hada+16)~ 30mJy/bの成分

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

M87 jet with KVN+NRO45@86GHz
pM87 observation with KVN+NRO45@86GHz- Allowing us to measure the jet motion from <100 Rs
M87 with VLBA+GBT@86GHz(Hada+16)
Restored with KVN+NRO beamnAvailability of regular monitor- KVN/KaVA: 10 months operation / year
- NRO: 6 months operation / year

nNRO45 provides us- Higher baseline sensitivity@86GH: ~10mJy@1sigma- Higher angular resolution@86GHz: < 0.4 mas along
the jet direction
Dynamic range > 300
20mJy component＠10σ• Corresponding to projected distance of ~60 Rs (or deprojected distance of ~90 Rs）

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Measuring velocity field:<100Rs – 10000Rsby truly simultaneous observation
Park et al. (2019)
Covered byKVN+NRO4586 GHz
Covered by
KaVA 43 GHz

Covered by
KaVA 22 GHz

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Summary and Future prospect
pCurrent situation of NRO45- QO: (almost) Ready- 86GHz VLBI: (almost) Ready for commissioning

pKVN/KaVA+NRO45 with QO- e.g., “truly” simultaneous & regular monitor will be available with <1mas-> measuring accurate v-field from <102 to 104 Rs

pKVN+NRO45@86GHz -> EAVN@86GHz- Transparency: upstream of the jet- Availability of regular monitor (e.g., bi-weekly or less)- Angular resolution (<0.4 mas): EAVN (including Urumqi) @43GHz / EATINGVLBI@22GHz

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

East Asia 3mm-VLBI Network
The Greenland Telescope(ASIAA, Taiwan)

JCMT, Hawaii (EAO)

NRO 45m, Japan

Korean VLBI Network

Based on Taehyun’s Talk
• Sejong, SRAO, QTTAGN JET WS@Tohoku Univ., 2020 Jan 20-22

Array: GLT/JCMT + NRO45@86 GHz
SEFD (Jy)

KVN

VERA

NRO45

23 GHz1300 (L/R)

2300 (L/R)

280 (L/R)

43 GHz2000 (L/R)

4800 (L/R)

490 (L)86 GHz3200 (L/R)-~1000 (H/V)

VLBA

JCMT/GLT

3000 - 6000 (L/R)

3600 (L/R ?)Baseline Sens. (mJy @ 1σ)

KaVA

KVN+NRO45

KaVA+NRO4523 GHz
w 2Gbps, 2min

4-7-2-743 GHz
w 2Gbps, 1min

6 - 16-5 - 1686 GHzw 2Gbps, 0.5min

-12-

VLBA

NRO+GLT
NRO+JCMT

23 - 38

12AGN JET WS@Tohoku Univ., 2020 Jan 20-22

East Asia 3mm-VLBI Network
The Greenland Telescope(ASIAA, Taiwan)

JCMT, Hawaii (EAO)

VLBA+GBT (Hada+16)

NRO 45m, Japan

Korean VLBI Network

FWHM ~ 0.1mas

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Measuring velocity field:~30Rs – 10000Rs
by future EAVN@3mm monitor
Park et al. (2019)
Covered by
KVN+NRO4586 GHz
Covered by
KaVA 43 GHz

Covered by
KaVA 22 GHz
Covered by
EAVN 86 GHz

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Other sources ?

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

East Asia 3mm-VLBI Network
The Greenland Telescope(ASIAA, Taiwan)

JCMT, Hawaii (EAO)
Mrk 421 (δ=38deg)

NRO 45m, Japan

Korean VLBI Network

FWHM < 0.1mas

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

e.g. Blazar Markarian 421
pThe first Very High Energy (TeV) - gamma detection
pThe most nearby TeV-blazar (z = 0.031)- Best source to investigate HE emitting region by VLBI

• 0.1 mas = 0.062 pc = 1770 Rs (de-projected, MBH ~ 3.6 x 108 Msolar, Wagner 2008)- Detailed longitudinal/transversal structure from 1000 Rs• Velocity field / Collimation profile of blazar (Nakamura-san’s talk)• Broad Line RegionpNo (or few?) sub-pc scale 3mm (or shorter-λ) VLBI images- Expected 3mm peak flux in sub-pc scale is ~ 100mJy/b or less

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Other activities:
1. Lower frequency

2. Higher frequency (EAVN-Hi(1mm))

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Activity 1: low-frequency partpWe operates two large radio telescopes- Yamaguchi Univ. operates 32m and 34m at 6/8 GHz- Recently operation as interferometer was started (good sensitivity):
Yamaguchi Interferometer (YI)

pDevelopment of “On the Fly mapping by interferometer(OtFI)” method toward SKA era- Aiming for establishing the technique and conducting un-biased survey fora region of 5deg2 < a day• Time-domain studies (radio follow-up of huge error circle of GW or ν events)• Regular monitor of the large number of sources showing high-energy flare• Survey for radio transients or variable objects• Survey for new radio sources without dependence on existing catalog.

Yamaguchi Interferometer (YI)
Observing Band

6 GHz / 512 MHz
8 GHz / 512 MHz

Baseline

110 m (32m&34m)

Beam size

6 GHz: 1’.4
8 GHz: 1’.1

Data rate

2 Gbps/Antenna

Integration time

1 hours

1σ sensitivity

0.15 mJy

Observing Time3000 hours/yr

YI is used for...
Daily monitoring of compact object/AGN/YSO

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

Un-biased survey by OtFI~1arcmin

5 deg2< 1 day

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

East Asia 1mm-VLBI Experiment

Overview of EAVN-Hi activity
The Greenland Telescope(ASIAA, Taiwan)

Observing schedule madeby Lu, Hada, Asada

SRAO (SNU, Korea)

SPART (OPU, Japan)

AGN JET WS@Tohoku Univ., 2020 Jan 20-22

EAVN@1mm VLBI Experience
CO(J2-1), DR21

led by Aoki-san (Japan-side)

Unfortunately, no fringe, but good experience
for us
The first experiences for most of Japanesecolleagues participating to set up VLBI systemand to perform observation for 1mm-VLBI