HINOTORI(Hybrid Installation project in Nobeyama, Triple-band Oriented)

SiO masers around
WX Psc(Yun et al. 2016)

Hiroshi Imai

Research and Education Assembly Science and Engineering Area,
International Radio Astronomy Collaboration Promotion Office
Kagoshima University

MEXT KAKENHI Category A project (FY2016—2019)
NRO 45 m system upgrade (VLBI, quasi-optics)• HINOTORI (“phoenix” in Japanese)(Hybrid Installation program in Nobeyama, Triple-band Oriented)
Scientific operation in FY2019
Combined with NAOJ Development Program (P.I. T. Manabe)

KaVA Large Programs on Circumstellar Masers• ESTEMA (“family tree” in Spanish)(Expanded Study on Stellar Masers)
Snapshot VLBI images of 80 evolved stars in masers during 2015—2016• KaVA decadal monitoring observations of stellar masers
Intensive monitoring during 2017—2025(?)

HINOTORI team Kagoshima University
H. Imai※, H. Shinnaga, S. Sawada-Satoh†, A. Nakagawa,K. Mizukubo, T. Handa +α Osaka Prefecture University
H. Ogawa, K. Kimura, T. Manabe, M. Chiba, Y. Nanbu,
Y. Hasegawa, +β NAOJ Mizusawa VLBI Observatory
T. Oyama, Y. Kono, N. Sakai, T. Hirota, Y. Tamura,
K.M. Shibata, M. Honma
Headquarters
 NAOJ Nobeyama Radio Observatory
Quasi-optics
T. Minamidani, M. Saito +γVLBI
 Yamaguchi UniversityPolarization
K. Fujisawa, K. Niinuma, N. Matsumoto +δ
VLBI data analysis
 Ibaraki UniversityGeodesy
Y. Yonekura NAOJ ALMA/radio
Y. Asaki, S. Kameno, H. Kobayashi, M. Miyoshi※Project P.I. †From 2016 October 1

Multiple radio-bands observing systemⒸKASI

KVN quasi-optics for multi-band receiving system

 Source-frequency phase-referencing (SFPR) technique with KVN(Dodson et al. 2014; Rioja et al. 2014)

 Band-to-band calibration in ALMA Quasi-optics installed in KVN, Yebes (in plan), Tianma (in plan) Quasi-optics (K/Q) installed in VERA temporarily (in Mizusawa, Iriki)

Triple-band VLBI (KaVA @22GHz+KVN @22/43/86GHz)
Red supergiant
S Per(Asaki et al. in prep.)
Band-to-band transferof phase calibration
solutions

Confidential

Continuous tracing ofmass loss flows ofdying stars
Episodic mass ejection
on decade scale?
H2O (22GHz) SiO J=10 v=1 (43GHz) SiO J=10 v=2 (43GHz)
SiO J=21 (86GHz, one KVN baseline)

Groves of maser lines (22, 43, 86 GHz bands) H2O masers(22.2 GHz) SiO masers

v=(0,) 1,2,3 J=10(42.5—43.5 GHz)
V=1, (2,) 3 J=21(85.0—86.3 GHz)

 NH3 masers(22.6—23.7 GHz)

 CH3OH masers(23.1, 23.4, 44.1, 84.5,88.9 GHz) HCN masers(88.6 GHz)

Molecular and atomic absorptions towards AGNs
 Many lines

 HCO+ (89.2 GHz) HCN (88.6 GHz) SiO (86.9 GHz)
 CH3OH (84.5 GHz)

 C2H (87.3 GHz) RRLs (Radio recombination lines) Tracing 1—10 pc molecular

torus around AGNs
(c.f. HI on ~100 pc)
12C-bared line 13C-beard line (x30)

Toward J1717-337 with ALMA
(Ando et al. 2015)

 Detecting high-Vabsorptions(Δv~1000 km/s → Δf~300 MHz) Foreground

Milky Way absorptions

c.f. HCN absorption towards NGC1052(Sawada-Satoh et al. in prep.) Tracing tiny clumps (<100 AU)~1000 km baselines are ideal

New multi-band quasi-optics in NRO 45 m telescope Multiple beamtransfer systemwith reflection
mirrors (#1—5)
from theNasmyth focus

 VLBI with one oftwo beam blocks

#5

#3&4

Malti-band quasi optics @NRO 45m
telescopeReplacing

mirrors intoband selectionfilters
Using existingreceivers H22@22GHz
 H40@43GHz

Moving/reusing

decommissioned
receiver(TZ: 84—116 GHz)

1—2mm bandin the future(?)

Frequency selection filter
in JCSA (Jerusalem Cross Slot Array)First experiment in NRO(Irimajiri & Takano 1991)

Difficulty in structure strength
for the large filter (φ~60 cm)
and band width expansion
Multilayer filter inetching pattern printing(Manabe & Ogawa)1.784 mm for 86GHz
3.567 mm for 43 GHz
8.963 mm for 22 GHz

Manabe et al. 2014

Simulated characteristics of JCSA(Band pass in 82.7—89.3 GHz )Best scientificselection in84—93 GHz

For vertical/horizontal linear polarization

Manabe & Ogawa 2015

Other filter designs (Q-band, ongoing) 1/2

Design 1

Design 2

42—45.5 GHz

41—47 GHz

Other filter designs (Q-band, ongoing) 2/2

Design 3

Design 4

13

Multiple layers
may be necessary.

Challenging issues

 Physically strong

frames and filters

 Sufficiently widefilter band width

Mirror/filter setting(frame thickness: ~1cm)

Frames, a reflection ,and a JCSA filter(Irimajiri & Takano 1995) in the NRO 45m telescope

Deformedby 1 mm
⬇️Stronger framefor operation
as a slit!

Photo on2015
November27

Filter measurement system@Osaka Prefecture University

まとめ

Port_2
Reflection
反射系測定

measurement

Absorber
電波吸収体

Tested band pass filter

200062

DUT(周波数選択膜)

SignalPort_1

generator

Transparency
Port_3measurement
透過系測定

Design of the new NRO signal transmission system
HINOTORI version on 2016 July 12

Band/polarization selection

512 MHz x 4ch /IF(final)
IF selector
should be delivered.

Toward East Asian high sensitivity mm-VLBI• FY2016
New VLBI
backend@NRO• FY2017
QO (K/Q-band)commissioning
KaVA/NROframework• FY2018
QO (K/Q/W-band)commissioning
EAVN fremework• FY2019
Regular operation

Tianma65 m(K/Q)