南極高地からの高解像度テラヘルツ天体観測
High Angular Resolution
Terahertz Astronomy from Dome A

Hiroshi Matsuo (ATC/NAOJ)

THz Observation
High Angular Resolution
THz Atmosphere
Intensity Interferometry

The Most Distant z=9.11
Spectroscopic Identification
with [OIII] 88 mm

Hashimoto et al., Nature (2018)

Structure of an AGN
1-10 arcsec~0.01 arcsec~0.001 arcsec
Angular Scales for 16 Mpc
Such as NGC1068~0.1 arcsec

Urry and Padovani (1995)

FIR atomic fine structure lines
4.745THz
2.060THz

Critical Densities
5.0×105 cm-3
1.5×105 cm-3

5.786THz
3.393THz

3.4×103 cm-3
5.0×102 cm-3

2.461THz
1.460THz

2.8×102 cm-3
4.5×101 cm-3

5.229THz

3×103 cm-3

1.901THz

2.7×103 cm-3

⚫ OI

– 63.185mm– 145.54mm⚫ OIII

35.1eV– 51.815mm– 88.356mm⚫ NII 14.5eV– 121.80mm– 205.30mm⚫ NIII 29.6eV– 57.330mm⚫ CII 11.3eV– 157.68mm

FIR atomic fine structure lines
4.745THz
2.060THz

Critical Densities
5.0×105 cm-3
1.5×105 cm-3

5.786THz
3.393THz

3.4×103 cm-3
5.0×102 cm-3

2.461THz
1.460THz

2.8×102 cm-3
4.5×101 cm-35.229THz

3×103 cm-3

1.901THz

2.7×103 cm-3

⚫ OI– 63.185mm– 145.54mm⚫ OIII35.1eV– 51.815mm– 88.356mm⚫ NII 14.5eV– 121.80mm– 205.30mm⚫ NIII 29.6eV– 57.330mm⚫ CII 11.3eV– 157.68mm

Atmospheric Windows from Atacama（alt. 4800m）
1mm

500um

300um

200um
z = 9.11

Matsushita, Matsuo et al. PASJ (1999)OIII 88um

AST/ROSPIFI

Fabry-Perot
Spectrometer5x5 bolometer
array
From the submillimeter astronomy group, Cornell University

[NII] 205 mm from South Pole
Atmospheric Transmission
only 3-6 %Obserst et al. (2011)

FTS in Dome A, Antarctica

Terahertz and far-infrared windows
opened at Dome A in Antarctica

Shi et al.
Nature Astronomy (2016)

6 THz

9 THz

12THz

Zenith Transmittance

Annual and winter (AprilSeptember) transmittancespectra measured at Dome A
during 2010-11.

3 THz

Zenith Transmittance

0 THz

1 THz

2 THz

3 THz

15THz

The Most Transparent Atmosphere
Ice Feature at 7 THz[NII]
1.5 THz[OIII]
5.8 THz[OIII]
3.4 THz

August 9th 12-18h UTC, 2010
Matsuo et al. APS (2019)

Windows for [NII], [OIII] andIce Feature

August 9th 12-18h UTC, 2010
Matsuo et al. APS in pressTransmission at 4 windows

Cumulative Analysis (Apr.-Sep.)

Can we observe [OIII] 88 mmat 3.393 THz ?

in July - August, 2010
Matsuo et al. APS in press

The Most Transparent Atmosphere
Ice Feature at 7 THz[NII]
1.5 THz[OIII]
5.8 THz[OIII]
3.4 THz

August 9th 12-18h UTC, 2010
Matsuo et al. APS (2019)

Water ice feature of HD142527 by ISO

Malfait et al. (1999)

Structure of a protoplanetary disk
Dullemond and Monnier (2010)

Scales are for Taurus and Auriga region

Heterodyne or Intensity ?
⚫ Start with heterodyne interferometry– Shorter baselines, [NII]⚫ Challenge with intensity interferometry– Longer baselines, [OIII] and water ice feature[OIII] 88mm

Water ice feature

Hashimoto et al. (2018)

HD142527
Malfait et al. (1999)

ALMA (ESO/NAOJ/NRAO)

Narrabri Stellar Intensity Interferometer

Hanbury-Brown et al. (1974)
Diameter of 32 early-type stars
were measured.

Long Baseline
Interferometry

RecorderB > 1GHz

RecorderB > 1GHz

Calculate correlation and delay

Nobeyema Radioheliograph at 17 GHz
Antenna Temperature T A* [K]Amplitude
Correlation

IntensityCorrelation

System Temperature Tsys [K]delay

Correlation amplitude

Ezawa, Matsuo et al. (2015)

Frequency  [Hz]Bandwidth  [Hz]Tsys11t = * [s]
T A   
 = 2t [rad]Experiment at 17 GHzwith Nobeyama Radioheligraph⚫ Real Part– (Intensity Correlation)0.5⚫ Imaginary Part– Δφ = 2 π ν Δt
Van Cittert
ZernikeRequirements to Detectors⚫ Sensitive to THz photons– Photon energy ~10-21 Joule⚫ Fast response– 1 GHz bandwidth for 100 M photons/s⚫ NEP(Noise Equivalent Power)

10-21 × (1 GHz)0.5~ 10-17 W/Hz0.5

NEP for photon counting
NEP = hΤ 𝜏vs. time resolution
Matsuo and Ezawa, JLTP (2016)

/ = 3Our Target
SPICASIS Photon Detectorse
S = 
[A/W]h
N = 2eI 0 [A/ Hz ]h

2I 0NEP =[W/ Hz ]e

Photon Assisted Tunneling
Ih/eV

NEP  3  10 −18 W/ Hzfor I 0 = 1 pA  = 0.5
at 650 GHz2/eDesign Parameters⚫ Nb-SIS 33 mm2 with Jc= 300 A/cm2⚫ Rn ~ 100 W– wRnCj ~ 150 at 500 GHz–  ~ 3 GHz⚫ Parallel Connected Twin Junction⚫ Twin-slot antenna and 50 W CPW⚫ Readout using low gate leakage transistors– GaAs-JFETs

Antenna, CPW, PCTJ, Choke

An antenna-coupled Nb-SIS
photon detector at 500 GHz
fabricated in CRAVITYPCTJ designed with SISMA
Shan et al. IRMMW-THz2018

Experimental Setup Plan
Input Optics

SIS-PC

Recorder

0.8K Fridge

CryogenicElectronics
4K Cooler

Thermal Source

Interferometry from Antarctica
South Pole

Dome F

Dome A

Dome CUSGS image

30Dor region andR136300 Mo stars◆[OIII] 88mm isobserved widelydistributed around
R136
Contour: MIPS 24mm
Kawada et al. (2011)

Heterodyne or Intensity ?
⚫ Start with heterodyne interferometry– Shorter baselines, [NII]⚫ Challenge with intensity interferometry– Longer baselines, [OIII] and water ice feature[OIII] 88mm

Water ice feature

Hashimoto et al. (2018)

HD142527
Malfait et al. (1999)

ALMA (ESO/NAOJ/NRAO)

THz Observation
High Angular Resolution
THz Atmosphere
Intensity Interferometry