2019.11.24 VLBI symposium @Otsuma women’s university

多波長 VLBI 観測によるクェーサー 3C 273 のジェット収束領域の特定

沖野 大貴 ( 東京大学 / 国立天文台 )共同研究者の方々秋山 和徳 (NRAO/MIT), 浅田 圭一 , 中村 雅徳 (ASIAA),
秦 和弘 , 本間 希樹 (NAOJ), Jose L. Gomes (IAA),
GMVA+ALMA 3C 273 Collaboration

2019.11.24 VLBI symposium @Otsuma women’s university

Open questions for AGN Jets
VLBA+GBT 86 GHz

M87
HST image

Event Horizon Telescope
230 GHz

1 kpc = 2*106 Rs

Hada et al. 2016
EHT Collaboration● Collimation● Acceleration● AGN feed backCredit:NASA and The Hubble Heritage
Team (STScI/AURA)

Shape of the Jets2019.11.24 VLBI symposium @Otsuma women’s university

Jet collimation profiles of LLAGNDistance from the BH (pc)

M87
Distance from the BH (Rg)

Nakamura et al. 2018

● Transition of the jet shape at 105-6 Rsfrom conical to parabolic● A universal property of AGN Jets?
(e.g., NGC4261(Nakahara+2018); Cygnus A (Boccardi+ 2016))

Kovalev et al. 2019

2019.11.24 VLBI symposium @Otsuma women’s university

LLAGN vs Quasar
Jets are confined by ...
● Geometrically thick disk
● Disk winds● Magnetic field
LLAGN● External medium(M87)

Quasar?
BH
Geometrically thickHot (T~109 K)?
BH

RIAFStandarddisk

Geometrically thin
Cool (T~106 K)

2019.11.24 VLBI symposium @Otsuma women’s university

Target source: quasar 3C 273● Relativistic jet● z = 0.158● MBH ~2.6×108 Msun (GRAVITY Collaboration 2018)
1 mas ~ 2.7 pc ~ 1.2✕105 Rs● Bolometric Luminosity
Lbol ~ 0.8 LEdd (Park & Trippe 2017)
HST Optical image(Credit: NASA/STScI)For M87,
Lbol ~ 10-6 LEdd (Prieto et al. 2016)
3C 273

M87Ousuga & Mineshige, 2011

2019.11.24 VLBI symposium @Otsuma women’s university

Observation

Map: Courtesy of Sara Issaoun● 1.6 GHz VLBA

2019.11.24 VLBI symposium @Otsuma women’s university

Observation

Map: Courtesy of Sara Issaoun

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1.6 GHz VLBA
15 GHz HSA (VLBA+Effelsberg)
22 GHz HSA (VLBA+Effelsberg)
43 GHz HSA (VLBA+Effelsberg)

2019.11.24 VLBI symposium @Otsuma women’s university

Observation

Map: Courtesy of Sara Issaoun

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1.6 GHz VLBA
15 GHz HSA (VLBA+Effelsberg)
22 GHz HSA (VLBA+Effelsberg)
43 GHz HSA (VLBA+Effelsberg)
86 GHz GMVA + ALMAHiroki Okino, Instituto de Astrofísica de Andalucía, Granada,2019/10/22

RML Imaging
Central black hole of M87

EHT Collaboration 2019, paper IV

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NRAO 530

Sgr A*Issaoun et al. 2019

Regularized Maximum Likelihood (RML) methods
Robust imaging using closure amplitudes and closure phases
Wide range of imaging parameters with multiple regularizations (~100)
Images with good fit to data (χ2<1.5) were used in further analysis

Hiroki Okino, Instituto de Astrofísica de Andalucía, Granada,2019/10/22

Top set images at 15 GHz

2019.11.24 VLBI symposium @Otsuma women’s university

Multi-frequency 3C 273 images
VLBA 1.6 GHz

HSA 15 GHz

HSA 43 GHz

GMVA+ALMA86 GHz2019.11.24 VLBI symposium @Otsuma women’s university

Core shift

Blandford & Königl 1979
Lobanov 1998

Low freq

M87

Hada et al. 2011

High freq

Black hole position

2019.11.24 VLBI symposium @Otsuma women’s university

Core shift measurements● 2D cross-correlation method(eg. Croke & Gabuzda 2008, Pushkarev+ 2012, Fromm+ 2013)
maskingmasking
22 GHz15 GHz

Cross-Corroffset(Δx, Δy)Core offset

2019.11.24 VLBI symposium @Otsuma women’s university

Results: Core shift~ 8.6×103 Rs (De-projected)

2019.11.24 VLBI symposium @Otsuma women’s university

Results: 3C 273 Collimation profile2019.11.24 VLBI symposium @Otsuma women’s university

Results: 3C 273 Collimation profile●930.

noC0. 5pl icobara

:r∝z

2

alci∝
r:z

Transition in the shapefrom conical to parabolic
shape at ~ 106 Rs.

2019.11.24 VLBI symposium @Otsuma women’s university

Results: 3C 273 Collimation profile●●

EHT observation?

Transition in the shapefrom conical to parabolic
shape at ~ 106 Rs.
Jet may propagate inside thebroad line region and hot dusttorus.
RBLR ~ 46μas ~ 5.5×103 Rs

Hot dust torus(GRAVITY Collaboration, 2018)

RDust ~ 150μas ~ 1.8×104 Rs(Kishmoto et al. 2011;
GRAVITY Collaboration, 2019)

BLRJet2019.11.24 VLBI symposium @Otsuma women’s university

Results: 3C 273 Collimation profile●●

Transition in the shapefrom conical to parabolic
shape at ~ 106 Rs.
Jet may propagate inside thebroad line region and hot dusttorus.
RBLR ~ 46μas ~ 5.5×103 Rs(GRAVITY Collaboration, 2018)

RDust ~ 150μas ~ 1.8×104 Rs(Kishmoto et al. 2011;
GRAVITY Collaboration, 2019)●Similar profile to LLAGN M87
Bondi radius ~ 3.8×105 Rs(Allen et al. 2006)

2019.11.24 VLBI symposium @Otsuma women’s university

Summary and future work
● We performed multi-frequency observations of the nearby
quasar 3C 273 at 15, 22, 43 and 86 GHz with HSA andGMVA+ALMA.
● The jet structures on a wide range of scales (105 - 108 Rs)
were successfully imaged with the state-of-the-art RML
imaging techniques.
● The core shift and jet radius were measured with many multifrequency images.
● The transition of the jet shape was robustly confirmed in aquasar jet with a surprising similarity to the LLAGN jet in M87.
● Future work: multi-frequency polarimetry to probe the 3D
magnetic structure and circum jet material.