First VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

VLA 1.4 GHz image

032cpkFirst VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

VLA 1.4 GHz image

032cpkLarge scale view of 4C 50.55 (Molina et al. 2007)- FR II radio galaxy- viewing angle ~ 35
- Unknown which side is approachingFirst VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

VLA 1.4 GHz image

032cpkLarge scale view of 4C 50.55 (Molina et al. 2007)- FR II radio galaxy- viewing angle ~ 35
- Unknown which side is approaching
Accretion of 4C 50.55 (Tazaki et al. 2010)- High Eddington ratio (Lbol/LEdd ~ 0.4)
- Weak reﬂection from optically thick disk
- Optically-thick Compton coronaFirst VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

VLA 1.4 GHz image

03
2cpk

Large scale view of 4C 50.55 (Molina et al. 2007)- FR II radio galaxy- viewing angle ~ 35
- Unknown which side is approaching
Accretion of 4C 50.55 (Tazaki et al. 2010)- High Eddington ratio (Lbol/LEdd ~ 0.4)
- Weak reﬂection from optically thick disk
- Optically-thick Compton corona

How are FR II jets collimated?
Is AGN jet affected by high-rate accretion
and Compton-thick corona?

First VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

VLA 1.4 GHz image

032cpkLarge scale view of 4C 50.55 (Molina et al. 2007)- FR II radio galaxy- viewing angle ~ 35
- Unknown which side is approaching
Accretion of 4C 50.55 (Tazaki et al. 2010)- High Eddington ratio (Lbol/LEdd ~ 0.4)
- Weak reﬂection from optically thick disk
- Optically-thick Compton corona

How are FR II jets collimated?
Is AGN jet affected by high-rate accretion
and Compton-thick corona?

Sub-pc/pc scale image is important!

First VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)First VLBI Images of 4C 50.55

2017/11/24

5 mas~ 2 pc2019/03/01

5 mas

First VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)First VLBI Images of 4C 50.55

2017/11/24

2019/03/01

participating stations for KaVA
participating stations for EAVN

Fig. 3: Location of EAVN site. (Image credit of ground photo: NASA’ s EarthObservatory)

5 mas~ 2 pc

5 mas

Observed with KaVA
(Japan & Korea VLBI network)First VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)First VLBI Images of 4C 50.55

2017/11/24

2019/03/01

participating stations for KaVA
participating stations for EAVN

Fig. 3: Location of EAVN site. (Image credit of ground photo: NASA’ s Earth
Observatory)

5 mas~ 2 pc5 mas

Observed with KaVA
(Japan & Korea VLBI network)- Reconstructed images with the conventional method: CLEAN.
- Bright core and ejected component to the north-west .

First VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)First VLBI Images of 4C 50.55

2017/11/24

2019/03/01

participating stations for KaVA
participating stations for EAVN

Fig. 3: Location of EAVN site. (Image credit of ground photo: NASA’ s EarthObservatory)

5 mas~ 2 pc5 mas

Observed with KaVA
(Japan & Korea VLBI network)- Reconstructed images with the conventional method: CLEAN.
- Bright core and ejected component to the north-west .
Approaching side is northwest!

First VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

Proper Motion & New-born Component

2017/11/24

2019/03/01

C1

C15 mas~ 2 pc5 mas

First VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

Proper Motion & New-born Component

2017/11/24

2019/03/01

C1

C15 mas~ 2 pc5 mas

C1 component
Apparent velocity~ 0.8 mas/year~ 1.2cIntrinsic velocity (θ~35 )~ 0.8cFirst VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

Proper Motion & New-born Component

2017/11/24

2019/03/01

C1

C15 mas~ 2 pc5 mas

C2
2019/03/01
Core image with SMILIC1 component
Apparent velocity~ 0.8 mas/year~ 1.2cIntrinsic velocity (θ~35 )~ 0.8cFirst VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

Proper Motion & New-born Component

2017/11/24

2019/03/01

C1

C15 mas~ 2 pc5 mas

Apparent velocity~ 0.8 mas/year~ 1.2cIntrinsic velocity (θ~35 )~ 0.8cC2 component

C2
2019/03/01
Core image with SMILIC1 component

New-born jet ~ 1.2 masfrom the radio core.

First VLBI Study of FR II Radio Galaxy 4C 50.55
Fumie Tazaki (NAOJ)

Proper Motion & New-born Component

2017/11/24

C15 mas~ 2 pcmoCe

C1to

C1 component

2019/03/01

m2019/03/01
Core image with SMILIyp

5 mas

oissu

Apparent velocity~ 0.8 mas/year~ 1.2ccisdr Intrinsic velocity (θ~35 )ofretso!
n~ 0.8c

C2 component

C2New-born jet ~ 1.2 masfrom the radio core.

General relativistic radiation magnetohydrodynamics simulationsof super-Eddington accretion disks
around prograde and retrograde black holes
Aoto Utsum𝐢𝟏) ,Ken Ohsug𝐚𝟏) Hiroyuki Takahash𝐢𝟐) ,Yuta Asahin𝐚𝟏)

Purpose1) Univ. of Tsukuba, 2) Komazawa Univ.

We investigate the dependence of luminosity and jet poweron spin parameters in Super-Eddington accretion disks.

Overview
2.5-dimensional General Relativistic Radiation MagnetoHydroDynamics(GR-RMHD) simulation for MBH = 10M⊙ .
Time-evolution of the density (color) andfluid velocity lines. (edge-on)

𝑍/𝑟𝑔𝒂∗ = 𝟎𝑟/𝑟𝑔

𝑟/𝑟𝑔

𝑟/𝑟𝑔

Initial maximum mass density
𝜌0 = 1.4 × 10−2 g cm−3Prograde(𝑎∗ = 0.9)

The Jet and the outflow andthe Supercritical accretion
flow are dominant in radiation.

𝑎∗ = 0Global structure does notdepend on spin parameters.

Retrograde(𝑎 ∗ = −0.9)

Spin parameter dependence𝑎 ∗ = 0.9

𝑀ሶ 𝐵𝐻
𝑀ሶ 𝐸𝑑𝑑𝑀ሶ 𝑜𝑢𝑡𝑀ሶ 𝐸𝑑𝑑

𝜂𝑡𝑜𝑡 [%]

240

1924

𝐿𝑟𝑎𝑑
𝐿𝐸𝑑𝑑

𝐿𝑘𝑖𝑛
𝐿𝐸𝑑𝑑

𝐿𝑚𝑎𝑔
𝐿𝐸𝑑𝑑

The mass inflow andoutflow rate𝑀ሶ = 2𝜋∫ 𝜌𝑢𝑟 −𝑔𝑑𝜃152715Luminosity : 𝐿𝑎∗ = 0410

2.73.48.0

5.60.1𝑎 ∗ = −0.9720129.02035

10The energy conversion
efficiency
𝐿𝜂𝑡𝑜𝑡 = 𝑀ሶ 𝑡𝑜𝑡𝑐 2 × 100 [%]𝐵𝐻𝒂∗ = 𝟎. 𝟗𝒂∗ = 𝟎𝒂∗ = −𝟎. 𝟗•

𝑴ሶ 𝑩𝑯 𝒂∗ = 𝟎. 𝟗 < 𝑴ሶ 𝑩𝑯 𝒂∗ = 𝟎 < 𝑴ሶ 𝑩𝑯 𝒂∗ = −𝟎. 𝟗•𝑴ሶ 𝒐𝒖𝒕 𝒂∗ = 𝟎 < 𝑴ሶ 𝒐𝒖𝒕 𝒂∗ = −𝟎. 𝟗 < 𝑴ሶ 𝒐𝒖𝒕 𝒂∗ = 𝟎. 𝟗𝑍/𝑟𝑔

We think that the mass ejection rate is related tothe Poynting flux. (The Blandford-Znajek effect)

𝑟/𝑟𝑔

𝑟/𝑟𝑔

𝑟/𝑟𝑔

Proﬁles of the outward Poynting ﬂux.
Blue lines indicate the magnetic field lines.

•𝜼𝒕𝒐𝒕 𝒂∗ = 𝟎 < 𝜼𝒕𝒐𝒕 𝒂∗ = −𝟎. 𝟗 < 𝜼𝒕𝒐𝒕 𝒂∗ = 𝟎. 𝟗••

The non-spinning BH : 𝐋𝒎𝒂𝒈 < 𝐋𝒌𝒊𝒏 < 𝑳𝒓𝒂𝒅
The spinning BH : 𝐋𝐫𝐚𝐝 ~𝐋𝐦𝐚𝐠 < 𝑳𝒌𝒊𝒏

If you have any questions, please come to my poster.

RADIATION MAGNETOHYDRODYNAMIC
SIMULATIONS OF CHANGING LOOKAGNS AND INTERMITTENT JET
EJECTIONTAICHI IGARASHI (五十嵐YOSHIAKI KATO, RIKEN太一), CHIBA UNIV.

HIROYUKI TAKAHASHI, KOMAZAWA UNIV.
KEN OHSUGA, TSUKUBAI UNIV.

YOSUKE MATSUMOTO, CHIBA UNIV.
RYOJI MATSUMOTO, CHIBA UNIV.

Intensity

CHANGING LOOK AGN (CLAGN)

HβH"Disappearbroadline!

State transition

H"

Shorttimevariation
WavelengthCont.

Hβ49000

Optical spectrum & light curve of NGC 3516 (Shapovalova et al. 2019)

JD

59000

Narrow line」
sN
GA
flo.
es
d
NoG
Broad linemAd
LeCi
fi
enni
「U expaltʼn
Optical image of Seyfert galaxyacNGC 1068

Schematic picture of「Unified model ofAGN」Beckmann 2012

NASA, ESA & A. van der Hoeven

CLAGN : SOFT X-RAY EXCESSAGN (M"# = 5×10* M⊙)

X-ray intensity

Stellar mass BH (M"# = 10 M⊙)

Spectrum of Mrk 1018
Noda & Done 20138

energy keVSpectrum of Cygnus X-1
Yamada et al.2013

energy keV• Soft X-ray excess is prominent when the source is bright.
• Similar to the hard-to-soft (soft-to-hard) transition instellar-mass BH.

State transition exists in the accretion flow inthe near region from BH.

RESULT
Before transitionHotaccretionflow

After transition

Relatively cool(~10$ − 10& K)
region formed.

Temperature distribution••••Relatively cool (~10$ − 10& K)
Non-axisymmetric structure (m=1)
Strong radiation pressure
Origin of Soft X-ray emission

Rz slice ofdensity and temperature

RESULT

Photon luminosity

Mass out flow rate

Temp. at midplane• Relatively cool region oscillates quasi periodically.
• We reproduce the short time variability.
• The variability follows the cool blob variability.
• Jet ejected intermittently.
• Jet suppressed in the later stage.

P4

Polarization study of the jet of gamma-ray emitting narrow-line
Seyfert 1 galaxy 1H0323+342 with high-resolution VLBIMieko Takamura(UTokyo / NAOJ, M1)

Third class of AGN with powerful relativistic jets
Radio-loud NLS1

Blazar/Radio galaxy

Black hole massBlack hole mass

= 106 M⊙ − 108M⊙
L
LEdd= 108M⊙ − 1010 M⊙
L~1

LEdd
Non-blazar

28%

2%

Blazars ofunknown type

28%

FSRQs

BL Lac objects

42%

Gamma-ray AGN(3LAC using the first four years of the Fermi-LAT datalist 1444 gamma-ray AGN)

<1

(Hada et al. 2018)(Paliya et al. 2019)l o g(MBH)
M⊙

ObjectRedshift z

Luminosity(erg/s)

1H0323+342

0.0612.1×1044

7.17

SBS 0946+513

0.584

3.2×1046

7.59

PMN J0948+0022

0.585

7.5×1046

7.5

IERS B1303+515

0.787

6.9×1045−B3 1441+476

0.705

4.7×1045

7.4

PKS 1502+036

0.408

1.0×1046

8.84

FBQS J1644+2619

0.145

2.7×1044

8.32

PKS 2004-447

0.24

1.7×1045

6.7TXS 2116-077

0.26

7.2×1044

7.21

It is important to investigate the relativistic jet launching,collimation and acceleration of NLS1s

Imaging & Polarization analysis

2010/10

2011/03

2011/05

2011/07

2011/122012/072012/122013/072019/01

Imaging & Polarization analysis

2010/10

2011/03
Where standing shocks might be.

2011/05
In each epoch, strong
polarization flux was
detected in these two regions

2011/07

2011/122012/07
The possibility of existenceof compressed uniform
magnetic field structures

2019/01

2012/122013/07

2019/01

Constructing a GRMHDApproximate Solution for AGN Jets
Taiki Ogihara, Kenji Toma (Tohoku Univ.)“Active Galactic Nucleus Jets in the Event Horizon Telescope Era”, 20 Jan. 2020 @Tohoku University

EHT image = Disk Emission

EHT Collaboration

EHT Paper 5

How about Jet Emission?
Detection is expected in EHT 2020 observations
linear contour
線形コントア

一般相対論的GRMHD
simulation
輻射磁気流体モデル

EHT 2017のEHT 2017
観測条件にmock observation
基づく模擬観測EHT 2020のEHT 2020
観測条件にmock observation
基づく模擬観測(Chael et al. 2019)log contour
対数コントアਤ 1.

Akiyama, Asada, Hada
天文月報 2019 年 7 月号 ASTRO NEWSࠓ‫ޙ‬ͷ Produce
M87*ͷ‫؍‬ଌ༧૝ɻຊ‫؍‬ଌ͕࣮ࢪ͞Εͨ
jet image2017೥ʹ͸࣮ޮ‫౓ײ‬ෆ଍ͷͨΊʹ‫ݕ‬ग़͕೉͔ͬ͠
with ANALYTICAL JET MODEL

Constructing a GRMHD Approximate Solution for AGN Jets
Taiki Ogihara, Kenji Toma (Tohoku Univ.)• method• analytically solve GRMHD equations• assume poloidal magnetic fieldstructure instead of solving GS
equation (trans-field component ofEoM)• constrain parameters to satisfy GS
equation at the stagnation surface=> derive density, velocity, magnetic fieldConstructing a GRMHD Approximate Solution for AGN Jets
Taiki Ogihara, Kenji Toma (Tohoku Univ.)• preliminary results• in force-free case,

we obtained the appropriate
solution at the stagnation
surface• future work
• expand model to MHD• apply radiative transfer andmake jet image