Expectations of the EAVN from
Theoretical Issues on AGN Jets

Masanori Nakamura (ASIAA)EAVW2019, Sep 23-26, 2019, Mito, Ibaraki, Japan

Outline• “VLBI study of AGN Jets” during the last decade①Many thrilling results, but the horizon-scale M87
jet is still unknown and/or has no strong constraints②Instructive lesson from M87 to other RGs/Blazars:
ACZ (Marscher+ 2008) as “Pipeline” of AGN jets
(Marscher & Gear 1985) and JCB (Asada & MN 2012)• Any unique usage of EAVN facilities to understandthe fundamental physics in AGN jets?
09/24/2019, Mito• BH Mass:
SANE, Rhigh = 80, a* = − 0.94

SANE, Rhigh = 10, a* = 0

M∙ = (6.5 ± 0.7) × 10 M⊙

MAD, Rhigh = 10, a* = 0.94

9• Mass accretion rate:

· ·
−7
−4
·
m (≡ M/ MEdd) ≃ 5 × 10 −3 × 10

• Jet power:
42−1

50 μasFigure 4. Top: three example models of some of the best-ﬁttingfrom
the image libraryof GRMHD simulations for April 11 corresponding to different spin
fromsnapshotspaper
I (EHTC
2019a)
parameters and accretion ﬂows. Bottom: the same theoretical models, processed through a VLBI simulation pipeline with the same schedule, telescope characteristics,
and weather parameters as in the April 11 run and imaged in the same way as Figure 3. Note that although the ﬁt to the observations is equally good in the three cases,
they refer to radically different physical scenarios; this highlights that a single good ﬁt does not imply that a model is preferred over others (see Paper V).

• Synthesized emission: the funnel wall and/or

10

erg s

43

< Pjet ( ≲ 10−1

erg s )

• BH spin (*a=0 can’t do >1042 erg/s ):accretion
flow
with
σ
<
1:
Γ
∞→1
|
|
a
≤
0.94
spin energy through mechanisms akin to the Blandford–Znajek
The diameters of the geometric crescent models measure theprocess.

σ: Poynting flux per unit matter energy flux

characteristic sizes of the emitting regions that surround the
shadows and not the sizes of the shadows themselves (see, e.g.,
Psaltis et al. 2015; Johannsen et al. 2016; Kuramochi et al.
2018, for potential biases).
We model the crescent angular diameter d in terms of thegravitational radius and distance, Rg w GM c 2D, as d= αθg,where α is a function of spin, inclination, and Rhigh (α;9.6–10.4
corresponds to emission from the lensed photon ring only). We
calibrate α by ﬁtting the geometric crescent models to a large
number of visibility data generated from the Image Library. We
can also ﬁt the model visibilities generated from the Image Libraryto the M87* data, which allows us to measure θg directly.
However, such a procedure is complicated by the stochastic natureof the emission in the accretion ﬂow(see,e.g., Kim et al. 2016).
PA43GHz ∼ 288∘ (Walker + 2018)
To accountfor this turbulent structure, we developed a formalism
EAVN Collaborationand multiple algorithms that estimate the statistics of the stochastic
components using ensembles of images from individual GRMHD
simulations. We ﬁnd that the visibility data are not inconsistent
with being a realization of many of the GRMHD simulations. We
conclude that the recovered model parameters are consistent• Connection with the extended jet (relativistic
7. Model Comparison and Parameter Estimation

outflow: Γ ≫ 1) is unclear∞ is derived from ﬁtting to the
In Paper VI, the black hole mass
visibility data of geometric and GRMHD models, as well asfrom measurements of the ring diameter in the image domain.
Our measurements remain consistent across methodologies,
algorithms, data representations, and observed data sets.
Motivated by the asymmetric emission ring structures seen in
the reconstructed images (Section 5) and the similar emission
structures seen in the images from GRMHD simulations(Section 6), we developed a family of geometric crescentmodels(see, e.g., Kamruddin & Dexter 2013) to compare directly
to the visibility data. We used two distinct Bayesian-inference
Collaboration
algorithms andEHTdemonstratethat such crescent models are
statistically preferred over other comparably complex geometricmodels that we have explored. We ﬁnd that the crescent models
provide ﬁts to the data that are statistically comparable to those of
the reconstructed images presented in Section 5, allowing us todetermine the basic parameters of the crescents. The best-ﬁt• Magnetic flux:

ϕ = 3.6 − 56.5 (units of
SANE

MAD

· 2
MRg c)• Electron temperature:

Te ≃ Ti /(10 − 160)

• PAGRMHD (forward jet):
∘±
∘

235

65 (Apr 5 − 11)

Cui’s talk
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Z

2⇡Bp rdr•

A.
Tchekhovskoy
Poloidal magnetic

field supports the accreting gas
against the BH gravity (Narayan+ 2003; Igmenshchev 2008)
2
Bp

GM ⇢
2
'
= ⇢c
8⇡
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'

q

10

2
2
Ṁ Rg c G cm

33

1/2

ṁ

3/2
2
m9 Mx (G cm )ṁ . 0.01 (RGs, BL Lacs)<latexit sha1_base64="Of92/zcaqTtK51+g3Msfi6t1cNg=">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</latexit>• Simulations:ϕ < 10 (SANE), ϕ ∼ 40 − 80 (MAD) (Narayan+ 2012; Sadowski+ 2013)•
Image
courtesy:A.
Tchekhovskoy
ertical slice through BH accretion system illustrates how theObservations:balance of forces

31
35
he maximum possible field strength on the BH. The BH, shownΦ
as a =black
circle,is10 − 10 Mx (Zamaninsab+ 2014)jeth vertical magnetic field, whose lines of force are shown with blue lines. The magnetic
ce, FB , pushes outward on the accretion disk gas, which is shown in red. Clearly,
ed the disk, the magnetic field would leave the BH due to the “no-hair theorem”,· 2 (Ghisellini+ 2014)
Pjet ≳ Mc
09/24/2019, Mito

41
10

0

Efficiency: η (%)

300

· 2
Pjet0.8> Mc
0.2 MAD0.4Can Make
0.6
a

MAD
SANE

200

EM energy extraction from a spinning BH (Blandford & Znajek 1977)

PBZ(Φ, a)
η=
×
100
· 2
Mc

ϕ = 60100
ηmax for thin disk (a=0.998)

0

1

0

0.2

0.4

ϕ = 10
a

0.6

0.8

1
09/24/2019, Mito

M87
VLBI core obs.
GRMHD sim.

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2
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Resolving a jet in the direction transverse to its axis isimportant for understanding the opening angle, collimation
efﬁciency, and possible velocity gradient across the jet. To
perform this, one needs a high-quality image at a sufﬁcientangular resolution across the jet. The new 86 GHz image
presented here allows us to analyze the detailed transverse
structure of the jet-launch region near the black hole.

Quasi-symmetricdistorsion→ |B| (z < 50 rg)

Hada+ (2012, 2016); Kino+ (2014, 2015)
43 230 GHz' (12) ⇥ 10<latexit sha1_base64="j5U/djhzCXGgF9YMs5m4tgI9JBo=">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</latexit>

3.3. Transverse Jet Structure~1000 rg

We don’t know where/how
SL knots are formed…

• SSA thick VLBI cores

located with respect to the core, while case (2) is also possible
if we additionally consider the relativistic “arm-length ratio”
that reﬂects apparent motions differing by a factor of ∼2
between the jet and the counter jet.
In the case of (1), when compared using the total ﬂux densities,
the BR is 25.2 at 86 GHz or 5.7 at 43 GHz. In the case of (2), theBR is 22.0 at 86 GHz or 4.4 at 43 GHz. Alternatively, if we use
the peak ﬂux densities, the BR is 25.3/4.7 at 86/43 GHz for case(1), or 21.4/5.6 at 86/43 GHz for case (2).
It is not clear yet whether the resulting difference in BR
between 86 and 43 GHz is real or not. We consider that themeasurements at 43 GHz would be more secure due to the higher
S/N for the counter jet. Conservatively, here we conclude thatthe BR is between ∼5 and ∼25 within the central 1 mas region.

HSA 86GHz (Hada+ 2016)

Figure 8. Close-up view of the innermost region of the M87 jet observed with
VLBA+GBT at 86 GHz. The image is restored with a 0.11 mas circular
Gaussian beam, which is equivalent to that of the minor axis of the synthesized
beam. The image is rotated on the sky by 23n in order to align the jet central
axis to the horizontal direction. For reference, on the origin of the coordinates
we place a green-colored circle with a diameter of 40 μas, which is equivalent
to the size of the 230 GHz core reported by Doeleman et al. (2012). The arrows
indicate where the jet shape is locally shrinking.

Innermost Structure of the M87 Jet

33

2

Mx (G cm )• Enclosed current Ipol

along each B-field line

e.g. Mestel (1969); Okamoto (1978);Beskin (1997); Narayan+ (2007)c
I( ) = RB ⇡
2

⌦F
2⇡

' (1.517<latexit sha1_base64="G4fjqV7pBsANit1cfp9kI0Bu2NM=">AAAG93icjdTNaxNBFADw16hrrR9N9SJ4WQyRejBMomARhBLbaAvFfLfQLWF3O0mG7Bezm2hc9h/wH/DgQRQURTz4N3jx4E08FPQPEI8VvHjw7YeIHawzIdm3b95v9u0ExvAs5geE7M3kjhw9phyfPTF38tTpM/P5hbNd3x1zk3ZM13L5lqH71GIO7QQssOiWx6luGxbdNEa34vnNCeU+c512MPXojq0PHNZnph5gqpe/vbao1Yfs8k2tz3UzNKOwEjXVai/UvCGLVE33PO7eV6+k09pdmw50nOS2WsNZlAg0j0W9fIGUSDJUMShnQQGyUXcXch9Ag11wwYQx2EDBgQBjC3Tw8bMNZSDgYW4HQsxxjFgyTyGCObRjrKJYoWN2hL8DvNvOsg7ex2v6iTbxKRZ+OUoViuQTeUX2yXvymnwlP/+5VpisEfcyxauRWur15h+eb/34r7LxGsDwjzq05wD6sJT0yrB3L8nEb2GmfvLg0X7rRrMYXiLPyDfs/ynZI+/wDZzJd/N5gzYfH9KPgb1EUMR1jGQfdjH63V2sHKy6l+yRneQdrAgxn1bHux1m9zZKNclEEnIgyIGkHAlyJCm5ILmknAhyIilXBbkqKVcEuSIpq4KsSsp1Qa5Lyq4gu5KyLci2pKwLsi4p1wS5Jik3BLkhKRuCbEjKmiBrkrIvyL6kbAmylUo8y8sHT24x6FZK5aulSuNaYXkpO9Vn4QJchEU8ua/DMtzB/6qDT38DH+EzfFGmyhPlhfIyLc3NZOYc/DWUt78AZdV58w==</latexit><latexit sha1_base64="6E3L85MF/WsY8y0pd8D9L8+LQT8=">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</latexit>3) ⇥ 10A• Electromagnetic(Poynting) luminousity

LEM = I 2 z ' (4—σ=1—βp = 1 — ur = 0 (Stagnation) MN+ (2018)<latexit sha1_base64="3U7+vVxjC+e+zEfSIScJcJ2nDeo=">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</latexit>15) ⇥ 1043 erg s 1
09/24/2019, MitoBAF / ADAF
s= 0
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10-1

Kuo+ (2014)Ṁ /ṀB

10-2

5
.
0
s=

=
s

1

S
O
DI

F
A
D
C

'

RB

210 pc✓kTB
0.9 keV◆ 1✓M•
6.2 ⇥ 109 M

3.6 ⇥ 105 Rs
⇣ n
⌘
e,B
' 0.2 M yr 1
0.3 cm 3✓◆ 3/2 ✓
◆2kTB
M•
0.9 keV
6.2 ⇥ 109 M'<latexit sha1_base64="+3zGD5+gP5kZ4o9q4OlWxdzbcGs=">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</latexit>

ṀB<latexit sha1_base64="FRBH9sPvS5D1oKxxK6jTAV/zXFI=">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</latexit>· 2
Pjet(= 5 × 10 erg/s)/ Mc ∼ 1

ṀEdd<latexit sha1_base64="Z//vej3AntBx+FCIjLpOKOY8i2g=">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</latexit>=

136.4 M yr 1◆⇣✏ ⌘ 1 ✓M•
acc
0.1
6.2 ⇥ 109 M

X-ray / Pol. obs.

ne / R 1 (R . 5000 Rs ) : s ' 0.5<latexit sha1_base64="mZxLA4gtJ7dyXIrvuIxwtZqsokE=">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</latexit>

10-4

Russell+ (2015) - X-ray
Park+ (2019) - VLBA Pol. (≦ 5 GHz)

To be explored w/ HSA Pol. (≦ 22 GHz, PI: Park)Ṁ (r) = Ṁout

10-5

✓

R
Rout

◆s

Ṁ . 9.2 ⇥ 10 4 M yr 1 (R ' 20 Rs )<latexit sha1_base64="Lp67wpoqGkzWKUDmdgR+MQau4bs=">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</latexit>

Kuo+ (2014) - SMA Pol.

, 0s1e.g., Yuan & Narayan (2014) ARAA

10-6
1

101

102

103
R/Rs

◆

Di Mateo+ (2003); Rafferty+ (2006); Russell+ (2015)43· 2
Pjet > Mc

10-3

A

(2
+
k
Par

X-ray obs.

104

Ṁ |R=10 Rs ' 5.3 ⇥ 10 4 M yr 1

105ṁ ' 3.9 ⇥ 10 6<latexit sha1_base64="WrbFlD+KgG9Thi7KoiEeZdQ48Jc=">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</latexit>Ṁ c2 ' 3.0 ⇥ 1043 erg s 1

09/24/2019, Mito

M87

33

≃ (1 − 2) × 10

GRMHD sim.

<latexit sha1_base64="/ThWlbwn7VTvD+vfDrMZjBOldBQ=">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</latexit>from paper V (EHTC 2019e)=q

2Ṁ Rg c≃ 3 × 1031

VLBI core obs.

≈ 30 − 70
Pol. / X-ray obs.

09/24/2019, Mito

Lateral Expansion & Acceleration
SANE

SANE

MAD

MAD

MAD

--σ=1
— BP82-type(z ~ R1.6)
FFE solution

MN, in prep.

•

Clear dependence on the jet acceleration w.r.t φ (large value causes alateral expansion)
09/24/2019, Mito

Acceleration in a Magnetic Nozzle
8π

2
p
>
1
p

S1

S1 <

S2

S2

102

ΓSheath

>

F= −∇

2
Bϕ

101

F= −

R

Bp (R) / R⇠“Fast sheath”

ΓβFFE

ΓSpinez ∝ R 1.6z ∝ R2z ∝ R 2.7

2
Bϕ

1

4πR

“Slow spine”<latexit sha1_base64="j3DC2fvEai6Eu5TLjWnnifgb1Hk=">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</latexit><latexit sha1_base64="3kmm//nEzeYE2oxIWTCOhAW5E8E=">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</latexit><latexitµ/Γ = 1 + σ
ξ = 2: Γ∞ → µ (σ << 1) 10
1µ ~ σ (>>1) Γ = 1 at the jet base ξ = 1: Γ∞ → µ/2 (σ ~ 1)-1µ: Total (matter + electromagnetic) energy flux per unit rest-mass energy flux

Bp (R) / R

101

⇠

102
Jet axial distance: z (rg)

103

104

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09/24/2019, MitoJet axial distance (projected): z (μas)
1

Jet radius: R (rg)

102

101

ϕ ∼ 60 (cgs) ←102

Observations(Area) Force-free parabolic jet solution
a = 0.5 (upper edge) - 0.99 (lower edge)ϕ ∼ 4 (cgs) ←101

from GMVA+ALMA Cy 7 proposal (PI: Kim, J.)

φ~100, a=0.9
φ~70, a=0.9
φ~30, a=0.9
φ~10, a=0.9

1

MN, in prep.

1

101

102

Jet axial distance (de-projected): z (rg)Figure 2: GRMHD+GRRT images and simulated GMVA(+ALMA)
thelegend for references).
Top: jet formation• Adequate
expansion oftheandjet bottom
in the lateral
directionwith highleft• toright : images
fromsimulations,
Γ increases
due tothethemagnetic
nozzlesynthetic
effect GMVA+AL
without ALMA.
• Unexpected counter jet emission is suppressed
the structure of the onset of the jet, (iii) establish firm ev• Quasi-symmetriclaunchingin M 87 basedon polarization
limb-brightens
featuremeasurement.
appears in theapproaching
jet side :3 Immediate
Objectives

from EHT+ALMA Cy 7 proposal (PI: Doeleman, S.)• Proving presence/absence of a ring-like feature at 3 mm
• “Jet” imaging w/ EHT@230GHz / GMVA@86GHz in 2020?
recent state-of-the-art numerical simulations predict bright synchr
phology at the base of jet (Fig. 2). In the standard jet formatio
09/24/2019, Mito
angular momentum by surrounding magnetic field (B-field) leads toQuasi-simultaneous Monitoring of Flux Density

A&A 610, L5 (2018)

J.-Y. Kim et al. : KVN M 87 VLBI monitoring

Emerging
knots?

Kim+ (2018)

Fig. 3. Radio spectrum of the M 87 core region in log-log scale. Different KVN observing epochs are indicated by different colors in the legend. The
2rrows indicate upper and lower limits. References of other multi-frequency flux information(in order of increasing radio frequency): Pushkarev& Kovalev (2012); Lister et al. (2016); Doeleman et al. (2012); Akiyama et al. (2015).
Fig. 1. Four-frequency core flux light curves obtained by the KVN

Measurement within a 0.5 × 0.5mas box around the peak

Flux density (Jy)EAVN@22GHz, Apr. 17, 2017
EAVN@43GHz, Apr. 18, 2017
rend of spectral steepening
over a longer
period.
By averagKVN@86GHz,
Apr.
19, 2017
KVN@129GHz,
Apr.the19,
2017
ng the spectral2 index light
curve, we obtained
mean
spectralFig. 2. Sp
epoch• Significant
observations.effects on the spectral steeping w/ each
KVN;
power-law(Fig. 3). In particular, the long-term 15 GHz core flux is quite(u, v) coverage and/or structure blendingand standa
comparable to our four-year measurements made theby the limited
KVN

ndex h↵i = 0.37 ± 0.10, which corresponds to a mildly steep at 86 and 129 GHz. Since the angular resolution of the KVN at
1(iMOGABA)
program(e.g.,
Lee
et
al.
2016)
. The observations
pectrum.
short millimeter wavelengths is comparable to •that of VLBA at
However, wewere performed simultaneously at four observing frequencies ⌫1 note that the limited (u, v) coverage of KVN 15 GHz, we can calculate a non-simultaneous but resolution3. Resulcould have a significant effect on the core spectral index mea- matched spectral index, finding ↵(15 129) GHz = 0.03 ± 0.23
21.700–21.764 GHz (K band), 43.400–43.464 GHz (Q band),urement because of the different array sensitivity to extended between 15–129 GHz. Such a flat spectrum •agrees withoftheemission at different
frequencies. In order to study the effect 230 GHz flux lower limit constrained by the EHT observa86.800–86.864 GHz (W band),and 129.300–129.364 GHz 3.1. Core-122-86GHz5×10gof the (u, v) coverage, we have performed a dedicated imaging tions. Although the 22 GHz KVN flux appears slightly high(D band). Each band has 64 MHz of total bandwidth. The
imulation (see Appendix
A).
We
find
that
an
artificial
speccompared
to
the
15
GHz
flux,
we
note
that
this
is
most
likely
1
1
1
2
2
10
2
×
10
5
×
10
10
2
×
10
was observed in left-circular polarization. Details on In Tableral steepening of ↵ ⇠ 0.2 could be possible for the M 87-like due to the blending effect we mentioned in• Sect. 3.1.source
The
Frequency(GHz)core flux between 5–22 GHz indeed shows
et structure only due to the (u, v)-coverage effect (equivalent
to resolution-matched
the iMOGABA program (data acquisition, correlation, post- results of⇠36% of flux decrease from 22 to 129 GHz). Furthermore, M 87 a substantially flat spectrum within ⇠1 mas from➡the intensity
76%, andprocessing,andcalibration,
especiallyconcerningthefrequencyData
from
paper
IV
(EHTC
2019d)
has a substantially extended jet, whose spectrum is quite steep peak (see Fig. 4 of Hada et al. 2012). Therefore, we conclude
already at &0.2 mas core separation (↵ . 0.7; Hovatta et al. that the M 87 core on a submilliarcsecond scale has a substanphase transfer) are provided elsewhere (see Lee et al. 2015, at K, Q, W
2014; Hada et al. 2016). Therefore, the structure blending effect tially flat radio spectrum between 15–129 GHz and possibly up
ofthe res
2016;
Algabaetal.
2015;
Hodgsonetal.
2016).
Owing
tothe
09/24/2019,
Mito
could make the KVN M 87 core spectrum steeper even if the to 230 GHz.

True spectrum of the jet base can be flat up to 129 GHz?

GRMHD simulations suggest an emerging knot at
are located (MN+ 2018)
R ≳ 10 R where VLBI cores
Monitoring VLBI core flux/size at 22-129GHz?
One of most robust estimations of Φ at 86-129GHz

0.13, and

Exploring M87 w/ EAVN
• Successof KaVA/EAVN high-cadence monitoring(22/43GHz: Park+, submitted)• Further downstream w/ lower frequencies• Structure variation such as Jet PA, tracing knots(Cui’s talk, Niinuma+ 2004)• Spectrum analysis (Ro’s talk)• Jetmagnetic flux (and EM power) during EHT
campaign w/ simultaneous EAVN/KVN (22/43/86/129
GHz) monitoring w/ a high-res imaging with GMVA/
ALMA
09/24/2019, Mito

Acceleration & Collimation Zone in AGN Jets
A&A 558, A144 (2013)

fast spine

JI[ RGs?


Blazars?

δ (Γ=10)

h
t
a
e
h
s
w
o
l
s

20
10

z ∝R

θRGs ~ θBlazars?

1z ∝ R2

θapp= ρ0.2

Clausen-Brown+ (2013)

ρeff

0.15

Γθj ≃ 0.1 − 0.2

Jorstad+ (2005); Pushkarev+(2009);(2013)
Fig. 1. Meridional slice ofa jetClausen-Brown+
illustrating twocases: (i) jets aligned

0.1

0.2

0.3

0.4

0.5

M87 & NGC 6251

0.1
0.05

Algaba, MN+ (2017)
close to the line of sight where emission is dominated by the fast in0
• ner
0
0.1
0.2
0.3
0.4
0.5
θRGs
≫ and
θBlazars? misaligned jets where the emission from outerspine;(ii) more• VLBI cores of nearby RGs/blazers
in the ACZθ(radians)
layerscontributes asofwell.
• slower
Lateralstratification
Γ in MHD jets ( Γ ∝ R )app• ”Slow spine and fast sheath” may provide

0.6• Non-conical (parabolic) LB stream: BH-driven

Fig. 2. Doppler
factorand Takahashi+⇢e↵ as a function(Blandford& Znajek
1977;
2018of)? a jet’s apparent ha limb-brightened (LB) feature (MN+ 2018)
opening angle✓app . The semi-logarithmic
factorplot
inthe• Revisiting“standard”
conical jet (EDoppler/E
equipartition,
Be
The simplest way to model the e↵ect that velocity shear and per panel is for a jet with = 10 and ⇢ = 0.21, and uses Eq. (4)veloc.
asBlandford & Königl 1979) paradigm?
beaming have on jet appearence is to postulate that jets that have constantconvert ✓app to ✓ob . The lower panel plot shows ⇢e↵ as a function of ✓✓ob < 1/ have an e↵ective jet opening angle ✓ j,e↵ = ⇢e↵ / , from Eq. (9) using ⇢ = 0.21 and fsh = 0.33, the best fit values found
09/24/2019, Mito
where ✓ j,e↵ is some fraction of the true jet opening angle such Sect. 3.2.

Resolved Pipeline (ACZ) in RG
Jet axial distance (de-projected): z (pc)(b) EVN 1.6GHz

10-1

101

1

MERLIN 1.8 GHz (AN12)

VLBA 15 GHz (AN12, H13)

EVN 1.6 GHz (AN12)

VLBA 22 GHz (H13)

VLBA 2.3 GHz (H13)

VLBA 43 GHz (AN12, H13)

VLBA 5 GHz (H13)

HSA 86 GHz (H16)

102

HST-1
Jet radius: R (rg)104(c) VLBA 15GHz

VLBA Core 5, 8, 15, 24, 43, & 86 GHz (H13), HSA Core 86 GHz (H16)Q
DTC(Area) FFE genuine parabolic jet (NMF07, TMN08)

103

a = 0.5 (upper edge) - 0.99 (lower edge)

C
R
ň

HST-1

“Re-collimation
shock(RCS)”

102

101
(d) VLBA+GBT 86GHz“Acceleration &collimation zone (ACZ)”

1

1Radio images of the M87 jet. (a) MERLIN 1.6GHz image (taken from Asada & Nakamura
VN 1.6GHz image (taken from Asada & Nakamura 2012). (c) VLBA 15GHz image (taken fromrchive). (d) VLBA+GBT 86GHz image (taken from Hada et al. 2016).

101

102

103

Related study:• N6251: Tseng+ (2016)• 3C 273: Akiyama+ (2018)• N4261: Nakahara+ (2018)• 1H0323+342: Hada+ (2018)• Cyg-A: Nakahara+ (2019)• N1052: Nakahara+ (2019)• NGC315: Park+, in prep.
• Mrk501: Koyama+, in prep.
• 1928+738: Lee+, in prep.
…
*Thesis related

ŉ
E
NK

EHT Core 230 GHz (D12, A15)
(Area) FFE parabolic jet (NMF07, TMN08)

104

ňE

VLBA 8.4 GHz (H13)
VLBA Core 43 & 86 GHz (NA13)

103

ŉ

10-2

EC
N

105

10-3

QP
K

106

10-4

104

105

Bondi radius

M87(a) MERLIN 1.6GHz“Jet Collimation
break (JCB)”
106

107

108

Jet axial distance (de-projected): z (rg)Asada & MN (2012); MN & Asada (2013), Hada+ (2013, 2016), MN, Asada, Hada+ (2018)31

09/24/2019, MitoVLBI Cores in BL Lacs
Mrk 421

Piner+ (2010)• LB feature; either i) a higher Doppler factor or ii) a higher synchrotron emissivity in the jet limbs

relative to the jet spine (Piner+ 2010)09/24/2019, MitoVLBI Cores in BL Lacs
12 Feb. 2012 - Feb. 15 2013

NE
Relative Declination (mas)Mrk 501

0

-0.5

-1.0

A

NE’

Core
C3
C2

C1
0.5
0
Ascension (mas)Relative Right Acsension

Image: VLBA-BU Blazar Monitoring Program

Koyama+ (2016)• VLBI core (43GHz) at ~ 103 rg (Croke+ 2010; Giroletti+ 2004) and a clear LB feature in the downstream• Presence of two humps is also indicated around the core component (Koyama+ 2016)09/24/2019, Mito

Resolving ACZ in FSRQs?
Astrophysical Journal Letters, 857:L6 (6pp), 2018 April 10

Doi et al.

∘∘θv ∼ 12 .8

θv ∼ 2 .5

1928+738“RCS”

γ-ray RLNLS1 1H0323+342•

Double ridge nozzle toward a focal point?

Doi+ (2018)

ure 5. Jet structure of 1H0323+342. Contours represent the total intensity map of MOJAVE data on the epoch MJD=55757. Sub-ﬁgures show the sliced
nsity proﬁles in transverse direction at the locations z=6 (red color) and z=9 (blue color) from the core. Bold lines illustrate a putative sheath layer in the jet as aked plasma after a recollimation shock.

Lee’s talk
09/24/2019, MitoGlobal Structure of AGN Jets106

M87 + NGC 6251 + NGC 315
105

M∙ = 6.2 × 109 M⊙ (M87)8

Jet radius: R (rg)104M∙ = 6 × 10 M⊙ (N6251)
M∙ = 2 × 109 M⊙ (N315)

103

102

101

1

1

101

102

103

104

105

Jet axial distance (de-projected): z (rg)

106

107

108

Tseng+ (2016); MN+ (2018); Park+, in prep.

09/24/2019, Mito

Structure Analysis w/ KaVA/EAVN

Hada+ (2017)•

Koyama+, in prep.

ACZ+JCB in a BLO:
Koyama’s poster

Ready to work on resolving the ACZ in AGN Jets
09/24/2019, Mito

02014.0 2014.5 2015.0 2015.5 2016.0 2016.5 2017.0
TIME [yr]

MOJAVEJET SPEED [v/c]

14
12
10
8
6
4
2
0
0

2

4
6
8
10
12
PROJECTED DISTANCE [pc]

14

2418

T. Lee et al.

20

JET SPEED [v/c]

PROJECTED DIS

5

Downloaded from https://academic.oup.com/mnras/article-abstract/486/2/2412/54

Kinematics Analysis w/ KaVA/EAVN

10

15

43GHz
VLBA
VLBA with KaVA-like uv
KaVA

10
5

0
Figure 3. A 43 GHz KaVA image of 4C+21.35. The
0
5
10
15 −1
three times
the rms noise
value (1.14
mJy beam ), an
PROJECTEDDISTANCE[pc]√

Figure 9. Jet kinematics derived from MOJAVE 15.4 GHz data. Top panel:
2. The two circles labelled with letters mark jet com
Core distanceas a functionof time forderived
four jet components.
BottomFigure2. Jetkinematics
from the22panel:GHz KaVA maps. TopLee+
panel:(2019) 8. Jet
able
to
track
reliably,
the
two
grey
crossedcirclesma
Figurecomponent
speedsasafunctionof
core
distanceforthree
Jet component speed as a function of core distance. The 1σ error bars are
Projected distance from the core as a function of time for all five different
jet
could
trackKaVA
reliably.
The CLEAN
43 GHzdatanotsets.re-identity
Blue: VLBA;orgreen:
data; skyblue:
VLBA bsmaller than the symbols.

components, separately for the outer components in the 10-mas blob (upperwith KaVA-likebars represent
uncertainties.
on uv-coverage.
the bottomError
left (0.79
mas ×1σ0.63
mas).
diagram)the three
innerscales
jet components(lower diagram). Bottom panel:orientationsandon parsec
to kiloparsec(Kharb, Lister & Cooper
09/24/2019, Mito
BU data; at 13 pc, however, the estimated speed was ∼7c. This is
Apparent speeds of the three inner components as a function of projectedExploring Blazars w/ EAVN
• Structure & proper motion (high-cadence monitoring:a large program for blazars?) of the ACZ• 1928+ (Lee’s talk); 1633+ (Algaba’s talk);
1803+ (GMVA PI: Cui); Mrk 501 (KaVA PI: Koyama);
Success
story
in
the
EA
VLBI
proposal
NGC 315 (VLBA, KaVA PI: Park) writing camp@Taipei (Jan. 2019)• RM study of the jet confining material (jet sheath /accretion flow / wind: Park+ 2018, 2019; Kam’s talk)inside the ACZ where the jet is presumably parabolic• Core shift? Blazar monitoring (Mrk 421/501)?
09/24/2019, MitoMessier 87 (M87)
5,000 ly

NASA, ESA and the Hubble Heritage Team (STScI/AURA)

0.5 lyEAVN Collaboration

0.01 ly

100,000 light year (ly)CFHT

EHT Collaboration
05/17/2019,
Taipei