Closing Remarks
Tamna 21 m

Miyun 50 m

Sejong 22 m

Yonsei 21 m

Ulsan 21 m

Gifu 11 m

Usuda 64 m

KVN

Nanshan 26 m

Mizusawa 20 m

Takahagi 32 m

CVNVERAJVN

Tianma 65 m

Kunming 40 m

Sheshan 25 m

Yamaguchi 32 m

(Image Credit: Reto Stöckli, NASA Earth Observatory)

Kenji TOMA (Tohoku U)

Hitachi 32 m

Ishigakijima 20 m

Kashima 34 m

6.7 GHz
8 GHz
22 GHz43 GHzIriki 20 m

Nobeyama 45 m

Ogasawara 20 m

Wind (or Accretion?)

Bondi radius?

Disk

BHJet

Mazin, Chamani, Hayashida

Limb-brightening

EHT 2017 & next
- Jet driving mechanism
LBZ = LBZ(WH, BH)- BH spin, gravity theories- Polarization/time domain- GLT (350 GHz)& more stations- Space VLBI
- Sims: Rhigh, density floor
Tazaki, Akiyama,
Mizuno, Kawashima

Gamma-rays/X-rays- Jet, disk, magnetosphere?
- Fe lines- X-ray interferometerBlazars- EHT view, kinematics- Polarization Kim, Shin,

K-W Lee
EAVN & next
Radio Galaxies- Jet kinematics- LLAGN, NLSy1- Width profiles- Two key “3”s Ohsuga,- Acceleration mechanism - Population
Hada, K Lee- Core shift:Plasma microphysics
B field strength- Te/Tp- Energetics- Non-thermal p / neutrinos
Park, Nakahara, Jung, Niinuma,- Jet MHD breakdown
Nakamura, Kino, Tanaka,Ohmura

Kawazura, Kimura, Kisaka

KaVA, 22 GHz

napp = n(1cos ✓v )<latexit sha1_base64="gL4fK38tuxthHD91F5S/v7eOEK8=">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</latexit>• Number of faster blobs looks smallerDec (mas)

One point

4202
WISE - 0.2 mas

40510RA (mas)152025Park, Hada, Kino et al. 2019tFig. 6.— Stacked maps of the CLEAN images at 22 (left) andp43 GHz (right) rot
Contours start at 0.8 mJy per beam and increase by factors of 2. The displaceme
at the finest SWD scales are shown with the arrows (see Section 4.3 for more details

BlobstLight

FasterWe assumed the minimum scale to be ⇡ 1/5 of thebeam size and maximum scale to be about one beam
blobs
size. We applied the SWD on three spatial scales of 0.2(0.12), 0.4 (0.24) and 0.8 (0.48) mas and amended themwith the IWD on scales of 0.3 (0.18), 0.6 (0.36), and 1.2(0.72) mas at 22 (43) GHz. We identify SSPs in adjacent epochs by using the MCC method with a tolerance
factor of 1.5 and a correlation threshold of 0.7. In theMCC analysis, we search for velocity vectors with symmetric search windows of [ 31, +31] mas/yr and [ 18,+18] mas/yr in a longitudinal direction relative to thejet axis at 22 and 43 GHz, respectively. We used searchwindows of [ 10, +10] mas/yr and [ 5, +5] mas/yr in atransverse direction at 22 and 43 GHz, respectively. This
constraint is based on the maximum SWD/IWD scales
and the typical time separation between adjacent epochs.
We use velocity vectors of the SSPs matched in at least
four successive epochs for our further analysis. We obtained the apparent speeds by fitting linear functions totheir separation from the core with time.
We note that we used symmetric velocity searchwindows, while previous studies using WISE analysis
adopted asymmetric search windows in a longitudinal direction (Mertens et al. 2016; Boccardi et al. 2019). The
reason for using asymmetric windows in those studies isbased on our prior knowledge that fast inward motions
are not physically realistic. However, at least for thepresent study, we found that using an asymmetric velocity search window can lead to biased results towards
detecting faster speeds. In Appendix B, we perform several tests by using one hundred randomly shu✏ed images of the VLBA 1.7 GHz data presented in Section 5,
which provide us with a number of detected WISE vec-Light
ObserverObserver-rrthat false
suppressed
matched ina number
dom data
sive epocha longer leepochs, ifless, we haages and u
Instead, w
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Boccardi eprobability
We fo
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because this short enweeks, Meon this arscales, whlution amo
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motions to-See Komissarov & Falle 1997
4.4. Jet AMany thanks for your participations,contributions & discussions!
Let us keep in touch & make ourcommunity more active.
We will prepare a next BH/jet workshop.