Collimation, Acceleration, and Recollimation
Shock in the Jet of Gamma-Ray Emitting
Radio-loud NLSy1 Galaxy 1H 0323+342

Optical/HST(Foschini+)

AGN jet workshop 2020, Jan 20-22 2020, Sendai
Kazuhiro Hada (NAOJ)

Collimation, Acceleration, and Recollimation
Shock in the Jet of Gamma-Ray Emitting
Radio-loud NLSy1 Galaxy 1H 0323+342

Optical/HST(Foschini+)

AGN jet workshop 2020, Jan 20-22 2020, Sendai
Kazuhiro Hada (NAOJ)

“Classical” AGN withpowerful relativistic jets
Radio galaxies(FR-I, FR-II)

M87Blazars(BLLac, FSRQ)

3C273• Hosted in massive elliptical galaxies• Large BH masses (>108-9Msun)• Low / Moderate accretion rates (L/LEdd < 0.1)

Discovery of γ-ray emission from NLSy1
Abdo+2009

Abdo+2009
Fermi-LATPMN J0948+0022••

A new class of AGN producing powerful jets
Jet formation in different (MBH, Mdot) domain from blazars and RG

50-5

Parsec-scale structures of γ-NLSy1

D1

D’Ammando 2019

C0
• Currently
9 NLSy1 areD2
confirmedin GeV γ-rays
5 pc(4FGLcatalog)
1050-52011 Fermi & Jansky: Our Evolving Understanding of AGN, St Michaels, MD, Nov. 10-12

PKS 1502+036

5VLBA 8.4 GHz

15.3 GHz(2005.636)
PMN
J0948+0022

PKS 1502+036

Peak = 536.1; f.c. = 0.6 (mJy/beam)

4D1b011/JAN/2002

6above 8.4 GHz make PKS 2004-447 a candidate ofbeing a young radio source rather than a blazar. To
unveil the nature of this source new multifrequency
observations with parsec-scale resolution have beenrequested.

2-5D2C0MilliARC SEC

Although the radio properties are important toconstrain the emission mechanisms in the low-energy
part of the spectrum of RL-NLS1s, at centimeter0wavelengths, i.e. those discussed here, their emission
is highly aﬀected by synchrotron self-absorption.
-2
The one-zone homogeneous model adopted for thebroad-band SED of these sources [e.g. Abdo et al.
2009b] is based on a single synchrotron emission-4
5 pc
component which does not fit the radio data,
Orienti+12
being all the emission below 1012 Hz considered
Doi+06
6
2011 Fermi & Jansky: Our Evolving Understandingself-absorbed.
of AGN, St Michaels,MD, Nov.
10-12mm/sub-mm
Informationon the6420-2-4-6
emission is fundamental to set tight constraints on
MilliARC SEC
1050-5
thelow-energy
emission,and ALMA
observations
will
PLot file version 1 created 01-MAR-2011 16:08:57
in France
for science
analysisduringthe operations
PKS2007-445
2004−447
CONT:
IPOL 1451.992 MHZ PKS2004B16.ICL001.1
open
for acknowledged.
investigating thesein
phaseaisnew
alsowindow
gratefully
Thesources
VLA andanFig. 1. VLBA contour maps of SDSS J094857.380+ 002225
on 2003f.c.=
October
30. The contour levels are
3σ
× −1,are1,frequency
2, 4, 8, domain.
16,
and Radio
theunexplored
VLBA
operatedby 32,
the 64,
US 128,National
peak=200.1;
0.9(mJy/beam)
6: VLBAimageat 15.3
GHz8.4,of PKS
Observatory
which isofa C0
facilityof the Na256,VLBA
where σis therms of image noise at eachFigure
frequency.
In theimages
at 5.0,and1502+036
15.4 GHz, “ + ” Astronomy
symbols represent
the positions
and C1
15.4
GHz
collected on 11 January 2002. On the image we provide
tional Science Foundation operated under cooperative
60
components,
which
wereidentified
byvisibility-basedmodel
fitting(subsection
3.1).
therestoringbeam,plottedinthebottom
leftcorner,the(2010.789)
agreement by Associated Universities, Inc. This repeak flux density in mJy/beam, and the first contour
search has made use of the NASA/IPAC Extragalac(f.c.)40 intensity in mJy/beam, which is 3 times thetic Data base (NED) which is operated by the Jet
C by a factor
oﬀ-source noise level. Contour levels increase
Propulsion Laboratory, California Institute of Techof 2.20
APKS 1502+036 15.3 GHz
21/JUL/2006
nology,under contract with the National
Aeronautics
in diameter. The VLBA observation should have the ability 3.3. Measured Flux Densities
and 6Space
Administration.
Peak = 521.7; f.c. = 0.5 (mJy/beam)
0to resolve a size of ∼ 0.10 mas for the andstronger
component.
PKS 1502+036 is dominatedTheby a measured
flat-spectrumflux densities are listed in table 2.
WeThe size of 0.10 mas corresponds to a decreaseof∼ 10%
incompactandbrightcomponentfrom which a fainter-20
4 from the root mean square of theestimatedthetotalerror
References
jet-like featureemerges.
the visibility amplitude at the longest baselineof theVLBABothBsources show substanflux density variability. uncertainty of amplitude calibration and the error in the-40
at 15 GHz. Because of the sufficiently tial
goodsensitivity
and2
In the case of PKS 1502+036,
the availability
ofGaussian
fitting (including
thermalnoise).
Abdo,A.A., et al.
2009a, ApJ, 707, 727
calibration, we were able to determine thefringe VLBAvisibilitytotwo-epoch
observations
at 15 GHz allowed
Abdo,
A.A.,
etal.
2009b,ApJ, 707,-60The
totalspectraoftheobserved
VLBA
fluxL142
densities
2 pc
us
todetectanewcomponent
atabout3mas
from
5% (see similar discussion
by Kellermann et al. 1998). Thus,Anton,S., et al. 2008,
0
Wajima+14+ α A&A, 490, 583
∝ν),
which
isconsistentwereslightlyinverted(α>0,S
the central region that was notvisible in the first
Orienti+12
Dallacasa, D.,ν et al. 2000, A&A, 363, 887
we assume that the effective resolution observingof -80our VLBA
epoch. obserAssuming thatthiscomponent
iswithpastobservations.
Nonsimultaneous
observations
fromD’AmmandoF., et al. 2012,
submitted to MNRAS
6040
200-20-40-60-80-100-2vation
is aboutknot aofquarterthe jetdetected
at about 1 mas
8 at 156 GHz is
4 around
2 0.100mas, which-2 the same
MilliARC
SEC
Deo,
R.P., et al. 2006, AJ, 132, 321
111.5
Center at RA 20 07 55.1880000 DEC -44 34
43.102000 mJy at 1.4 GHz by the FIRST survey (Becker et al. 1995)

PKS 2004-447

1H0323+342D3• Past VLBI suggests– Very compact (point like)– One-sided core-jet– Similar to blazars

C0-6-4

D2• Further details are still
poorly understoodMilliARC SEC

D1MilliARC SEC-202-10

D1a5

Downloaded from http://pasj.oxfordjournals.org/ at National AstronomicalObservatory, Japan on December 11, 2014

-10

VLBA 8.3 GHz(1996.374)

1H 0323+342

HST (Foschini 2011)

MOJAVE 15GHz(z = 0.06)• Nearest γ-ray NLSy1– Host galaxy spatially resolved•Abdo+2009
Fermi-LAT

Pc-scale jet well resolved– 1mas = 1.2pc (projected)

6pc(projected)•Hint of jet acceleration– <1c near core, ~9c in downstream•

Small viewing angle– θview< 4 - 12(Lister+16; Fuhrmann+16)•Lister+2016

Rebrightened feature “S”– Stationary over a decade (Wajima+14)

1H 0323+342

HST (Foschini 2011)

MOJAVE 15GHz

Stationary feature
at 7mas “S”(z = 0.06)• Nearest γ-ray NLSy1– Host galaxy spatially resolved•

Abdo+2009
Fermi-LAT

Pc-scale jet well resolved– 1mas = 1.2pc (projected)

6pc(projected)•Hint of jet acceleration– <1c near core, ~9c in downstream•

Small viewing angle– θview< 4 - 12(Lister+16; Fuhrmann+16)•Lister+2016

Rebrightened feature “S”– Stationary over a decade (Wajima+14)

New VLBI study of 1H 0323+342:
Motivation••

The source offers a privileged opportunity to study the details of jet
formation in NLS1(nearby, bright, resolved)
Despite this observational advantage, only a few basic jet
properties have been known yet– What is the nature of the stationary feature “S”?
– What is the difference from or similarity to jets in blazars / radiogalaxies?
– Spectral properties?
– Collimation / Acceleration properties?
– Where is the location of γ-ray emission?
– Any hints on BH mass (~107Msun vs >108Msun)?
• Leon Tavares+14, D’Ammando+18•

To address these questions in more detail, we performed a new
multi-frequency VLBA program

The Astrophysical Journal, 00:000000 (11pp), 2018 Month Day

Hada et al.

Jan2016

ADA ET AL .

Spectral index
distributions(A) α(2.3-5.0)(B) α(8.7-15.5)(C) α(15.5-23.9)(D) α(23.9-43.3)

6Core shiftH ADA

0.1pc

Figure 4. Spectral index (defined as Sν ∝ ν +α ) distribution of
1H 0323+342 for various frequency pairs (color maps): (A) between 2.3 and 5.0 GHz; (B) between 8.7 and 15.5 GHz; (C) 15.5
and 23.9 GHz; (D) 23.9 and 43.3 GHz. Contours in each inset are atotal intensity map at the lower frequency, starting from (1, 2, 4, 8,16, 32, 64,...) times 0.2 mJy/beam. Yellow ellipse in each inset isthe size of convolving beam.

Core: flat spectra → SSA thickJet: steep spectra → SSA thin

Very small core shift ( < 100uas)→ Small viewing angle

Figure 3. Astrometry of the core position of 1H 0323+342 at various frequencies. Position of the 24 GHz core is set to be the coordinate origin of this plot. Note that position of the 43 GHz core isalmost identical to that of the 22 GHz core. The contours are a total
intensity map 1H 0323+342 at 43 GHz. Grey-shaded ellipse indicates a best-fit elliptical Gaussian model to the 43 GHz core (seeTable 2). The cross symbol indicates an extrapolated position z0 ofthe origin of the parabolic jet (see Section 3.3), which is a likely

Just typical to blazars. Nothing surprising?

errors for each data are one-tenth of the beam size, which

Jet collimation profile
M ULTI - FREQUENCY VLBA STUDY OF 1H 0323+342

(C)
(B)

(A)

5

Jet collimation profile
M ULTI - FREQUENCY VLBA STUDY OF 1H 0323+342

50 .5z∝)(zraaP(A)

cWilbo8Co
nicalW(z )∝(B)

z 1 .4(C)Recollimation
at S (7mas)

Jet collimation profile
M ULTI - FREQUENCY VLBA STUDY OF 1H 0323+3425(C)Jet radius (Rs)

10 410 3102100 .5z∝)(zraaP∝(z )MERLIN 1.7GHz (AN12)
EVN 1.7 GHz (AN12)
VLBA 2.3 GHz (H13)
VLBA 5.0 GHz (H13)
VLBA 8.4 GHz (H13)
VLBA 15 GHz (AN12, H13)
VLBA 24 GHz (H13)
VLBA 43 GHz (AN12, H13)
VLBA 86 GHz (H13, H16)
EHT 230 GHz (D12, A15)W

105Conical6

Bondi radius

10z 1 .4(B)Remarkably similar to M87/HST-1!

8cWilbo

HST-1Recollimation
at S (7mas)

(A)

ISCO

Asada&Nakamura 2012
Hada+ 2013

110 -110 -1

11010 2

10 3

10 4

10 5

De-projected distance along jet (Rs)

10 6

10 7

10 8

Large(kpc)-scale jet586

STUDY OF 1H 0323+342

7

S. Antón et al.: The colour of the na

VLA 1.4GHzVLA(C)(B)

MERLIN

Fig. 6. VLA 1.4 GHz maps of 0324+3410 in A (left)
and C (right) configAnton+2008
the A-configuration and 0.0005 Jy/beam for the C-configuration.

⟨∆(B − R)/∆(log r)⟩ = − 0.09 ± 0.07 is cited for non-radio emitting galaxies (Peletier et al. 1990). Therefore the colour gradient(A)
of J0321+3410 is consistent with the above trends, but perhaps
a more extreme example.
There is a colour reversal, a blue-ward swing, at radial distances r(arcsec) < 3, clearly visible in the colour
image and profile, Fig. 4. The radial colour gradientFigure 5. Extended plot of jet width profile of 1H
0323+342
includis ∆(B− R)/∆(logr) = 0.3 ± 0.02. Since we are dealing with anLarge-scale jet
significantly deviatesfrom parabola5pc

Nature of S ?
(g) 15.5GHz•Observed jet collimation profile strongly
suggests that the parabolic-to-conicaltransition occurs in “S”•Very similar to HST-1 in many aspects– Quasi-stationary– Location from the core (~100pc)– Compressed and rebrightening•

Suggests a recollimation shock at theend of collimation zone

S2pc

Figure 1. VLBA images of 1H 0323+342. (a),(b),15.5, 23.9, 43.3 GHz, respectively. For each image
The yellow ellipse at the bottom-right corner of eac
7 mas from the core.

3.2. Jet width profile

Cheung+07Measuring the profile of jet width W (z)of radial distance z provides important clue
mation and collimation mechanisms of a r
as demonstrated in recent VLBI studies oH ADA ET AL .

IN/VLA data,approaching agests that therbolic/conicalS. This situof the jet inabolic to connary (and pos∼120 pc froms to be slightly
profile. Thisrecollimationng et al. 2007;

CoreBars: EVPA
EVPA NOT RMcorrectedS

1.2 pc (projected)

f jet width at-1. This feaFigure 6. VLBA 15 GHz polarization map of 1H 0323+342. We rend the present
examinedpolarization
properties
archivetrievedthe calibrated
data from the MOJAVE
15 GHzusingarchive.MOJAVETheWhile• in We
M87 further
total intensity distribution is shown by contours, while the fractional
mation• zone”
Stronglypolarization
polarizedfeatureon Sby(Fractional
distribution
is shown
color (the values Polare in~30%)
per1H 0323+342
cent).
Note that the
EVPA shown are not RM-corrected.
• =>ofHighlyorderedB-fields
t upstream
e of parabolicmeasure (RM)-corrected ones, preventing us from discussing
The rebrightthe intrinsic
geometryof Takamurathe B-fields associatedthe jet. polarization analysis
See posterby M.
for more withextensive
flattening at SM ULTI - FREQUENCY VLBA STUDY OF 1H 0323+342

Coexistence ofjet collimation &acceleration

7 jet (Nakamura & Asada 2013; Asada et al. 2014;
et al. 2016; Hada et al. 2017), and these studies areng to uncover the physical link and coexistence of thetion and collimation zone (ACZ) in this jet, which
eement with magnetic collimation and acceleration(e.g., Nakamura et al. 2018). However, hitherto very
ervational evidence of ACZ is obtained for other•S

Collimation profile seems to be

H 0323+342, Fuhrmann et al. (2016), Lister et al.
closelywith superlumijetnd Doi etal. (2018)correlated
detected significant
velocity
ons at parsec
scales.profile
Interestingly, they consistently
trend of gradualincrease ofjet proper motion with– Parabolic– acceleration. Also, the lower brightness temperature of the core– γ-ray
Jet speed
saturates
near S
se of typicalblazars indicatesa relatively
mildfactor in the core region, suggesting that the innerregion is still not fully accelerated (Wajima et al.
• Γφ ~ 0.01 <<1uhrmann et al. 2016). Therefore, it would be of great
Collimation/acceleration
to compare–thosevelocity results and the collimationbtained in ourcausallystudy.
connectedClausenure 7, we show
a combined plot of the proper moBrown+13
the literature, Lorentz factors (Γ) calculated basedroper motion results, jet collimation profile and theonding
opening anglewith
profiles,as a function of• fullConsistentmagnetic
cted distancefrom the core.
Herewe adopt θview =collimation
andacceleration
calculate the deprojected distance. We also assume
scenarios
proper motions
traced by jet components reflect bulk

Γ (θview= 5)φDeprojected distance (pc) for θview=5

9The Astrophysical Journal, 789:143 (15pp), 2014 July 10

γ-ray production
far from BH?

Paliya et al.

F0.1−100GeV

24

•

F1

18

F2F3

Fermi-LAT(Paliya+2014)

Q

126Feature S (z ~ 100pc for θview=5) The Astrophysical Journal Letters, 857:L6 (6pp), 2018 April 10
XRT– Counterpart of HST-1– Maximally beamed at the endof ACZ
Previous GeV flares coincided
Swith the passing of superluminal
Time (MJD - 54600)
components throughFigure
S3. Different activity periods selected for SED generation and modeling. Q corresponds to a quiescent state, while F1, F2, and F3 are three flaring states whenenhanced γ -ray emission is detected from the source. All units are the same as in Figure 1.
01.2

0.9

F0.3−10keV•

1 week binned
1 day binned

Fermi-LAT

0.6

0.3

0200

400

600

800

1000

1200

1400

1600

1800

2000

2200

(A color version of this figure is available in the online journal.)

However...
tvar~ R(1+z)/cδ ~ 30days– Too large to explain day-scale
γ-ray variabilities– Substructures in S
3.6

3.6

3.6

Flare-1

Flare-2

3.2

Flare-3

3.2

3.2

2.4

Γ0.1−100GeV

Γ0.1−100GeV

2.8

Γ0.1−100GeV

•
•

2.8

2.8

2.4

2.4

2.0

2.0

2.0

1.6

02468

10

Flux0.1−100GeV (10−7 ph cm−2 s−1)

1214048

Flux0.1−100GeV (10−7 ph cm−2 s−1)

1204Doi, KH+2018

812162024

Flux0.1−100GeV (10−7 ph cm−2 s−1)

Figure 4. Photon flux vs. photon index variations of 1H 0323+342 during different flaring states. The dashed line is the weighted linear least-squares fit to the data.

Suggested picture of
1H 0323 jetθv

ie wγ-rays?

γ-rays?
Γ~10Conicalexpansion

BHRadiocore

<1pc~


2
14-Recollimation
shock
Acceleration & collimation zone

~100pc~kpc

BH mass:
low or high ?

– Suggested by M-σ relation (eg,Leon Tavares+14)– Jet collimation break occurs
near the sphere of SMBH
gravitational influence– (RSGI = GMBH/σ2~106Rs)

Which is true?

S~RSGIS• If MBH ~ (3-5) x 108Msun

HST-1– Suggested by optical/X-raystudies (eg, Zhou+07, Landt+17)– Jet collimation must be
maintained over 100000000Rs
from BH !

HST-1• If MBH ~ (1-3) x 107Msun

Deprojected distance (Rs)Summary of this study•

We studied the detailed radio structures of the pc-scale jet of thenearest γ-NLSy1 1H 0323+342 using multi-λ VLBA

•A number of exciting discoveries !
– Highly polarized, recollimation shock feature S– Jet collimation break at the recollimation shock– Coexistence of jet collimation and acceleration– Possible gamma-ray production at ~100pc•

The pc-scale jet of 1H0323+342 is remarkably similar toM87/HST-1 (as well as some blazars), suggesting that a common
jet formation mechanism may be at work. But...

•

Why 1H/M87 jets so similar despite very different (MBH, Mdot)?
– True MBH (and Mdot) different from previously thought?
– Different BH spin? (Landt+ 2017)– Environmental effect? (Efficient winds from super-critical flows)Ongoing / planned MWL projects on NLSy1 jets

AppendixLimb-brightening structure
The Astrophysical Journal Letters, 857:L6 (6pp), 2018 April 10Doi et al.

Doi, KH+2018
Figure 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