Image credits: D. Battefeld“Joint XMM-Newton and NuSTAR
observations of the reflection spectrumof III Zw 2 “Wara Chamani, Karri Koljonen andTuomas Savolainen
Aalto University Metsähovi RadioObservatory, Finland
AGN Jet Workshop January 2020
Tohoku University, Sendai

Spin estimation ofthe Supermassive
Black Hole of III Zw 2

Black hole spin observations→ 22 robust spin values measured
using X-ray reflection method.
→ No Spin vs BH mass correlation.

Reynolds 2019.

Motivation of this work
→ A wide radio-loudness (R) distribution inAGN.
→ at leat 4 orders of magnitude of accretion
rate difference!.
What creates a powerful black hole jet?
“Spin paradigm” → attempts to explain thewide R (Wilson & Colbert 1995, Blandford 1999,Sikora+2007, Tschekhovskoy+2010).

Sikora+2007.

Powerful jet → High black hole spin?
Weak jet → Low black hole spin?
Which other parameter can dominate
besides the spin?

Motivation of this work
Magnetic flux threading the black hole →that launch powerfull jets.
“Magnetic flux paradigm” → may explain
the R dichotomy (Sikora & Begelman2007).
Magnetically Arrested Disk (MAD) (Narayan +2003; Tchekhovskoy +2011; McKinney + 2012)
explains the powerful jets.

Jet magnetic flux versus LaccMBH for
FSRL+RG+Low Luminosity Radio
Loud AGN. Solid line is the MAD
prediction. (Zamaninasab+2014)

Motivation of this work
Magnetic flux threading the black hole →that launch powerfull jets.
“Magnetic flux paradigm” → could explain
the R dichotomy (Sikora & Begelman2007)
Magnetically Arrested Disk (MAD) (Narayan +2003; Tchekhovskoy +2011; McKinney + 2012)
Tested in a sample of powerful jets.
Physical parameters MAD model: BH spin(X-rays) + Jet’s Magnetic field flux (VLBI).
Oursample(weakjets)(1<R<200):
E1821+643,
III Zw 2 (presented in this conference), PG
2209+184 and PG 1309+355.

Jet magnetic flux versus LaccMBH for
FSRL+RG+Low Luminosity Radio
Loud AGN. Solid line is the MAD
prediction. (Zamaninasab+2014)

The nature of III Zw 2.


A RIQ, it certainly emitsradiation from radio togamma-ray wavelengths.
Highly variable in radio bandemissions.
Li+2010:
Quasi
periodicactivity. Outburst period ~ 5years at 22 and 37 GHz. Thismight be due to the rotationof the helix in the jet.

VLBI observations of III Zw 2
Core dominated flat radio spectrum

It has a compact radio core.

VLA-A configuration 1.4 GHz
image in the MOJAVE sample(Cooper+2017).

MOJAVE archive.

A jetted source with a apparent superluminal
motion :1.58±0.29c (Lister et al. 2019).
Maximum jet’s viewing angle: 41o (Brunthaler+2000).
X-ray reflection spectrum
ObserverDirect Power-law

xx“Reflection”
spectrum
Accretion

BHdiskImage credits: Fabian 2016.

X-ray reflection spectrum
ObserverDirect Power-lawxx“Reflection”
spectrum
Accretion

BH

disk
Credits:
Fabian2016.
Image
credits:Fabian2016.

Black hole spin, FeK line at 6.4 keVImage taken NASA
from NASA
pictures..
pictures.

Black hole spin, FeK line at 6.4 keV
X-ray Reflection spectrum

Ionization
degreeImage
taken
fromNASA
NASApictures.
pictures..
Image
taken

Credits: Fabian+2000.

Simultaneous X-ray satellite observations ofIII Zw 2
●Our observations were made on 11.12.2017
NuSTAR
XMM-Newton
26.03 hours of exposure
11.94 hours of exposure=+Broad BandenergyX- rayobservations(0.2 – 70 keV)

Data reduction: running different pipelines and checking of pileups.
●Data analysis with the ISIS (Interactive Spectral Interpretation System) package.
●Reflection spectrum of III Zw 2

20172000

Our observations taken in2017 gathered more X-ray
data.
Hard X-ray detections >10keV.
XMM archival data of 2000.
X-ray flux increases after
17 years by a factor of ~2.

Search for the presence of FeK line
Residuals of Power Law fit to the spectra

Energy of the FeK line: 6.4 keV

Search for the presence of FeK line
Residuals of Power Law (PL) fit to the spectra
Soft-excess

Soft-excess
Iron line

Energy of the FeK line: 6.4 keV

FeK line detection(Salvi+2002, Piconcelli+2005,Jiménez-Bailón+2005).

Search for the presence of FeK line
Residuals of a Power law + Black Body fit

A good improvement on thefitting of the 2017-soft excess.
Soft-excess still visible on the2000 data.

Soft-excess
Iron line

Energy of the FeK line: 6.4 keVBlack body temperatures: 136144 eV >> standard disk
temperature (~10 eV).
Which mechanism is driving thesoft-excess?

X-ray relativistic reflection models
RELXILL modelRELXILL-LP (Lamp-post)(Garcia +2014).

model (Dauser+2013).

RELXILL code =XILLVER code
(reflected spectrum)+RELLINE code
(relativistic blurringeffects)

hImages credits: Chauvin+2018

X-ray relativistic reflection models
Physical parameters:
Spin: a

Reflection fraction: R

RELXILL modelRELXILL-LP (Lamp-post)(Garcia +2014).

model (Dauser+2013).

h

Disk Inclination: θIonization parameter: ξIron Abundance: AFE

Power Law photon index: ΓImages credits: Chauvin+2018

Fitting the data with RELXILL
Spin ‘a’ and other parameters obtained with a joint-fit
RELXILL fits abroad Fe linea > 0.98.
●
θ ~ 41o (pegged to the limit)● R~ 2* R2017
2000●

Relxill joint-fit results for different disk inclination

Relxill joint-fit results for different disk inclination

Chamani+2019, submitted to A&A

Summary and discussion








Soft -excess observed in the XMM 2000 and 2017 data sets.
A promiment Fe Kα line detected in the XMM 2000 data set(Salvi + 2002; Piconcelli + 2005; Gonzalez + 2018).
The relxill fits favour fast rotating black hole a~0.9 in III Zw 2,
but it has a weak jet!.
High spins does not produce necessarily powerful jets.
Do III Zw 2 jet is below the MAD level? We will measure themagnetic flux with VLBI observations (in collaboration withHada-san).

Thanks for your attention!