Compact Radio Structure of Fermi-detected Radio-

loud NLS1s

CHEN YONGJUN, GU MINGFENGShanghai Astronomical

Observatory, CAS

Definition of RL NLS1s

H slightly broader than forbidden lines (OIII, NII, SII), but generally < 2000 km/s

Relative weakness of OIII: [OIII]/H<3 Presence of emission lines from FeII or higher

ionization lines (Goodrich 1989) RL means: f(1.4GHz)/f (B) 10, a criteria from

Komossa & Voges 2006) (F5/FB )The narrowest Balmer lines, strongest FeII

emission and lowest ratios of [OIII]/H

Fundamental Features for RL NLS1s

Reverberation mapping and experimental relation from BLS1s systematically lower black hole mass (e.g. Boroson 2002) (X-ray variability, steller velocity & bulge luminosity)

High accretion rates close to or even above the Eddington rate (e.g. Komossa 2006): soft and hard X-ray

Host Galaxies: generally spiral First Fermi detected NLS1s: PMN J0948+0022,

7 with TS > 16, Third class of Gamma-ray AGN

Fermi Detected RLNS1s with TS>16

Source Red-shift

γ rays (ph cm-

2 s-1)Mon

TS Radio Morph.

1H 0323+342* 0.061 (1.60±0.06)×10-7 34 45 Core-jet (MOJAVE)

SBS 0846+513

0.584 (2.3±0.2)×10-7 36 560 Core-jet (MOJAVE)

PMN J0948+0022*

0.585

(3.2±0.2)×10-7 52 259 Core-jet (MOJAVE)

B2 1111+32 0.189

(2.4±0.3)×10-9 22 16 Core-jet (VLBA)

PKS 1502+036*

0.409

(7.3±2.4)×10-8 24 27 Core-jet (MOJAVE)

FBQS J1644+2619

0.145

(7.5±1.6)×10-8 51 27 Core-jet (VLBA)

PKS 2004−447*

0.240

(1.0±0.9)×10-9 3 10(43)

Core-jet (VLBA)

* With much larger TS shown in Abdo et al. (2009)

TS: http://www.brera.inaf.it/utenti/foschini/gNLS1/catalog.html

Radio Structure of 1H 0323+342 and SBS 0846+513

MOJAVE PROGRAMMOJAVE PROGRAM

Radio Structure of PMN J0948+0022 and

1502+036

VLBA OBSERVATION OF B2 1111+32

AT 2.3 AND 8.4 GHz Data: NRAO ARCHIVE Epoch: 2010 Nov 9-11, 20 min with 4

SCANS Instrumental Calibrator: 1749+096 Data Reduction: Standard method

VLBA Imaging Results

S Band X Band

D C D C

Radio Structure of FBQS J1644+2619 PKS 2004-

447

From Orienti et al. 2012From Doi et al. 2011

Core Nature of The Radio Structures

Source Flux (mJy) Brightness Temperature (K)

Spectral Index

Log(R)

1H 0323+342* 355.30 5.58e11 2.39

SBS 0846+513

284.33 1.16e12 ~0.0 3.16

PMN J0948+0022*

861.33 7.25e12 0.82 2.55

B2 1111+32 38.59 <5.50e10 -1.26

PKS 1502+036*

578.59 4.21e11 0.66 3.19

FBQS J1644+2619

82.4 (1.7 GHz)

~1e11 0.38 2.97

PKS 2004−447*

530.00 -0.67

Gamma and Radio Nature of

1H 0323+ 342 1H 0323+342 emits Gev, and even possibly

Tev radiation in a region very close to central black hole

MOJAVE shows an obvious one-sided structure with mild brightness temperature

A radio remarkable flare ever detected by a factor 3 with flat spectrum

Accretion rate: 90% Emission might be mildly Doppler-boosted

Gamma and Radio Nature of

SBS 0846+513 -ray luminosity~1048 erg s-1Doppler boosted

Core-jet structure on pc and unresolvable on kpc scale with superluminal motion 8.2c

Very bright core with TB above Comptom limit

Flat radio spectrum Radio and -ray emission

are both Doppler boostedFrom D’Ammando et al (2012)

Gamma and Radio Nature of PMN J0948+0022

The first source detected -ray emission and burst with ~1048 erg s-1presence relativistic jet (1.5e8 solar mass)

Very compact (~10 pc), very bright, core jet structure and strong polarization (3%)

Invert radio spectrum, the Comptom dominance is more extreme in SED relative to 3C273 (Forschini et al. 2010)

Yang, High accretion rate, Relativistic Jet

Gamma and Radio Nature of

B2 1111+32 B2 1111+32 is detected by fermi with

ts 16 The maximum core brightness

temperature: 5.50e+10 K Simultaneous core spectral indice:

= -1.260.07 for VLA obs. = -0.330.07 for VLBA obs. = -1.200.12 for EVN

It’s more like a GPS source with compact structure

VLA-A Structure at Epoch 1992 Dec. 20

FQ =1.43 GHzBEAM = 1.62 X 1.39 at -3.6

X

Unresolvable on subarcsec scale

S Band X Band

Doppler Boosting?

Komossa et al.(2006): = -0.56 (0.33 GHz and 1.4 GHz) = -1.24 (1.4 GHz and 4.85 GHz) Roughly agreement with our results Radio structure, spectral indices,

core brightness temperature GPS

With Non-simultaneous Data

Ghisellini et al. (1993)

X-ray data : 2002 Jun VLBA data: 2010 Nov 0.85The result argues against relativistic hypothesis

Gamma and Radio Nature of B2 1111+32

VLA-A and EVN with 5 an observations show compact radio structure, no extended emission was detected

Multi-frequency VLBA observation shows a signature of core-jet radio structure

Brightness temperature, spectral indices, flux variability and a rough estimate of Doppler factor argue more for GPS hypothesis with relatively strong radio emission

Gamma and Radio Nature of

PKS 1502+036 L0.1−100GeV = 7.8×1045 erg s−1

Unresolvable on VLA and core jet on vlbi scale

Invert radio spectrum 0.66, quite bright with T~4e11K

Superluminal motion not detected (multi-epoch)

Yang and slightly Doppler boosted From D’Ammando et al (2013)

Gamma and Radio Nature of FBQS J1644+2619

Intermediate -ray luminosity

Core-jet on pc and double structure on kpc scale

Flat spectrum, intermediate brightness temperature

Mildly Dopper-boosted

Gamma and Radio Nature of

PKS 2004-447 Relatively small Gamma-ray

luminosity with high confidence Unresolvalbe on ATCA scale and core-

jet-like structure on pc scale Steep above 8.4 GHz (-0.67) and

flatter (-0.33) below 4.8 GHz Like a CSO source and small Doppler

effect is expected as B2 1111+32

SUMMARY

For the 7 RL NLSY1s, two are strongly Doppler-boosted, 3 are mildly and 2 are trivially Doppler-boosted

Even for Fermi-detected RL NLSy1 sources, some are intrinsically radio and possibly -ray loud, some are Doppler boosted

All these Fermi-detected RL NLSY1s are expected to young objects with small black mass and high accretion rates

NLSy1s are younger and more Comptom dominant in comparison with Blazar objects

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