1. Compact Radio Structure of Fermi-detected Radio-loud NLS1s CHEN YONGJUN, GU MINGFENG Shanghai Astronomical Observatory, CAS

2. 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) (F 5 /F B ) The narrowest Balmer lines, strongest FeII emission and lowest ratios of [OIII]/H 

3. 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

4. Fermi Detected RLNS1s with TS>16 SourceRed -shift γ rays (ph cm -2 s -1 ) MonTSRadio Morph. 1H 0323+342*0.061(1.60±0.06)×10 -7 3445 Core-jet (MOJAVE) SBS 0846+513 0.584(2.3±0.2)×10 -7 36560 Core-jet (MOJAVE) PMN J0948+0022* 0.585(3.2±0.2)×10 -7 52259Core-jet (MOJAVE) B2 1111+320.189(2.4±0.3)×10 -9 2216Core-jet (VLBA) PKS 1502+036* 0.409(7.3±2.4)×10 -8 2427Core-jet (MOJAVE) FBQS J1644+2619 0.145(7.5±1.6)×10 -8 5127Core-jet (VLBA) PKS 2004−447* 0.240(1.0±0.9)×10 -9 310 (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

5. Radio Structure of 1H 0323+342 and SBS 0846+513 MOJAVE PROGRAM

6. Radio Structure of PMN J0948+0022 and 1502+036

7. 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

8. VLBA Imaging Results S BandX Band DC DC

9. Radio Structure of FBQS J1644+2619 PKS 2004-447 From Orienti et al. 2012 From Doi et al. 2011

10. Core Nature of The Radio Structures SourceFlux (mJy)Brightness Temperature (K) Spectral Index Log(R) 1H 0323+342* 355.305.58e112.39 SBS 0846+513 284.331.16e12~0.03.16 PMN J0948+0022* 861.337.25e120.822.55 B2 1111+3238.59<5.50e10-1.26 PKS 1502+036* 578.594.21e110.663.19 FBQS J1644+2619 82.4 (1.7 GHz)~1e110.382.97 PKS 2004−447* 530.00-0.67

11. 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

12. Gamma and Radio Nature of SBS 0846+513   -ray luminosity~10 48 erg s -1  Doppler boosted  Core-jet structure on pc and unresolvable on kpc scale with superluminal motion 8.2c  Very bright core with T B above Comptom limit  Flat radio spectrum  Radio and  -ray emission are both Doppler boosted From D’Ammando et al (2012)

13. Gamma and Radio Nature of PMN J0948+0022  The first source detected  -ray emission and burst with ~10 48 erg s -1  presence 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

14. 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:   = -1.26  0.07 for VLA obs.   = -0.33  0.07 for VLBA obs.   = -1.20  0.12 for EVN  It’s more like a GPS source with compact structure

15. VLA-A Structure at Epoch 1992 Dec. 20 FQ =1.43 GHz BEAM = 1.62 X 1.39 at -3.6 X Unresolvable on subarcsec scale S BandX Band

16. 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

17.  With Non-simultaneous Data Ghisellini et al. (1993) X-ray data : 2002 Jun VLBA data: 2010 Nov   0.85 The result argues against relativistic hypothesis

18. 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

19. Gamma and Radio Nature of PKS 1502+036  L 0.1−100GeV = 7.8×10 45 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)

20. 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

21. 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

22. 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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