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Compact Radio Structure of Fermi-detected Radio-loud NLS1s

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

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Compact Radio Structure of Fermi-detected Radio-loud NLS1s

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  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) (F5/FB ) 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 TS: http://www.brera.inaf.it/utenti/foschini/gNLS1/catalog.html * With much larger TS shown in Abdo et al. (2009)

  5. Radio Structure of 1H 0323+342 andSBS 0846+513 MOJAVE PROGRAM 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 Band X Band D C D C

  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

  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~1048 erg s-1Doppler 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 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 ~1048 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 S Band X Band Unresolvable on subarcsec scale

  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 • 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)

  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

  23. THANK YOU FOR YOUR ATTENTION

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