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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
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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
THANK YOU FOR YOUR ATTENTION