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Radio-loud Narrow-line Seyfert 1 galaxies introduction & motivation: - radio-loud radio-quiet bimodality - NLS1 galaxies GAVOGAVO search for radio-NLS1s.

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Presentation on theme: "Radio-loud Narrow-line Seyfert 1 galaxies introduction & motivation: - radio-loud radio-quiet bimodality - NLS1 galaxies GAVOGAVO search for radio-NLS1s."— Presentation transcript:

1 Radio-loud Narrow-line Seyfert 1 galaxies introduction & motivation: - radio-loud radio-quiet bimodality - NLS1 galaxies GAVOGAVO search for radio-NLS1s multi-  properties of radio-loud NLS1s models future follow-ups Stefanie Komossa, MPE Garching in collab. with, W. Voges, S. Mathur, D. Xu, H.-M. Adorf, G. Lemson, S. Anderson,. W. Duschl From Atoms to AGN, Tel Aviv, Feb. 2006

2 radio-loud NLS1s introduction: RL-RQ bimodality `RL-RQ´ dichotomy: quasars come in two flavors, radio-quiets and radio-louds with deficiency of sources at intermediate radio powers/indices [e.g., Kellermann et al. 89, Visnovsky et al. 92, Hooper et al. 95] recently debated: some samples don‘t [e.g., Cirasuolo & 03, White & 00], others do show the bimodality [e.g., Ivezic & 02, Sulentic & 03] what makes an object radio loud ? [e.g., Blandford 00, Wilson & Colbert 95, Laor 00, Ye & Wang 05, Best & 05, Metcalf & Magliochetti 05]

3 radio-loud NLS1s introduction: RL-RQ bimodality RL-RQ dichotomy in radio index (R) histogram R = f 5GHz / f 4400A R 5 > 10 (R 1.4 > 19) : RL [Kellermann et al. 89] RL-RQ distinction in `emission-line diagram´: [Sulentic et al. 03]

4 radio-loud NLS1s introduction: NLS1 galaxies defi: via optical spectral properties models: what drives correlations between line/ conti properties of AGN ? - (high) accretion rate and/or - (low) BH mass - inclination - metallicity - winds/density effects - absorption [e.g.,Osterbrock & Pogge 85] [e.g.,Boroson & Green 92, Pounds & 95, Wang & 96, Boller et al. 96, Laor & 97, Czerny & 97, Marziani & 01, Boroson 02, Xu & 03, 06b, Kawaguchi 03, Wang & Netzer 03, Grupe 01, 04, Grupe & Mathur 04, Botte et al. 04, Collin & Kawaguchi 04, Bachev & 04, Gallo & 05, Tanaka & 05; Osterbrock & Pogge 95, Puchnare- wicz & 02, Bian & Zhao 04; Mathur 00, 01, Komossa & Mathur 01, Shemmer & Netzer 02, Nagao & al 02, Warner & 04, Fields & 04; Xu & 06a, Lawrence & 97, Wills & 00, Bachev & 04; Komossa & Meerschwein- chen 00, Done & ] FeII [OIII] HH

5 introduction: NLS1 galaxies open questions, addressable with radio studies orientation m BH –  plane jet-disk coupling ? indications that Gal. XRBs in soft/hi state and AGN close to L Edd are radio weak.... This is the first systematic study of radio-loud NLS1s and their multi- properties*. Only 3-4 RL NLQSOs known previously: PKS , [Remillard & 86, Siebert & 99], RXJ [Grupe & 00], SDSS [Zhou & 03], SDSS [Komossa & 06], plus 1-2 cand.; and almost no prev. syst. radio studies of NLS1s [Ulvestad & 95, Moran 00, Greene & 06] * one study in parallel: [Whalen & 06, astro-ph]

6 GAVO GAVO search for radio-loud NLS1s cross-correlation of the Catalogue of quasars and AGN [Veron-Cetty et al. 2003] with radio and m B cat s using the matcher developed within the German Astrophysical. Virtual Observatory, [Adorf et al. 05] catalogues: PKS (4.85 GHz) PMN, 87 GB (2.7 GHz) VQC NVSS, FIRST (1.4 GHz) SUMSS (0.8 GHz) WENSS (0.3 GHz) USNO-A,B SDSS spec. GSC2.2 ROSAT, IRAS radio mBmB [Wright & Otrupcek 90, Griffith & 94, Gregory & Condon 90, Condon & 98, White & 97, Mauch & 03, de Bruyn & 98] [Monet & 03] [York & 00, Voges & 97] opt X, IR RL

7 search for radio-loud NLS1s: results 128 NLQSOs in VQC 90% within NVSS survey area, among these, 7% are radio-loud only ~2% exceed R=100 (for comp.: ~ 15% radio-louds among quasars) most radio-loud NLQSOs are compact, steep spectrum sources, not variable might be partly, but not fully, due to NLS1 definition as FWHM H  < 2000 km/s, indep. of L

8 radio-loud NLS1s: optical spectroscopy FWHM H ,dir = 960 – 2030 km/s, FeII/H  =0.5 – 3.2, [OIII]/H  = examples: H  - [OIII] 2 nd -most RL blazar ?? no strict NLS1 SBS SBS1517

9 radio-loud NLS1s: optical spectroscopy RXJ : extreme ´blue wingler´ in [OIII] FWHM [OIII],wing = 1550 km/s, v [OIII],wing = 1250 km/s [OIII] HH

10 radio-loud NLS1s: X-ray variability & spectroscopy  x = L sx ~ 10 erg/s X-ray data used for L/L Edd estimates SDSS , const. PKS , highly var. examples:

11 radio-loud NLS1s: results radio-loudness: radio indices

12 radio-loud NLS1s: results radio indices:

13 radio-loud NLS1s: results FeII-[OIII]-FWHM H  correlations: - radio-louds cover whole FeII-[OIII] range of NLS1s, - extend known radio-loud objects to those with small FWHM H  [Marziani & 01]

14 radio-loud NLS1s: results black hole masses*: - unusually low, given the radio-. loudness of the galaxies, but at upper end of NLS1s; - in a prev. rarely populated regime of the `Laor diagram´ * estimated from L (5100A) and FWHM H  [Kaspi & 05]

15 radio-loud NLS1s : models starburst contribution ? - radio powers P are all in RL regime - IRAS – radio corr.: P factor above expected starburst contrib. - ionisation para., SDSS : log U ~ -2.4 (typ. for Sy) EUV excess: NeIII/NeV is good indicator of continuum shape, once U is known

16 radio-loud NLS1s: models to explain lower frequency of RLs among NLS1s relativistic beaming ?  pole-on view - most are steep spectrum sources, with radio spectral indices  r < -0.5; beaming not expected - exceptions: SDSS , RXJ :  r =0.6, SDSS var. in radio, PKS0558 highly var. in X - X-ray spectra of beamed sources typically much flatter  : beaming cannot be excluded, but no positive evidence for it, with 2-3 exceptions Why are RL NLAGN more rare than RL BLAGN, and is the mechanism for RLness the same in NLAGN and BLAGN ?

17 radio-loud NLS1s: models to explain lower frequency of RLs among NLS1s accretion mode: in Gal. X-binaries in soft/high-state (&AGN), radio emi. quenched for high acc. rates [e.g., Maccarone &03, Greene & 06].  mechanism which suppresses radio- emi for high L/L Edd also responsible for low RL-fraction in NLS1s ? RL NLS1s: Eddington ratios: 10 L x /L Edd = more theoret. studies needed -- spin: spin-jet coupling e.g. via Blandford-Znajek or Blandford- Payne mechanism. Why, NLS1s on ave. less rapidly spinning BHs ?  BHs still growing ?? Then, few RL ones should be more evolved. Indeed, they are closer to M BH –  relation of AGN than other NLS1s [Mathur & Grupe 05]

18 radio-loud NLS1s: follow-up studies larger samples, based on SDSS: low-L NLS1s; radio-loudness etc. in dependence of FWHM; interesting individual objects (jet sources ?) optical spectroscopy: line-profiles, exti,  R, M BH make use of line ratios wih diagn. power radio imaging: how compact are the sources ? at diff. : spectral indices, steepness monitoring: variability, beaming ? X-rays: spectra, absorption, variability theory: jet-disk models, dep. on acc. rate

19 Summary identification of RL NLS1s radio: most sources are compact, of steep spectrum, and not variable; R of all det. sources covers > 4 orders of mag. BH masses in prev. rarely populated regime of Laor diagr. opt-X prop. similar to RQ NLS1, radio properties extend the range of RLness to small FWHM H  fraction of RL NLS1s (7%) < RL BLQSO mech.: no SBs, no positive evidence for beaming in most sources, so far. Accretion mode & spin ? future: larger samples; radio-obs: compactness of sources, spectral indices, variability; + multi- [Komossa et al. 06a, ApJ 639, in press; 06b, AJ, subm.]


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