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Radio-loud Narrow-line Seyfert 1 galaxies

From Atoms to AGN , Tel Aviv, Feb. 2006. Radio-loud Narrow-line Seyfert 1 galaxies. Stefanie Komossa, MPE Garching in collab. with, W. Voges, S. Mathur , D. Xu, H.-M. Adorf, G. Lemson, S. Anderson, . W. Duschl.

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Radio-loud Narrow-line Seyfert 1 galaxies

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

  2. radio-loud NLS1sintroduction: 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 NLS1sintroduction: RL-RQ bimodality • RL-RQ dichotomy in radio index (R) histogram R = f5GHz / f4400A R5 > 10 (R1.4 > 19) : RL [Kellermann et al. 89] • RL-RQ distinction in `emission-line diagram´: [Sulentic et al. 03] 0 1 2 3

  4. radio-loud NLS1sintroduction: NLS1 galaxies Hb [OIII] FeII FeII [e.g.,Osterbrock & Pogge 85] • 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.,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 & 04... ]

  5. introduction: NLS1 galaxiesopen questions, addressable with radio studies • orientation • mBH – s plane • jet-disk coupling ? indications thatGal. XRBs in soft/hi state and AGN close to LEdd are radio weak • .... This is the first systematic study of radio-loud NLS1s and their multi-l properties*. Only 3-4 RL NLQSOs known previously: PKS0558-504, [Remillard & 86, Siebert & 99], RXJ0134-4258 [Grupe & 00], SDSS0948+0022[Zhou & 03], SDSS1722+5654 [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 search for radio-loudNLS1s • cross-correlation of the Catalogue of quasars and AGN [Veron-Cetty et al. 2003]with radio and mB cats using the matcher developed within the German Astrophysical . Virtual Observatory, http://www.g-vo.org, [Adorf et al. 05] • catalogues: PKS (4.85 GHz) PMN, 87 GB (2.7 GHz) VQCNVSS, FIRST (1.4 GHz) SUMSS (0.8 GHz) WENSS (0.3 GHz) USNO-A,B SDSS spec. GSC2.2ROSAT, IRAS radio [Wright & Otrupcek 90, Griffith & 94, Gregory & Condon 90, Condon & 98, White & 97, Mauch & 03, de Bruyn & 98] RL opt X, IR mB [Monet & 03] [York & 00, Voges & 97]

  7. search for radio-loud NLS1s: results might be partly, but not fully, due to NLS1 definition as FWHMHb < 2000 km/s, indep. of L • 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

  8. examples: radio-loud NLS1s: optical spectroscopy SBS1517+520 blazar ?? 2nd-most RL no strict NLS1 Hb - [OIII] FWHMHb,dir= 960 – 2030 km/s, FeII/Hb =0.5 – 3.2, [OIII]/Hb = 0.05-3 SBS1517

  9. radio-loud NLS1s: optical spectroscopy RXJ23149+2243:extreme ´blue wingler´ in [OIII] Hb [OIII] FWHM[OIII],wing = 1550 km/s, v[OIII],wing = 1250 km/s

  10. radio-loud NLS1s:X-ray variability & spectroscopy examples: PKS0558-504, highly var. Gx = -2 ... -3.5 Lsx ~ 10 erg/s X-ray data used for L/LEdd estimates 44 - 46 SDSS1722+5654, const.

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

  12. radio-loud NLS1s: results • radio indices:

  13. radio-loud NLS1s: results • FeII-[OIII]-FWHMHb correlations: - radio-louds cover whole FeII-[OIII] range of NLS1s, - extend known radio-loud objects to those with small FWHMHb [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 Ll(5100A) and FWHMHb[Kaspi & 05]

  15. radio-loud NLS1s: models • starburst contribution? - radio powersP are all in RLregime - IRAS – radiocorr.: P factor 10-120 above expected starburst contrib. - ionisation para.,SDSS1722+56: 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 Why are RL NLAGN more rare than RL BLAGN, and is the mechanism for RLness the same in NLAGN and BLAGN ? • relativistic beaming ?  pole-on view - most are steep spectrum sources, with radio spectral indices ar< -0.5; beaming not expected - exceptions: SDSS0948+0022, RXJ16290+4007: ar=0.6, 0.4 - SDSS0948+0022 var. in radio, PKS0558 highly var. in X - X-ray spectra of beamed sources typically much flatter S: beaming cannot be excluded, but no positive evidence for it, with 2-3 exceptions

  17. radio-loud NLS1s: models to explain lower frequency of RLs among NLS1s RL NLS1s: Eddington ratios: 10 Lx/LEdd = 0.2-6 • 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/LEdd also responsible for low RL-fraction in NLS1s ? • 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 MBH – s relation of AGN than other NLS1s [Mathur & Grupe 05] -- more theoret. studies needed --

  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, MBH make use of line ratios wih diagn. power • radio imaging: how compact are the sources ? at diff. n: 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 FWHMHb • 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-l [Komossa et al. 06a, ApJ 639, in press; 06b, AJ, subm.]

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