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

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]

radio-loud NLS1s

introduction: 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

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 & 04... ]

FeIIFeII

[OIII]H

introduction: NLS1 galaxies

open questions, addressable with radio studies• orientation • mBH – plane• jet-disk coupling ? indications that Gal. 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- 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]

GAVOGAVO search for radio-loud NLS1s• 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)

VQC NVSS, FIRST (1.4 GHz) SUMSS (0.8 GHz)

WENSS (0.3 GHz) USNO-A,B SDSS spec.

GSC2.2 ROSAT, IRAS

radio

mB

[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, IRRL

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 FWHMH < 2000 km/s, indep. of L

radio-loud NLS1s: optical spectroscopy

FWHMH,dir= 960 – 2030 km/s, FeII/H=0.5 – 3.2, [OIII]/H = 0.05-3

examples:

H - [OIII]

2nd-most RL blazar ??no strict NLS1

SBS1517+520

SBS1517

radio-loud NLS1s: optical spectroscopyRXJ23149+2243: extreme ´blue wingler´ in [OIII]

FWHM[OIII],wing = 1550 km/s,

v[OIII],wing = 1250 km/s

[OIII]

H

radio-loud NLS1s: X-ray variability & spectroscopy

x = -2 ... -3.5

Lsx ~ 10 erg/s

X-ray data used for L/LEdd estimates

SDSS1722+5654, const.

PKS0558-504, highly var.examples:

44 - 46

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

radio-loud NLS1s: results• radio indices:

radio-loud NLS1s: results• FeII-[OIII]-FWHMH correlations:

- radio-louds cover whole FeII-[OIII] range of NLS1s,

- extend known radio-loud objects to those with small FWHMH

[Marziani & 01]

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 FWHMH [Kaspi & 05]

radio-loud NLS1s: models

• starburst contribution ?

- radio powers P are all in RL regime

- IRAS – radio corr.: 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

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: SDSS0948+0022, RXJ16290+4007: r=0.6, 0.4 - SDSS0948+0022 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 ?

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/LEdd also responsible for low RL-fraction in NLS1s ?

RL NLS1s: Eddington ratios: 10 Lx/LEdd = 0.2-6

-- 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 MBH – relation of AGN than other NLS1s [Mathur & Grupe 05]

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. : spectral indices, steepness monitoring: variability, beaming ?• X-rays: spectra, absorption, variability • theory: jet-disk models, dep. on acc. rate

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 FWHMH

• 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. 0

6a, ApJ 639, in

press;

06b, AJ, su

bm.]