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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. - PowerPoint PPT Presentation
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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
• 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.]