Radio-loud Narrow-line Seyfert 1 galaxies

1
Radio-loud Narrow-line Seyfert 1 galaxies
From Atoms to AGN, Tel Aviv, Feb. 2006
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 dont
  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

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radio-loud NLS1sintroduction RL-RQ bimodality

• RL-RQ dichotomy in
• radio index (R) histogram
• R f5GHz / f4400A
• R5 gt 10 (R1.4 gt 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

• 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

OIII
FeII
FeII
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...
5
introduction NLS1 galaxies open questions,
addressable with radio studies

• orientation
• mBH s 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-l properties. Only 3-4
RL NLQSOs known previously PKS0558-504,
Remillard 86, Siebert 99, RXJ0134-4258
Grupe 00, SDSS09480022 Zhou 03,
SDSS17225654 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-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
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
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search for radio-loud NLS1s results
might be partly, but not fully, due to NLS1
definition as FWHMHb lt 2000 km/s, indep. of L

• 128 NLQSOs in VQC
• 90 within NVSS survey area,
• among these, 7 are radio-loud
• only 2 exceed R100
• (for comp. 15 radio-louds among quasars)
• most radio-loud NLQSOs are compact, steep
  spectrum sources, not variable

8
radio-loud NLS1s optical spectroscopy
examples
SBS1517520
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
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radio-loud NLS1s optical spectroscopy
RXJ231492243 extreme blue wingler in OIII
Hb
OIII
FWHMOIII,wing 1550 km/s, vOIII,wing 1250
km/s
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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
SDSS17225654, const.
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radio-loud NLS1s results

• radio-loudness radio indices

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radio-loud NLS1s results

• radio indices

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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
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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
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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., SDSS172256
• log U -2.4 (typ. for Sy)
• EUV excess
• NeIII/NeV is good indicator of continuum
  shape, once U is known

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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 lt -0.5 beaming not
  expected
• - exceptions SDSS09480022, RXJ162904007
  ar0.6, 0.4
• - SDSS09480022 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

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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

• 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 --
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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

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Summary

• identification of RL NLS1s
• radio most sources are compact, of steep
  spectrum, and not variable R of all det. sources
  covers gt 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) lt 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.