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Radio-loud Narrow-Line Seyfert 1
Galaxies
- intro
- the first 2 decades; optical and X-rays
- the radio view
- first g-ray detections
- recent highlights on radio-loud NLS1 galaxies
- 3 case studies: 1H0323+342, RXJ2314+2243, SDSSJ1222+0413
S. Komossa, MPIfR
Jet Triggering Mechanisms in Black Hole Sources, Mumbai, January 20-23, 2016
NLS1s are AGN with extreme multi-wavelength
properties
Elliptical Mrk 699
• defined as AGN with
narrow BLR Balmer lines
FWHMHb < 2000 km/s
strong FeII,
faint [OIII]/Hb < 3
super-soft X-ray spectra,
enhanced X-ray variability,
CIV asymm., strong
outflows, low nNLR, enh. SB
...
FeII FeII [OIII]
Hb
Narrow-line Seyfert 1 galaxies (NLS1s)
[e.g., Osterbrock & Pogge 1985,
Goodrich 1990, Boroson & Green
92.....review: Komossa 08]
• defined as AGN with
narrow BLR Balmer lines
FWHMHb < 2000 km/s
strong FeII,
faint [OIII]/Hb < 3
super-soft X-ray spectra,
enhanced X-ray variability,
CIV asymm., strong
outflows, low nNLR, enh. SB,...
FeII FeII [OIII]
Hb
NLS1s are AGN with low BH
masses & high Eddington
rates L/Ledd
Narrow-line Seyfert 1 galaxies (NLS1s)
rapidly growing BHs in local
universe hold key clues on
physics of the central engine, feeding & feedback,
BH growth, galaxy-BH (co)-evolution
Xu+ 12
[e.g., Osterbrock & Pogge 1985,
Goodrich 1990, Boroson & Green
92.....review: Komossa 08]
• NLS1s overall follow host-BH scaling relations of non-active galaxies & BLS1s, with large scatter
(in s*, and when using FWHM[OIII]
or [SII] as surrogate, but only after
removing objects dominated by
outflow in [OIII] )
[e.g., Peterson 00, 11, Komossa & Xu 07; McHardy+ 06, Xu+12, Wang+ 14, Woo+ 15]
MBH & scaling relations of NLS1 galaxies
• evidence for low BH masses of NLS1s from reverberation-mapping of a few, & from X-ray variability methods: e.g., NGC 4051: ~106 Msun ,
Mrk 335: ~107 Msun
Peterson 11
BH
mass
MBH - s[SII]
o BLS1
NLS1
- „blue outliers“,
have their whole
[OIII] profile blue-
shifted, implying gas
in outflow ; up to
1000 km/s in high-ion
lines
- comes with
dramatic line
broadening
- phenomenon so far
almost exclusively obs.
in NLS1s; in16% of
population
[Komossa & Xu+ 08, 16--inprep]
a population of NLS1 galaxies with strong outflows
MBH - s[OIII]
nearby (z<0.04-0.07) NLS1s show
• no excess companions
• no evidence for recent mergers
• a higher fraction of bars; & nuclear dust-spirals &
stellar rings than BLS1s (C03-sample[13NLS1]: 65% of
NLS1 spirals have bars, 25% of BLS1 spirals have bars;
z<0.04. O07-sample [50NLS1]: ~60-70% NLS1 have bars,
~40-70% BLS1 have bars)
no merger-induced accretion, but bar may play a role
(secular processes) in fuelling
note: hosts of more distant/luminous NLS1s/Q1s, and radio
NLQ1s not yet known [likely ellipticals, like in BLQ1s)
[e.g., Krongold+ 00, Crenshaw+ 03, Deo+ 06, Ohta+ 07, Ryan+ 07, Orban de
Xivry+ 11, Mathur+ 12, Xu+ 12, .....]
NLS1 host galaxies
Ohta+ 07
Crenshaw+ 03
Elliptical Mrk 699
• smallest Balmer lines come with
steepest X-ray spectra, on
average
• NLS1s show excess variability in
X-rays w.r.t. BLS1s
• ongoing discussion whether X-ray
spectral complexity (incl. „soft
excess“) is dominated by
emission/reflection or absorption
and therefore, whether their spin
is low, or high, or unconstrained
NLS1 galaxies in X-rays
[e.g., Leighly 97, Boller+ 96, McHardy+ 06, Tanaka+
03, Gallo+ 11a,b, Grupe+ 10, 12, Fabian+ 12,
Komossa+ 14, Yao+ 15, Gallo+15, Gardner & Done
15, Pal+ 16........]
Boller+ 96
Mrk 335 (5yr Swift )
• Mrk 335 monitoring with Swift, and XMM follow-ups at deep low-states:
NLS1 galaxies in X-rays: the case of Mrk 335
[Mrk 335: Grupe,Komossa,Gallo+ 07, 08, 12; Longinotti+ 13, Gallo+ 13, Parker+ 14, Komossa+ 14,
Chainakun & Young+ 15, Keek & Ballantyne 15, Sarma+ 15, Gallo+ 15, Wilkins+ 15]
X-ray & UV lightcurve, from sev. yrs of Swift monitoring 2007 Swift low-state vs 2000 XMM
XMM low-state modelling:
broad ‘relativistic’ iron-line
profile or partial covering
absorber both successful
NLS1 galaxies in X-rays: the case of Mrk 335
[Mrk 335: Grupe,Komossa,Gallo+ 07, 08, 12; Longinotti+ 13, Gallo+ 13, Parker+ 14, Komossa+ 14,
Chainakun & Young+ 15, Keek & Ballantyne 15, Sarma+ 15, Gallo+ 15, Wilkins+ 15]
NLS1 galaxies in X-rays: the case of Mrk 335
• almost unexplored territory, pre-
2006; except for ~3-4 RLs
• extreme properties in radio, too ?
• new test of NLS1 (orientation)
models: e.g., if our view is
preferentially pole-on, there‘d
be an excess of beamed NLS1s
• fresh look at RL – RQ dichotomy
of AGN, its presence & its cause
• driver(s) of RLness
• physics of jet launching under high
accretion rates
radio properties of NLS1s - motivation
first systematic study of radio-properties of NLS1s, and search for radio-loud
ones (R5 = f5GHz / f4400)
based on all known NLS1s in VQC, cross-matched with FIRST, NVSS, SUMSS, WENSS, PMN, 87GB,
and PKS radio surveys
radio properties of NLS1 galaxies
[Komossa+ 06a,b]
- RLness much less common in NLS1s than in BLS1s:
only 7% of all NLS1s are RL (vs ~20% BLS1s)
only 2.5% above R=100 (vs ~14% BLS1s)
- most are steep-spectrum sources (a <= -0.5),
and ‚compact‘ (< few kpc); share similarities with CSS,
- while 2-3 have inverted radio spectra,
and share similarities with blazars
- extended RLness to low BH masses
• all radio-loud NLS1s are bona fide NLS1s optically;
and particularly strong FeII emitters
radio-loud NLS1 galaxies
[Komossa+ 06a]
• black hole masses*: much lower than commonly seen in RL objects,
in a previously rarely populated regime of the `Laor diagram´
*estimated from
Ll(5100A) and FWHMHb
[Kaspi & 05]
[Laor 00, Lacy et al. 01;
larger coverage: Woo &
Urry 02, McLure & Jarvis
04, Metcalf &
Magliocchetti 06]
radio-loud NLS1 galaxies
[Komossa+ 06a]
g-ray discovery of NLS1s
• Fermi-LAT detection of several (RL)
NLS1s in g–rays for the 1st time [PMN 0948+0022, 1H0323+342,
PKS1502+036, PKS2004-447]
• repeat & rapid flaring, Dt ~ 3-30d
• high (isotropic) luminosities, up to
Lpeak~1048 erg/s (PMN0948+0022)
g-ray discovery of NLS1 galaxies
[discovery papers: Abdo+ 09ab, Foschini 11,
D‘Ammando+ 12, 15, Yao+ 15b]
[Foschin
i 11]
[D‘A
mm
ando+
13]
g-ray discovery of NLS1 galaxies
[discovery papers: Abdo+ 09ab, Foschini 11,
D‘Ammando+ 12, 15, Yao+ 15b, Liao+ 15]
[Foschin
i 11]
g NLS1
FSRQs
BL Lacs
radio gals
[D‘A
mm
ando+
13]
• Fermi-LAT detection of several (RL)
NLS1s in g–rays for the 1st time [PMN 0948+0022, 1H0323+342,
PKS1502+036, PKS2004-447]
• repeat & rapid flaring, Dt ~ 3-30d
• high (isotropic) luminosities, up to
Lpeak~1048 erg/s (PMN0948+0022)
confirmed presence of relativistic
jets are they a new class of
jet-emitting sources, or the low-
mass extension of the blazar
phenomenon ?
• ongoing MW campaigns
• rapid, repeat flaring
• more prominent at higher
frequencies, strong spectral
evolution (consist. with shocks)
• moderate var. brightness
temperatures (& associated
Doppler factors) (only) mildly
relativistic jets
radio-loud NLS1s: radio variability
[Angelakis+ 15]
overall consistent with blazars
(except lower luminosities; lower
speeds; lower masses)
Effelsberg monitoring of 4 g-NLS1s, longest duration, most frequencies,
so far
largest sample of RL NLS1s today
imaged with VLBI [Gu+ 15]:
• ~50% are CSS-like
• ~50% one-sided jet-core structure
on pc scales
• a few with faint extended emission
on kpc scales
• core brightness temperature, on
order <1011 K; less than the
classical blazar population
(<1011-13 K)
radio-loud NLS1s: radio morphology
[e.g.,Doi+ 06,07,11,12, Gu & Chen 10,
Giroletti+ 11, D‘Ammando+ 12, 13, Wajima+ 14,
Richards+ 15, Orienti+ 15, Schulz+ 15, Gu+ 15]
SDSS J144318+4725
VLBI at 5 GHz; Gu+ 15.
• X-ray spectra: flatter than rq-NLS1s;
some dominated by IC; but others
still show classical soft excess from
disc/corona
• SEDs: double-humped structure of
blazars (synchro-peak at IR/opt, IC
peak at MeV/GeV); plus acc disc
g-NLS1s well modelled by one-zone
leptonic jet models; resemble FSRQs
radio-loud NLS1s: recent multi-l studies / SEDs
[Foschini+ 15, Sun+ 15; also: Abdo+ 09a,b, D‘Ammando+ 12,15,
Foschini+ 12, Paliya+13, 14, Zhang+ 13, Maune+ 14, Yao+15a, Sun+ 14, ...]
Foschini+ 15
Suni+ 15
3 case studies
1H0323+342: relativistic jet in a ring/spiral host
RXJ2314.9+2243: steep-spectrum source, with
possible g emission &
super-strong outflow
SDSSJ1222+0413: new g emitting NLS1, at high z
• optical spectrum of classical NLS1
(FWHM(H)= 1600 km/s)
• highly variable at all frequencies
opt, X (RXTE, ROSAT, Swift,...),
radio
marginal TeV detection (Whipple)
• compact bright radio core
• RL, with R=50
• in a nearby spiral (or ring) galaxy
at z=0.06
- high L/LEdd = 0.1, low BH mass
1H0323+342 – initial puzzles and surprises
[Zhou+ 07]
• g-ray detection with Fermi
• correlated X-UV variability with
Swift; and SED modelling,
X-rays from disc-corona; other
parts jet-dominated
• rapid X-ray variability with
Suzaku
• independent BH mass estimate
from X-ray excess variance
confirms low mass, M~107 Msun
1H0323+342 – recent results
[Abdo+ 09, Paliya+ 14, Yao+ 15a]
Yao+ 15
Yao+ 15
• - core-jet structure (Mojave)
- multiple components on pc
scales,
- at superluminal speeds;
b=1-7c
• rapid variability
DS=400 mJy in 16d
1H0323+342 – recent results
[Wajima+ 14, Angelakis + 15, Karamanavis 15, Fuhrmann+ 16]
Fuhrmann+ 16
RXJ2314.9+2243
[Komossa+ 15]
• radio-loud NLS1 (z=0.17)
• perhaps marginal g–ray detection (L.
Foschini, priv. com.), var.
• (but) steep radio spectrum,
a=-0.76 (Effelsberg)
• luminous IR (LIRG)
• very steep UV spectrum, but no
evidence for optical reddening
• flat, variable X-ray spect (Swift)
• SED likely dom by non-thermal
emi (X: corona; IR-UV: synchro)
• very broad & blueshifted (v=1260
km/s) [OIII]5007 emission strong
outflow
• a case of strong AGN-induced
feedback in local universe
[OIII]
Hb
+ RXJ2314.9+2243
__ rq NLS1 average
• new (7th) g-emitting NLS1,
detected with Fermi, known as
FSRQ, but only new SDSS-
BOSS spectra revealed its NLS1
nature
SDSSJ1222+0413: a new g-emitting NLS1
[Yao+ 15b]
• rapid WISE-IR variability jet
• high-E SED consistent with EC
processes with seed photon field
from dusty torus
• NLS1 galaxies are AGN with extreme multi-wavelength properties,
with low BH masses, high Eddington ratios, i.e. rapidly growing their BHs;
rich X-ray spectral structures in low-flux states; a sub-population is radio-loud &
g-ray detected, and hosts relativistic jets
new insights on physics of central engine
scaling relations, BH-host co-evolution, feeding & feedback
nature of inner accretions disk, relativistic effects, BH spin
and/or absorption/outflows
physics of jet launching & evolution, at high L/Ledd,
• need to increase number of (radio-)NLS1s with broad –band X-ray
spectra, and good multi-wavelength coverage (radio to X-rays, quasi-
simultaneous) ASTROSAT !
summary