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