Radio-loud Narrow-Line Seyfert 1 Galaxies

Transcription

1 Jet Triggering Mechanisms in Black Hole Sources, Mumbai, January 20-23, 2016 Radio-loud Narrow-Line Seyfert 1 Galaxies S. Komossa, MPIfR - 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: 1H , RXJ , SDSSJ

2 NLS1s are AGN with extreme multi-wavelength properties Elliptical Mrk 699

3 Narrow-line Seyfert 1 galaxies (NLS1s) defined as AGN with narrow BLR Balmer lines FWHM Hb < 2000 km/s strong FeII, faint [OIII]/Hb < 3 FeII Hb [OIII] FeII super-soft X-ray spectra, enhanced X-ray variability, CIV asymm., strong outflows, low n NLR, enh. SB... [e.g., Osterbrock & Pogge 1985, Goodrich 1990, Boroson & Green 92...review: Komossa 08]

4 Narrow-line Seyfert 1 galaxies (NLS1s) defined as AGN with narrow BLR Balmer lines FWHM Hb < 2000 km/s strong FeII, faint [OIII]/Hb < 3 FeII Hb [OIII] FeII super-soft X-ray spectra, enhanced X-ray variability, CIV asymm., strong outflows, low n NLR, enh. SB,... NLS1s are AGN with low BH masses & high Eddington rates L/L edd [e.g., Osterbrock & Pogge 1985, Goodrich 1990, Boroson & Green 92...review: Komossa 08] Xu+ 12 rapidly growing BHs in local universe hold key clues on physics of the central engine, feeding & feedback, BH growth, galaxy-bh (co)-evolution

5 BH mass M BH & 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: ~10 6 M sun, Mrk 335: ~10 7 M sun Peterson 11 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] ) o BLS1 M BH - s [SII] NLS1 [e.g., Peterson 00, 11, Komossa & Xu 07; McHardy+ 06, Xu+12, Wang+ 14, Woo+ 15]

6 a population of NLS1 galaxies with strong outflows - blue outliers, have their whole [OIII] profile blueshifted, implying gas in outflow ; up to 1000 km/s in high-ion lines M BH - s [OIII] - comes with dramatic line broadening - phenomenon so far almost exclusively obs. in NLS1s; in16% of population [Komossa & Xu+ 08, 16--inprep]

7 NLS1 host galaxies nearby (z< ) 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) Crenshaw+ 03 Elliptical Mrk 699 Ohta+ 07 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,...]

8 smallest Balmer lines come with steepest X-ray spectra, on average NLS1s show excess variability in X-rays w.r.t. BLS1s NLS1 galaxies in X-rays ongoing discussion whether X-ray spectral complexity (incl. soft excess ) is dominated by emission/reflection or absorption Boller+ 96 and therefore, whether their spin is low, or high, or unconstrained Mrk 335 (5yr Swift ) [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 ]

9 NLS1 galaxies in X-rays: the case of Mrk 335 Mrk 335 monitoring with Swift, and XMM follow-ups at deep low-states: 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 [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]

10 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]

11 NLS1 galaxies in X-rays: the case of Mrk 335

12 radio properties of NLS1s - motivation 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

13 radio properties of NLS1 galaxies first systematic study of radio-properties of NLS1s, and search for radio-loud ones (R 5 = f 5GHz / f 4400 ) based on all known NLS1s in VQC, cross-matched with FIRST, NVSS, SUMSS, WENSS, PMN, 87GB, and PKS radio surveys - 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 [Komossa+ 06a,b]

14 radio-loud NLS1 galaxies all radio-loud NLS1s are bona fide NLS1s optically; and particularly strong FeII emitters [Komossa+ 06a]

15 radio-loud NLS1 galaxies black hole masses*: much lower than commonly seen in RL objects, in a previously rarely populated regime of the `Laor diagram [Laor 00, Lacy et al. 01; larger coverage: Woo & Urry 02, McLure & Jarvis 04, Metcalf & Magliocchetti 06] *estimated from L l (5100A) and FWHM Hb [Kaspi & 05] [Komossa+ 06a]

16 g-ray discovery of NLS1s

17 [Foschini 11] [D Ammando+ 13] g-ray discovery of NLS1 galaxies Fermi-LAT detection of several (RL) NLS1s in g rays for the 1st time [PMN , 1H , PKS , PKS ] repeat & rapid flaring, Dt ~ 3-30d high (isotropic) luminosities, up to L peak ~10 48 erg/s (PMN ) [discovery papers: Abdo+ 09ab, Foschini 11, D Ammando+ 12, 15, Yao+ 15b]

18 [Foschini 11] [D Ammando+ 13] g-ray discovery of NLS1 galaxies Fermi-LAT detection of several (RL) NLS1s in g rays for the 1st time [PMN , 1H , PKS , PKS ] repeat & rapid flaring, Dt ~ 3-30d high (isotropic) luminosities, up to L peak ~10 48 erg/s (PMN ) confirmed presence of relativistic jets are they a new class of jet-emitting sources, or the lowmass extension of the blazar phenomenon? ongoing MW campaigns [discovery papers: Abdo+ 09ab, Foschini 11, D Ammando+ 12, 15, Yao+ 15b, Liao+ 15] g NLS1 FSRQs BL Lacs radio gals

19 rapid, repeat flaring radio-loud NLS1s: radio variability Effelsberg monitoring of 4 g-nls1s, longest duration, most frequencies, so far more prominent at higher frequencies, strong spectral evolution (consist. with shocks) moderate var. brightness temperatures (& associated Doppler factors) (only) mildly relativistic jets overall consistent with blazars (except lower luminosities; lower speeds; lower masses) [Angelakis+ 15]

20 radio-loud NLS1s: radio morphology 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 SDSS J VLBI at 5 GHz; Gu+ 15. core brightness temperature, on order <10 11 K; less than the classical blazar population (< K) [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]

21 radio-loud NLS1s: recent multi-l studies / SEDs 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 Foschini+ 15 [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,...] Suni+ 15

22 3 case studies 1H : relativistic jet in a ring/spiral host RXJ : steep-spectrum source, with possible g emission & super-strong outflow SDSSJ : new g emitting NLS1, at high z

23 1H initial puzzles and surprises 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= high L/L Edd = 0.1, low BH mass [Zhou+ 07]

24 g-ray detection with Fermi correlated X-UV variability with Swift; and SED modelling, X-rays from disc-corona; other parts jet-dominated 1H recent results rapid X-ray variability with Suzaku Yao+ 15 independent BH mass estimate from X-ray excess variance confirms low mass, M~10 7 M sun [Abdo+ 09, Paliya+ 14, Yao+ 15a] Yao+ 15

25 - core-jet structure (Mojave) 1H recent results - multiple components on pc scales, - at superluminal speeds; b=1-7c Fuhrmann+ 16 rapid variability DS=400 mjy in 16d [Wajima+ 14, Angelakis + 15, Karamanavis 15, Fuhrmann+ 16]

26 RXJ radio-loud NLS1 (z=0.17) perhaps marginal g ray detection (L. Foschini, priv. com.), var. (but) steep radio spectrum, a=-0.76 (Effelsberg) + RXJ rq NLS1 average 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 [Komossa+ 15] Hb [OIII]

27 SDSSJ : a new g-emitting NLS1 new (7 th ) g-emitting NLS1, detected with Fermi, known as FSRQ, but only new SDSS- BOSS spectra revealed its NLS1 nature rapid WISE-IR variability jet high-e SED consistent with EC processes with seed photon field from dusty torus [Yao+ 15b]

28 summary 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, quasisimultaneous) ASTROSAT!