Kyoto, Oct. 2003 NLS1 - A Review; bol/kyoto Thomas Boller1 Narrow-Line Seyfert 1 Galaxies Observational and Theoretical Progress until

Kyoto, Oct. 2003 NLS1 - A Review; www.xray.mpe.mpg.de/~bol/kyoto Thomas Boller

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Narrow-Line Seyfert 1 Galaxies

Observational and Theoretical Progress until 2003 The Review

Thomas BollerMax-Planck-Institut für extraterrestrische Physik Garching

Germany


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Narrow-Line Seyfert 1´s

H[OIII]

Broad-Line Seyfert 1´s

H [OIII]

Flu

x [e

rg c

m s

Hz

]-2

-1

-1

[A]

Fe II Fe II

Giant soft X-ray excess

Narrow H

Strong Fe II

Weak [OIII]

Moderate soft X-ray excess

Broad H

Weak Fe II

Strong [OIII]

Enlarging the Seyfertparameter space

0. Definition and the enlarged observational parameter space


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I. Historical Review

1971 Zwicky: first report on extreme variability ‘optical outbursts in I Zw1‘

1. In the beginning

1987 Halpern & Oke: importance as X-ray sources

1992 Puchnarewicz: report on steep X-ray spectra

1985 Osterbrock & Pogge: Definition 1. Permitted lines are only slightly broader than the forbidden lines 2. Fe [VII], Fe [X] emission lines 3. [OIII]/H < 3 4. FWHM H < 2000 km s-1 (Goodrich 1989)

R. Pogge


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1993 Boller,Trümper,Fink, Molendi & Dennefeld discovery of extreme and rapid X-ray variability t = 800 s, L = 1044 erg s-1

2. The ROSAT/ASCA Renaissance

1996 Boller,Brandt & Fink soft X-ray continuum and optical line width relation

1997 Boller,Brandt,Fabian &Fink discovery of persistent, rapid and giant X-ray variability factor of 60 in 1 day

1997 Laoranalysis of quasar sample

1999 Leighly, Vaughan ASCA statistics on soft X-ray excess sources


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3. The XMM-Newton/Chandra Era

The XMM-Newton GT/AO Programme on NLS1

> 2000 Boller, Tanaka, Fabian, Brandt, Gallo et al.

2002 Fabian, Lee, BranduardiNature of the soft X-ray spectral complexity

2000 MineshigeSlim disc models for NLS1


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II. What have we learned from ROSAT, ASCA and BeppoSAX

1. The influence of the emission from the inner ~100 light seconds to the BLR and NLR Boller, Leighly, Brandt, Wills, et al.

2. NLS1s as the most X-ray variable radio-quiet AGN (Boller et al. , Leighly et al.)


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0.1 1 5 10 Energy [keV]

100

1

01

1

02

rel

. Flu

x

BLS1

0.1 1 5 10 Energy [keV]

100

1

01

1

02

103

re

l. Fl

ux

NLS1

Giant soft X-ray emissionModerate soft X-ray emission

Power-law approximation F ~ E- ~2.3 for E=(0.1-2.4 keV)

strongest disc emission yet foundin Seyfert galaxies

F ~ E-with up to 5

NLS1 and their giant soft X-ray excess emission


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Soft X-ray slope - optical BLR line width relation

Emission from the

accretion disc

determines v-dispersion

in the BLR

hotter dishotter discc ROSAT results

ext

rem

e s o

f t ex

c es s

~ velocity dispersion in the BLR

mod

erat

e

Boller, Brandt, Fink 1996


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NLS1 publication statistics

FWHM H - relation

Osterbrock &Pogge


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BLS1 publication rate:

2003: ~5000 papers

NLS1 publication rate:

d(paper) / dt [NLS1] = 8..10

2007: ~5000 papers


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The underlying physical parameter

L(accretion) = L(Planck) T ~ MM2

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lower black hole mass and/or higher accretion rate

U = nneRR

e2

Ionization parameter U + Kepler motions

FWHM = (GM/R)1/2

NLS1 form the low-mass black hole range of AGN

M2

M

FWHM ~ T34

-U ne

14

U ne14

316~

Boller 2000


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Reverberation results

NLS1 as low mass black holes

NLS1: The young Seyfert‘s

Super-solar metalliticiesNLS1 are AGN in the makingAGN with the lowest BH masses

B. Peterson S.Mathur

Fe Absorption must result into Fe K Re-emission Why do we not detect the Fe K line emission ??

Discrepancy between absorption and emission (>5)

Energy [keV]

IRAS 13224-3809

EPIC pn

0.2 1 2 3 5 10

Boller, Tanaka, Fabian 2003

Cou

nts

s-1 k

eV-1

Spectral drop at 8.2 keV

0.2 1 2 3 5 10

Energy [keV]

EPIC pn

EPIC MOS

1H 0707-495 Boller, Fabian, Sunyaev, Trümper 2002

Cou

nts

s-1 k

eV-1

Spectral drop at 7.1 keVNo line at 6.4 keV

3. XMM-Newton discoveries: New puzzles3.1. Detections of sharp spectral drops > 7 keV

Boller, Tanaka, Fabian, Brandt, Sunyaev, Gallo, Anabuki, Haba


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Possible explanation Partial covering

Solution: place the absorber into the accretion disc region

High density cool cloud at distance rSmall solid angle coveredTherefore minor Fe K re-emission

Observers sees full absorption Unabsorbed radiation

Unabsorbed radiation

Accretion discAbsorbing cloudobserver

Probability problem when source is too far away from the black hole P(1Lj) = 10-9


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IRAS 13224-3809Fe L Absorption

IRAS 13224-3809

Variable Absorption Profile

1H 0707-495 (AO2)Soft X-ray emission line?

Will be discussed by Prof. Tanaka

Edge energy shift

7.10 7.44 Energy [keV]

flux

2000

1H0707 (AO1)

2002

1H0707 (AO2)

3.2. Puzzling new observational facts

(AO1)


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Problems with the current models

1. Problem with the absorption model:- Absorption edge at 8.2 keV arises from Fe XIX - XXIII (7.93,8.07,8,21,8.35, 8.49 keV), edge should be broad, with ~ 600 eV, rather than sharp (<100 eV)- The feature may be a neutral edge in approaching matter- Power-law cut-off model used to get: Fe 3-10 solar

3. Problem with the line interpretation: large equivalent width

2. Soft X-ray spectral features difficult to understandAbsorption line profile changes not understoodBroad emission line, without presence of other alpha elements is puzzling

It might be another, new physical mechanism, weare not aware of so far


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Model-indepenent implications

Curved X-ray continua insources with sharp spectraldrops remove part of the relativistic redshift based on a simple power-law continuum

Other effects: - ionization state of the disc - light bending (Iwasawa, Miniutti)

relativistic Fe K line detections are difficult with the present generation of X-ray telescopes


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Simulation of line profiles for ionized discsCompton broadeningfor > 300

P hot

ons

c m-2

s-1 ke

V-1 Compton broadening+ relativistic motions

XEUS ´fit`

Line detectable

Energy [keV]

Curvature of the continuum makes Fe K line very difficult to detect

XMM-Newton ´fit`

Relativistic line notdetectable

Energy [keV]

Coun

ts s

-1 k

eV-1

ratio


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ESA, NASA, Japanese long term X-ray projects

NASA

Japanese Ginga ASCA Astro-EII

ESA Exosat ROSAT XMM-Newton ROSITA XEUS

Chandra Constellation-X

1980 1990 2000 2005 2011 2017 2020

Maxim

NEXTMAXI

4. Implications for future missions


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NLS1 research and future missions

XMM-Newton/Chandra:>500 ks exposure times required to solve the nature of sharp spectral drops

Astro-E2: important to study NLS1s: understand the physics of NLS1s more precisely

XEUS/Con-X: fundamental increase of understanding the Seyfert phenomenon still expected


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XEUS - ESA mission under study


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AGN QPO´s: precessing discs or orbital motions?

2G/c2 J r-3

Precession: no spectral variability

Orbital motions: strong Doppler boosting and associated spectral variability


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Present NLS1 StatusEstablished properties

Steepest soft and hard X-rayspectra yet detected in AGN

Presence of sharp spectral dropswithout Fe K re-emission

Narrow optical line widths

The strongest Fe II emitters inthe universe

Set of radio-, optical-, UV-, X-raycorrelations between NLS1 andBLS1

The most X-ray variable AGN

Key of understanding the Seyfert phenomenon more generally

Work in progress

Underlying physical parameterfor spectral properties: low M, high dM/dt

Observational constrains from sharp spectral drops

Missing relativistic Fe K lines in most objects

Understanding the different X-ray variability properties

Higher metallicities as indicator of AGNs just in the forming

Comptonized soft X-ray spectra

Unsolved problemsNature of sharp spectral drops > 7 keV

The sharpness of the spectral drop

The time-dependent changes in the spectraldrop energy, variableFe L resonance absorptionfeatures, presence of singlesoft emission lines without other -elements

The nature of the soft X-raycomplexity

Nature of X-ray variations

High energy >10 keV spectralproperties


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The end - thank you!


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Timing properties

Please see Karen´s Leighly talk

and

Poster by Luigi Gallo #19

A few examples


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Light curve Fractional amplitude variability

Tanaka, Gallo, Boller (in prep.)


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The significance of the detection and available photon statistics

Spectral dropdetected withhigh significance

Photon statisticsabove 7 keVlimited, only about 30 photons

~500 ks observationrequired

source + background spectrum

background


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huge filling factor in BLR strong narrow [OIII] emission

Seyfert 1 unification through physical processes

Broad-Line Seyfert 1 Narrow-Line Seyfert 1

weak strong disc emissiondM/dt, M

broad narrow optical linesdM/dt, M

moderate extreme X-ray variability smaller M, relativistic effects

flat steep power-lawsinverse Compton effect

Weak strong Fe II emission ?


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XEUS NFI2

Con-X calorimeter E = 2eV

Schwarzschild BH Kerr BHincl 6 10 14

incl 56 60 64

Torres et al. 03


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Gallo et al. 2003


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3.2. Recent discoveries in the soft X-ray range

Fe L absorption at ~ 1.2 keV

Variable Fe L profile changes on ~ 1000 s

Single soft and strong emission line without presence of other elements

Time dependency of the the presence of soft X-ray lines, luminositiescolumn densities/covering fractions

Time dependent changes of the edge energy from 7.10 to 7.44 keVwithin two years (1H 0707-495)

Please see talk by Y. Tanaka


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Statistical significance of the X-ray oscillations

3

2

1

Long-term flux increase included Long-term flux increase detrended

Periodicity peaks at 2100 and 4200 sLow statistical significance

Boller, Timmer

Time [sec] Time [sec]

2


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BH Merger


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1985 Osterbrock & Pogge: Definition 1. Permitted lines are only slightly broader than the forbidden lines 2. Fe [VII], Fe [X] emission lines 3. [OIII]/H < 3 4. FWHM H < 2000 km s-1 (Goodrich 1989)

1987 Halpern & Oke: importance as X-ray sources

1989 Stephens: high fraction in X-ray samples `X-ray selection may be an effective way to find NLS1‘

1992 Puchnarewicz: report on steep X-ray spectra

R. Pogge


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The relevance of NLS1 for understanding the Seyfert phenomenon more generally

NLS1 are more than just Seyfert 1s with narrow linesNLS1 are more than just Seyfert 1s with narrow lines

1. Extreme X-ray spectral slopes and variability

2. Extreme progress in defining the observational parameters of NLS1

3. Now important member of the AGN family

4. Whenever we observe NLS1, new observational properties are discovered

5. NLS1 allow a more general understanding of many problems posed by the Seyfert phenomenon


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Warm absorber and/or relativistically broadened C,N,O lines?

presence of relativistically-broadened O,N,C lines are claimedfrom RGS spectraBranduardi-Raymont et al. 2001

Chandra HETG spectraprovide a different view


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Lee et al. 2001: major feature at ~0.7 keV: neutral iron absorption

Fe L3Fe L2OVII absorption

explain

feature between0.7 –0.75 keV

Presence ofsignificantionizedabsorption


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G. BranduardiBroad Oxygen Lines

J. LeeFe L edges

A.C. Fabian in X-rays from AGN: Relativistically broadended emission lines

potential problem with line interpretation of 707 eV drop 1. EW = 150 eV (much higher than expected) 2. Sharpness 10 eV (RGS) 3 eV (HETG) - O lines produced in highly ionised medium with significant Thomson depth - lines broadended considerable more than 10 eV + Doppler and gravitational redshifts


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I. Historical Review (partially based on Pogge 2000)

1978 Davidson&Kinman: first note on narrow lines `On the possible importance of Mrk 359` `Seyfert I spectrum with unusually narrow permitted lines` `This unusual object merits further observations…‘

1983 Osterbrock & Dahari: 4 NLS1

1971 Zwicky: first report on extreme variability ‘optical outbursts in I Zw1‘

Osterbrock initiates systematic investigation on NLS1

1. In the beginning

Documents

Kyoto, Oct. 2003 NLS1 - A Review; bol/kyoto Thomas Boller1 Narrow-Line Seyfert 1 Galaxies Observational and Theoretical Progress until