Kyoto, Oct NLS1 - A Review; Thomas Boller1 Narrow-Line Seyfert 1 Galaxies Observational and Theoretical Progress until 2003 The Review Thomas Boller Max-Planck-Institut für extraterrestrische Physik Garching Germany
Kyoto, Oct NLS1 - A Review; Thomas Boller2 Narrow-Line Seyfert 1´s HH [OIII] Broad-Line Seyfert 1´s HH [OIII] Flu x [erg cm s Hz ] [A] 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 Seyfert parameter space 0. Definition and the enlarged observational parameter space
Kyoto, Oct NLS1 - A Review; Thomas Boller3 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
Kyoto, Oct NLS1 - A Review; Thomas Boller Boller,Trümper,Fink, Molendi & Dennefeld discovery of extreme and rapid X-ray variability t = 800 s, L = erg s 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 Laor analysis of quasar sample 1999 Leighly, Vaughan ASCA statistics on soft X-ray excess sources
Kyoto, Oct NLS1 - A Review; Thomas Boller5 3. The XMM-Newton/Chandra Era The XMM-Newton GT/AO Programme on NLS1 > 2000 Boller, Tanaka, Fabian, Brandt, Gallo et al Fabian, Lee, Branduardi Nature of the soft X-ray spectral complexity 2000 Mineshige Slim disc models for NLS1
Kyoto, Oct NLS1 - A Review; Thomas Boller6 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.)
Kyoto, Oct NLS1 - A Review; Thomas Boller Energy [keV] rel. Flux BLS Energy [keV] rel. Flux NLS1 Giant soft X-ray emission Moderate soft X-ray emission Power-law approximation F ~ E - ~2.3 for E=( keV) strongest disc emission yet found in Seyfert galaxies F ~ E - with up to 5 NLS1 and their giant soft X-ray excess emission
Kyoto, Oct NLS1 - A Review; Thomas Boller8 Soft X-ray slope - optical BLR line width relation Emission from the accretion disc determines v-dispersion in the BLR hotter disc hotter disc ROSAT results extreme soft excess ~ velocity dispersion in the BLR moderate Boller, Brandt, Fink 1996
Kyoto, Oct NLS1 - A Review; Thomas Boller9 NLS1 publication statistics FWHM H - relation Osterbrock & Pogge
Kyoto, Oct NLS1 - A Review; Thomas Boller10 BLS1 publication rate: 2003: ~5000 papers NLS1 publication rate: d(paper) / dt [NLS1] = 2007: ~5000 papers
Kyoto, Oct NLS1 - A Review; Thomas Boller11 The underlying physical parameter L(accretion) = L(Planck) T ~ MMMM lower black hole mass and/or higher accretion rate U = n n e RRRR e 2 Ionization parameter U + Kepler motions FWHM = (GM/R) 1/2 NLS1 form the low-mass black hole range of AGN M2MM2M FWHM ~ T U n e 1414 U n e 1414 3 16 ~ Boller 2000
Kyoto, Oct NLS1 - A Review; Thomas Boller12 Reverberation results NLS1 as low mass black holes NLS1: The young Seyfert‘s Super-solar metalliticies NLS1 are AGN in the making AGN 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 EPIC pn Boller, Tanaka, Fabian 2003 Counts s -1 keV -1 Spectral drop at 8.2 keV Energy [keV] EPIC pn EPIC MOS 1H Boller, Fabian, Sunyaev, Trümper 2002 Counts s -1 keV -1 Spectral drop at 7.1 keV No line at 6.4 keV 3. XMM-Newton discoveries: New puzzles 3.1. Detections of sharp spectral drops > 7 keV Boller, Tanaka, Fabian, Brandt, Sunyaev, Gallo, Anabuki, Haba
Kyoto, Oct NLS1 - A Review; Thomas Boller14 Possible explanation Partial covering Solution: place the absorber into the accretion disc region High density cool cloud at distance r Small solid angle covered Therefore minor Fe K re-emission Observers sees full absorption Unabsorbed radiation Accretion disc Absorbing cloud observer Probability problem when source is too far away from the black hole P(1Lj) = 10 -9
Kyoto, Oct NLS1 - A Review; Thomas Boller15 IRAS Fe L Absorption IRAS Variable Absorption Profile 1H (AO2) Soft X-ray emission line? Will be discussed by Prof. Tanaka Edge energy shift Energy [keV] flux H0707 (AO1) H0707 (AO2) 3.2. Puzzling new observational facts (AO1)
Kyoto, Oct NLS1 - A Review; Thomas Boller16 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 understand Absorption line profile changes not understood Broad emission line, without presence of other alpha elements is puzzling It might be another, new physical mechanism, we are not aware of so far
Kyoto, Oct NLS1 - A Review; Thomas Boller17 Model-indepenent implications Curved X-ray continua in sources with sharp spectral drops 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
Kyoto, Oct NLS1 - A Review; Thomas Boller18 Simulation of line profiles for ionized discs Compton broadening for > 300 Photons cm -2 s -1 keV -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 not detectable Energy [keV] Counts s -1 keV -1 ratio
Kyoto, Oct NLS1 - A Review; Thomas Boller19 ESA, NASA, Japanese long term X-ray projects NASA Japanese Ginga ASCA Astro-EII ESA ExosatROSATXMM-Newton ROSITA XEUS Chandra Constellation-X Maxim NEXTMAXI 4. Implications for future missions
Kyoto, Oct NLS1 - A Review; Thomas Boller20 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
Kyoto, Oct NLS1 - A Review; Thomas Boller21 XEUS - ESA mission under study
Kyoto, Oct NLS1 - A Review; Thomas Boller22 AGN QPO´s: precessing discs or orbital motions? 2G/c 2 J r -3 Precession: no spectral variability Orbital motions: strong Doppler boosting and associated spectral variability
Kyoto, Oct NLS1 - A Review; Thomas Boller23 Present NLS1 Status Established properties Steepest soft and hard X-ray spectra yet detected in AGN Presence of sharp spectral drops without Fe K re-emission Narrow optical line widths The strongest Fe II emitters in the universe Set of radio-, optical-, UV-, X-ray correlations between NLS1 and BLS1 The most X-ray variable AGN Key of understanding the Seyfert phenomenon more generally Work in progress Underlying physical parameter for 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 problems Nature of sharp spectral drops > 7 keV The sharpness of the spectral drop The time-dependent changes in the spectral drop energy, variable Fe L resonance absorption features, presence of single soft emission lines without other -elements The nature of the soft X-ray complexity Nature of X-ray variations High energy >10 keV spectral properties
Kyoto, Oct NLS1 - A Review; Thomas Boller24 The end - thank you!
Kyoto, Oct NLS1 - A Review; Thomas Boller25 Timing properties Please see Karen´s Leighly talk and Poster by Luigi Gallo #19 A few examples
Kyoto, Oct NLS1 - A Review; Thomas Boller26 Light curveFractional amplitude variability Tanaka, Gallo, Boller (in prep.)
Kyoto, Oct NLS1 - A Review; Thomas Boller27 The significance of the detection and available photon statistics Spectral drop detected with high significance Photon statistics above 7 keV limited, only about 30 photons ~500 ks observation required source + background spectrum background
Kyoto, Oct NLS1 - A Review; Thomas Boller28 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 emission dM/dt, M broad narrow optical lines dM/dt, M moderate extreme X-ray variability smaller M, relativistic effects flat steep power-laws inverse Compton effect Weak strong Fe II emission ?
Kyoto, Oct NLS1 - A Review; Thomas Boller29 XEUS NFI2 Con-X calorimeter E = 2eV Schwarzschild BH Kerr BH incl incl Torres et al. 03
Kyoto, Oct NLS1 - A Review; Thomas Boller30 Gallo et al. 2003
Kyoto, Oct NLS1 - A Review; Thomas Boller 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, luminosities column densities/covering fractions Time dependent changes of the edge energy from 7.10 to 7.44 keV within two years (1H ) Please see talk by Y. Tanaka
Kyoto, Oct NLS1 - A Review; Thomas Boller32 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] 22
Kyoto, Oct NLS1 - A Review; Thomas Boller33 BH Merger
Kyoto, Oct NLS1 - A Review; Thomas Boller 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
Kyoto, Oct NLS1 - A Review; Thomas Boller35 The relevance of NLS1 for understanding the Seyfert phenomenon more generally NLS1 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
Kyoto, Oct NLS1 - A Review; Thomas Boller36 Warm absorber and/or relativistically broadened C,N,O lines? presence of relativistically- broadened O,N,C lines are claimed from RGS spectra Branduardi-Raymont et al Chandra HETG spectra provide a different view
Kyoto, Oct NLS1 - A Review; Thomas Boller37 Lee et al. 2001: major feature at ~0.7 keV: neutral iron absorption Fe L3 Fe L2 OVII absorption explain feature between 0.7 –0.75 keV Presence of significant ionized absorption
Kyoto, Oct NLS1 - A Review; Thomas Boller38 G. Branduardi Broad Oxygen Lines J. Lee Fe 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
Kyoto, Oct NLS1 - A Review; Thomas Boller39 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 NLS Zwicky: first report on extreme variability ‘optical outbursts in I Zw1‘ Osterbrock initiates systematic investigation on NLS1 1. In the beginning