The Structure of Active Galactic Nuclei on Scales from 100mas to 100µas

Transcription

1 The Structure of Active Galactic Nuclei on Scales from 100mas to 100µas Martin Elvis Harvard-Smithsonian Center for Astrophysics

2 Quasars the Quintessential Point Sources 100,000 th Hubble Exposure, credit: STScI, Steidel (Caltech)

3 Scales in AGNs Painfully deduced from decades of spectroscopy and variabiity studies cm Host Narrow Emission Lines (NLR) bicones 1 mas ~100 l-day ~3x10 17 cm cm Cool Dust Hot Dust Broad Emission Lines cm 1 AU Seyferts 107 M Wind 20 Mpc Low High Black Hole Torus X-ray Continuum SMBH Sphere of influence Optical/UV continuum Many structures in common with stars

4 Sensitivity is Crucial extra mags would open a huge discovery space N K Vega nuclear Data thanks to Leonard Burtscher

5 The Quasar Standard Model No prediction of: Atomic Features: AGN types Maximally Hot dust X-rays Evolution

6 The Broad Emission Line Region

7 Quasar Atomic Features: Broad Emission Lines Ly 1216 N V 1240 FWHM~ few %c 10 Si IV 1400 C IV 1549 F (arbitrary units) 5 C III] 1909 Mg II 2798 [Ne V] 3426 H 4340 H 4101 [O III] 4959, 5007 He II 1640 O VI 1035 C II] 2326 [O II] 3727 [Ne III] 3869 H Rest wavelength (Å) Dense, high ionization gas close to black hole Peterson 1999

8 Quasar Sizes (& Black Hole Masses) v 2 r=const Keplerian v 2 r= GM Keplerian R=L 1/2 ~0.3 mas In Nearest AGNs R (cm) Lag (days) v2r Reverberation Mapping Peterson et al. 1993, PASP, 105, 247; 2006MmSAI P R( r g ) FWHM Peterson & Wandel 1999

9 BEL Polarimetry Warning: Implies significant electron-scattered light polarization PA Mrk 985 Position angle swing by 40 o Hydrogen Balmer α total flux Smith et al. 2005, MNRAS in press. astro-ph/ Smith J.E., 2005, MNRAS astro-ph/ Smith J.E., 2002, MNRAS astro-ph/

10 A Simple Wind Model Risaliti & Elvis, 2010, A&A 516, A 89 High Ionization Absorber Warm Absorber/ High ionization BLR Cold Eclipsers/ Low ionization BLR Slow Cold Eclipsers NLR Bicones BALs Failed Compton wind Line-Driven Wind Failed wind Dust-Driven Wind Czerny et al. Image in type 1? The 3 Forms of Radiation Pressure Explain Quasar Structure

11 Resolving the Broad Emission Line Region Hβ BLR diameters (mas)

12 Near-Infrared Broad Emission Lines J Y H K 10% IRTF/SPEX YJHK Spectra of AGN Landt et al. 2008

13 Accretion Disk Winds: the 4 th Element Explains: Broad, Narrow Absorption Lines, High Ionization Emission Lines, hot dust No prediction of: Maximally Hot dust X-rays Evolution

14 Hot Dust in AGNs

15 Scales in AGNs cm Host Narrow Emission Lines (NLR) bicones 1 mas ~100 l-day ~3x10 17 cm cm Cool Dust Hot Dust Broad Emission Lines cm 1 AU Seyferts 107 M Wind 20 Mpc Low High Black Hole Torus SMBH Sphere of influence X-ray Continuum Optical/UV continuum

16 Maximally Hot Dust Glickman et al Not seen in starburst galaxies T=1260 K R sub = 0.13 L 44 1/2 T = 1.5x10 6 R g Barvainis 1987, Lawrence & Elvis 2010

17 The Quasar Torus Emission Radio! Dust emission Torus IR! accre(on disk Opt/UV! EUV! X-ray! α ox Peak~10µm T~150K Large Area ~10,000 A Short limit~1µm T~1500K Small area, A 18 Well-suited to interferometry Elvis et al ApJS, 95, 1

18 AGN Flattened Obscurers NGC1068 Hidden Broad Emission Line Polarized flux spectrum Antonucci & Miller 1985 ApJ 297, 621 Warning: Implies significant electron-scattered light

19 Dust reprocesses UV, X-rays accre(on disk Radio! IR! Opt/UV! EUV! X-ray! Dust Reddening α ox Lyman Limit 912A Photoelectric Absorption 18 Elvis et al ApJS, 95, 1

20 Hot Dust Region Size Agrees roughly with Prediction Details tell dust properties Suganuma et al ApJ, 639, 46 MAGNUM Project ~0.5 mas Rapid dust formation as AGN luminosity dims (~1yr) Koshida et al. 2009

21 The Mid-IR Dust and Narrow Emission Line Regions

22 Scales in AGNs cm Host Narrow Emission Lines (NLR) bicones 1 mas ~100 l-day ~3x10 17 cm cm Cool Dust Hot Dust Broad Emission Lines cm 1 AU Seyferts 107 M Wind 20 Mpc Low High Black Hole Torus SMBH Sphere of influence X-ray Continuum Optical/UV continuum

23 Gap between100pc and sub-100pc mid-ir emission VISIR 12µm imaging Gandhi et al <100 σ =0.18 Log[F(Mid-IR)/f(X-ray)] Well-defined IR core

24 Quasar Atomic Features: Narrow Forbidden Emission Lines Ly 1216 N V 1240 FWHM~ km/s 10 Si IV 1400 C IV 1549 F (arbitrary units) 5 C III] 1909 Mg II 2798 [Ne V] 3426 H 4340 H 4101 [O III] 4959, 5007 He II 1640 O VI 1035 C II] 2326 [O II] 3727 [Ne III] 3869 H Rest wavelength (Å) Peterson 1999 Low density, high ionization gas far from the black hole

25 Narrow Line Bi-cones in AGNs Opt. Continuum [OIII] 5007 Tadhunter & Tsvetanov 1989 Nature 341, 422

26 The Bi-cone Region: Feeding and Feedback Storchi-Bergman et al.; Wang J. et al. (2011a) NGC4151: Bicones show feedback Spiral inflow shows feeding Need to follow structure well within black hole sphere of influence <10pc, <100 mas Contours = H 2 emission Colors = X-ray Hardness ~ N H

27 The Bi-cone Region: Feeding and Feedback Storchi-Bergman et al.; Wang J. et al. (2011a) NGC4151: Bicones show feedback Spiral inflow shows feeding Need to follow structure well within black hole sphere of influence <10pc, <100 mas Contours = H 2 emission Colors = X-ray Hardness ~ N H

28 Near-Infrared Narrow Emission Lines Mostly weak Landt et al. 2008

29 Warped Disk Obscurers NGC4258 Maser also Circinus Gal Center? Rijkhorst et al Observed warps: Maser disks CO disks NGC1068 CO disk Schinnerer et al Produced by isotropic accretion molecular clouds or minor mergers Volonteri et al. 2007

30 Warped Mid-IR Disk Obscurers Predicts: correct Type1:Type2 ratio* Jet-obscurer axis misalignments Observable with VLT-I MIDI?

31 High Redshift Quasars

32 Cosmology: Angular dia. vs. Linear dia. = metric Angular dia. vs. z SN1a CIV from ground Λ=0, Ω=1 Λ=0.7, Ω=0.3 1µas dia.

33 Magdelena Ridge Observatory Interferometer True imaging with many baselines: ~1mas ~0.1pc = Hot dust region Sensitive enough to detect many AGNs: Needs ~US$50M

34 Magdelena Ridge Observatory Interferometer True imaging with many baselines: ~1mas ~0.1pc = Hot dust region Sensitive enough to detect many AGNs: Needs ~US$50M

35 AGN Interferometer Wish List Host 1. K ~0.1mas 2. N~1mas Narrow Emission Lines (NLR) bicones 1 mas ~100 l-day ~3x10 17 cm mag. more sensitivity: K> cm 4. Emission cm line centroiding cm to <0.1mas 1 AU Seyferts 107 M 5. US$50M for MRO-I Cool Dust Hot Dust Broad Emission Lines Wind 20 Mpc Low High Black Hole Torus SMBH Sphere of influence X-ray Continuum Optical/UV continuum

36 Broader Interferometry Considerations

37 Movies, not Snapshots Astronomy suffers from a static illusion What we can image changes on timescales longer than our lifetimes At sub- arcsec resolution we start to see changing structures At mas resolution everything moves Qualitatively new view of universe A partial list: (please send additions) Galactic Center stars (AO) HH-30 expanding jets (HST) Rotating pinwheel around WR104 XZ Tau expanding jet (HST) Mizar A binary orbit V1663Aql - Nova expansion SN 1987A expansion/rings (speckle, HST) Crab nebula wisps (Chandra) Vela SN jet (Chandra) Superluminal radio jets (VLBA)

38 Imaging Quasars What we really want is to look at quasar structure Imaging reverberation mapping of Broad Emission Line Region: 6-D: 3 space, 3 velocity Also hot dust region Imaging [x, y, v(z)] Reverberation lag [z] y 100 microarcsec scale ~ independent of redshift [v(x,y)] x z

39 Imaging Quasars What we really want is to look at quasar structure Imaging reverberation mapping of Broad Emission Line Region: 6-D: 3 space, 3 velocity Also hot dust region 100 microarcsec scale ~ independent of redshift Ideal: 5 km-10 km IR 2µm interferometer at Antarctica Dome A or C, Greenland ice peak ½-1km UV space interferometer

40 A Sociological Note Extragalactic astronomers don t ask for high angular resolution because what they do doesn t need it What they do doesn t need high angular resolution because they can t do it I.e. They never thought about it Need to proseletyse

41 Angular Sizes of Astronomical Objects Are we missing classes of objects? Image Sn1a to get Baade-Wesselink distances? axion constraints from stellar diameters/ pulsations? [Physics Today] 1mas 0.1mas

42 X-ray Interferometry X-ray lab fringes Cash et al Nature

43 X-ray Telephoto Interferometer Willingale, Butcher &Stevenson, 2005 SPIE, 5900, large flat mirrors M1,M3,M4 ~1 meter 1keV Nesting of parallel systems. Slatted mirror M2

44 Gamma-ray Interferometry ~0.1 µarcsec, ~100,000 km focal length Fresnel/Laue Imagers In Gamma-rays Skinner G., 2004 Applied Optics, 43, 4845