INTRODUCTION to AGN “Sometimes you can’t stick your head in the engine, so you have to examine...
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Transcript of INTRODUCTION to AGN “Sometimes you can’t stick your head in the engine, so you have to examine...
INTRODUCTION to AGN
“Sometimes you can’t stick your head in the engine, so you have to examine the exhaust”-- D. E. Osterbrock
Astro 596G Spring 2007
In 2006, there were 2151 papers in ADS with “quasar” or “AGN” in their abstracts
Key Questions
• Growth of SMBHs1. Due to mergers, accretion, stellar captures?
• SMBHs and Galaxy/LSS formation1. Were BHs seeds or byproducts of galaxy formation?
2. How important is is the feedback from SMBHs in structure formation?
• Jets in AGN1. Are jets matter or Poynting flux dominated?
2. Why are some AGN radio-loud, some radio-quiet?
• Accretion Physics1. Is our basic cartoon of the central engine correct?
2. Is the unified model viable? Useful?
3. Have we included the essential physics?
AGN & Related Objects
• Energy output not related to “ordinary” stellar processes• Continuum bright in virtually every wave band• Mass accretion onto supermassive black holes
• Radio Galaxies• Radio-Loud Quasars• BL Lac’s, Blazars, OVV’s (Optically Violent Variables)• Radio-Quiet QSOs (Quasi-Stellar Objects)• Seyfert 1 & 2 Galaxies• LINERS (Low ionization nuclear emission line regions)• Starburst galaxies; ULIRGS (Ultraluminous IR Galaxies)
Refn: An Introduction to Active Galactic Nuclei, by Brad Peterson
Why study quasar emission lines?
• Probe inner few pc’s of the AGN• Learn about the unobservable UV continuum c.f. Zanstra temperatures UV originates in the inner region of the accretion disk UV photons from quasars an important contributor to the metagalactic UV background• Interesting line-formation phenomena because conditions are extreme• Want to understand the source of the gas which fuels the central engine• Unique probe of abundances at z=5-6• Possible uses as cosmological probes (e.g. Baldwin effect)• Use to measure central black hole masses in AGN
Broad red wing of Fe Kalpha emission reflection of X-ray continuum off inner accretion disk
Nandra et al. ASCA composite for Sy1’s
Radio: Synchrotron (relativistic electrons in B-field)Mm-1 micron: Dust emission1 micron - .2 keV: Thermal emission from optically thick accretion diskX-rays: Synchrotron, Inverse Compton, Hot corona + reflection
Continuum Spectral energy distributions:
Quasar and Seyfert 1 Spectra:
Broad permitted lines (widths > 10,000 km/sec)
Narrow forbidden lines (widths only few hundred km/sec), e.g. [OIII] 4959, 5007
CIII] 1909 is broad
Forbidden Lines: [O III]
Semi-Forbidden: C III]
Recombination:Ly alpha, Halpha
Aside of forbidden v. permitted lines, recombination lines:
In photoionized gas, the lines of hydrogen and helium are“recombination” lines, and to first order do not depend on physical conditions like density or temperature.
e-
Photon of Ly alpha, Halpha, etc
1
2
Most metals are collisionally excited (the first excited level is low enoughthat for nebular temperatures, collisions can populate the upper levels)
Whether or not the electron de-excites via emitting a photon orby a collision with a free electron depends on (1) density of particles,and (2) the Einstein A for the radiative de-excitation transition.
Permitted lines: Radiative de-excitation is fast (Einstein A is high) , so atom radiatively de-excites before a collisionForbidden lines: Radiative de-excitation is not likely. If the density is low enough, a collision will not happen, and the atom will de-excite radiatively we see the line. If the density is greater than the “Critical density” then the atom collisionally de-excites before it emits a photon no line
Ionization Parameter
dEcNr
UE
E H
ELE
2
1
2 4
Emission Lines arise in 2 separate “regions”
1. Narrow Line Region (NLR)• Extended spatially (~kpc) in nearby Seyferts• Low density n~ 10 3-6 cm-3 since you see forbidden lines like [OIII]• FWHM < 1000 km/s• Line diagnostics photoionized gas
2. Broad Line Region (BLR)• Permitted Lines only• T~10,000 K from CIII 977 / CIII]1909 ratios• Line widths up to ~40,000 km/sec
Recall thermal gas at T=104 K has width of ~10 km/sec Must have Doppler broadening due to bulk motion of emitting gas
* Densities n~109-10 cm -3
Since you don’t see forbidden lines, n>n(critical)they must be collisionally de-excited, although you do see broad CIII] so n<n(critical) for CIII]
NLRG, Seyfert 2’s: NLR only, BLR obscured or absentSeyfert 1’s, Quasars, BLRG: NLR and BLR visible
Unified Models for Sy1’s and Sy2’s: Antonucci & Miller 1985 ApJ 297, 621 Antonucci 1993 ARAA Vol. 31, p. 473
Spectropolarimetry of the Seyfert 2 galaxy NGC 1068:
Polarized Flux shows broad permitted lines:Looks like a Sy 1 in polarizedlightHβ [OIII]
Unified Model:
Sy 1’s and Sy 2’s are the same object, seen at different aspect angles.Polarized light is Thomson scattered BLR
Obscuring Torus
BLR light scattered by
electrons to us
BLR
Scatteringelectrons
Although local Seyferts, imaged with HST, often show disk-like, dustystructures in their cores on relatively large scales, direct evidence for an obscuring torus, required by the Unified Models, doesn’t really exist.
Theoretically, it’s not clear how you’d “make” a torus and why it wouldbe where it is
WFPC images of Seyfert Nuclei
Another part of the puzzle: Broad Absorption Line Quasars (BAL QSOs) Warm (i.e. ionized) UV and Xray absorbers Associated Absorbers
All these objects have outflowing, radiatively driven winds In a few cases, the absorption varies with time must be very close to the central engine Typically see very high ionization states, not typical of ISM clouds, e.g. NV, OVI, OVII etc
Although BAL winds are thought to be radiatively driven, it’s hard to haveenough radiation force without totally ionizing the material and making itImpossible to radiatively drive out
Perhaps the winds and the BLR are one and the same
Double-peaked Balmer-line profiles are seen in a few AGN
Shape and variability of line profile suggest an origin for Hbeta in a rotating disk
NGC 1097Storchi-Bergmann et al. (2003)
Reverberation MappingBrad Peterson and many collaborators
• Powerful probe of BLR structure and kinematics
• Measure the emission-line response to continuum variations
• Need good enough time sampling to derive time lags between continuum and emission line variations unambiguously
• Emission lines respond to changes in
the continuum flux with a “lag” corresponding to the light travel time from the ionizing source to the BLR
First Campaign: NGC 5548
Obs. With IUE every 4 days
in 1988-1989 season
Continuum
Emission line
NGC 5578
= r/c
“Isodelay Surfaces”
All pointson an “isodelaysurface” have the same extralight-travel timeto the observer,relative to photonsfrom the continuumsource.
= r/cCourtesy B. Peterson
Key Assumptions1 Continuum originates in a single central source.
– Continuum source (1013–14 cm) is much smaller than BLR (~1016 cm)
– Continuum source not necessarily isotropic
2 Light-travel time is most important time scale.• Cloud response instantaneous
rec = ( ne B)1 0.1 n101 hr
• BLR structure stable dyn = (R/VFWHM) 3 – 5 yrs
3 There is a simple, though not necessarily linear, relationship between the observed continuum and the ionizing continuum.
Reverberation Mapping Results
• Reverberation lags have been measured for 36 AGNs, mostly for H, but in some cases for multiple lines.
• AGNs with lags for multiple lines show that highest ionization emission lines respond most rapidly ionization stratification
• No significant lag is seen between the optical and UV continuum
• The delays for the different emission lines are smaller than models predicted
• The lag increases with decreasing ionization one zone models are out, must have radial stratification of BLR
• Revised BLR models since the BLR gas is closer to the ionizing photon source than previously thought, so density must be higher to keep the ionization parameter constant
n~ 1011 cm-3 Really optically thick
Time-Variable Lagsin NGC 5548
• 14 years of observing the H response in NGC 5548 shows that lags increase with the mean continuum flux.
• Measured lags range from 6 to 26 days
• Best fit is lag Lopt0.9
• Structural changes in
the BLR
Lopt0.9
Optical luminosity
Hbetalag
Locally Optimally Emitting Clouds Baldwin, Ferland, Korista & Verner 1995 ApJ 455, L119 Ferguson+ 1997 ApJ 487, 122
• All quasar emission line spectra “look alike” i.e. A single-zone model is pretty successful with a narrow range of density and ionization parameter implausible “fine-tuning” of BLR parameters
• Use CLOUDY to make a huge grid of BLR models as a function of density and ionization parameter (i.e. distance from the central engine)
• For each emission line, there is a narrow range of density & ionization parameter where the line formation is “maximally efficient” and most of the line emission is formed
• So you can have a completely chaotic BLR with no preferred density, etc.The observed spectrum is some average of the “full family” of models
Locally optimally-emitting cloud (LOC) model
• The flux variations in each line are responsivity-weighted.– Determined by where physical
conditions (mainly flux and particle density) give the largest response for given continuum increase.
• Emission in a particular line comes predominantly from clouds with optimal conditions for that line.
Ioni
zing
flu
x
Particle density