Active Galactic Nuclei
Karina Caputi
Physics of Galaxies 2016-2017 Q4
Rijksuniversiteit Groningen
A bit of history…
Seyfert galaxies
Broad-line emission from galactic nuclei are know since early 1900’s
The displayed broad lines could only be excited by photons more energetic than those from young stars
Carl Seyfert
QSO first discovery
Boom of radioastronomy in 1950s: Third Cambridge (3C) Catalogue
Most 3C sources were identified with elliptical galaxies
…but a few looked point-like (like stars)
They indicated redshifts unusually high for such bright objects
Maarten Schmidt 3C 273 has B,V < 13 mag and z=0.158
And contemporary works by Sandage, Matthews, etc.
Farthest QSO known to date
Mortlock et al. (2011)
z=7.085
Peak of QSO activity at z~2-3 (age of Universe ~ 2-3 Gyr)
More recent source discovered at z>8, but it is still unclear whether AGN
The AGN components
QSO and AGN
AGN/QSO classification is complex - QSO are the the most luminous AGN
(outshine host galaxy, so they look point-like)
Credit: A. Simonnet
✦ blue light excess
✦ light variability in some cases
✦ optical light polarisation
✦ X-ray emission due to accretion
✦ radio quiet or loud (some with jets)
✦ some have broad (> 1000 km/s) line emission (permitted lines) - due e 1
✦ Others only narrow lines - AGN type 2
The central engine
The central engine is a supermassive black hole accreting gas
Black hole mass ~ 10 - 10 Msun - event horizon size of solar system
6 8Gas supplied at a rate of ~ 1 Msun/yr
Gas being accreted forms a disk which is heated by friction UV, optical and X-ray
14.3. MAXIMUM ENERGY RELEASE IN SPHERICAL ACCRETION 337
Table 14.1: Energy released by accretion onto various objects Accretion onto Max energy released (erg g−1) Ratio to fusion
Black hole 4.5 × 1020 75
Neutron star 1.3 × 1020 20
White dwarf 1.3 × 1017 0.02
Normal star 1.9 × 1015 10−4
14.3 Maximum Energy Release in Spherical Accretion
The most spectacular consequence of accretion is that it is an efficient mechanism for extracting gravitational energy.
• The energy released by accretion is approximately
∆Eacc = G Mm R ,
where M is the mass of the object, R is its radius, and m is the mass accreted.
• In Table 14.1 the amount of energy released per gram of hydrogen accreted onto the surface of various ob- jects is summarized (see Exercise).
• From Table 14.1, we see that accretion onto very compact objects is a much more efficient source of energy than is hydrogen fusion.
• But accretion onto normal stars or even white dwarfs is much less efficient than converting the equivalent amount of mass to energy by fusion.
14.3. MAXIMUM ENERGY RELEASE IN SPHERICAL ACCRETION 337
Table 14.1: Energy released by accretion onto various objects Accretion onto Max energy released (erg g−1) Ratio to fusion
Black hole 4.5 × 1020 75
Neutron star 1.3 × 1020 20
White dwarf 1.3 × 1017 0.02
Normal star 1.9 × 1015 10−4
14.3 Maximum Energy Release in Spherical Accretion
The most spectacular consequence of accretion is that it is an efficient mechanism for extracting gravitational energy.
• The energy released by accretion is approximately
∆E
acc= G Mm R ,
where M is the mass of the object, R is its radius, and m is the mass accreted.
• In Table 14.1 the amount of energy released per gram of hydrogen accreted onto the surface of various ob- jects is summarized (see Exercise).
• From Table 14.1, we see that accretion onto very compact objects is a much more efficient source of energy than is hydrogen fusion.
• But accretion onto normal stars or even white dwarfs is much less efficient than converting the equivalent amount of mass to energy by fusion.
14.3. MAXIMUM ENERGY RELEASE IN SPHERICAL ACCRETION 337
Table 14.1: Energy released by accretion onto various objects Accretion onto Max energy released (erg g
−1) Ratio to fusion
Black hole 4.5 × 10
2075
Neutron star 1.3 × 10
2020
White dwarf 1.3 × 10
170.02
Normal star 1.9 × 10
1510
−414.3 Maximum Energy Release in Spherical Accretion
The most spectacular consequence of accretion is that it is an efficient mechanism for extracting gravitational energy.
• The energy released by accretion is approximately
∆E
acc= G Mm R ,
where M is the mass of the object, R is its radius, and m is the mass accreted.
• In Table 14.1 the amount of energy released per gram of hydrogen accreted onto the surface of various ob- jects is summarized (see Exercise).
• From Table 14.1, we see that accretion onto very compact objects is a much more efficient source of energy than is hydrogen fusion.
• But accretion onto normal stars or even white dwarfs is much less efficient than converting the equivalent amount of mass to energy by fusion.
Credit: M. Guidry
338 CHAPTER 14. BLACK HOLES AS CENTRAL ENGINES
Let us assume for the moment, unrealistically, that all ki- netic energy generated by conversion of gravitational en- ergy in accretion is radiated from the system (we address the issue of efficiency for realistic accretion shortly). Then the accretion luminosity is
Lacc = GM ˙M
R ≃ 1.3 × 1021! M/M⊙ R/km
" ! M˙ g s−1
"
erg s−1,
if we assume a steady accretion rate M.˙
The central engine (cont.)
14.3. MAXIMUM ENERGY RELEASE IN SPHERICAL ACCRETION 339
Table 14.2: Some Eddington-limited accretion rates Compact object Radius (km) Max accretion rate (g s−1)
White dwarf ∼ 104 1021
Neutron star ∼ 10 1018
14.3.1 Limits on Accretion Rates
The Eddington luminosity is
Ledd = 4
π
GMmpcσ
,with σ ithe effective cross section for photon scattering.
• For fully ionized hydrogen, we may approximate σ by the Thomson cross section to give
Ledd ≃ 1.3 × 1038! M M⊙
"
erg s−1.
• If the Eddington luminosity is exceeded (in which case we say that the luminosity is
super-Eddington),accretion will be blocked by the radiation pressure, implying that there is a maximum accretion rate on compact objects.
• Equating
Laccand
Leddgives
M˙max ≃ 1017! R km
"
g s−1
Eddington-limited accretion rates based on this formula are given in Table 14.2.
14.3. MAXIMUM ENERGY RELEASE IN SPHERICAL ACCRETION 339
Table 14.2: Some Eddington-limited accretion rates Compact object Radius (km) Max accretion rate (g s−1)
White dwarf ∼ 104 1021
Neutron star ∼ 10 1018
14.3.1 Limits on Accretion Rates
The Eddington luminosity is
Ledd = 4πGMmpc
σ ,
with
σithe effective cross section for photon scattering.
• For fully ionized hydrogen, we may approximate
σby the Thomson cross section to give
Ledd ≃ 1.3 × 1038! M M⊙
"
erg s−1.
• If the Eddington luminosity is exceeded (in which case we say that the luminosity is
super-Eddington),accretion will be blocked by the radiation pressure, implying that there is a maximum accretion rate on compact objects.
• Equating
Laccand
Leddgives
M˙max ≃ 1017! R km
"
g s−1
Eddington-limited accretion rates based on this formula are given in Table 14.2.
14.3. MAXIMUM ENERGY RELEASE IN SPHERICAL ACCRETION 339
Table 14.2: Some Eddington-limited accretion rates Compact object Radius (km) Max accretion rate (g s−1)
White dwarf ∼ 104 1021
Neutron star ∼ 10 1018
14.3.1 Limits on Accretion Rates
The Eddington luminosity is
L
edd= 4πGMm
pc
σ ,
with σ ithe effective cross section for photon scattering.
• For fully ionized hydrogen, we may approximate σ by the Thomson cross section to give
L
edd≃ 1.3 × 10
38! M M
⊙"
erg s
−1.
• If the Eddington luminosity is exceeded (in which case we say that the luminosity is super-Eddington), accretion will be blocked by the radiation pressure, implying that there is a maximum accretion rate on compact objects.
• Equating L
accand L
eddgives
M ˙
max≃ 10
17! R km
"
g s
−1Eddington-limited accretion rates based on this formula are given in Table 14.2.
14.3. MAXIMUM ENERGY RELEASE IN SPHERICAL ACCRETION 339
Table 14.2: Some Eddington-limited accretion rates Compact object Radius (km) Max accretion rate (g s−1)
White dwarf ∼ 104 1021
Neutron star ∼ 10 1018
14.3.1 Limits on Accretion Rates The Eddington luminosity is
L
edd= 4πGMm
pc
σ ,
with σ ithe effective cross section for photon scattering.
• For fully ionized hydrogen, we may approximate σ by the Thomson cross section to give
L
edd≃ 1.3 × 10
38! M M
⊙"
erg s
−1.
• If the Eddington luminosity is exceeded (in which case we say that the luminosity is super-Eddington), accretion will be blocked by the radiation pressure, implying that there is a maximum accretion rate on compact objects.
• Equating L
accand L
eddgives
M ˙
max≃ 10
17! R km
"
g s
−1Eddington-limited accretion rates based on this formula are given in Table 14.2.
Credit: M. Guidry
Accretion efficiencies:
340 CHAPTER 14. BLACK HOLES AS CENTRAL ENGINES
14.3.2 Accretion Efficiencies
• For the gravitational energy released by accretion to be extracted, it must be radiated or matter must be ejected at high kinetic en- ergy (for example, in AGN jets).
• Generally, we expect that such processes are inefficient and that only a fraction of the potential energy available from accretion can be extracted to do external work.
• This issue is particularly critical when black holes are the cen- tral accreting object, since they have no “surface” onto which accretion may take place and the event horizon makes energy extraction acutely problematic.
• Let us modify our previous equation for accretion power by in- troducing an efficiency factor η that ranges from 0 to 1:
Lacc = 2ηGM ˙M R .
• Specializing for the black hole case, it is logical to take the Schwarzschild radius (the radius of the event horizon for a spher- ical black hole), which is given by
Rsc = 2GM
c2 = 2.95! M M⊙
"
km,
to define the “accretion radius”, since any energy to be extracted from accretion must be emitted from outside that radius.
340 CHAPTER 14. BLACK HOLES AS CENTRAL ENGINES
14.3.2 Accretion Efficiencies
• For the gravitational energy released by accretion to be extracted, it must be radiated or matter must be ejected at high kinetic en- ergy (for example, in AGN jets).
• Generally, we expect that such processes are inefficient and that only a fraction of the potential energy available from accretion can be extracted to do external work.
• This issue is particularly critical when black holes are the cen- tral accreting object, since they have no “surface” onto which accretion may take place and the event horizon makes energy extraction acutely problematic.
• Let us modify our previous equation for accretion power by in- troducing an efficiency factor η that ranges from 0 to 1:
Lacc = 2ηGM ˙M R .
• Specializing for the black hole case, it is logical to take the Schwarzschild radius (the radius of the event horizon for a spher- ical black hole), which is given by
Rsc = 2GM
c2 = 2.95! M M⊙
"
km,
to define the “accretion radius”, since any energy to be extracted from accretion must be emitted from outside that radius.
η=0.1 - typical value
(up to 0.3-0.4 for rotating black holes)
The broad-line region
Urry & Padovani (1995)
Broad-line region extends 0.01-0.1 pc around central engine
Very hot gas clouds w/ v ~1000-10,000 km/s
Although different components are present (scaled) in both stellar and supermassive black holes, broad-line regions are exclusive to supermassive black holes
Direct visibility is extremely difficult
The dusty torus
Current evidence suggests that dusty torus is clumpy rather than homogenous
Tristram et al.
Circinus
The narrow-line region
Urry & Padovani (1995)
Narrow-line region extends 100-1000 pc out of central engine
Well resolved for nearby AGN with HST Gas clouds w/ v ~100-500 km/s
Overlaps host galaxy (distinction unclear)
AGN Classification
The Unification Scheme
Urry & Padovani (1995)
AGN type 1-2 classification depends only on the viewing angle
Key: polarised light
Radiative versus jet mode
– 9 –(more recent classif.)
Direct AGN light
Jet mode Radiative mode
Low−excitation radio source
Type 2 Type 1
High−excitation radio source
Light dominated by host galaxy
Edd L/L > 0.01Edd
Radio LoudRadio Quiet
* Weak (or absent) narrow, low
* Old stellar population; little SF
* FR1 or FR2 radio morphology
* Moderate radio luminosity
* Very massive early−type galaxy
* Very massive black hole
* Massive early−type galaxy
* Massive black hole
* Old stellar population with some on−going star formation
* High radio luminosity
* Mostly FR2 morphology
* Strong high−ionisation narrow lines
excitation radio source, but with addition of:
* Direct AGN light
* Broad permitted emission lines
Host galaxy properties like Type−2
* Direct AGN light
* Broad permitted emission lines
* Bias towards face−on orientation
* Sometimes, beamed radio emission
AGN LINER
* Old stellar population; little SF
* Weak, small−scale radio jets
* Massive early−type galaxy
* Massive black hole
* Moderate strength, low−ionisation narrow emission lines
* Moderate mass black hole
* Weak or no radio jets
* Strong high−ionisation narrow lines galaxy with pseudo−bulge
ionisation emission lines
Host galaxy properties like high−
* Significant central star−formation
L/L < 0.01~ ~
Radio−loud QSO
Radio Quiet QSO / Seyfert 1 Type 2 QSO / Seyfert 2
* QSOs more luminous than Seyferts
QSO and Seyfert 2, respectively, but with addition of:
* Moderately massive early−type disk
Fig. 4.— The categorisation of the local AGN population adopted throughout this review. The blue text describes typical properties of each AGN class. These, together with the spread of properties for each class, will be justified throughout the review.
2.2. Finding AGN
This review is focused on insights into the co-evolution of SMBHs and galaxies that have been derived from large surveys of the local universe. For such investigations of the radiative-mode AGN it is the obscured (Type 2) AGN that are far and away the more valuable. In these objects the blinding glare of the UV and optical continuum emission from the central accretion disk has been blocked by the natural coronagraph created by the dusty obscuring structure. The remaining UV and optical continuum is generally dominated by the galaxy’s stellar component (Kauffmann et al. 2003a) which can then be readily characterized. In the sections to follow we will therefore restrict our discussion of radiative-mode AGN to techniques that can recognize Type 2 AGN. For the jet-mode AGN the intrinsic UV and optical emission from the AGN is generally weak or absent unless the observer is looking directly down the jet axis (e.g. Urry & Padovani 1995). Thus, the host galaxy properties can be easily studied without contamination.
Heckman & Best (2013)
Spectral Properties
The X-ray spectrum
Credit: G. Risaliti
The optical spectrum
Broad lines
Narrow lines
BPT
diagram
The infrared spectrum
Quasar 3C249.1
Siebenmorgen et al. (2005) dusty torus
(power law at 1-5 um)
Silicate absorption
The importance of silicate absorption and PAH emission varies among AGN
AGN host galaxies
How to study AGN host galaxies
PSF subtraction is critical
point-like source
(AGN) can outshine
host in some cases
AGN feedback: positive or negative?
Negative feedback (i.e., which suppresses star formation) is
necessary to explain SF quenching of massive galaxies
Credit: J. Silk
radiative mode: large amounts of gas flow onto AGN
jet mode: AGN drives powerful jets and cocoons that heat circumgalactic and halo gas
…but AGN outflows can also compress gas clouds and trigger
new star formation:
positive feedback
Cresci et al. (2015)