Radio Galaxies part 4 Apart from the radio

Radio Galaxies part 4

Apart from the radio the thin accretion disk around the AGN produces optical, UV, X-ray radiation The optical spectrum emitted by the gas depends upon the abundances of different elements, local ionization, density and temperature. § Photons with energy > 13. 6 e. V are absorbed by hydrogen atoms. In the process of recombining, line photons are emitted and this is the origin e. g. of Balmer-line spectra. § Collision between thermal electrons and ions excites the low-energy level of the ions, downward transition leads to the emission of so-called “forbidden-line” spectrum (possible in low density conditions).

Example of broad line radio galaxy (3 C 390. 3)

Optical spectrum, what can we derive: ü which lines ü flux/luminosity ü width (kinematics) ü ionization mechanism (line ratios) ü density/temperature of the emitting gas ü morphology of the ionized gas (any relation with the radio? ) ü continuum and stellar population using spectra and narrow band images

q Ionization parameter: ratio between ionizing photon flux/gas density q Temperature of the emitting gas q Mass of the emitting gas

photoionization models for different ionization parameters Examples of diagnostic diagrams

Broad line regions (BLR): § typical size (from variability) of 10 -100 light-days (Seyferts) up to few light-years (few x 0. 3 pc, quasars). § electron density is at least 108 cm-3 (from the absence of broad forbidden lines) § typical velocities 3000 -10000 km/s Narrow line regions (NLR): § typical density 103 to 106 cm-3 § gas velocity 300 – 1000 km/s § large range in size: from 100 -300 pc to tens of kpc

Powerful radio galaxies: energetics " Radiation Quasar luminosity: 1044 — 1047 erg s-1 Luminosity integrated over lifetime: 1057— 1062 erg " Jets " 43 46 -1 Winds Total wind power: 10 — 10 erg s Jet power: 1043 — 1047 erg s-1 Jet power integrated over lifetime: 1057 — 1062 erg Wind power integrated over lifetime: 1056 — 1061 erg + Starburst-induced superwinds….

Emission line nebulae: what can we learn?

Emission line haloes: <1 kpc scale " " " Kinematics. The emission line kinematics comprise a combination of gravitational motions, AGN-induced outflows, and AGN-induced turbulence Black hole masses. Now possible to determine direct dynamical masses for nearby PRG using near-nuclear emission line kinematics Feedback. The outflow component provides direct evidence for the AGN-induced feedback in the nearnuclear regions the presence of the nuclear activity could influence the evolution of the galaxy (e. g. clear gas away from the nuclear regions)

Cygnus A viewed by HST NICMOS 2. 0 mm Optical images

2. 0 micron image HST/NICMOS Evidence for a super-massive black hole in Cygnus A

Correlation between black hole mass and galaxy bulge mass/luminosity Cygnus A

§ broad permitted line seen in polarized line: only the scattered component can be seen Broad- and narrow line radio galaxies become undistinguishable

Emission line nebulae: 1 -5 kpc scale " Kinematics. " Ionization. Emission line kinematics a combination of AGN-induced and gravitational motions the AGN Outflows. Gas predominantly photoionized by Clear evidence for emission line outflows in Cygnus A and some compact radio sources, but outflow driving mechanism uncertain

Example of complex kinematics (IC 5063) 700 km/s Complex kinematics of the ionized gas in coincidence with the radio emission: this suggests interaction between radio plasma and ISM

Emission lines in (powerful) radio galaxies 6 [O III]λλ 4959, 5007 z = 0. 1501 ± 0. 0002 FWHM ~ 1350 km s-1 Relative flux 4 2 Δz ~ 600 km s 1 [O II] λλ 3727 [O III] z = 0. 1526 ± 0. 0002 H FWHM ~[O 650 s-1 II] km [Ne III] [Ne V] Wavelength (Å) (Tadhunter et al 2001)

Diagnostic diagrams including ionization from shocks

Emission line nebulae: 5 -100 kpc scale " Kinematics. Activity-induced gas motions are important along the full spatial extent of the radio structures, regardless of the ionization mechanism " Jet-induced shocks. " Gravitational motions. " Starbursts. The shocks that boost the surface brightness of the structures along the radio axes also induce extreme kinematics disturbance Require full spatial mapping of the emission line kinematics in order to disentangle gravitational from AGN-induced gas motions Starburst-induced superwinds may also affect the gas kinematics out to 10’s of kpc

Gas with very high ionization at 8 kpc from the nucleus Even if the nucleus is obscured by the torus, the extended emission line regions can tell us about the UV radiation from the nucleus.

Emission line “clouds” in the halo of Cen. A: D~3 Mpc

1000 km/s

Contours: radio Colors: ionized gas In some cases the radio galaxy seems to have a strong effect on the medium around. Diagnostic diagrams important to understand which mechanism is dominant

Radio galaxies at high redshift § Morphology of the extended emission line regions depends on the size of the radio source § Alignment between the emission lines and the radio axis § Interaction between radio and medium: does this also trigger star formation?

Any difference (in the optical lines) between low and high power radio galaxies?

What makes the difference? Well known dichotomy: low vs high power radio galaxies Differences not only in the radio WHY? high-power radio galaxy Intrinsic differences in the nuclear regions? Accretion occurring at low rate and/or radiative efficiency? No thick tori? low-power radio galaxy

The central regions of low-power radio galaxies No optical core Optical core No strong obscuration: optical core very often detected

From HST and X-ray The HST observations: ü High rate of optical cores detected ü Correlation between fluxes of optical and radio cores But so far we haven’t seen broad permitted lines

More on the host galaxy

The optical continuum of Radio Galaxies Usually the old stellar population is the dominant - as usual in elliptical galaxies - but in some cases a young stellar population component is observed (typical ages between 0. 5 and 2 Gyr). 3 C 321 § consistent with the merger hypothesis for the triggering of the radio activity. § but not a single type of merger § AGN appears late after the merger old stellar pop. young stellar pop. power law

3 C 305 3 C 293 Results from UV imaging 3 C 321 Allen et al. 2002

The young stellar component may come from a recent merger o We can use the age of the stars to date when this merger occurred o To be compared with the age of the radio source