Clive Tadhunter University of Sheffield Starbursts and the triggering of the activity in low redshift radio galaxies Clive Tadhunter University of Sheffield Collaborators: J. Holt, D. Dicken, C. Ramos Almeida, R. Gonzalez Delgado, R. Morganti, J. Rodriguez-Zaurin, K. Inskip, K. Wills

Triggering mechanisms Galaxy mergers and interactions (Heckman et al. 1986, Smith & Heckman 1989) Accretion of gas from hot X-ray haloes - Bondi accretion of hot gas (Allen et al. 2006, Best et al. 2006, Hardcastle et al. 2007, Buttiglione et al. 2009) - Accretion of cool gas from cooling flow (e.g. Bremer et al. 1997) Cold accretion from large-scale filamentary structures (e.g. Keres 2005, Dekel et al. 2009)

Evidence for galaxy interactions and mergers in non-starburst radio galaxies Deep Gemini+GMOS imaging observations of 2Jy sample A large proportion of nearby radio galaxies show evidence for morphological disturbance consistent with triggering in major galaxy mergers and interactions (see talk by Cristina Ramos Almeida)

Triggering starbursts in major galaxy mergers Cox et al. (2008)

Starbursts in radio galaxies: occurrence Starburst rate from optical spectroscopy I: - 2Jy(0.15 < z < 0.7): 20 -- 35% (22 objects) Tadhunter et al. (2002) - 3CR(z<0.2): 33% (14 objects) Aretxaga et al. (2001), Wills et al. (2002) - 2Jy (z<0.08, FRIs): 25% (12 objects) Wills et al. (2004) UV imaging with HST - 3C (z<0.1): 100% HEG (6 objects); 5% LEG Baldi et al. (2008) Detection of PAH at mid-IR wavelengths - 3C (z<0.1, FRIs): 75% (24 objects) Leipski et al. (2009) Combined optical+far-IR continuum excess+MFIR colours+PAH - 2Jy(0.05 < z < 0.7): 15--35% Dicken et al. (2009,2010) UV and PAH techniques particularly sensitive to low levels of SF, especially if level of AGN activity weak

The reddened nuclear starburst in 3C305 WHT/ISIS Starburst Properties Age: 0.4 - 0.9 Gyr E(B-V)=0.4 - 0.8 mag Mass:1.5+/-0.5x1010 Msun (16 - 40% of total stellar mass) Hd CaII K Bruzual & Charlot(1996) models Salpeter IMF (0.1-125 Msun) 3C305 (z=0.042) Heckman et al. 1986

Starburst dominated Objects (z>0.15) 3C459 (z=0.22) NTT+EMMI YSP Properties Age: 0.05 Gyr Mass:4x109 Msun (>5% of total stellar mass in slit)

Objects with v.young starburst components PKS0023-26 (z=0.340) - VLT/FORS2 PKS0409-75 (z=0.69) - VLT/FORS2 YSP age: 30Myr Reddening: E(B-V)=0.8 YSP mass proportion: 9% YSP age: 10Myr Reddening: E(B-V)=0.9 YSP mass proportion: 4% These objects have: - Low UV polarization - Relatively weak narrow lines - No broad lines detected Holt et al. (2007)

The Ages of the YSP in ULIRG and PRG Tadhunter et al. (2005) Holt et al. (2006,2007) Wills et al. (2008) Tadhunter et al. (2010) Rodriguez-Zaurin et al. (2007,2008,2009,2010) Typical maximum age of radio source

Two main groups of starburst radio galaxies LIRG/ULIRG-like systems (tysp < 0.1Gyr) - Most have: - Radio source triggered quasi-simultaneously with starburst Post-starburst systems (tysp > 0.2 Gyr) - Radio source triggered (or retriggered) a significant period after the starburst episode

Starburst radio galaxies general properties Based on a detailed spectrosynthesis modelling of a sample of 22 radio galaxies with good evidence for YSP: 95% of starburst radio galaxies show signs of morphological disturbance (tidal tails, fans, shells, dust lanes, double nuclei etc.) Young stellar populations (YSP) contribute a significant proportion of the total stellar masses (5-40%) The YSP are spatially extended -- they generally detected across the full extents of the host galaxies over which accurate measurements can be made (although brightest in the nuclei) Overall, the results are consistent with the triggering of the activity in major, gas-rich galaxy mergers/interactions

Merger sequence for starburst radio galaxies

Cooling flow driven activity in Hydra A? Gemini+GMOS Hydra A, z=0.054, FRI Spitzer+IRS The similarity between the SRF rate and hot X-ray cooling rate is consistent with triggering by a cooling flow Rafferty et al. (2006)

PKS0023-26: a compact radio source at the centre of a cluster z=0.322, CSS Spitzer+IRS PAH

Star Formation in 4C41.17 at z=3.8? La Dunlop et al. 1994 Star formation rate: 2,000 - 10,000 M0/yr Dey et al. 1997

3C Radio Galaxies at 60mm with IRAS Only ~30% of 3CR radio galaxies at z<0.5 were detected by IRAS at 60mm

Spitzer/MIPS observations of complete samples of radio-loud AGN 2Jy sample S2.7GHz > 2.0 Jy Intermediate redshifts (0.05 < z < 0.7) Steep radio spectra (a1.4-5GHz < -0.5) 46 objects 3CRR sample S178MHz > 10.0 Jy Low redshifts (z < 0.1) FRII only 19 objects Spitzer/MIPS detection rates: 100% at 24m and 90% at 70m All objects have deep optical spectra, allowing accurate spectral classification, measurements of emission line luminosities, and assessment of stellar population mix

Correlations between MFIR and optical properties The 24m luminosity is strongly correlated with the [OIII]5007 emission line luminosity The 70m luminosity is also strongly correlated with the [OIII] luminosity, but with increased scatter The slopes of the 24m and 70m correlations are similar Tadhunter et al. (2007), Dicken et al. (2008,2009)

The starburst contribution to the far-IR SB Heating AGN Heating The far-IR emitting dust is predominantly heated by AGN illumination Starburst heating only significant in a minority of objects (~17 -- 35%) Tadhunter et al. (2007) Dicken et al. (2009, 2010)

A simple model for the dust/emission line structures Assume that both the emission lines and MFIR emission produced by AGN illumination Covering factors of mid-IR and far-IR emitting dust structures, and NLR: Cmir, Cfir and Cnlr

Energetic feasibility of AGN illumination Dicken et al. (2009) Allowing for a modest amount of intrinsic extinction, it is plausible that much of the far-IR continuum is in most radio galaxies is produced by AGN illumination of the NLR clouds

Triggering non-starburst radio galaxies Non-starburst radio galaxies make up >60% of the population of powerful radio galaxies Most non-starburst RG belong to the class of strong-lined objects that are thought to be powered by cold accretion Triggering possibilities include: - Gas accretion in a tidal encounter, or around the time of first pass of nuclei in a merger - Re-triggering the activity a substantial period (>1Gyr) after the major merger-induced starburst - Minor mergers (>3:1 mass ratio)

Triggering starbursts in major galaxy mergers Cox et al. (2008)

Evidence for galaxy interactions and mergers in non-starburst radio galaxies Deep Gemini+GMOS imaging observations of 2Jy sample 0.05 < z < 0.7, 46 objects, r’ or i’ band 85% of the non-starburst radio galaxies in 2Jy sample show signs of morphological disturbance (Ramos Almeida et al. 2009)

How do the WLRG fit in? Commonly proposed that weak line radio galaxies (WLRG) are triggered/fuelled by Bondi accretion of the hot ISM in the host galaxies/clusters But significant proportion of the optical starburst radio galaxies (~40%) -- particularly those with older young stellar populations -- are WLRG (e.g. Fornax A, Cen A, Hydra A, PKS0347+09, PKS0620-52, 3C213.1, 3C236, 3C292, NGC612) The presence of SF provides evidence of cold accretion into the circum-nuclear regions of some WLRG Most such objects show evidence for a rich ISM in the form of dust lanes; many also show PAH features in their mid-IR spectra

Star formation in Fornax A Evidence for young stellar populations: - Diffuse stellar light has luminosity weighted age 2-3 Gyr (Kuntschner 2002) - Globular clusters have ages 3+/-0.5 Gyr (Goudfrooij et al. 2003) ----> current galaxy formed from a major merger of gas-rich galaxies 2-3 Gyr ago HST+ACS Goudfrooij et al. (2005)

The double AGN in PKS0347+05 WLRG Spitzer+IRS This WLRG is clearly in an interacting system with a rich ISM and plenty of star formation. PAH Sy 1 z=0.339, FRII

A torus in the WLRG PKS0043-42? PKS0043-42 Spitzer+IRS z=0.116, FRII Silicate absorption Dicken et al. (2010)

Detection of weak PAH in nearby FRI galaxies 75% of the sample of 24 nearby FRI radio galaxies presented by Leipski et al.(2009) show PAH features Possible evidence for low-level star formation in the circum-nuclear regions

Evidence for a rich ISM in the nuclear regions of WLRG Dust lanes (e.g. Fornax A, Cen A, Hydra A) Circum-nuclear (warm) gas disks (e.g. M87), and cool molecular disks Detection of hot dust emission at mid-IR wavelengths (e.g. PKS0043-42, Leipski et al. 2009) Detection of PAH features in mid-IR spectra of a large proportion of nearby FRI sources (Leipski et al. 2009) Detection of compact emission line regions associated with the compact optical cores of FRI radio sources (e.g. Capetti et al. 2005)

Conclusions Most SB radio galaxies consistent with triggering in major gas-rich mergers; but triggering can occur before, around or a long time after the coalescence of the merging nuclei Non-starburst radio galaxies also likely to be triggered in galaxy mergers and interactions (but much earlier or later in sequence, or by more minor mergers) Radio-loud AGN activity is not solely associated with a particular phase of unique type of gas accretion event The heating of the far-IR emitting dust is likely to be dominated by AGN illumination in the majority of PRG; the far-IR doesn’t always provide a good diagnostic of SF Evidence for cool/warm gas accretion into the circum-nuclear regions of WLRG

Correlation analysis -- 2Jy sample L24 vs Lrad L24 vs L[OIII] L[OIII] vs Lrad L24 vs z

An evolutionary link with ULIRGs? Some powerful radio galaxies are ULIRGs (3C48, PKS1345+12, PKS1549-79, PKS2135-20, 3C459) ULIRG radio galaxies have stellar populations properties similar to the general population of ULIRGs (tysp < 0.1 Gyr) The stellar masses of the intermediate age, post-starburst stellar populations in some radio galaxies are consistent with the idea that they have evolved from ULIRG/LIRGs

ULIRG/starburst radio galaxy stellar mass comparison Nearby 1Jy ULIRGs (z<0.18) (Rodriguez Zaurin et al. 2009, 2010) Not all starburst radio galaxies can have evolved from ULIRGs Starburst radio galaxies (z<0.7) (Tadhunter et al. 2010)

Star formation in major mergers Springel et al. (2005)

Activity and galaxy evolution Evolution of activity and star formation Black hole vs. galaxy bulge properties z Dunlop & Peacock 1990, Madau 1987 Tremaine et al. (2002) Triggering? Feedback?

Outstanding questions