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Impact of Jet Feedback on H 2 and Star Formation in Radio Galaxies

Patrick Ogle (Caltech, Spitzer Science Center) R. Antonucci, C. Leipski, Phil Appleton, Francois Boulanger. Impact of Jet Feedback on H 2 and Star Formation in Radio Galaxies. Normal Star-Forming Galaxies. Spitzer SINGS survey of nearby galaxies (Smith 07).

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Impact of Jet Feedback on H 2 and Star Formation in Radio Galaxies

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  1. Patrick Ogle (Caltech, Spitzer Science Center) R. Antonucci, C. Leipski, Phil Appleton, Francois Boulanger Impact of Jet Feedback on H2 and Star Formation in Radio Galaxies

  2. Normal Star-Forming Galaxies • Spitzer SINGS survey of nearby galaxies (Smith 07). • Polycyclic Aromatic Hydrocarbon (PAH) dust is excited by UV in stellar photodissociation regions. • PAH emission is useful for estimating star-formation rates in AGN hosts. The 7.7 um feature is not excited by AGN activity. • H2 emission is weak. H2 PAHs

  3. Spitzer IRS radio galaxy survey: 17/57 (30%) of 3C radio galaxies at z<0.2 have strong H2! Environment: • 14/17 have close or interacting companions. • 6/17 live in cool-core clusters. (Ogle et al. 08, in prep.) Radio Galaxies with Extreme H2

  4. Radio Galaxy 3C 326 (z=0.089) WSRT 21cm 1.9 Mpc radio lobes (Leahy). • Spitzer IRS spectrum dominated by pure-rotational H2 lines: • L(H2)=81041 erg/s • L(H2)/LIR~0.05-0.1 • M(H2)=1.1109 M (Ogle et al. 2007) Spitzer IRAC: galaxy pair (sep. 42 kpc), connected by tidal bridge.

  5. H2 Emission dominates cooling in C-type shocks (Le Bourlot 02) H2 Shock-Excitation in 3C 326 • T(H2)=150-1000 K • Magnetic (C-type) shock model: 2 velocities: v=4, 20 km/s • nH=104 cm-3, B=100 G (Guillard 08, in prep)

  6. MOHEGs = H2 Emission Galaxies L(H2)/L(IR)>210-3 • Stephan's Quintet shock (Appleton et al. 06). • Zw 3146 cool-core cluster cD (Egami et al. 06). • SINGS AGNs (Roussel et al. 07) • Radio Galaxies (Ogle et al. 07,08) Infrared Luminosity

  7. Shocks vs. Star Formation • H2and PAH dust occupy same ISM phase. • Star forming galaxies have L(H2)/L(7.7 m PAH)~810-3 • Larger H2/PAH indicates shock heatedH2 in: -Radio galaxies (Ogle 08) -LINERs, Seyferts (Roussel 07) -Dusty ellipticals (Kaneda 08). Infrared Luminosity (Ogle et al. 2008)

  8. Shocks vs. AGN X-ray Heating • AGN X-ray luminosities from Chandra (Evans 06; Hardcastle 06; Balmaverde 06; Ho 01) • XDR maximum theoretical X-ray to H2 conversion ~ 5% (Maloney 1996) • Most of the AGN are not strong enough X-ray emitters to power the H2. AGN X-ray Luminosity

  9. Radio Jet Mechanical Heating? • Radio jet cavity powers are measured for 6/17 MOHEGs. (Rafferty 06; Bîrzan 04) • P(jet cavity) = 4pV/t(bouyant) p,V, t estimated via Chandra. • L(H2)/P(jet)=10-4 -- 210-3 • Jet-driven H2 outflow or fountain? (FWHM ~ 500 km/s seen in some sources.) • H2 cooling time ~104 yr. --Requires sustained heating Radio Jet Cavity Power

  10. Perseus A-- Multiphase ISM H H2 CO (2-1) • M(cold H2)=41010 M from CO (2-1) (Salome 06) • M(4.0,0.6 keV)~(1011,109 M) (Chandra, Fabian 06) • M(warm H2)>7107 M(Johnstone 07) • M(H II)= 3107 M(Conselice 01)

  11. 1000 km/s H I and [O II] outflows (Morganti 03; Emonts 05). • Possible jet/CO interaction. • M(H2 cold)=1.51010 M (A. Evans et al. 1999) • M(H2 warm)=1109 M (Ogle 2008) 3C 293 Jet-Induced Outflow . M(HI)=20 M/yr M(HI)=107 M Mion=0.1 M/yr .

  12. 3C 31 Rogues Gallery 3C 315 3C 310 3C 436 3C 326 3C 386 3C 433 3C 338 3C Credit: DRAGN Atlas

  13. Star Formation Rates • MOHEG star formation rates are modest: 0.01-3 M/yr (from PAH inside 3.7” slit) Will add little to ~ 1011M stellar bulge in a Hubble time. • SFR does not correlate with warm H2 mass. • H2 depletion timescales: 3107--71010 yr Ogle et al. 2008

  14. Star Formation Efficiency • 3C 326 and 293 fall below Schmidt law for star formation in normal galaxies. • 3C 326 SFR~0.1M/yr at R<3.1 kpc. Our PdB CO observations indicate (H2)>350 M/pc2 • Jets may suppress disk formation by driving H2 outflows or fountains with large velocity dispersion and low volume filling factors. 293 ? PdB 326 Kennicutt 1998

  15. Future Directions COMING SOON: • Spitzer IRS spectra of more radio galaxies with H I outflows. • Spitzer spectra of compact (CSS/GPS) radio sources • Spitzer spectral map of MRC 1138 (z=2) radio galaxy. • VLT/SINFONI IFU spectral maps of near-IR rovibrational H2 • CO maps and cold H2 masses, ’s with PdB interferometer. ALSO NEEDED: • More AGN X-ray fluxes (Chandra) • Jet power estimates for non-cavity radio sources. • THEORY! How do jets gently heat 1109 M of H2 to 200 K??

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