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Dense Outflows in the type II quasar SDSS 1324+0537

Tinggui Wang( 王挺贵 ), Hongyan Zhou, Honglin Lu CfA, University of Science and Technology of China Hongguan Shan, Weimin Yuan Yunnan Observatory. Dense Outflows in the type II quasar SDSS 1324+0537. Motivation.

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Dense Outflows in the type II quasar SDSS 1324+0537

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  1. Tinggui Wang(王挺贵), Hongyan Zhou, Honglin Lu CfA, University of Science and Technology of China Hongguan Shan, Weimin Yuan Yunnan Observatory Dense Outflows in the type II quasar SDSS 1324+0537

  2. Motivation • Massive outflows in AGN and starburst are ubiquitous,but physical properties of these outflows are not well understood. (Shapley et al. 2003, Heckman et al. 2002 ,Rupke et al. 2005; Lipari et al. 2005; Crenshaw et al. 2004, Whittle et al. 2005) Starburst+AGN composite? • Growth of black hole and star-formation, coeval or lag? (Heckman et al. 2004; Ho et al. 2005; Zhou, Wang, and Dong et al. 2005; Zhou, Wang, Yuan et al. 2006, also Yuan et al. this conference)

  3. IRAS 1321+0552 Misclassified as Seyfert 1(e.g., Remillard et al. 1993, Zheng et al. 2002, Kuraszkiewicz et al. 2004;Veilleux et al. 2006),but is actually a type II quasar(Lipari et al. 2003). Identified incorrectly as counterparts to HEAO-A2 and Bepposax sources, but actually X-ray dummy (not detected in 16ks XMM observation, Bianchi et al 2005), Compton-thick? Ultra-luminous infrared (>1012 L⊙), with elliptical host (e.g.,Veilleux et al. 2006), late stage merging system

  4. HST FOS Main data used in this work SDSS

  5. Stellar continuum UV continuum is modeled with a reddened single stellar population (Starburst99;Vazquez & Leitherer 2005). Reddening curves: Calzetti et al (2002) and SMC-type Optical continuum is initially modeled with reddened IC templates (Lu et al. 2006) in continuum-subtraction for measurements of emission line parameters, laterwith SSPs (Bruzual & Charlot 2003) to get stellar population.

  6. A single young stellar population with either SMC and Calzetti-type reddening can reproduce the UV continuum, but with very different stellar mass: Age: ~1 Myr Calzetti: E(B-V)=0.66; M*=1.1 1010M⊙ SMC: E(B-V)=0.26; M*=4.5 108 M⊙ With optical spectrum, SMC-like reddening is preferred with an additional stellar population: Calzetti: E(B-V)=0.39, age of 0.51 Gyr M*=5.8 1010M⊙ SMC: E(B-V)=0.38, age of 0.8Gyr M*=5.1 1010M⊙ Calzetti’s SMC

  7. Emission lines 4 components: C1: narrow (160km/s) component at the systematic velocity(-90km/s) Hα, Hβ, Hγ, [OIII],[OII],[NII],[SII],[OI] C2: narrow (σ=180km/s) component blueshifted by ~-500 km/s strong: Hα, Hβ, Hγ, [OIII], weak: [OII],[NII],[SII],[OI] C3: broad (940km/s) component with blueshift (-430km/s) [OIII], Hα, Hβ, Hγ, CIII],SiIII],AlIII,[NeIII] C4: broad (750km/s) component with larger blueshift (-1910km/s). [OIII], Hα, Hβ, Hγ, CIV,CIII],SiIII],AlIII,NIII,NIV, [NeIII]

  8. On BPT diagram, C1:LINER C2:H II C2 component has a large Balmer decrement heavily reddened

  9. Comparison with grid photo-ionization models Model parameters: ionizing continuum: Typical AGN Density: 102-10 cm-3 Column density: (1,3,10) x 1022 cm-2 Ionization parameters: logU~(-3.5,0.5) Metal abundance: 1.0 Z⊙, 5.0Z⊙ CLOUDY

  10. C1: low density gas <100 cm-3, [SII]6716/6731~1.5 and [OII]3729/3726~1.4 C3: SiIII]/CIII]  n>109.5 cm-3 , but [OIII]4363/5007 n~107cm-3. multiple-phase? CIII]/CIVlow ionization, logU~-3.0 C4: high density, multiple-density, moderate ionization, nitrogen-enhanced?, Z=5Z⊙ 1022.5cm-2

  11. SFR and black hole growth SFR: UV, SMC-dust 450 M⊙ yr-1 LFIR  300 M⊙ yr-1 LHα,C2  10 M⊙ yr-1 L[OII], C20.4 M⊙ yr-1 extinction-corrected (Hα/Hβ~15), all consistency Lmir~2x1046 erg/s  =3-10 M⊙ yr-1 If emitting at Eddington luminosity,  MBH=108M⊙ MBH/M*~0.2% Q composite reddened by E(B-V)=4.5 Richards et al. composite NGC 6240

  12. Summary We identify two dense outflow components in the emission lines of the type-II QSO with the outflow velocities of -400 and -1900 km/s, and the density is as high as in BLR. Both starburst and nucleus continuum are heavily obscured, but the outflow components are not. dense outflows beyond the torus scale? Extinction correction is extremely important to the estimate of SFR in the quasar host; or star formation region in the quasar is dusty. Thank you!

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