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COSMIC DOWNSIZING and AGN METALLICITY at HIGH REDSHIFT

COSMIC DOWNSIZING and AGN METALLICITY at HIGH REDSHIFT. Roberto Maiolino INAF - Oss. Arcetri & Oss. Roma Tohru Nagao INAF - Oss. Arcetri & NAOJ Alessandro Marconi INAF - Oss. Arcetri. Mass-Metallicity relation in galaxies at z=0. Tremonti et al. 2004. QSOs. QSOs.

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COSMIC DOWNSIZING and AGN METALLICITY at HIGH REDSHIFT

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  1. COSMIC DOWNSIZING and AGN METALLICITY at HIGH REDSHIFT Roberto Maiolino INAF - Oss. Arcetri & Oss. Roma Tohru Nagao INAF - Oss. Arcetri & NAOJ Alessandro Marconi INAF - Oss. Arcetri

  2. Mass-Metallicity relation in galaxies at z=0 Tremonti et al. 2004

  3. QSOs QSOs Chemical version of the cosmic downsizing (anti-hierarchical growth) Evolution of the Mass-Metallicity relation: massive galaxies chemically evolve rapidly at high-z 12 11 z=0 1 10 3 5 9 lg M* = 8 (Kobulnicky et al. 2003, Shapley et al. 2005, Savaglio et al. 2005, Maiolino et al. 2006)

  4. The metallicity of the Broad Line Region at 2<z<4.5 ~ 5000 QSO optical spectra (UV-rest) from SDSS DR2 Sample large enough to disentagle the dependence on redshift and on luminosity 22 high quality composite spectra in bins of redshift and luminosity Lya NV CIV SiII OIV] SiIV CIII] HeII NIV] SiIII] OIII] AlII AlIII OI+SiII “1600A bump” CII NIV+AlII+NIII+Fe fit residuals Nagao, Marconi & Maiolino 2006

  5. Photoionization models: • Cloudy • Integration over different • distributions (in r and n) • of gas clouds • Spanning various gas • metallicities (abundances • prop. to solar, except for N) Accurate fluxes for 15 emission lines matching flux ratios (+ constraints from EW) Hagai (!) “best” metallicity for each [z,L] bin Nagao et al. 2006

  6. Metallicity of the BLR at 2<z<4.5 Average trends • Significant dependence • on Luminosity Consequence of the mass-metallicity relation Z  M* MBH LQSO ...but also dependence on accretion rate (Shemmer et al. 2004) • No evolution with redshift

  7. No metallicity evolution even in the most distant QSOs at 4.5<z<6.4 (close to re-ionization) From near-IR spectra (=UV rest-frame) of 20 QSO J1148+52 z=6.4

  8. QSOs probe the most extreme cases of anti-hierarchical growth: their host galaxies are fully evolved, from the chemicalpoint of view, already at very high redshift QSOs QSOs 12 11 z=0 1 10 3 5 9 lg M* = 8

  9. Large number of emission lines: possible to contrain abundances patterns Best matches with abundances at/after the wind QSOs best fit Selection effects associated with QSO-galaxy coevolution Passive evolution + Unobscured QSO Star formation + Obscured AGN           wind Pipino & Matteucci 2004 Granato et al. 2004

  10. Use Narrow Lines in obscured AGNs The Broad Lines sample only a tiny, nuclear region ... not representative of the host galaxy?

  11. NLR evolution at 1.2<z<3.8 - 51 optical spectra (UV-rest) of high redshift narrow line radio galaxies (HzRG) - 10 optical spectra (UV-rest) of high redshfit X-ray selected QSO2 in the Chandra Deep Field South CIV/HeII vs. CIII]/CIV diagram: - sensitive to metallicity - removes degeneracy from U - possible to control effects of shocks and dust Nagao, Maiolino & Marconi 2006

  12. NLR evolution at 1.2<z<3.8 3 CIV / HeII (local) 1 No evolution with redshift among HzRG at 1.2<z<3.8 0.5 3 Dependence on Luminosity CIV / HeII (local) 1 0.5 0.3 1 CIII] / CIV

  13. At z>4 little information on NLR metallicity ...but information on gas in host galaxy for some QSOs J1148+52 z=6.4 same [CII]/FIR as loc. ULIRGs same [CII]/CO as loc. ULIRGs • strong enrichment of carbon in the host already at z=6.4

  14. CONCLUSIONS Luminosity-Metallicity relation: consequence of Mass-Metallicity relation in galaxies BLR & NLR No metallicity evolution with redshift: QSO are extreme cases of the cosmic downsizing (in its chemical version) Abundance patterns matching expectations of AGN-galaxy joint evolutionary models

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