Metallicity and Black Hole Masses of Redshift 6 Quasars Jaron Kurk (MPIA, D) The evening star (Mucha, 1902) The moon (Mucha, 1902) Fabian Walter, Dominik Riechers (MPIA, D) Laura Pentericci (Monte Porzio, I) Xiaohui Fan (Steward, AZ) In the Universe at z > 6.0  0.5 In the Universe at z > 6

Introduction QSOs are most luminous objects known close to reionization epoch Once thought to be possible sources of reionization Size of H II spheres are probes of ionization state Driven by massive black holes, hosted by the (progenitors) of massive galaxies and therefore within massive dark matter halos NIR spectroscopy to study –BH masses –enrichment –more accurate redshifts

Introduction J z = 6.4 (Barth et al. 2003) J z = 5.8 J z = 6.3 J z = 5.8 (Freudling et al. 2003) Fig. by G. Djorgovski et al. J z = 6.3 J z = 5.8 J z = 6.2 J z = 6.4 J z = 6.0 (Maiolino et al. 2004) J z = 6.3 J z = 6.0 (Pentericci et al. 2002) J z = 6.4 (Willott et al. 2003)

Introduction Fig. by G. Djorgovski et al. J z = 5.9 J z = 5.8 J z = 6.3 J z = 6.0 J z = 6.0 (Kurk et al., in prep.) Large(r) sample with higher S/N and coverage of both C IV and Mg II

NIR spectroscopy Sample of five QSOs at z > 5.8 observable with VLT ISAAC MR spectroscopy in SZ, J, and K bands T exp ~ 3 hours per object per band QSOz*zReference J Fan et al. (2001) J Fan et al. (2001) J Fan et al. (2004) J Fan et al. (2001) J Fan et al. (2004)

Spectroscopy of emission lines From spectroscopy of 1400 < < 3600 Å, one can derive –metallicy from Fe II / Mg II ratios, but not trivial –independent measurements of BH mass –accurate redshift for molecular line follow-up –power-law slope of continuum –absorption by intervening or co-spatial gas

Long spectrum (hidden title) Kz’SZ Fan et al.

Mean SDSS QSO Spectrum Vanden Berk et al. (2001) PL-slope  = z = _

SDSS Iron Template (hidden title) Vanden Berk et al. (2001) Power-law continuum Balmer continuum SDSS “Fe II ” template

Vestergaard & Wilkes Fe II template FeII emission under MgII line Sigut & Pradhan (2003) Vestergaard & Wilkes (2001)

Smoothed Vestergaard template Mean SDSS QSO template Mg II line Fe II template Comparison

ISAAC MR K-band Mg II spectra

SDSS “FeII” template Simultaneous fit of power-law continuum, Balmer pseudo- continuum and template Mg II spectra

Vestergaard template Simultaneous fit of power-law continuum, Balmer pseudo- continuum and template Mg II spectra

Mg II line fit After subtraction of continua and template Mg II spectra

C IV spectra SZ and J band spectra

C IV spectra SZ and J band spectra Lorentzian curves fitted with underlying polynomial

Long spec again (hidden title)

Long spec with fit (hidden title)

Redshifts C IV emission 0 <  v < 4000 km s -1 blueward of Mg II Mg II and Ly  can differ by  z = 0.02 New redshift accuracy on the order of  z ~ QSOz REF z Mg II z FE II z C IV J J J J J

Black Holes Masses Mg II McLure & Jarvis (2002) C IV Vestergaard (2002) Edd Wandel, Peterson & Malkan (1999)

Black Holes Masses QSOz REF M BH,Mg II M BH,C IV M BH,Edd J J J J J Black hole masses in 10 9 M 

Fe II/ Mg II ratios 2.2 < Fe II /Mg II < 4.7, consistent with solar metallicity Dietrich et al. (2003)  Dietrich et al. (2003)  Wills, Netzer, & Wills (1985)  Thompson et al. (1999)   Iwamuro et al. (2002)  Freudling et al. (2003)

Conclusions Black Hole masses from 0.2 to M  –not only the most massive galaxies –therefore M BH -  BULGE relation can hold up to the highest redshifts No evolution in FeII/MgII ratios up to z = 6 –star formed at z > 10 –or indication for decline? BH masses differ much more than enrichment Accurate redshifts for follow-up and better H II region determination Not mentioned: power-law slopes, absorption by intervening gas and/or gas within the system The morning star (Mucha, 1902) The pole star (Mucha, 1902)