Metallicity and Black Hole Masses of Redshift 6 Quasars

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Metallicity and Black Hole Masses of Redshift 6
Quasars
In the Universe at z gt 6
In the Universe at z gt 6.0 ? 0.5

• Jaron Kurk (MPIA, D)

Fabian Walter, Dominik Riechers (MPIA, D) Laura
Pentericci (Monte Porzio, I) Xiaohui Fan
(Steward, AZ)
The evening star (Mucha, 1902)
The moon (Mucha, 1902)
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Introduction

• QSOs are most luminous objects known close to
  reionization epoch
• Once thought to be possible sources of
  reionization
• Size of HII 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

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Introduction
J10300524 z 6.3 J13060356 z 6.0 (Pentericci
et al. 2002)
J11485251 z 6.4 (Barth et al. 2003)
J08360054 z 5.8 J10300524 z 6.3 J1044--0125
z 5.8 (Freudling et al. 2003)
J11485251 z 6.4 (Willott et al. 2003)
J10300524 z 6.3 J1044--0125 z 5.8 J10484637
z 6.2 J11485251 z 6.4 J13060356 z
6.0 (Maiolino et al. 2004)
Fig. by G. Djorgovski et al.
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Introduction
J0005--0006 z 5.9 J08360054 z 5.8 J10300524
z 6.3 J13060356 z 6.0 J14111217 z
6.0 (Kurk et al., in prep.)
Large(r) sample with higher S/N and coverage of
both CIV and MgII
Fig. by G. Djorgovski et al.
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NIR spectroscopy

• Sample of five QSOs at z gt 5.8 observable with
  VLT
• ISAAC MR spectroscopy in SZ, J, and K bands
• Texp 3 hours per object per band

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Spectroscopy of emission lines

• From spectroscopy of 1400 lt ? lt 3600 Å, one can
  derive
• metallicy from FeII / MgII 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

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Long spectrum (hidden title)
K
z
SZ
Fan et al.
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Mean SDSS QSO Spectrum
Vanden Berk et al. (2001)
PL-slope ?? --1.56
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SDSS Iron Template (hidden title)
SDSS FeII template
Balmer continuum
Power-law continuum
Vanden Berk et al. (2001)
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Vestergaard Wilkes FeII template
Sigut Pradhan (2003)

• FeII emission under MgII line

Vestergaard Wilkes (2001)
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FeII template Comparison
MgII line
Smoothed Vestergaard template
Mean SDSS QSO template
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MgII spectra

• ISAAC MR K-band

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MgII spectra

• SDSS FeII template
• Simultaneous fit of power-law continuum, Balmer
  pseudo-continuum and template

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MgII spectra

• Vestergaard template
• Simultaneous fit of power-law continuum, Balmer
  pseudo-continuum and template

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MgII spectra

• MgII line fit
• After subtraction of continua and template

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CIV spectra

• SZ and J band spectra

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CIV spectra
SZ and J band spectra Lorentzian curves fitted
with underlying polynomial
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Long spec again (hidden title)
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Long spec with fit (hidden title)
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Redshifts

• CIV emission 0 lt ?v lt 4000 km s-1 blueward of
  MgII
• MgII and Ly? can differ by ?z 0.02
• New redshift accuracy on the order of ?z 0.002

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Black Holes Masses

• MgII
• McLure Jarvis (2002)
• CIV
• Vestergaard (2002)
• Edd
• Wandel, Peterson Malkan (1999)

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Black Holes Masses
Black hole masses in 109 M?
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FeII/MgII ratios

• 2.2 lt FeII/MgII lt 4.7, consistent with solar
  metallicity

?? Dietrich et al. (2003) ? Wills, Netzer,
Wills (1985) ? Thompson et al. (1999) ??
Iwamuro et al. (2002) ? Freudling et al.
(2003)
Dietrich et al. (2003)
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Conclusions

• Black Hole masses from 0.2 to 1.6 109 M?
• not only the most massive galaxies
• therefore MBH-?BULGE relation can hold up to the
  highest redshifts
• No evolution in FeII/MgII ratios up to z 6
• star formed at z gt 10
• or indication for decline?
• BH masses differ much more than enrichment
• Accurate redshifts for follow-up and better HII
  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)