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 0.5In the Universe at z > 6

Introduction

J1148+5251 z = 6.4(Barth et al. 2003)J0836+0054 z = 5.8J1030+0524 z = 6.3J1044--0125 z = 5.8(Freudling et al. 2003)

Fig. by G. Djorgovski et al.

J1030+0524 z = 6.3J1044--0125 z = 5.8J1048+4637 z = 6.2J1148+5251 z = 6.4J1306+0356 z = 6.0(Maiolino et al. 2004)

J1030+0524 z = 6.3J1306+0356 z = 6.0(Pentericci et al. 2002)

J1148+5251 z = 6.4(Willott et al. 2003)

Introduction

Fig. by G. Djorgovski et al.

J0005--0006 z = 5.9J0836+0054 z = 5.8J1030+0524 z = 6.3J1306+0356 z = 6.0J1411+1217 z = 6.0(Kurk et al., in prep.)

Large(r) sample with higher S/N and coverage of both CIV and MgII

NIR spectroscopy

• Sample of five QSOs at z > 5.8 observable with VLT

• ISAAC MR spectroscopy in SZ, J, and K bands

• Texp ~ 3 hours per object per bandQSO z* z Reference

J0836+0054

18.74 5.82 Fan et al.

(2001)J1306+03

5619.47 5.99 Fan et al.

(2001)J1411+12

1719.64 5.95 Fan et al.

(2004)J1030+05

2420.05 6.28 Fan et al.

(2001)J0005-0006

20.54 5.85 Fan et al.

(2004)

Long spectrum (hidden title)

Kz’ SZ

Fan et al.

Mean SDSS QSO SpectrumVanden Berk et al. (2001)

PL-slope = --1.56

z = 1.253_

SDSS Iron Template (hidden title)

Vanden Berk et al. (2001)

Power-law continuum

Balmer continuum

SDSS “FeII” template

Vestergaard & Wilkes FeII template

FeII emission under MgII line

Sigut & Pradhan (2003)

Vestergaard & Wilkes (2001)

Smoothed Vestergaard templateMean SDSS QSO template

MgII line

FeII template Comparison

ISAAC MR K-band

MgII spectra

SDSS “FeII” template

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

MgII spectra

Vestergaard template

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

MgII spectra

MgII line fit

After subtraction of continua and template

MgII spectra

CIV spectra

SZ and J band spectra

CIV spectra

SZ and J band spectra

Lorentzian curves fitted with underlying polynomial

Long spec again (hidden title)

Long spec with fit (hidden title)

Redshifts• CIV emission 0 < v < 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

QSO zREF zMgII zFEII zCIV

J0836+0054 5.82 5.80

75.807

J1306+0356 5.99 6.01

56.030

6.007

J1411+1217 5.95 5.89

85.936

5.815

J1030+0524 6.28 6.30

06.315

6.282

J0005-0006 5.85 5.84

25.856

5.861

Black Holes Masses

• MgIIMcLure & Jarvis (2002)

• CIVVestergaard (2002)

• EddWandel, Peterson & Malkan (1999)

Black Holes Masses

QSO zREF MBH,MgII MBH,CIV MBH,Edd

J0836+0054

5.82 1.2 6.5

J1306+0356

5.99 1.1 1.6 2.0

J1411+1217

5.95 0.3 0.2 1.5

J1030+0524

6.28 0.7 1.3 1.9

J0005-0006

5.85 0.2 0.3 0.7

Black hole masses in 109 M

FeII/MgII ratios2.2 < FeII/MgII < 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 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 > 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)