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High-z (z > 3) QSOs studied with Subaru/HSC

Learn about high-z QSOs and their significance, explore QSOs at z>7 and low-luminosity QSOs at z=3-6. Understand the co-evolution of supermassive black holes (SMBHs) and galaxies. Discover research on SMBHs in spheroid galaxies and the impact of high-z QSOs on re-ionization. Find insights on QSO detection, survey strategies, and the link between QSO activity and galaxy evolution.

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High-z (z > 3) QSOs studied with Subaru/HSC

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  1. High-z (z > 3) QSOs studied with Subaru/HSC Masa Imanishi (NAOJ) Tohru Nagao (NAOJ)

  2. Outline • Importance and current understanding • of high-z QSOs (AGNs) 2. QSOs at z > 7 (M.Imanishi) (Subaru/HSC + UKIRT/WFCAM) 3. Low-luminosity QSOs at z = 3-6 (Subaru/HSC) (T.Nagao)

  3. (2) Co-Evolution of SMBHs and Galaxies M(BH) SMBHs are ubiquitous in spheroid galaxies M(gal) Why High-z QSOs(AGNs) ? (1) Very bright MBH =106-9Msun DLA, LyA forest IGM properties (re-ionization)

  4. High-z QSO found by SDSS >1000 QSOs at z>3 1um @z~7 Bright QSOs only ! z>7 QSO not detectable in the optical z=6.42: Most distant Fan 2006

  5. Post SDSS QSO Survey What next? (1) Search for z > 7 QSOs NIR data required (UKIRT/WFCAM) (2) Search for lower-Luminosity QSOs at z = 3-6

  6. Very deep Moderately deep H K J Z Y 1. z>7 QSOs filters optical NIR

  7. Y=20.5,J=20.0, H=18.8,K=18.4 UKIRT/WFCAM/LAS z>7 QSOs: ~10 expected Northern: 1907.6 deg^2 Equatorial: 1907.6 deg^2

  8. No deepz-bandimage: z>7 QSO candidates cannot be selected z’ - J z’ - J z>7 QSO: z– NIR = very large SDSS + >2 mag needed J - K J - K

  9. Y-band WFCAM team compromise Green：QSO Y z i Red：BD J i’ - Y Y-J color difference (small) Severe contamination i ,Y: limiting mag differs only 2mag Y - J

  10. The planned Subaru/HSC >1000 deg 2 survey be executed at (northern) WFCAM/LAS DEC RA RA widely distributed Proposal >1000 deg 2(wide),z>23.5mag (deep) survey Possible only with Subaru/HSC

  11. Why Japan? Deep, wide z-band survey only possible with HSC Southern VISTA : Z<21.5 （?） At z~7, z-ID requires 0.9-1.5um spectroscopy Subaru/MOIRCS can Japan can lead this area, if we do follow-up before HSC data become archival !

  12. Z-band (um) 0.8 1 SDSS z Issues to be solved SDSS z or Z Y dwarf

  13. ２ｄＦ z<2.3 Croom et al. (2001) faint bright SDSS z>3.6 QSO UV background: dominated by faint end bright Fan et al. (2001) 2. low-luminosity QSOs (z=3-6) QSO LF: bright end only at z>3

  14. QSO (Mathews & Ferland 1989) Starburst, Z=0.05 Zsolar Starburst, Z=1.00 Zsolar (Leitherer et al. 1999) HeII re-ionization 54.4eV Effect on galaxy formation 24.6eV 13.6eV UV Background from QSOs at z=3-6 QSO UV is hard QSOs Stars Energy (Rydberg)

  15. z > 3:unknown log MDH/Msun=12.5 108yr z < 3 bias 7 7 12.0 Croom et al. (2005) 6 6 f f e b 107yr 5 5 bias 11.5 4 4 2 0 1 3 3 3 . 5 4 4 . 5 5 Redshift z Redshift Enoki et al. (2003) QSO Correlation Func. Faint, numerous QSOs Corr.Func.  bias  M(halo)  QSO lifetime

  16. Strategy Moderately Deep and Moderately Wide QSO Surveys SDSS ~ too shallow… Deep Surveys (UDF, SDF) ~ too narrow…

  17. Selection in Color-Color Diagram g’r’i’  3.6 < z < 4.4 r’i’z’  4.6 < z < 5.1 i’ — z’ r’ — i’ g’ — r’ r’ — i’ Richards et al. (2001) Survey Strategy Multi-band Selection g u r i z 3000 Wavelength(A) 10000

  18. g’ r’ i’ z’ 26.6mag (23.3) 26.2mag (23.1) 25.5mag (22.3) 24.4mag (20.8) 20min/band/FOV (5σ, 0.7”seeing, 2”φ) 100 QSOs ~ 140 sq.deg. ~ 100 FOV ~ 400 pointing ~ 2 weeks Multi-band HSC Survey HSC • g’ r’ i’ z’ (3mag deeper than SDSS)

  19. Summary 1. QSOs at z > 7 (Subaru/HSC + UKIRT/WFCAM) 2. Low-luminosity QSOs at z = 3-6 (Subaru/HSC)

  20. End

  21. QSO Environment QSO Activity  Interaction Borne et al. (2000) Blank-field QSOs excess Bright galaxy number excess around QSOs Results at z=0.2(McLure & Dunlop 2001)

  22. Strategy Trigger of QSO Activity Growth of SMBHs in QSOs Relation with Galaxy Evolution SDSS ~ too shallow… Deep Surveys (UDF, SDF) ~ too narrow… Luminosity Function of QSOs Correlation Function of QSOs Environments of QSOs Moderately Deep and Moderately Wide QSO Surveys We need a QSO sample ~ with wide luminosity range ~ with enough number density

  23. log MDH/Msun=12.5 7 7 tQ=3x108 yr 12.0 6 6 f f e b 5 5 tQ=3x107 yr 11.5 4 4 3 3 . 5 4 4 . 5 5 Enoki et al. (2003) z QSO Correlation Func. Croom et al. (2005) ～ Corr.Func.  bias  Mhalo ～ bias  QSO Lifetime — mass-accretion timescale Redshift

  24. Marconi & Hunt (2004) Ferrarese & Meritt (2000) MBH [Msun] log MBH [Msun] MBH/Mgal～0.002 Non-AGNs stellar velocity dispersion log Mgal [Msun] Co-Evolution of SMBHs and Galaxies ～ Evolutionary link between SMBHs and galaxies ～ Every galaxies may once experienced an AGN phase

  25. Richards et al. (2006) SDSS QSO Survey: Redshift Distribution Schneider et al. (2005) u’-dropout g’-dropout 46420 QSOs in SDSS DR3 0 1 2 3 4 5 Redshift

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