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Spectroscopy of HSC-detected QSOs at z~7.10 and z~6.300: Using PFS for AGN science

This request is for the operation of the Prime Focus Spectrograph (PFS) in order to conduct spectroscopy of high-redshift quasars (QSOs) detected by the Hyper Suprime-Cam (HSC). The goal is to study the physics of the most distant and brightest QSOs, as well as investigate the ionization of the intergalactic medium (IGM). The request includes the use of extra fibers in other galaxy surveys. PFS is crucial for this research and its high sensitivity at wavelengths above 9000A is advantageous. The request also suggests two possible scenarios for PFS operation, either soon after the HSC survey or more than three years later.

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Spectroscopy of HSC-detected QSOs at z~7.10 and z~6.300: Using PFS for AGN science

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  1. Requests for PFS- as an AGN researcher- Masa Imanishi NAOJ/Subaru Telescope With help from SWANS team

  2. AGN science using PFS：Spectroscopy of HSC-detected QSOs ・ z~7 10 （1000 deg2)（candidates = X a few ?） Use extra several fibers in other galaxy surveys but see my remark later ・ z~6 300 （1000 deg2）（candidates = X a few ?） Use extra several fibers in other galaxy surveys ・z=3-5 10-1000（1 deg2）（candidates = X <a few ?） PFS very important

  3. Most distant, bright QSOs Constraints on SMBH formation theory z=25 : 100Mo BH Eddington growth z=6.5 :109 Mo z=7.5 : 108 Mo 1. z~7 QSO science Currently, most distant QSO : z~6.4 Study the physics (including neutral fraction) of more distant IGM with high S/N

  4. HSC z,y filters 8000A g r i z y 10000A Up to z~7.3 QSO High-z = Longer λ Fan+06 8000A 9000A

  5. High-z QSOand brown dwarf (BD) Gradually increase flux Galactic BD wavelength flux Sharp gap High-z QSO wavelength

  6. z~7 QSO g y r z i z-y BD Assumption y-J HSC wide survey (i,z,y) = (20m, 20m, 20m) = (26.0, 24.9, 23.8) AB z~7 QSO (z-dropout,y-detected) z-y>2-2.3 selection（remove BD） In VIKING field (J=22.2)AB, z-y>1.5-1.7, y-J<1 Kashikawa10

  7. z~7 QSO QSO number decreases with high-z QSO number density ∝ 10-0.47(z-6) Willott+10 z=6→7 : ~1/3 Richards+06

  8. Selectable z~7 QSO: 7/1000 deg2 12（VIKING） （conservative） g y r z i HSC/wide（z~7） Jiang+09 Lim-mag: (z,y) = (24.9, 23.8) AB M1450A faint bright z~7 QSO Number of faint QSOs : Smaller than previously expected z~7 QSOs included in y-band : ~35/1000deg2 Selection z-y>1.5

  9. At least cover Lyα : 9000 - 10500A High sensitivity required SMBH mass MOIRCS IGM physics TMT PFS（z~7 QSO） Follow-up spectroscopy of HSC z~7 QSO candidates Several 10s candidates/1000 deg2 Use extra several fibers in other galaxy surveys

  10. 4 5 6 2. z~6 QSO science Many faint z~6 QSO z~6 IGM study in many sightlines (neutral fraction increases?) Fan+06

  11. g y r z i HSC/wide（z~6） Jiang+09 M1450A faint bright 2. z~6 QSO (i-dropout, z-detected) i-z red（>1.8）：by IGM absorption z-y blue（<0.5）：BD removal 350/1000 deg2 （conservative） Selection : i=26.0,z=24.2, y=23.8 (AB)

  12. At least cover Lyα : 8000 – 9000A High sensitivity required z~6 IGM multiple sightlines TMT PFS（z~6 QSO） Follow-up spectroscopy of HSC z~6 QSO candidates 1000 candidates/1000 deg2（1/deg2） Use extra several fibers in other galaxy survey

  13. log MDH/Msun=12.5 7 7 QSO-QSO、QSO-galaxy correlation（bias） tQ=3x108 yr 12.0 6 6 f f e b beff QSO lifetime 5 5 Halo mass tQ=3x107 yr 11.5 4 4 Enoki et al. (2003) 3 3 . 5 4 4 . 5 5 z z 3. z=3-5 QSO science Faint, numerous z=3-5 QSOs LF faint end Origin of ionizing UV background

  14. g y r z i QSO QSO i’ — z’ r’ — i’ g’ — r’ r’ — i’ Richards et al. (2001) 3. z~3-5 QSO (g,r,i-selection) riz : z=4.6-5.1 gri : z=3.6-4.4 i - z r - i g - r r - i

  15. Casey+08 z=3-5.5 100/deg2 PLE LDDE number 18 i=24 PFS（z=3-5 QSO） Follow-up spectroscopy of HSC z=3-5 QSO candidates 10-1000/deg2 PFS very important Cover Lyα,CIV(1549A) 6000 - 9500A LF、two-point spatial correlation: Completely solved with HSC+PFS！

  16. Summary ・ z~7 10 （1000 deg2) (a few times candidates?） 9000-10500A Use extra several fibers in other galaxy surveys High-sensitivity but see my remark later ・ z~6 300 （1000 deg2）（a few times candidates?） 8000-9000A Use extra several fibers in other galaxy surveys High-sensitivity ・z=3-5 10-1000（1 deg2）（<a few times candidates?） 4500-9500A PFS very important

  17. ・ z>6 QSOs : number density too small High sensitivity spectrograph at 9000-10500A better (FOCAS、MOIRCS） PFS operation (personal opinion) ・ Red-optimized (>6000A) PFS is powerful to z=3-5 QSOs Can be done with PFS, if high sensitivity at 9000-10500A ?

  18. Request for PFS operation （case 1） PFS : soon after HSC survey If Subaru open use is dominated by PFS SSP, z>6 QSO spectroscopy will not proceed, and interesting results may be robbed by other telescopes. SSP must be <25％ of Subaru open use

  19. PFS survey （several 100 deg^2）of y-detected, z-undetected (but z-y<1.5) sources may increase the number of z ~7 QSO SSP can be >25％ of Subaru open use Request for PFS operation （case 2） PFS : >3 yr after HSC survey HSC-selectable z~7 QSO : ~10 / 1000deg2 z~7 QSOs included in HSC-y-band : ~35 / 1000deg2

  20. Request for PFS specification High sensitivity at >9000A is an advantage of Subaru (because of Hamamatsu CCD) Powerful to spectroscopy of z>6 QSO In any case, PFS should have high sensitivity at 9000-10500A

  21. End

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