Tomo GOTO z>7 QSOs and QSOs and 1.25<z<1.75 galaxy cluster search with the HyperSprimeCam(HSC)and WFMOS Tomo GOTO (IfA, Univ. of Hawaii/NAOJ) new z~6 QSOnew galaxy cluster Goto T., 2006, MNRAS,371,769 Goto et al.2002, AJ, 123, 1801 Goto, 2005,MNRAS, 359,1415 Masamune Oguri(Stanford) The SWANS team

Tomo GOTO Why z>7 QSOs are important?

Tomo GOTO Why z>7 QSOs are important? 1.QSO/AGN evolution (LF/number evolution, why metallicity so high?) (LF/number evolution, why metallicity so high?) 2.Formation of super massive black holes (Can a black hole of billion Msun be formed in 1 Gyr?) 3.Direct probe of re-ionization of the Universe

Tomo GOTO Reionization of the Universe (Jelle Ritzerveld & Rien van de Weijgaert & Vincent Icke)Jelle RitzerveldRien van de WeijgaertVincent Icke When and how our Universe reionized? One of the outstanding questions on observational cosmology.

Tomo GOTO Reionization through QSO Ionized bubbles Galaxy continuum is too faint. LF is indirect, depends on evolution, dust, model…etc. GRBs disappear too quickly. Neutral Hydrogen

Tomo GOTO Current status of high-z QSO surveys

Tomo GOTO High-z QSO surveys in the past ←Complete Gunn-Peterson trough ←Remaining flux(White et al. 2003,AJ,126,1) →Reionization depends line-of- sight The resolution of these questions will have to wait for the discovery of additional z>6 quasars. (Richard L. White) ｚ =6.28 z=6.28 z=6.42

Tomo GOTO Japan/Subaru has been contributing: A new QSO at z=5.96 M AB,1450 = −26.9 (H 0 = 50 km s 1 Mpc 1, q 0 = 0.5). Lyα + N v 、 Lyβ + O vi→z=5.96 Goto T., 2006, MNRAS,371,769

Tomo GOTO Japan/Subaru has been contributing: z=6.06 (Goto in prep.)

Tomo GOTO Japan/Subaru has been contributing: Lyα at 9246 Å → most distant QSO at z=6.6? No questions on this slide please (not published yet).

Tomo GOTO How do we make progress?

Tomo GOTO →How do we find such QSOs ？ We need to go redder, wider and deeper. →perfect for the HSC/WFMOS 1.z=6.4 is the limit of optical surveys  near IR large survey for z>7.  HSC y-band 2. Deeper survey for fainter QSO -spatial dependence of reionization, -break of the LF, QSO evolution -contribution to the reionization Limitations of the current surveys:

Tomo GOTO z=6.4 is the limit of optical surveys Redder: HSC Y-band can find 6.8<z<7.8 QSOs opticalnear infrared

Tomo GOTO Wider & Deeper QSO density is very small. Only 20 z=6 QSOs in 6000sq.deg → We need to go wide. QSO LF is very steep. → We need to go deep. 8x10 2x10 7x10 HSC/WFMOS can do both!

Tomo GOTO z=7 QSO selection ：ｚ－ y-J © Asami QSO z ～ 6 QSO selection : i-z-y Method: 1.color selection(HSC) 2.id spectroscopy(WFMOS)

Tomo GOTO Expected results

Tomo GOTO 5.8<z<6.4 Based on the wide survey depth: I=25.8(15min), z=24.9AB(20min), Y=23.7AB(25min) (I- z>2mag. to rule out brown-dwarfs)depth: I=25.8(15min), z=24.9AB(20min), Y=23.7AB(25min) (I- z>2mag. to rule out brown-dwarfs) area:2000 sq.degarea:2000 sq.deg How many QSOs can be found?  2000deg 2, z=23.6AB=> 4000  (imag is the limit here.)  Escaping flux correlation function. Spatial fluctuation of the reionization (note only 800 for GP-test to z<22.5mag).  3mag deeper than SDSS. Meaningful LF (M= – 22mag) at z=6 to constrain reionization photon from QSO.

Tomo GOTO 6.8<z<7.8 Based on the wide survey z=24.9AB(20min), Y=23.7AB(25min) (Z-Y>2mag. to rule out brown- dwarfs)z=24.9AB(20min), Y=23.7AB(25min) (Z-Y>2mag. to rule out brown- dwarfs) area:2000 sq.degarea:2000 sq.deg How many QSOs can be found? 3 mag deeper than UKIDSS. x20 times larger source density (1 mag deeper, x6 sources). 3 mag deeper than UKIDSS. x20 times larger source density (1 mag deeper, x6 sources).  2000deg 2, Y=23.0AB=> 90 (depth, especially in Z wins here.) –Complete GP-trough at any direction

Tomo GOTO How many WFMOS fibers? Z ～ 6Z ～ 6 –spectroscopy success rate ～ 15%(Fan 、 Goto 2005). –4000 QSOs (26000spectra) in 2000sq.deg, –13 fibers/sq.deg. Z ～ 7Z ～ 7 –for 90 QSOs (600 spectra) in 2000sq.deg. –only 0.3 fibers/sq.deg. Easy to be part of the WFMOS survey. WFMOS CCDs needs to be red sensitive.

Tomo GOTO QSO: Summary With 0.3(13)/deg 2 WFMOS fiber for z ～ 7(6) depth: I=25.8(15min), z=24.9AB(20min), Y=23.7AB(25min)depth: I=25.8(15min), z=24.9AB(20min), Y=23.7AB(25min) area:2000 sq.degarea:2000 sq.deg HSC/WFMOS can find 90 QSOs Z ～ /deg 2 WFMOS fibers90 QSOs Z ～ /deg 2 WFMOS fibers –Complete GP-trough at any direction 4000 QSOs z ～ 6. 13/deg 2 WFMOS fibers4000 QSOs z ～ 6. 13/deg 2 WFMOS fibers –first spatial variation of reionization, LF, density to M= – 22mag

Tomo GOTO Why galaxy cluster search with the HSC/WFMOS? Why galaxy cluster search with the HSC/WFMOS? 1.missing link in cluster galaxy evolution 2. estimating w Tomo GOTO (Ifa, Univ. of Hawaii) Masamune Ooguri(Stanford)

Tomo GOTO z>2.1 (proto) clusters are groups of star-forming galaxies (Lya emitters, LBG), very different from low-z red-sequence clusters. red, dead Reason: selection effect. 4000A break selected vs Lya/LBG selected Evolutionary path unknown

Tomo GOTO missing link: What are 1<z<2 clusters like? Is there any link between proto- and today ’ s clusters?

Tomo GOTO z-band was the limit for the 4000A break search (z<1.27): with the HSC Y-band, we can extend the 4000A cluster search to 1.25<z<1.75 low z example Goto et al.2002, AJ, 123, 1801 In HSC z-Y color M* galaxy Coma CMR color-cut Specz from WFMOS

Tomo GOTO 1.SDSS Data3.Enhance4.Detection SDSS Cut&Enhance Galaxy Cluster Catalog (Goto et al.2002, AJ, 123, 1801) 2.Color cuts For 34 color cuts. 5.Cluster catalog RA DEC

Tomo GOTO Waldo is obvious after color-cut

Tomo GOTO color-cut works: Newly discovered clusters with the SDSS (Goto et al.2002, AJ, 123, 1801 Goto, 2005,MNRAS, 359,1415,) This cluster finder can be easily adopted to HSC z-Y.

Tomo GOTO AKARI (the first Japanese IR satellite) is finding 0.9<z<1.6 clusters. (Goto et al PASJ in press) HSC can find 10 5 of these.

Tomo GOTO Purpose 2: estimating w. By revealing cluster mass function at 1.25<z<1.75,By revealing cluster mass function at 1.25<z<1.75,  we can obtain independent estimate on w.

Tomo GOTO © Oguri

Tomo GOTO Is cluster count still useful in WMAP era? ↑ Independent estimate on Ω mIndependent estimate on Ω m Statistical error is comparable to WMAPStatistical error is comparable to WMAP higher z than weak lensinghigher z than weak lensing

Tomo GOTO Tight correlation: optical richness vs cluster mass. Reyes etal. 2008

Tomo GOTO Survey design and expected results DesignDesign z=24.9AB(20min), Y=23.7AB(25min)z=24.9AB(20min), Y=23.7AB(25min) area:2000 sq.degarea:2000 sq.deg expected resultsexpected results Volume=4x10 9 Mpc 3 at 1.25<z<1.75Volume=4x10 9 Mpc 3 at 1.25<z<1.75 Assuming LCDM Universe,Assuming LCDM Universe, →10 4 clusters with Msun→10 4 clusters with Msun →3x10 5 clusters with Msun (only optical can find.)→3x10 5 clusters with Msun (only optical can find.) →σ （ｗ）～ 0.07 (Oguri-san ’ s talk) precision cosmology with cluster counts.

Tomo GOTO How many WFMOS fibers? 10 5 clusters in 2000sq.deg.10 5 clusters in 2000sq.deg. –25 fibers/deg 2. Can be part of the WFMOS survey.

Tomo GOTO Summary

Summary Working with the HSC, WFMOS can find: Clusters: 10 5 clusters at 1<z<1.75 with 25 fibers/deg 2 revealing missing link between proto- and old galaxy clusters.revealing missing link between proto- and old galaxy clusters. Independent constraints on dark energyIndependent constraints on dark energy →σ （ｗ）～ 0.07→σ （ｗ）～ 0.07 QSOs: –90 0.3/deg 2 WFMOS fibers First sample to study spatial variation of the complete GP- troughFirst sample to study spatial variation of the complete GP- trough –4000 QSOs z ～ 6. 13/deg 2 WFMOS fibers –first spatial variation of reionization, LF, n-density to M= – 22mag

Tomo GOTO 終わり