Quasar/LyAF Science & Cosmology• Nao Suzuki (nsuzuki@lbl.gov)

Lawrence Berkeley National Lab:
Supernova Cosmology Project• Menu
• Introduction to Ly alpha Forest• Quasar/LyAF Key Projects• LyAF BAO• LyAF Forecast• Quasar/LyAF Wish List

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Quasar Ly alpha Forest

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Quasar/LyAF : Advantage I :Probing high-z universe (2000 deg2)
mag

z=0.5

z=1.0

z=2.5

z=3.5

z=4.5

z=5.5

z=6.5

QSO

LyAF1667

60

25

36

00015528

17414463

185

40

54

001,110

233

18

1,960

2,860

1,070

198

32190

6,120

1,300

19

6,820

13,100

5,360

876

123

12

0

26,300

6,380

20

16,20037,20019,400

3,500

429

44

0

76,70023,30021

27,50069,30045,30011,300

1,400

138

3

155,000

53,20022

33,600104,000

35,60026,900

4,120

399

16

245,000

107,400

23

19,300144,000

106,000

47,60010,3001,090

53

328,000

164,700

Total

106,000

373,600

212,940

90,45016,4581,702

72821,000

412,961

From LSST Bluebook arxive/0912.0201

SDSS/DR7=100,000 Quasrs with 10,000 LyAF , BOSS 160,000 LyAF

LyAF : Advantage II : Small Scale Probe

Max Tegmark• BAO• Growth Factor• Small ScalePower Spectrum• slope n : dlogn/dke-foldings ofInflation• Upper limit ofNeutrino mass
• ChemicalEvolution in IGM
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Quasar Spectrum Key Projects• I : IGM Ionization Historya) HI reionization 6 < z < 10? (Imanishi san’s talk)b) HeII reionization z = 3• II: Chemical Evolution History• III: Absorber vs. Galaxy Correlation (Brice’s talk)• IV: Black Hole Mass & Mass Accretion Rates• V : Cosmologya) BAO, b) AP test, c) Growth Factor (Sep PFS),d) Power Spectrum• => expect to grow a community of 20 core people
with 50 close collaborators (based on BOSS)

Key Project I : Ionization History (HI)HI Reionization : 6 < z < 10?
Important for the future of
21cm cosmology
Q. Inhomogenity of UV or Density?

Becker et al.
z > 5 quasars
SDSS/DR7: 50 quasars=> PFS: 2000 quasars
expect to find z > 7 quasars

Baek et al (2010) :Red: Neutral HI Blue: Ionized HI

Key Project I: Ionization History (HeII)
HeII Reionization : z = 3.2??
Important for the high energy UVphotons and SFR z < 3.

z vs. opacity : Dall’Aglio et al. (2008)z > 2.2 quasars
SDSS/DR7: 10,000 quasars=> PFS: 500,000 quasars

Zheng et al (2008) : z=3.51 Quasar
HeII reionization has not happened
at z=3.5 (304 x (1.0+3.5)=1370)

Key Project II: Chemical Evolution
Metal Absorbers (LLS/DLA)
Chemical composition (0 < z < 8)Composite Metal Lines : Pieri et al. (2010)

MgII : 0.35 < z < 3.64,
CIV : z > 1.6
SDSS/DR7: 100,000 quasars=> PFS: 1,000,000 quasars

Kobayashi & Nomoto (2009)
SNIa does not happen [Fe/H] < -1.1

Key Project V: Cosmology
From Deceleration to Acceleration
SNe : (space)SNe : (ground)• ` BAO : (z=0.3 SDSS)

LyAF: (z > 2.2)

BAO : (z=0.7 SDSSIII/BOSS)
9w=P/ρ : Equation of State today( statistical err < systematic err)
E ∝ a−3(1+w)•w=-1 : cosmological constant•w=0 : matter•w=1/3: radiation
SNe + BAO + CMB
For a flat universe:
w = -0.997 ± 0.052(stat) ± 0.082(sys)For a non-flat universe
w = -1.038 ± 0.056(stat) ± 0.093(sys)
SCP UNION2 Amanullah et al. 201010Λ Business Market Values in 2010
Dark Energy Task Force(DETF)
Figure of Merit : FoM

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σ(w0 )σ(wa )

w(a)=w0+(1-a)wa
FoM=1.0(Amanulla et al 2010,SCP UNION2)

Key Project V: Cosmology LyaF BAO
ξf f (r) = B(r)ξδδ (r) + A(r)ξf f (r)Flux Fluctuation :What we can observe(correlation x: transverse y: radial)ξδδ (r)Density Fluctuation:
What we want to know

Simulation(30003 Particle, Box 1500 Mpc/h) by Slosar et al. (2009)

Key Project V: Cosmology LyaF BAO
ξf f (r) = B(r)ξδδ (r) + A(r)ξf f (r)Flux Fluctuation :What we can observe(correlation x: transverse y: radial)ξδδ (r)Density Fluctuation:
What we want to know

Simulation(40003 Particle, Box 700 Mpc/h) by White et al. (2010)

Key Project V: Cosmology LyaF BAO
ξf f (r) = B(r)ξδδ (r) + A(r)B(r) = ξf f (r)/ξδδ (r)Flux Bias:
Flux Fluctuation :Density Fluctuation:
Flux to Mass Translator
What we can observe
What we want to know
Bias=> Scale Independent!
(correlation x: transverse y: radial)
Simulation(40003 Particle, Box 700 Mpc/h) by White et al. (2010)

PFS Quasar BAO Survey at z=2.64
Probing high-z universe (2000 deg2)
magexptime(min)nightsN(quasar) N(fibers)(/deg2)(/1.8deg2)

dH/H

dDa/DaN(total)

21

1021

8.8

32

0.049

0.091 17,600

2220

41

22.5

810.0210.035 45,000

23

48

99

45.0

162

0.015

0.021 90,000

24120

246

76.6

276

0.013

0.017 153,200

Based on McDonald & Eisentein (2007)

SDSS/DR7=10,000 LyAF , BOSS 160,000 LyAF with 8000 deg2

LyAF Wish List

• Read-Out Noise < 3e please!
• Wavelength Coverage=> Blue Side!

λ3800-10000 ( 2.2 < z < 4)
λ3200-10000 ( 1.6 < z < 4)Note: Missing Range (BOSS): 1.6 < z < 2.2• Fiber:

20-50 quasars/deg2 (mag dependent)
Success Rate: 50%
80-200 fibers/ 1.8 deg2

• Resolution:

R=2000 (v=150km/s) Good for LyAF BAO
R=4000 (v=75km/s) Metal Line Studies

16Known Unknowns 1 :Metal Line Contamination
High Resolution Helps
R=2,000• SDSS
v=150km/s
R=3,000• LRIS
v=100km/s
R=4,200• ESI
v=72km/s• HIRES R=37,500v=8km/sKnown Unknown 2Target Selection :• Quasar Locus Crosses Stellar Locus at certain
redshifts• Vairability! Helps (95% Quasar)18

Cosmology Wish List
• Needs to optimize each methods strength!!
• 1. Supsernova Cosmology (0.5 < z < 1.4)
Synergy with Quasar/LyAF Sciencea) Target Selection b) w complimentarity• 2. Weak Lensing• 3. Galaxy BAO ( 0.7 < z < 1.4)
• 4. LyAF BAO ( 2.2 < z < 4)
• 5. Cluster Counts• 6. Growth Factor Measurement (WL, LyAF)

19White Paper Revisions• Aim FoM > 300 by optimizing Survey

Strategies (SN+WL+CMB(planck)+BAO)• Select Key Projects and Review• S/N unit is not clear : /pix, /A, /FWHM?a)
Target Selection b) w complementarity• Target Selection efficiency is not clear (forquasars, 50%)

• Survey Strategy is not clear (Wide orPointed?)20

Cosmology in 2015-20• Let’s Aim FoM > 300 by optimizing Survey
Strategies (SN+WL+CMB(planck)+BAO)• Review Survey every 2 years and optimize
strategies• With TMT, JWST, LLST, and WFIRST theworld would not be the same and PFS is thebest choice not only for Japan but also for theworld!!
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Back-up Slides

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Supernova Ia from SDSS DR7
Janos Botyanszki, Kimberly Aller,
Josh Meyers (code), Nao Suzuki(eigen spectra)

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aSDSS DR7 : 1 SNIa / 6000 Galaxies
26Quasar Basics 1:
Number Density Evolution•

Red (M < -27) Green (M < -26) Blue (M< -25) Black (M < -24) :Combo-17 Survey (MPG/ESO 2.2 m : Wolf et al. 2003)

Quasar Basics 2 : SED
UV ExcessPhysics of UV Excess
Accretion disk surrounds thesuper massive black hole
SED(Mass, Accretion Rate)

Ionization Rate : 2009
Dall’Aglio et al 200930

HST Cluster SN Survey
HSTKeckVLT

Nao Suzuki & SCP
PI: Saul Perlmutter

SubaruSNIa Spectral Diversity