Ly-alpha emission line

16
Ly-alpha emission line Ly-beta emission line

description

Ly-beta emission line. Ly-alpha emission line. LyaF Future: 3D map of LSS. SDSS-III/BOSS quasar density (20 per sq. deg.) WFMOS can do up to ~8 times denser 100 Mpc/h deep 400 times this volume in SDSS. Current: very sparse. SDSS-II quasar density (1 per sq. deg.) 100 Mpc/h deep - PowerPoint PPT Presentation

Transcript of Ly-alpha emission line

Page 1: Ly-alpha emission line

Ly-alpha emission lineLy-beta emission line

Page 2: Ly-alpha emission line

LyaF Future: 3D map of LSS• SDSS-III/

BOSS quasar density (20 per sq. deg.)

• WFMOS can do up to ~8 times denser

• 100 Mpc/h deep

• 400 times this volume in SDSS

Page 3: Ly-alpha emission line

Current: very sparse• SDSS-II

quasar density (1 per sq. deg.)

• 100 Mpc/h deep

• 400 times this volume in SDSS

Page 4: Ly-alpha emission line

Primordial power spectrum parameters

WMAP 5-year

Eisenstein et al. BAO

Includes tensors

Page 5: Ly-alpha emission line

Matter density-power amplitude constraint

WMAP 5-year

Eisenstein et al. BAO

Includes tensors

Page 6: Ly-alpha emission line

Primordial power spectrum parameters

WMAP 5-year

Eisenstein et al. BAO

Page 7: Ly-alpha emission line

Current parameter highlights (all including tensors, kp=0.05 1/Mpc,

WMAP5+Eisenstein BAO+LyaF)

(for T/S, BAO & LyaF independently find this level)

• With WMAP3, sum m_nu < 0.2 eV

Page 8: Ly-alpha emission line

Observed (3D) power

Ideal 3D power (perfectly sampled)

Sampling noisen=surface density of lines of sight(analogous to galaxy shot noise)

Resolution

Detector noise

Page 9: Ly-alpha emission line

Simulated 3D flux power, relative to real-space linear theory (McDonald 2003)

Bottom to top on left:

mu=

0-0.25,

0.25-0.5,

0.5-0.75,

0.75-1.0

Page 10: Ly-alpha emission line

Theory/fitting formula for redshift-space power

• Linear theory on large scales

• Non-linearity + pressure + fingers-of-god

• Baryon wiggles simply modify P_L(k)

Page 11: Ly-alpha emission line

Parameter dependence of 3D flux power (McDonald 2003)

Black - increased amplitude

Red - increased slope

Solid - LOS

Dotted - transverse

Page 12: Ly-alpha emission line

Parameter dependence of 3D flux power (McDonald 2003)

Black - increased temperature

Red - increased dependence of temperature on density (gamma-1)

Solid - LOS

Dotted - transverse

Page 13: Ly-alpha emission line

Parameter dependence of 3D flux power (McDonald 2003)

Black - increased <F>

Red - never mind (related to Jeans filtering)

Solid - LOS

Dotted - transverse

Page 14: Ly-alpha emission line

Future BAO: Measure 3D power• Band power

measurement from BOSS

• Black: radial• Green:

transverse• Red: diagonal• Dotted: Seo &

Eisenstein non-linear smearing

• Normalizations compressed.

Page 15: Ly-alpha emission line

Constraints vs.

resolution

R=62.5, 125, 250,2000

(This was for a WFMOS-like survey, less area than BOSS)

Page 16: Ly-alpha emission line

Expected BAO distance scale constraints from BOSS