BAO experiments comparison
BAO experiments comparison
BAO experiments comparison
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<strong>BAO</strong> <strong>experiments</strong><br />
<strong>comparison</strong><br />
Francisco Javier Castander<br />
Institut de Ciències de l’Espai, IEEC/CSIC, Barcelona<br />
Euclid/DUNE <strong>BAO</strong> WG
Summary<br />
• <strong>BAO</strong> <strong>experiments</strong><br />
• Parameters <strong>comparison</strong><br />
• Fisher Matrix analysis<br />
• Cosmology constraints <strong>comparison</strong> (FoM)
<strong>BAO</strong> <strong>experiments</strong><br />
Photometric<br />
• DES<br />
• PanSTARRS<br />
• PAU<br />
Spectroscopic<br />
• WiggleZ<br />
• HETDEX<br />
• BOSS<br />
• WFMOS<br />
Space<br />
• Euclid<br />
• JDEM (ADEPT?)
The Dark Energy Survey<br />
100<br />
90<br />
80<br />
70<br />
60<br />
50<br />
40<br />
30<br />
20<br />
10<br />
DECam / Mosaic II QE <strong>comparison</strong><br />
QE, LBNL<br />
(%)<br />
QE, SITe<br />
(%)<br />
0<br />
300 400 500 600 700 800 900 1000 1100<br />
Wavelength (nm)<br />
http://www.darkenergysurvey.org/
Dark Energy Survey (DES)<br />
http://www.darkenergysurvey.org<br />
• Area: 5000 deg2<br />
• Magnitude limit: i
PanSTARRS
PanSTARRS (Panoramic Survey Telescope &<br />
Rapid Response System)<br />
http://panstarrs.ifa.hawaii.edu/<br />
• Area: 3π deg2 (useful extragalactic ~20000 deg2)<br />
• Magnitude limit: PS1: i
Physics of the Accelerating Universe (PAU)
Physics of the Accelerating Universe (PAU)<br />
http://www.ice.csic.es/research/PAU/<br />
• Area: 8000 deg2<br />
• Magnitude limit: i
WiggleZ
WiggleZ<br />
http://wigglez.swin.edu.au/<br />
• AAT + AAOmega<br />
• Area: 1000 deg2<br />
• Magnitude limit: r
HETDEX:
HETDEX (HET dark energy experiment)<br />
http://www.as.utexas.edu/hetdex/<br />
• HET + VIRUS<br />
• Area: 200 deg2<br />
• Magnitude limit:<br />
• Number of galaxies: 1 10 6<br />
• Redshift range: 1.8
BOSS
BOSS (Baryon Oscilations Spectroscopic Survey)<br />
http://www.sdss3.org/cosmology.php<br />
Luminous Red Galaxies<br />
• SDSS<br />
• Area: 10000 deg2<br />
• Magnitude limit: r
WFMOS
WFMOS<br />
Emission line galaxies<br />
• Area: 2000 deg2<br />
• Magnitude limit: R_AB
Payload<br />
CDF study case<br />
Telescope<br />
1.2 meter Korsch TMA<br />
Euclid<br />
3 instruments<br />
Visible Imaging VIS: 0.21” PSF at 800 nm, 0.1”/pixel<br />
NIR Photometry NIP: 0.33”/pixel, 3 bands (Y, J, H)<br />
NIR Spectroscopy NIS: 0.91.7 µm, set of 3 cameras,<br />
multiobjects (micromirror array), R~400<br />
Each of them with a field of view ~0.48 deg 2<br />
Thermal<br />
Passive cooling<br />
170 K CCD<br />
140 K NIR detectors<br />
Power<br />
One power conditioning unit per instrument<br />
Total payload: ~200 W peak<br />
Datahandling<br />
Spectroscopy target selection<br />
Full frame images lossless compression<br />
NIR detectors noise reduction<br />
NIP<br />
Observation mode<br />
Step and stare case fully investigated<br />
Continuous scanning requires descan mechanism for<br />
infrared channels<br />
Payload mass<br />
~660 kg, including 300 kg for the 3 instruments<br />
NIS<br />
VIS
Euclid<br />
All galaxies<br />
• Area: 20000 deg2<br />
• Magnitude limit: H_AB
ADEPT
ADEPT<br />
• Area: 3π deg2 (useful extragalactic ~20000 deg2)<br />
• Magnitude limit: ?<br />
• Spectroscopy: slitless in NIR<br />
• Redshift range: 1.0
<strong>BAO</strong> surveys <strong>comparison</strong><br />
spec<br />
112<br />
20000<br />
ALL<br />
1.5e+8<br />
0.3
Expected <strong>BAO</strong> performance<br />
Scaling error forecasts for different surveys:<br />
delta (w) ~ Δ P/P ~ 1/sqrt(V) (1 + 1/nP)
<strong>BAO</strong> constraints with<br />
Seo & Eisenstein 2007<br />
formalism
Seo & Eisentein 2007 formalism<br />
ApJ, 2007, 665, 14<br />
• Start Fisher matrix formalism (Seo & Eisentein 2003)<br />
• Isolate information from baryonic peaks<br />
• accommodate Lagrangian displacement distribution into FM (reflect loss of<br />
information: nonlinear growth, nonlinear bias, nonlinear redshift distortions)<br />
• Contract multidimensional FM (12 d) into a two dimensional (errors on Da/s and<br />
H*s)<br />
• Agreement with simulations
Seo & Eisentein 2007 formalism<br />
Fisher matrix formalism (Seo & Eisenstein 2003)
Seo & Eisentein 2007 formalism<br />
Fisher matrix formalism (Seo & Eisenstein 2003)
Seo & Eisentein 2007 formalism<br />
Lagrangian displacements (Eisenstein et a 2007)<br />
• Approximated as elliptical Gaussian function<br />
• Most of the effect comes from bulk flows
Seo & Eisentein 2007 formalism<br />
Reformulated Fisher Matrix
Seo & Eisentein 2007 formalism<br />
Fisher Matrix for the location of the peak
Seo & Eisentein 2007 formalism<br />
Fisher Matrix for the location of the peak
Seo & Eisentein 2007 formalism<br />
Fisher Matrix for Da/s and H*s<br />
linear redshift distortion
Seo & Eisentein 2007 formalism<br />
Fisher Matrix for Da/s and H*s
Seo & Eisentein 2007 formalism<br />
Fisher Matrix for Da/s and H*s
Seo & Eisentein 2007 formalism<br />
Fisher Matrix for Da/s and H*s (adding uncertainty<br />
in the radial direction)
Cosmological constraints<br />
Transform the FM in Da/s and H*s into a FM<br />
depending on cosmological parameters
<strong>BAO</strong> surveys <strong>comparison</strong><br />
213<br />
spec<br />
112<br />
20000<br />
ALL<br />
1.5e+8<br />
0.3
<strong>BAO</strong> cosmological constraints (Euclid)<br />
Parameter<br />
No prior<br />
error<br />
Δw<br />
o 0.40<br />
Planck Prior<br />
0.21<br />
ΔΩ M<br />
0.10 0.018<br />
Δw<br />
a<br />
2.16 0.59<br />
Δw<br />
p<br />
0.12 0.034<br />
Δn<br />
s<br />
0.0047<br />
ΔΩ DE<br />
0.11 0.017<br />
Δσ 8<br />
0.054<br />
ΔΩ b<br />
0.0032<br />
Δh 0.025
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