1. For the Large-Scale Structure Science Collaboration
LSS Projects with LSST
Hu Zhan (UC Davis)
For the Large-Scale Structure Science Collaboration
S. Allen (Stanford)
A. Hamilton (UC Boulder)
T. Quinn (UW)
R. Ansari (LAL)
J.-C. Hamilton (APC)
P. Ricker (UIUC)
E. Aubourg (APC)
Z. Ivezic (UW)
M. Strauss (Princeton)
A. Barrau (LPSC)
B. Jain (UPenn)
A. Szalay (JHU)
J. Bartlett (APC)
J. Jee (UC Davis)
J. Thaler (UIUC)
R. Brunner (UIUC)
L. Lubin (UC Davis)
J.A. Tyson (UC Davis)
T. Budavari (JHU)
C. Miller (NOAO)
L. Verde (CSIC-IEEC)
A. Cooray (UC Irvine)
J. Mohr (UIUC)
B. Wandelt (UIUC)
L. Derome (LPSC)
M. Moniez (LAL)
R. Wechsler (Stanford)
E. Gawiser (Rutgers)
J. Newman (UPitt)
D. Wittman (UC Davis)
H. Zhan (UC Davis)
LSST AHM, NCSA, 5/20/2008

2. Large-Scale Structure: An Introduction
(1980)
Homogeneous background + fluctuations
Evolution of fluctuations
LSST AHM, NCSA, 5/20/2008

3. Large-Scale Structure: Tools
SDSS DR3
SDSS DR5, Percival et al. (2008)
Baryon Acoustic Oscillations → standard ruler → dark energy
LSST AHM, NCSA, 5/20/2008

4. Large-Scale Structure: A Journey
Galaxies are more or less transparent to CMB photons. Alternative ending.
WMAP map.gsfc.nasa.gov
LSST AHM, NCSA, 5/20/2008

5. Large-Scale Structure: A Journey
Large-scales linear -> BAO standard ruler, inflation/initial condition, small scales nonlinear, WL as well
Fluctuations in the early universe are imprinted in the CMB, overdensities grow under gravitational instability, and galaxies form in local density peaks.
LSST AHM, NCSA, 5/20/2008

6. Different types as well.
Projects with LSST
Power Spectrum/2-point Correlation Function (galaxies, quasars, SNe, galaxy clusters…)
Baryon acoustic oscillations, distance, dark energy/modified gravity, wm, wb, mn, Wk, ns, as, primordial fluctuations (power on very-large scales), inflation.
Joint Analysis of Galaxy Overdensity & Weak Lensing Shear Maps
S.A.A., but achieving much stronger constraints with the extra galaxy-shear information and mutual calibration of systematic uncertainties, intrinsic alignment, galaxy & halo formation, halo model, baryonic effects, galaxy bias.
Clusters (optical, WL, X-ray, & Sunyaev‒Zel’dovich)
Self-calibration of the mass-observable relation and the mass threshold with counts & variance, joint analysis with WL, SZ, & X-ray (SPT, Planck, eROSITA), halo assembly bias, Wm, s8, dark energy, dark matter, substructure, cluster galaxy evolution.
Galaxy Cross Correlations (photo‒photo, photo‒spec, galaxy‒SN, galaxy‒SN mag.)
Calibrating the photo-z error distribution, checks for systematics, SN magnification.
N-Point Statistics (N > 2) & Beyond
Galaxy bias, non-Gaussianity, nonlinear evolution, dark energy, galaxy formation.
Integrated Sacks-Wolfe Effect (Correlation with CMB)
Very-large-scale structure formation, dark energy.
Galaxy Counts-in-Cells (beyond Cosmology)
Galactic extinction, dust map (w/ IR).
Different types as well.
LSST AHM, NCSA, 5/20/2008

7. Baryon Acoustic Oscillations
CMB temp. fluctuations (WMAP)
Imprints on the matter power spectrum (White 2005)
LSST galaxy angular PS (Zhan 2006)
BAOs in multipole space
DLS survey
RS~150 Mpc
Angular diameter distance
RS = Dq DA
(Sound horizon at recombination)
LSST AHM, NCSA, 5/20/2008

8. Lya Emitter Clustering in MUSYC-ECDFS
(Gawiser et al. 2007, ApJ 671, 278)
Just demonstrate clustering of different (sub-types of) objects
162 LAE candidates
Clustering analysis by Harold Francke
Bias evolution suggests that LAEs at z = 3.1 evolve into ~L* galaxies at z = 0.
LSST AHM, NCSA, 5/20/2008

9. D(z) and G(z) from LSST BAO and WL
Zhan, Knox, & Tyson, in prep
D1 … D14 from z = 0.14 to 5; G0 … G14 from z = 0 to 5.
BAO distances are generally more accurate than WL ones.
But WL has eigenmodes that are better determined than all BAO modes.
Joint results are less sensitive to the systematics of each technique.
LSST AHM, NCSA, 5/20/2008

10. Complementarity between BAO and WL
Projection of errors of distance eigenmodes onto w0‒wa space.
5 WL distance eigenmodes account for most of the WL constraints on w0 & wa.
BAO & WL are highly complementary.
LSST AHM, NCSA, 5/20/2008

11. s(wp)×s(wa) Dependence on Photo-z RMS
The error product (EP) is NOT for the LSST galaxy BAO, but the trend is applicable to photo-z angular BAO measurements.
The impact of uncertainties in the photo-z bias and rms depends on the survey.
Cross-correlations between redshift bins will help reduce the photo-z uncertainties.
At large sz , the EP is roughly proportional to sz .
Radial BAO information becomes available at sz < 0.01(1 + z).
Zhan et al. (2008)
LSST AHM, NCSA, 5/20/2008

12. Improved Galaxy Spectral Templates
New, physically motivated, high-resolution templates for photo-zs.
(Niemack et al. 2008)
Application to SDSS+GALEX
From Licia Verde
LSST AHM, NCSA, 5/20/2008

13. Photo-z Calibration with Cross Correlations
Photo-z distribution in red, spectroscopic samples in green, blue, & yellow. The cross-correlations between the photo-z sample and spectroscopic samples increase as the photo-z distribution peaks. This, together with the auto-correlations of each sample, can be used to calibrate the photo-z distribution (Newman 2008, ).
LSST AHM, NCSA, 5/20/2008

14. Photo-z Calibration with Cross Correlations
Photometric redshift bins
Kernel ∝ galaxy distribution in true-redshift space
Photo-z‒photo-z cross correlations will also help calibrate the photo-z error distribution (Zhan 2006; Schneider et al. 2006).
LSST AHM, NCSA, 5/20/2008

15. Primordial Non-Gaussianity
Large-scale clustering of halos is a good probe of primordial non-Gaussianity and hence inflation. The effect of NG appears at large scales. As for BAOs surveys, large volumes need to be covered.
Tests on simulations and forecast errors is on going.
fNL = 100
(Mpc-1)
F = f + fNL * (f2 - ‹f2›)
WMAP results (Komatsu et al. 2008)
-9 < fNLlocal < 111 &
-151 < fNLequil < 253 (95% CL)
Matarrese & Verde (2008); Carbone et al. (2008); Grossi et al. (2008)
From Licia Verde
LSST AHM, NCSA, 5/20/2008

16. Cluster Counting tCDM vs. LCDM (Evrard et al. 2002)
Dark energy sensitivity (Mohr 2004)
No redshift
With redshifts
Sensitive to both cosmic expansion and growth histories, but also prone to errors in the mass-observable relation. Multi-wavelength observations are helpful. See also self-calibrations:
Lima & Hu (2004, 2005); Majumdar & Mohr (2004)
Planck SZ clusters
Importance of redshifts (Geisbusch & Hobson 2007)
LSST AHM, NCSA, 5/20/2008

17. SN Magnification‒Galaxy Correlation
The effect should be there and is useful for cross-check. However, it is hard to detect for individual SNe. LSST can improve the detection with angular correlation between SN residual magnitudes and foreground galaxy over-densities.
SN residual magnitude vs. expected magnification from foreground galaxy distribution.
This is an example of synergy between LSST LSS, SN, & WL Science Collaborations.
Tentative detection of the gravitational magnification of Type Ia SNe (Jonsson et al. 2006, 2007)
Suggested by Asantha Cooray
LSST AHM, NCSA, 5/20/2008

18. Projects with LSST
Power Spectrum/2-point Correlation Function (galaxies, quasars, SNe, galaxy clusters…)
Baryon acoustic oscillations, distance, dark energy/modified gravity, wm, wb, mn, Wk, ns, as, primordial fluctuations (power on very-large scales), inflation.
Joint Analysis of Galaxy Overdensity & Weak Lensing Shear Maps
S.A.A., but achieving much stronger constraints with the extra galaxy-shear information and mutual calibration of systematic uncertainties, intrinsic alignment, galaxy & halo formation, halo model, baryonic effects, galaxy bias.
Clusters (optical, WL, X-ray, & Sunyaev‒Zel’dovich)
Self-calibration of the mass-observable relation and the mass threshold with counts & variance, joint analysis with WL, SZ, & X-ray (SPT, Planck, eROSITA), halo assembly bias, Wm, s8, dark energy, dark matter, substructure, cluster galaxy evolution.
Galaxy Cross Correlations (photo‒photo, photo‒spec, galaxy‒SN, galaxy‒SN mag.)
Calibrating the photo-z error distribution, checks for systematics, SN magnification.
N-Point Statistics (N > 2) & Beyond
Galaxy bias, non-Gaussianity, nonlinear evolution, dark energy, galaxy formation.
Integrated Sacks-Wolfe Effect (Correlation with CMB)
Very-large-scale structure formation, dark energy.
Galaxy Counts-in-Cells (beyond Cosmology)
Galactic extinction, dust map (w/ IR).
LSST AHM, NCSA, 5/20/2008