Dragan Huterer : Measure Cls by replicating the quarter of the sky to full sky, z~0-1.1, 10^13 Msun, cosmic variance errors
Mortonson: Mass function, negative fnl 2 sigma away from zero.
Park, Code from Elise Jennings: P(k) by splitting into small boxes, 0.6-0.8, >10^13 Msun, Tommaso Giannantonio: Projected clustering, w(theta), using Healpix, Monte Carlo errors!?, z~0-1.1, ?!
Elizabeth Krause: Projected clustering (w_p), Covariance from jackknife, 10^14 Msun.
Carlos Cunha: 3-d xi(r) small mass haloes, 0 - 0.8, 1-1.5E13 Msun, and calculating the two point correlation function, jackknife errors.
Sign of fnl in the correlation function, causes the bump in the correlation function to go up and down. The zero at the correlation function can disappear for high fnl (~200) values.
One has to worry about volume regularization, satisfying integral constraint.
Will Percival: xi(r) is useful. And one has to be careful about the large angle separation, so keep both \xi(r,mu,theta).
Mass is 1.306E13 in 200 critical units=200/0.27=740.47 rhobar units.
This mass is 1.611E13 in Mvir, which is 1.869E13 in M200.
The effective bias then should be ~3.3. People are getting biases of the order of ~2.7, so something fishy but maybe they are including some other cuts at the high mass end.
Tomasso
SPICE: Cl_cut = \Sum_l_l' M_l_l' Cl_fullsky
Cross correlating clusters of different masses can help a lot to remove cosmic variance issues.
Sarah Shandera:
==
b_NL = b0 + fn^{eff}(M)/k^alpha
alpha=2 local
alpha=2\pm (ns-1) -> Multifield. Fields < H
0<alpha<2 quasi single field. fields order H
alpha<=3: modified initial state.
fnl ~ 1
Carlos Cunha:
If you use small area spectroscopic samples, you need to worry about sample variance, this can only be beaten down by more area and it is expensive. And you need to go to the full depth of your sample to get the spectroscopic redshifts.
Complicated photometric calibration over the entire area. The redshift distribution is not the same at all angular scales.. Photometric errors can also have angular dependencies.
Redshifts- Spectroscopic -
- Photometric -
Ashley Ross:
Experience from BOSS: DR9 goes online July 2012.
Fraction of galaxies as a function of stellar number density decreases. Usually you expect it to be correlated, but you see anti-correlation.
Mortonson: Mass function, negative fnl 2 sigma away from zero.
Park, Code from Elise Jennings: P(k) by splitting into small boxes, 0.6-0.8, >10^13 Msun,
Tommaso Giannantonio: Projected clustering, w(theta), using Healpix, Monte Carlo errors!?, z~0-1.1, ?!
Elizabeth Krause: Projected clustering (w_p), Covariance from jackknife, 10^14 Msun.
Carlos Cunha: 3-d xi(r) small mass haloes, 0 - 0.8, 1-1.5E13 Msun, and calculating the two point correlation function, jackknife errors.
Sign of fnl in the correlation function, causes the bump in the correlation function to go up and down. The zero at the correlation function can disappear for high fnl (~200) values.
One has to worry about volume regularization, satisfying integral constraint.
Will Percival: xi(r) is useful. And one has to be careful about the large angle separation, so keep both \xi(r,mu,theta).
1) Derive the bias, fnl.
btot = [\int \int (M n(M,z) b(M,z) dM Da^2(z) Dchi/dz dz) ] / [\int \int (M n(M,z) dM dz Da^2(z) Dchi/dz dz) ]
M=1E13 Msun and above.
Mass is 1.306E13 in 200 critical units=200/0.27=740.47 rhobar units.
This mass is 1.611E13 in Mvir, which is 1.869E13 in M200.
The effective bias then should be ~3.3. People are getting biases of the order of ~2.7, so something fishy but maybe they are including some other cuts at the high mass end.
Marilena:
Phi=\delta(phi) + fnl \delta(phi)^2
Phi=\delta(phi) + gnl \delta(phi)^3
fnl, gnl, taunl: Depending on how you put nongaussianity. Local nongaussinity, need not be necessary.
Bispectrum: Largest in squeezed limit
Trispectrum: squashed limit with 4 k vectors.
Coupling between small and long wavelength modes.
Single field local nongaussianities vanish in the squeezed limit.
b_fnl(k) = b + 2 delta_c fnl (b-1)/k^2
b_gnl(k)=b+gnl/k^2 nonlinear-function(b)=b+3 gnl/k^2 \del ln n(M)/del fnl
Break out sessions:
====
TomassoSPICE: Cl_cut = \Sum_l_l' M_l_l' Cl_fullsky
Cross correlating clusters of different masses can help a lot to remove cosmic variance issues.
Sarah Shandera:
==
b_NL = b0 + fn^{eff}(M)/k^alphaalpha=2 local
alpha=2\pm (ns-1) -> Multifield. Fields < H
0<alpha<2 quasi single field. fields order H
alpha<=3: modified initial state.
fnl ~ 1
Carlos Cunha:
If you use small area spectroscopic samples, you need to worry about sample variance, this can only be beaten down by more area and it is expensive. And you need to go to the full depth of your sample to get the spectroscopic redshifts.
Complicated photometric calibration over the entire area. The redshift distribution is not the same at all angular scales.. Photometric errors can also have angular dependencies.
Redshifts- Spectroscopic -
- Photometric -
Ashley Ross:
Experience from BOSS: DR9 goes online July 2012.
Fraction of galaxies as a function of stellar number density decreases. Usually you expect it to be correlated, but you see anti-correlation.