I would like to use the extended version of CAMB (http://camb.info/sources/) which also gives the theoretical cl ISW-LSS but I have some doubts about the outputs of the code. If the params.ini is as attached below, which is the ISW-LSS cross-correlation column in the output file (C

_{Phi}C

_{PhiT}C

_{win_1}C

_{win_2}... C

_{Win_T1}C

_{Win_T2}.... C

_{win1_win2}...)?

And about this, how to set the count_* parameters to have just ISW? Do I have to put just

count_ISW = T

?

If I wish to consider a 'mean' redshift = 1 and a bias term = 1.98, should I consider

redshift_bias(1) = 1.98

?

And how can I take into account the window function of the survey? with the redshift_sigma(1)?

Another issue is the units of the angular power spectrum of the cross-correlations (which I understand as band powers, right?).

Thanks,

francesca

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

#Parameters for CAMB with 21cm, lensing and number counts

#output_root is prefixed to output file names

output_root = test

#for 21cm C

_{l}with sharp window use get_transfer=T, transfer_21cm_cl=T

#for broad window and other sources use get_scalar_cls=T

get_scalar_cls = T

get_transfer = F

get_vector_cls = F

get_tensor_cls = F

want_CMB = T

#Whether transfer functions are 21cm (monopole and velocity), or standard

Do21cm = F

#l

_{max_scalar}= 10000

#for 21cm k_eta_max_scalar need to be at least 5000; for lensing is re-set automatically

#k_eta_max_scalar = 20000

l

_{max_scalar}= 2000

k_eta_max_scalar = 4000

# 0: linear, 1: non-linear matter power (HALOFIT), 2: non-linear C

_{l}(HALOFIT approx)

#Or compile with NONLINEAR = nonlinear_PT to use perturbation theory, e.g. for 21cm non-linear approx

do_nonlinear = 0

#only use limber approx if you don't want cross-correlation

limber_windows = F

#output 21cm spectra in mK (rather than dimensionless)

use_mK = F

### 21cm ###

line_basic = F

line_distortions = F

line_extra = F

line_phot_quadrupole = F

line_phot_dipole = F

line_reionization = F

#### number counts ####

#whether spectra include lensing effect

DoRedshiftLensing = T

counts_density = T

counts_redshift = F

counts_radial = F

counts_timedelay = F

counts_ISW =T

counts_velocity =F

counts_potential = F

#counts_evolve =T allows for non-constant comoving source density

#uses function counts_background_z in modules_redshift space;

#if T by default assumes window includes all sources; if F then assumes constant comoving source density

counts_evolve = F

### window functions ###

#Number of z-windows to use for sources. assumed Gaussian - edit Window_f

_{a}in modules.f90.

num_redshiftwindows = 1

#Set of indexed parameters for each window function

#Redshift of the window for C

_{l}

redshift(1) =50

# 21cm, counts or lensing

redshift_kind(1) = counts

# if 21cm, width of T

_{b}window in Mhz

redshift_sigma_Mhz(1) = 0.01

#if not 21cm, width in z

redshift_sigma(1) = 1

#if counts (change redshift_kind(1)), the bias

redshift_bias(1) = 4.5

#for counts magnitude-limited survey; often called s or p, assumed constant

redshift_dlog10Ndm(1) = 0.42

massless_neutrinos = 3.04

massive_neutrinos = 0

nu_mass_eigenstates = 1

nu_mass_degeneracies = 1

#nu_mass_fractions = .4285714286 .5714285714

nu_mass_fractions = 1

#massive_nu_approx: 0 - integrate distribution function

# 1 - switch to series in velocity weight once non-relativistic

# 2 - use fast approximate scheme (CMB only- accurate for light neutrinos)

massive_nu_approx = 3

#Settings for transfer functions/matter power spectrum/21cm sharp-z power spectrum

transfer_high_precision = T

transfer_kmax = 500

transfer_k

_{per_logint}= 0

transfer_num_redshifts = 1

transfer_redshift(1) = 50

#Whether to compute 21cm C

_{l}from transfer functions for sharp redshift window

#using only monopole source and redshift distortions

transfer_21cm_cl = F

#Whether to turn off small-scale late time radiation hierarchies (save time,v. accurate)

# not tested with redshift window functions

do_late_rad_trunction = F

RECFAST_fudge = 1.14

#if do_lensing then scalar_output_file contains additional columns of l

^{4}C

_{l}

^{pp}and l

^{3}C

_{l}

^{pT}

#where p is the projected potential. Output lensed CMB Cls (without tensors) are in lensed_output_file below.

do_lensing = F

#Maximum multipole and k*eta.

# Note that C

_{ls}near l

_{max}are inaccurate (about 5%), go to 50 more than you need

# Lensed power spectra are computed to l

_{max_scalar}−250 where accurate at %-level

# For high accuracy lensed spectra set l

_{max_scalar}= (l you need) + 500

# To get accurate lensed BB need to have l

_{max_scalar}>2000,

k_eta_max_scalar > 10000

# Otherwise k_eta_max_scalar=2*l

_{max_scalar}usually suffices

# Tensor settings should be less than or equal to the above

l

_{max_tensor}= 500

k_eta_max_tensor = 4000

#Main cosmological parameters, neutrino masses are assumed degenerate

# If use_phyical set phyiscal densities in baryone, CDM and neutrinos + Omega_k

use_physical = F

#ombh2 = 0.223253E−01

#omch2 = 0.104284E+00

#omk = 0

#omnuh2 = 0

hubble = 0.731586E+02

#effective equation of state parameter for dark energy, assumed

constant w = −1

#constant comoving sound speed of the dark energy (1=quintessence) cs2_lam = 1

#if use_physical = F set parameters as here

omega_baryon = 0.0462

omega_cdm = 0.2538

omega_lambda = 0.7

omega_neutrino = 0

#massless_neutrinos is the effective number (for QED + non-instantaneous decoupling)

temp_cmb = 2.725

helium_fraction = 0.24

#Reionization (assumed sharp), ignored unless reionization = T

reionization = T

re_use_optical_depth = T

re_optical_depth = 0.912305E−01

#If re_use_optical_depth = F then use following, otherwise ignored

re_redshift = 12

re_ionization_frac = 1

#Initial power spectrum, amplitude, spectral index and running

initial_power_num = 1

scalar_amp(1) = 2.0424e−009

scalar_spectral_index(1) = 0.954663E+00

scalar_nrun(1) = 0

tensor_spectral_index(1) = 0

#ratio is that of the initial tens/scal power spectrum amplitudes

initial_ratio(1) = 0.1

#note vector modes use the scalar settings above

#Initial scalar perturbation mode (adiabatic=1, CDM iso=2, Baryon iso=3,

#neutrino density iso =4, neutrino velocity iso = 5)

initial_condition = 1

#If above is zero, use modes in the following (totally correlated)

proportions

#Note: we assume all modes have the same initial power spectrum

initial_vector = −1 0 0 0 0

#For vector modes: 0 for regular (neutrino vorticity mode), 1 for magnetic

vector_mode = 0

#Normalization

COBE_normalize = F

##CMB_outputscale scales the output Cls

#To get MuK

^{2}set realistic initial amplitude (e.g. scalar_amp(1) = 2.3e−9

above) and

#otherwise for dimensionless transfer functions set scalar_amp(1)=1 and use

CMB_outputscale = 1

#CMB_outputscale = 7.4311e12

#Transfer function settings, transfer_kmax=0.5 is enough for sigma_8

transfer_filename(1) =

#Matter power spectrum output against k/h in units of h

^{3}Mpc

^{−3}

transfer_matterpower(1) =

#21cm C

_{l}for sharp window

transfer_cl_filename(1) =

#Output files not produced if blank. make camb_fits to use use the FITS

setting.

scalar_output_file = scalCls.dat

scalar_covariance_output_file = scalCovCls.dat

vector_output_file = vecCls.dat

tensor_output_file = tensCls.dat

total_output_file = totCls.dat

lensed_output_file = lensedCls.dat

FITS_filename = scalCls.fits

##Optional parameters to control the computation speed,accuracy and feedback

#If feedback_level > 0 print out useful information computed about the model

feedback_level = 1

# 1: curved correlation function, 2: flat correlation function, 3: inaccurate harmonic method

lensing_method = 1

accurate_BB =T

#Recombination calculation: 1: RECFAST, 2: RECFAST+astro-ph/0501672

corrections

recombination = 1

#Whether you are bothered about polarization.

accurate_polarization = T

#Whether you are bothered about percent accuracy on EE from reionization

accurate_reionization = T

#whether or not to include neutrinos in the tensor evolution equations

do_tensor_neutrinos = F

#if true, get accurate gas temperature evolution given recombination model including

#approximate perturbed recombination; also affects baryons for k >~ 300/Mpc.

evolve_delta_xe = F

#Computation parameters

#if number_of_threads=0 assigned automatically

number_of_threads = 0

#Default scalar accuracy is about 0.3% (except lensed BB).

#For 0.1%-level try accuracy_boost=2, l_accuracy_boost=2.

#Increase accuracy_boost to decrease time steps, use more k values, etc.

#Decrease to speed up at cost of worse accuracy. Suggest 0.8 to 3.

accuracy_boost = 1

#Larger to keep more terms in the hierarchy evolution.

l_accuracy_boost = 1

#Increase to use more C

_{l}values for interpolation.

#Increasing a bit will improve the polarization accuracy at l up to 200 -

#interpolation errors may be up to 3%

#Decrease to speed up non-flat models a bit

l_sample_boost = 1