mocking the hera 21cm sky - · mocking the hera 21cm sky marcelo alvarez uc berkeley with input...
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Mocking the HERA 21cm Sky
Marcelo Alvarez UC Berkeley
with input from Josh Dillon, Adam Lanman, Adrian Liu,
Aaron Parsons, Jonathan Pober
Mocking the HERA 21cm Sky
Marcelo Alvarez UC Berkeley
with input from Josh Dillon, Adam Lanman, Adrian Liu,
Aaron Parsons, Jonathan Pober
shameless plug…Full-Sky Extragalactic CMB/CIB Mocks & Halo Lightcone Catalog
available atmocks.cita.utoronto.ca
21cm
polarized foregrounds
array/survey configuration
RFI
SKY RESPONSE TO VISIBILITIES
cross-talk
gain errors
realistic beams
RESPONSE TO SKY
ANALYSIS
power spectrum
ionosphere
imaging
cross correlations
higher order statistics
End-to-End HERA Simulation Pipeline
21cm
polarized foregrounds
array/survey configuration
RFI
cross-talk
gain errors
realistic beams
power spectrum
ionosphere
imaging
cross correlations
higher order statistics
End-to-End HERA Simulation Pipeline
SKY RESPONSE TO VISIBILITIES
RESPONSE TO SKY
ANALYSIS
21cm
polarized foregrounds
array/survey configuration
RFI
cross-talk
gain errors
realistic beams
power spectrum
ionosphere
imaging
cross correlations
higher order statistics
End-to-End HERA Simulation Pipeline
Need to understand how actual, non-Gaussianstructures on the sky affect interplay with sample
variance, primary beam sidelobes, foreground contamination, etc.- Jonathan Pober
SKY RESPONSE TO VISIBILITIES
RESPONSE TO SKY
ANALYSIS
1. Representative
2. Wide-field
3. Efficient
4. Correlated with other tracers
End-to-End HERA Simulation Pipeline:Requirements for 21cm Sky Model
21cm
polarized foregrounds
array/survey configuration
RFI
cross-talk
gain errors
realistic beams
power spectrum
ionosphere
imaging
cross correlations
higher order statistics
End-to-End HERA Simulation Pipeline:cal-sky eor map module v0
SKYRESPONSE
TO VISIBILITIESRESPONSE
TO SKYANALYSIS
End-to-End HERA Simulation Pipeline:cal-sky eor map module v0
End-to-End HERA Simulation Pipeline:cal-sky eor map module v0
δ(r| cosmology)
INITIAL CONDITIONS
End-to-End HERA Simulation Pipeline:cal-sky eor map module v0
δ(r| cosmology)
s(1)(r), s(2)(r)
perturbation theory
INITIAL CONDITIONS
DYNAMICAL COEFFICIENTS
End-to-End HERA Simulation Pipeline:cal-sky eor map module v0
δ(r| cosmology)
zreion(r) = F(ζ, Mmin, λmfp)
s(1)(r), s(2)(r)
bubble model (MA & Abel 2012)
perturbation theory
ζ, Mmin, λmfp
INITIAL CONDITIONS
DYNAMICAL COEFFICIENTS
MODEL PARAMETERS
End-to-End HERA Simulation Pipeline:cal-sky eor map module v0
δ(r| cosmology)
zreion(r) = F(ζ, Mmin, λmfp)
s(1)(r), s(2)(r)
bubble model (MA & Abel 2012)
perturbation theory
ζ, Mmin, λmfp
lightcone time slicing
robs
ρ(r), v(r), xHI(r), Ts(r),
etc…
MODEL PARAMETERS
DYNAMICAL COEFFICIENTS
REIONIZATION REDSHIFTS
INITIAL CONDITIONS
OBSERVER POSITION
End-to-End HERA Simulation Pipeline:cal-sky eor map module v0
δ(r| cosmology)
zreion(r) = F(ζ, Mmin, λmfp)
s(1)(r), s(2)(r)
bubble model (MA & Abel 2012)
perturbation theory
ζ, Mmin, λmfp
lightcone time slicing
robs
map projection
tiling
INITIAL CONDITIONS
MODEL PARAMETERS
DYNAMICAL COEFFICIENTS
REIONIZATION REDSHIFTS
ρ(r), v(r), xHI(r), Ts(r),
etc…
OBSERVER POSITION
End-to-End HERA Simulation Pipeline:cal-sky eor map module v0
δ(r| cosmology)
zreion(r) = F(ζ, Mmin, λmfp)
s(1)(r), s(2)(r)
bubble model (MA & Abel 2012)
perturbation theory
ζ, Mmin, λmfp
lightcone time slicing
robs
map projection
δTb(n, ν)ˆ tiling
INITIAL CONDITIONS
MODEL PARAMETERS
DYNAMICAL COEFFICIENTS
REIONIZATION REDSHIFTS
ρ(r), v(r), xHI(r), Ts(r),
etc…
OBSERVER POSITION
End-to-End HERA Simulation Pipeline:cal-sky eor map module v0
δ(r| cosmology)
zreion(r) = F(ζ, Mmin, λmfp)
s(1)(r), s(2)(r)
perturbation theory
initial conditions
reionization redshifts
ζ, Mmin, λmfp
model parameters
dynamical coefficients
lightcone time slicing
robs
observer position
ρ(r), v(r), xHI(r), Ts(r),
etc…
map projection
δTb(n, ν)ˆ tiling
bubble model (MA & Abel 2012)
The Effect of Absorption Systems on Reionization
MA & Abel (2012)arXiv:1003.6132
Minimum Halo mass: Mmin Ionizing photon mean free path: λabs
Ionizing Efficiency: ζ
The Effect of Absorption Systems on Reionization
MA & Abel (2012)arXiv:1003.6132
2 Gpc/h
128 Mpc/h
Timely Application:
21cm x CMB aka
HERA x Simons
δ(r| cosmology)
zreion(r) = F(ζ, Mmin, λmfp)
s(1)(r), s(2)(r)
bubble model (MA & Abel 2012)
perturbation theory
ζ, Mmin, λmfp
MODEL PARAMETERS
lightcone time slicing
robs
ρ(r), v(r), xHI(r), Ts(r),
etc…
map projection
δTb(n, ν=150 MHz)ˆtiling
INITIAL CONDITIONS
DYNAMICAL COEFFICIENTS
REIONIZATION REDSHIFTS
OBSERVER POSITION
TkSZ(n)ˆ
kSZ x 21cm
kSZ x 21cm
kSZ x 21cm
Alvarez (2016)
Cross-correlation Comes from the Doppler
Cross-correlation Comes from the Doppler
MA, Komatsu, Dore, Shapiro (2006)
Background Negligible
ForegroundNegligible
LargeScale
SmallScale
Primary CMB in kSZ
Galactic Synchrotron in 21cm
Linearly BiasedDensity and Velocity
Patchiness in Ionization Fraction
?TkSZ x δTb
(TkSZ)2 x δTb
TkSZ (δTb)2 x
(TkSZ)2 (δTb)2 x
???
fg+bgnoise
bgnoise
fgnoise
Cross-correlation Comes from the Doppler … but is buried behind Primary CMB
Dillon & Parsons (2016)
Squaring T21 will be a Challenge without Imaging
DeBoer et al. (2016)
Summary Efficient pipeline for generating seamless full-sky 21cm intensity maps is ready for end-to-end simulations
Next Steps Begin testing power spectrum estimation
for HERA analysis pipeline
Inject signal maps into imaging pipeline for realistic kSZ cross-correlation
Additional tracers with peak patch halos: CO, CII, LAEs
More Realistic IGM opacity (λabs)and X-ray heating
github.com/marcelo-alvarez/cal-sky
1 10 100arcmin
DeBoer et al. (2016)