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)