CMB lensing and delensing - kiss. · PDF fileGoals for CMB lensing/delensing •4-pt...
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Transcript of CMB lensing and delensing - kiss. · PDF fileGoals for CMB lensing/delensing •4-pt...
CMB lensing and delensing
Anthony Challinor and Olivier Dor
Current state of the art
Planck Collaboration 2016
4,000 resolved modesS/N = 40 (power spectrum)
Where we want to be
>105 resolved modesS/N > 300 (power spectrum)
TT/EB dominance in future
EB particularly helpful for pol. noise < 5 K arcmin- Polarization reconstructions less susceptible to extragalactic contamintion (e.g., tSZ) but more so to Galactic foregrounds
S/N = 40 S/N > 300
Goals for CMB lensing/delensing
4-pt x (neutrino mass etc.)
3-pt xLSS (growth of structure, dark energy, mitigation of systematics/self-calibration)
Delensing (improve inflation constraints + Neff etc.)
Halo lensing (cluster mass calibration at high redshift)
Issues addressed in this session
How do we achieve these goals?
Survey requirements (resolution, sensitivity, frequency coverage, sky coverage)
Space or ground?
An ultimate diffuse lensing mission?
Sensitivity and resolution
EB
TT
S
N
2
= fsky
X
L
2L+ 1
2
CL
CL +N(0)
L
!2
=N
modes
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
Pol. noise level
Cosmology from x
Neutrino masses
0 500 1000 1500 2000 2500`
0.10
0.05
0.00
0.05
0.10
C
`(
m)
C
`(
m=
0)C
`(
m=
0)
m = 60 meV
m = 120 meV
S3-wide
S4
104 103 102 101 100
k [h Mpc1]
0.30
0.25
0.20
0.15
0.10
0.05
0.00
0.05
P
m(k
)
P
m=
0(k)
P
m=
0(k)
m = 0.1 eV
m = 0.2 eV
m = 0.3 eV
Allison+ 2015
Complementary to optical weak lensing- Higher-z, mostly linear regime, no intrinsic-alignment issues
Comparable precision on neutrino mass to e.g., Euclid lensing
Parameter degeneracies for mn
0.1185 0.1200 0.1215
ch2
0.05
0.10
0.15
0.20
m
[e
V]
65.6 66.4 67.2 68.0
H0
0.056 0.060 0.064
2.100 2.115 2.130 2.145
109As
CORE CORE+BAO
X
m= 44meV CORE
X
m= 17meV +BAO
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
Constraint on t important: degrades to 30 meV with Planck prior s(t) = 0.01
Cosmic-variance-limited t [s(t) = 0.002] becomes limiting for Nmodes > 105
Issue I: extragalactic foregrounds Issue in T-based reconstruction tSZ and CIB
- tSZxtSZx and (tSZ)4 both important (van Engelen+ 2014) Mitigation:
- Masking (loss of signal for tSZ)- Modelling (e.g., Planck for unclustered sources)- tSZ nulling (on gradient leg; Madhavacheril & Hill 2018)
0 500 1000 1500 2000 2500 L
0.06
0.04
0.02
0.00
0.02
0.04
0.06
Fra
ctio
nal
CM
B L
ensi
ng B
ias
Standard masking, lmax = 3000
0 500 1000 1500 2000 2500 3000L
Aggressive masking, lmax = 2500
CIB2 corr.tSZ2 corr.CIB 4pt.tSZ 4pt.5 mJy
5x1014 Msol1 mJy1x1014 Msol
150 GHz
van Engelen+ 2014
Issue 2: Galactic foregrounds
Main issue for EB reconstruction
Care (mainly) about 4-pt non-Gaussianity on intermediate and small scales
- Very limited empirical information on these scales
Mitigation:- Multi-frequency cleaning- Local analysis with foreground power included in lensing filters to downweight contaminated modes
Results on 150 GHz simulations
Data-derived simulations (Planck FFP8) but do not capture small-scale NG from small-scale B field
No dust Worst 600-deg2 dust field Dust inc. in lensing filters
AC+CORE 2017
Requirements for x Mostly care about Nmodes for power spectrum science
- Generally favours large sky coverage at fixed Ndet
Neutrino mass requires precise t measurement- Low-l E-mode polarization from space (e.g., LiteBIRD)- Precision on mass (with BAO) saturates around Nmodes~105- kSZ from patchy reionization (Ferraro & Smith 2018)
Multi-frequency at high resolution prudent but less demanding than for low-l B-mode science
- Need for Galactic simulations properly capturing small-scale non-Gaussianity
Cosmology from xLSS
Giannantonio+ 2016
Growth of structurehCMBi / b(z)D2(z)hi / b2(z)D2(z)
0 500 1000 1500 2000 2500 3000
0.0
0.5
1.0
1.5
2.0
C
CM
Bgal
(
106) Planck
WMAP 9
Hand+2013; see also Liu & Hill 2015
Current detections around 3s Will improve to >50s with e.g., DES 5-yr x SPT-3G X-correlation more immune to additive systematic effects Full joint analysis can calibrate multiplicative bias effects in shape measurement and intrinsic alignments
Kirk+ 2016
Galaxy lensing-CMB lensing
Issue: extragalactic foregrounds
tSZ and CIB are issues in T-based reconstruction Only, e.g., tSZxtSZxLSS now enters Mitigation:
- Masking - Modelling - tSZ nulling (on gradient leg; Madhavacheril & Hill 2018)
h(c+ f, c+ f) LSSi = h(c, c) LSSi+ h(f, f) LSSi= h LSSi+ h(f, f) LSSi
AAAC33icnVJNbxMxEPVuaSkLbQMc