CMB lensing and delensing - kiss. · PDF fileGoals for CMB lensing/delensing •4-pt...

Click here to load reader

  • date post

    07-Nov-2018
  • Category

    Documents

  • view

    213
  • download

    0

Embed Size (px)

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