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Cosmology with the Square Kilometre Array - Stefano Camera on behalf of Matteo Viel - INDICO @ INAF
Cosmology with the
Square Kilometre Array
                  Stefano Camera
   Dipartimento di Fisica, Università degli Studi di Torino
           on behalf of Matteo Viel
                    SISSA, Trieste, Italy
Cosmology with the Square Kilometre Array - Stefano Camera on behalf of Matteo Viel - INDICO @ INAF
SKA cosmology                       UNIVERSITÀ
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S. Camera & M. Viel | SKA Italy   Cosmology with the SKA          Bologna | 4 · XII · 2018
Cosmology with the Square Kilometre Array - Stefano Camera on behalf of Matteo Viel - INDICO @ INAF
SKA cosmology                                                                          UNIVERSITÀ
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   Publications of the Astronomical Society of Australia (PASA)
   doi: 10.1017/pas.2018.xxx.
                                                                                                             [arXiv:1811.02743]

   Cosmology with Phase 1 of the Square Kilometre Array
   Red Book 2018: Technical specifications and performance forecasts

  David J. Bacon1 , Richard A. Battye2 , Philip Bull3,4,5 , Stefano Camera6,7,8,2 , Pedro G. Ferreira9 , Ian Harrison2,9 ,
  David Parkinson10 , Alkistis Pourtsidou5,1 , Mário G. Santos11,12 , Laura Wolz13 , Filipe Abdalla14,15 , Yashar
  Akrami16 , David Alonso9 , Sambatra Andrianomena11,12,17 , Mario Ballardini11 , José Luis Bernal18,19 ,
  Daniele Bertacca20,36 , Carlos A.P. Bengaly11 , Anna Bonaldi21 , Camille Bonvin22 , Michael L. Brown2 , Emma
  Chapman23 , Song Chen11 , Xuelei Chen24 , Steven Cunnington1 , Tamara M. Davis26 , Clive Dickinson2 , José
  Fonseca11 , Keith Grainge2 , Stuart Harper2 , Matt J. Jarvis9,11 , Roy Maartens1,11 , Natasha Maddox27 , Hamsa
  Padmanabhan28 , Jonathan R. Pritchard23 , Alvise Raccanelli18 , Marzia Rivi14,29 , Sambit Roychowdhury2 ,
  Martin Sahlén30 , Dominik J. Schwarz31 , Thilo M. Siewert31 , Matteo Viel32 , Francisco Villaescusa-Navarro32 ,
  Yidong Xu24 , Daisuke Yamauchi34 , Joe Zuntz35
  1 Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK
   2 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, U.K.
   3 Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA
   4 Radio &
S. Camera  Astronomy    Laboratory,
             M. Viel | SKA Italy    University of California Berkeley,
                                                              CosmologyBerkeley,
                                                                         with theCA 94720, USA
                                                                                  SKA                               Bologna | 4 · XII · 2018
Cosmology with the Square Kilometre Array - Stefano Camera on behalf of Matteo Viel - INDICO @ INAF
SKA cosmology                                                          UNIVERSITÀ
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   Publications of the Astronomical Society of Australia (PASA)
   doi: 10.1017/pas.2018.xxx.
                                                                                                [arXiv:1810.02680]

   Fundamental Physics with the Square Kilometre Array

   P. Bull,§ S. Camera,§ K. Kelley,§ H. Padmanabhan,§ J. Pritchard,§ A. Raccanelli,§ S. Riemer-Sørensen,§
   L. Shao,§ S. Andrianomena, E. Athanassoula, D. Bacon, R. Barkana, G. Bertone, C. Bonvin, A. Bosma,
   M. Brüggen, C. Burigana, C. Bœhm, F. Calore, J. A. R. Cembranos, C. Clarkson, R. M. T. Connors, Á. de la
   Cruz-Dombriz, P. K. S. Dunsby, N. Fornengo, D. Gaggero, I. Harrison, J. Larena, Y.-Z. Ma, R. Maartens, M.
   Méndez-Isla, S. D. Mohanty, S. G. Murray, D. Parkinson, A. Pourtsidou, P. J. Quinn, M. Regis, P. Saha, M.
   Sahlén, M. Sakellariadou, J. Silk, T. Trombetti, F. Vazza, T. Venumadhav, F. Vidotto, F. Villaescusa-Navarro, Y.
   Wang, C. Weniger, L. Wolz, F. Zhang, B. M. Gaensler,† A. Weltman†

   (Author affiliations are listed in §8 at the end of the paper.)

   § Section lead
    † Editor and convenor
S. Camera   & M. Viel | SKA Italy                          Cosmology with the SKA                      Bologna | 4 · XII · 2018
Cosmology with the Square Kilometre Array - Stefano Camera on behalf of Matteo Viel - INDICO @ INAF
SKA cosmology                                                          UNIVERSITÀ
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                                                                                                TAURINENSIS          TAURINENSIS

   Publications of the Astronomical Society of Australia (PASA)
   doi: 10.1017/pas.2018.xxx.
                                                                                                [arXiv:1810.02680]

   Fundamental Physics with the Square Kilometre Array

   P. Bull,§ S. Camera,§ K. Kelley,§ H. Padmanabhan,§ J. Pritchard,§ A. Raccanelli,§ S. Riemer-Sørensen,§
   L. Shao,§ S. Andrianomena, E. Athanassoula, D. Bacon, R. Barkana, G. Bertone, C. Bonvin, A. Bosma,
   M. Brüggen, C. Burigana, C. Bœhm, F. Calore, J. A. R. Cembranos, C. Clarkson, R. M. T. Connors, Á. de la
   Cruz-Dombriz, P. K. S. Dunsby, N. Fornengo, D. Gaggero, I. Harrison, J. Larena, Y.-Z. Ma, R. Maartens, M.
   Méndez-Isla, S. D. Mohanty, S. G. Murray, D. Parkinson, A. Pourtsidou, P. J. Quinn, M. Regis, P. Saha, M.
   Sahlén, M. Sakellariadou, J. Silk, T. Trombetti, F. Vazza, T. Venumadhav, F. Vidotto, F. Villaescusa-Navarro, Y.
   Wang, C. Weniger, L. Wolz, F. Zhang, B. M. Gaensler,† A. Weltman†

   (Author affiliations are listed in §8 at the end of the paper.)

   § Section lead
    † Editor and convenor
S. Camera   & M. Viel | SKA Italy                          Cosmology with the SKA                      Bologna | 4 · XII · 2018
Cosmology with the Square Kilometre Array - Stefano Camera on behalf of Matteo Viel - INDICO @ INAF
SKA cosmology                                          UNIVERSITÀ
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          •     SKA Cosmology SWG (R. Battye & L. Wolz)
               •    Continuum Focus Group (M. Jarvis & D. Parkinson)

               •    HI galaxy surveys Focus Group (P. Bull & N. Maddox)

               •    HI intensity mapping Focus Group (M. Santos & L. Wolz)

               •    Simulations Focus Group (D. Alonso & F. Villaescusa-Navarro)

               •    SKA1-LOW cosmology Focus Group (A. Pourtsidou & J. Pritchard)

               •    Synergies Focus Group (D. Bacon & S. Camera)

               •    Weak lensing Focus Group (M. Brown & I. Harrison)

S. Camera & M. Viel | SKA Italy              Cosmology with the SKA                  Bologna | 4 · XII · 2018
SKA cosmology                                                                          UNIVERSITÀ
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   Publications of the Astronomical Society of Australia (PASA)
   doi: 10.1017/pas.2018.xxx.
                                                                                                             [arXiv:1811.02743]

   Cosmology with Phase 1 of the Square Kilometre Array
   Red Book 2018: Technical specifications and performance forecasts

  David J. Bacon1 , Richard A. Battye2 , Philip Bull3,4,5 , Stefano Camera6,7,8,2 , Pedro G. Ferreira9 , Ian Harrison2,9 ,
            • Main   10 scientific goals 5,1
  David Parkinson       , Alkistis Pourtsidou , Mário G. Santos11,12 , Laura Wolz13 , Filipe Abdalla14,15 , Yashar
  Akrami16 , David Alonso9 , Sambatra Andrianomena11,12,17 , Mario Ballardini11 , José Luis Bernal18,19 ,
                • Dark     energy equation of state up to z = 3 from geometry (BAOs)
  Daniele Bertacca20,36 , Carlos A.P. Bengaly11 , Anna Bonaldi21 , Camille Bonvin22 , Michael L. Brown2 , Emma
  Chapman23 , Song     Chen11 , Xuelei
                • Measurements            Chen  24
                                                   , Steven  Cunnington    1
                                                                             , Tamara M. Davis   26
                                      of the growth of perturbations in linear and nonlinear regimes, Clive Dickinson2
                                                                                                                       , José
  Fonseca11 , Keith Grainge2 , Stuart Harper2 , Matt J. Jarvis9,11 , Roy Maartens1,11 , Natasha Maddox27 , Hamsa
                  28                              23                      18              14,29                             2
  Padmanabhan        , Jonathan
                • Accessing        R.largest
                                 the  Pritchard
                                              cosmic , Alvise
                                                        scalesRaccanelli     , Marzia Rivinon-Gaussianity,
                                                               (isotropy, homogeneity,          , Sambit Roychowdhury
                                                                                                              GR)             ,
  Martin Sahlén30 , Dominik J. Schwarz31 , Thilo M. Siewert31 , Matteo Viel32 , Francisco Villaescusa-Navarro32 ,
                • Measuring
  Yidong Xu24 , Daisuke           the H34
                            Yamauchi    I density  and35bias up to z = 6 to high accuracy
                                          , Joe Zuntz
  1 Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK
   2 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, U.K.
   3 Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA
   4 Radio &
S. Camera  Astronomy    Laboratory,
             M. Viel | SKA Italy    University of California Berkeley,
                                                              CosmologyBerkeley,
                                                                         with theCA 94720, USA
                                                                                  SKA                               Bologna | 4 · XII · 2018
3 surveys proposed

1) a medium deep band2 SKA1-MID         5000 deg2(z
Weak lensing sinergies - I
                                 Medium deep survey with DES 5yrs - WEAK
 GOAL: measure galaxy            LENSING
 shapes requirements that
 have to be obtained in the
 radio are similar to those of
 present optical surveys.
 Ellipticities measured to
 O(1.e-4).
Cross-correlations will be
crucial to get rid of
wavelength dependent
systematics (multiplicative
and additive biases will be
removed - Camera+17),
while constraining power
will be preserved
Weak lensing sinergies - II

Still Planck and CMB experiments will be driving the
constraints, but cross-correlation important
SKA radio weak lensing                                                    UNIVERSITÀ
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                                                                     [SC et al., 2017]

                                  wa

                                                                w0
S. Camera & M. Viel | SKA Italy        Cosmology with the SKA                      Bologna | 4 · XII · 2018
SKA radio weak lensing                                                    UNIVERSITÀ
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                                                                     [SC et al., 2017]

                                  wa

                                                                w0
S. Camera & M. Viel | SKA Italy        Cosmology with the SKA                      Bologna | 4 · XII · 2018
SKA radio weak lensing                                                    UNIVERSITÀ
                                                                            DEGLI STUDI
                                                                            DI TORINO
                                                                                               UNIVERSITÀ
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                                                                            TAURINENSIS          TAURINENSIS

                                                                     [SC et al., 2017]

                                  wa

                                                                w0
S. Camera & M. Viel | SKA Italy        Cosmology with the SKA                      Bologna | 4 · XII · 2018
SKA radio weak lensing                                                    UNIVERSITÀ
                                                                            DEGLI STUDI
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                                                                                               UNIVERSITÀ
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                                                                            TAURINENSIS          TAURINENSIS

                                                                     [SC et al., 2017]

                                  wa

                                                                w0
S. Camera & M. Viel | SKA Italy        Cosmology with the SKA                      Bologna | 4 · XII · 2018
SKA radio weak lensing                                                    UNIVERSITÀ
                                                                            DEGLI STUDI
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                                                                            TAURINENSIS          TAURINENSIS

                                                                     [SC et al., 2017]

                                  wa

                                                                w0
S. Camera & M. Viel | SKA Italy        Cosmology with the SKA                      Bologna | 4 · XII · 2018
Intensity Ma
 Hi Intensity
         HI intensity mapping                                                      UNIVERSITÀ
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                                   [Bharadwaj et al., 2001; Battye et al., 2004; Loeb & Whyte, 2008]
                                                                                                      UNIVERSITÀ
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          •

       ti on
    la
          •    Redshift for free: vobs = 1420 MHz / (1+z)
f
S. Camera & M. Viel | SKA Italy          Cosmology with the SKA                           Bologna | 4 · XII · 2018
HI intensity mapping                                   UNIVERSITÀ
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          •    HI intensity mapping and galaxy Med-Deep Band 2 surveys

S. Camera & M. Viel | SKA Italy      Cosmology with the SKA            Bologna | 4 · XII · 2018
Simulating intensity mapping signal: small scales

             HI put by hand
             at the center of the haloes

          Illustris TNG

                                           Villaescusa-Navarro+18

• Shot noise level in HI quite different from the standard case of galaxies and haloes
good amount of HI substructure within each DM halo

• Note further that numerical convergence of all quantities not fully achieved.
Simulating intensity mapping signal: WDM

                                               Carucci, Villaescusa, MV, Lapi 15

Probably able to rule out a 4 keV WDM model with 5000 hours of observations
at z > 3, while a smaller mass of 3 keV, comparable to present day
constraints, can be ruled out at more than 2    confidence level with 1000
hours of observations at z > 5 - Note that density inside haloes poorly
modelled.
MNRAS 000, 1–11 (2018)      Measuring the ISW effect
                                                                            Preprint 6 December 2018               Compiled using MNRAS LATEX style file v3.0

                                Measuring ISW with next-generation radio surveys

                                                 1,2 ?               1,3
                                Mario
                                1
                                      Ballardini       , Roy Maartens
                                  Department of Physics & Astronomy, University of the Western Cape, Cape Town 7535, South Africa
                                2 INAF/OAS     Bologna, via Gobetti 101, I-40129 Bologna, Italy
                                3 Institute of Cosmology & Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK

                                                                                                                                      gure 5. Example of the reconstruction procedure applied to

                                                                                                                                       uum survey (Scut = 22 µJy), and the bottom panel shows the

                                                                                                                                                                                                       ere ISW ( rec ) is the variance of the true (reconstructed)
                                                                                                                                                                                                      W map. We consider also a second statistical estimator,
                                                                                                                                                                                                      cause the estimator (34) is insensitive to changes in the
                                                                                                                                        ulations data as described in (30). The top panel shows the

                                                                                                                                        ate using CMB temperature in combination with SKA1 con-
                                                                                                                                      put ISW map, the central panel shows the recovered ISW es-

                                                                                                                                      covered ISW estimate using CMB temperature alone. All the
                                6 December 2018
36v1 [astro-ph.CO] 4 Dec 2018

                                                                ABSTRACT
                                                                The late-time integrated Sachs-Wolfe (ISW) signal in the CMB temperature
                                                                anisotropies is an important probe of dark energy when itExample        of theby
                                                                                                                             can be detected     reconstruction
                                                                                                                                                    cross-
                                                                correlation with large-scale structure surveys. Because of their huge volume, surveys
                                                                                                                           procedure applied to simulations
                                                                in the radio are well-suited to ISW detection. We show that 21cm intensity mapping
                                                                and radio continuum surveys with the SKA in Phase 1 promisedata.a ⇠ The
                                                                                                                                      5 left  panelwith
                                                                                                                                         detection,    shows the
                                                                a similar forecast for the precursor EMU survey. In SKA2,  input   ISW galaxy
                                                                                                                              the 21cm    map, redshift
                                                                                                                                                  the central panel
                                                                survey could deliver a ⇠ 6 detection, which is probably the maximum achievable
                                                                                                                           shows
                                                                                                                               radiothe  recovered      ISW

                                                                                                                                      aps have a resolution NSIDE = 32.
                                                                level. Our analysis includes the observational e↵ects on the          surveys  of lensing
                                                                                                                           estimate
                                                                magnification, Doppler and other relativistic corrections. These  e↵ectsusing  CMB
                                                                                                                                         alter the     temperature
                                                                                                                                                    shape
                                                                of the measured ISW signal, especially at high redshift. The cross-correlation between
                                                                lensing magnification and CMB temperature at high redshift in combination
                                                                                                                                is not a direct with
                                                                                                                                                probeSKA1
                                                                                                                                                        of
                                                                dark energy and could bias the ISW reconstruction. Wecontinuum            survey (Scut = 22
                                                                                                                            find that cross-correlation
                                                                between di↵erent redshift bins compensates the shift due to adding the relativistic
                                                                corrections in the ISW detection and improves the qualityµJy),
                                                                                                                            of the and
                                                                                                                                    ISW the   right panel shows
                                                                                                                                         reconstruction.
                                                                                                                   the recovered
                                                                Key words: cosmology: observations – cosmic background              ISW estimate using
                                                                                                                       radiation – large-scale
                                                                structure of Universe.                             CMB temperature alone.

                                1   INTRODUCTION                                                 2007; Ho et al. 2008; Giannantonio et al. 2008; Hernandez-
                                                                                                 Monteagudo 2010; Taburet et al. 2011; Ilic et al. 2011; Schi-
Probing GR at the largest scales

SKA2 should be able to detect the non-standard Doppler contribution to galaxy clustering.
Multi-tracing techniques
Non-Gaussianity

                  17
Particle DM searches

                  radio data is expected to
                  correlate with the gamma-ray
                  sky and can be exploited to filter
                  out the information concerning
                  the composition of the gamma-
                  ray background contained in
                  maps of the unresolved gamma-
                  ray emission.

                  SKA HI galaxies are at low-z
                  and with low shot-noise level, in
                  a regime heavily dominated by
                  astrophysics (spectroscopy is
                  important to get a precise
                  window/filter function).
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