Cosmology with the Square Kilometre Array - Stefano Camera on behalf of Matteo Viel - INDICO @ INAF
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Cosmology with the
Square Kilometre Array
Stefano Camera
Dipartimento di Fisica, Università degli Studi di Torino
on behalf of Matteo Viel
SISSA, Trieste, Italy
SKA cosmology UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
S. Camera & M. Viel | SKA Italy Cosmology with the SKA Bologna | 4 · XII · 2018
SKA cosmology UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
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
SKA cosmology UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
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
SKA cosmology UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
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
SKA cosmology UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
• 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 · 2018SKA cosmology UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
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 · 20183 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 preservedWeak lensing sinergies - II Still Planck and CMB experiments will be driving the constraints, but cross-correlation important
SKA radio weak lensing UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
[SC et al., 2017]
wa
w0
S. Camera & M. Viel | SKA Italy Cosmology with the SKA Bologna | 4 · XII · 2018SKA radio weak lensing UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
[SC et al., 2017]
wa
w0
S. Camera & M. Viel | SKA Italy Cosmology with the SKA Bologna | 4 · XII · 2018SKA radio weak lensing UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
[SC et al., 2017]
wa
w0
S. Camera & M. Viel | SKA Italy Cosmology with the SKA Bologna | 4 · XII · 2018SKA radio weak lensing UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
[SC et al., 2017]
wa
w0
S. Camera & M. Viel | SKA Italy Cosmology with the SKA Bologna | 4 · XII · 2018SKA radio weak lensing UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
[SC et al., 2017]
wa
w0
S. Camera & M. Viel | SKA Italy Cosmology with the SKA Bologna | 4 · XII · 2018Intensity Ma
Hi Intensity
HI intensity mapping UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS
TAURINENSIS
[Bharadwaj et al., 2001; Battye et al., 2004; Loeb & Whyte, 2008]
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS
TAURINENSIS
•
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 · 2018HI intensity mapping UNIVERSITÀ
DEGLI STUDI
DI TORINO
UNIVERSITÀ
DEGLI STUDI
DI TORINO
ALMA UNIVERSITAS ALMA UNIVERSITAS
TAURINENSIS TAURINENSIS
• HI intensity mapping and galaxy Med-Deep Band 2 surveys
S. Camera & M. Viel | SKA Italy Cosmology with the SKA Bologna | 4 · XII · 2018Simulating 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
17Particle 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).You can also read
