Cosmology with the SZE

Transcription

1 Vulcano Workshop 2010 May 24, 2010 Cosmology with the SZE News & Views Sergio Colafrancesco ASI-ASDC INAF- OAR 1

2 Cosmological scenario Main parameters Probe Geometry: Ωk,0 Matter/Energy ΩDE - Dark ΩDM - Ordinary: Ωb Ων Scales: H0 Dynamics: ä/a Eq. of state: w T/S ratio: r Power spec: σ8 ns Reionization zr CMB SN-BAO WL CL CMB SNe SNe SN-BAO CMB CL-WL CMB-CL CMB SN-CL

3 Cosmological scenario Main parameters Probe Geometry: Ωk,0 Matter/Energy ΩDE - Dark ΩDM - Ordinary: Ωb Ων Scales: H0 Dynamics: ä/a Eq. of state: w T/S ratio: r Power spec: σ8 ns Reionization zr CMB SN-BAO WL CL CMB SNe SNe SN-BAO CMB CL-WL CMB-CL CMB SN-CL SZ

4 The SZ Effect S.Colafrancesco 2007, NewAR, 51, 394 Beyond the Standard Lore of the SZ effect y(pe,ℓ) = Comptonization factor ğ(ν,t0,pe) = Spectral distribution Thermal I(x) I0(x) Irel(x) Relativistic thermal NR e - relativistic e- ν kt 4 e2 ν me c ν 4 2 γ ν 3

5 SZE: Observational fact This This

6 The origin of the SZ effect Non-coherent Compton Scattering Fall-out effect of the Cold War 1957 A.S. Kompaneets publishes his Compton scattering Fokker-Planck equation (derived by A.S. Kompaneets in Soviet Union 1950 but was classified due to nuclear bomb research until 1956) 1 Ya. B. Zel dovich & R. Sunyaev derive the thermal SZ effect (i.e., applied the Kompaneets eq.)

7 SZE: general relativistic derivation [Colafrancesco et al. 2003, A&A, 397, 27] Intensity change Pressure Thermal Relativistic Spectral shape Redistribution function P( s) = dpf ( p) P (s; p) e 0 s

8 SZE from various e- populations SZth SZwarm SZkin SZE amplitude: degeneracy in physical parameters SZrel SZE spectra: sensitivity to physical parameters SZDM P( s) = 0 dpf e ( p ) Ps ( s; p) = hν KTCMB

9 Physics with the SZE: thermal plasma (kt0 ) 3 I th = 2 yth g ( x) 2 (hc) T d ne kte me c 2 X 0,th a + bθ e + cθ e2 k T θ e B e2 me c g (x) yth = σ Temperature Pressure Density The best way to measure Te are: - SZE at high frequencies (> 300 GHz) - spectral slope around 220 GHz [Colafrancesco, Prokhorov, Dogiel 2009]

10 Astrophysics & Cosmology The SZE is independent of redshift and therefore it is an optimal tool for Cosmological applications Standard-rod physical effect ~ n kt X-rays ~n2(kt)1/2 X-rays X-rays The SZE depends directly on the electron distribution in the atmospheres of cosmic structures and therefore it is an optimal tool for Astrophysical applications

11 Astrophysical relevance Galaxy clusters Thermal particles Ee kev AGN jets/cavities DM nature Plasma physics B-fields Cluster Cavities MS (Chandra) SZE WIMPs Mχ GeV 1ES Radio Galaxy Lobes 3C432 (Chandra) Acceleration proc. Power-law Cosmic rays Ee 16GeV Bµ1/2(νGHz)1/2 Maxwellian

12 Cosmological relevance Galaxy clusters Hubble diagram AGN jets/cavities TCMB(z) DM nature Plasma physics Baryon fraction SUSY DM Excluded by WMAP Excluded by BBN ded Exclu 3C432 T (ktcmb ) 3 FIC γ (α 1) min α 1) / 2 E X (min Excluded by WMAP Light DM Cluster counts ΩDM ΩDE RG Excluded by BBN SNe C oma CR fraction Excluded by BBN TCMB(z) E in C b y SZ WMAP (95%) e- anomalous magnetic moment Bremsstrahlung in-flight annihilation WHIM

13 A few exemplary cases (Cosmology) Cosmological scenario ΛCDM model: cosmological parameters Extended-G model: ModG scales TCMB(z) Galaxy clusters (thermal SZE) RGs (non-thermal SZE) DM nature SZDM effect

14 Relevant Cosmic Parameters

15 Clusters: cosmological probes N(M,z) [#/M V] Clusters are excellent Cosmo-evolu-meters Understand their physics M proxy (DM, baryons, Galaxy feedback, CRs, B-field) YSZ Y~ n T Derive their total gravitational mass YSZ Mtot Collect large, unbiased catalogues N(YSZ,z) N(M,z)15

16 SZE: Cosmology ΛCDM model DE model Sensitivity to the DE equation of state Good DE probe if Mtot well sampled SZE

17 SZE Clusters and DE probes DE probes SZE from space SZE in galaxy clusters eliminates weaknesses & systematics SZE optimal tool

18 SZE spectroscopy: T-profiles [Colafrancesco & Marchegiani 2009] SZE spectroscopy will allow to derive spatially resolved T-profiles for nearby clusters out to large distances: Perseus Inversion Technique SZE T, τ, Vp, TCMB T profile with uncertainties similar to those of X-ray observations SZE X-Ray T profile uniquely sampled in the outer parts of the cluster Determination of temperature and density profiles from SZE observations will allow to estimate the total mass of the cluster, including the outer regions. Lensing (total mass) X-rays Unbiased probes for Cosmology SZE

19 SZE: modified G Hilbert-Einstein action in f(r) models [Capozziello, Colafrancesco, DeLaurentis, Milano 2010] Variance Increase at high-m ModG1 ModG2 Modified-G potential Modified-G mass assembly

20 Mod-G vs DE: SZ Clusters + SNe Mod-G (DGP) SNe Clusters (SZE) SNe + SZ clusters can distinguish ModG from DE models Need ~200 clusters in bins of width z = 0.1 [Tang et al. 2006]

21 CMB temperature

22 TCMB(z) (From Lima et al. 2000)

23 Clusters: TCMB(z) from SZE spectra Four unknown TCMB(z) Vr τ Te Full SZE spectrum GHz [Colafrancesco et al. 2010] x= hν ktcmb (z ) kte θe = me c 2

24 RGs: TCMB(z) from SZE + X-rays [Colafrancesco 2008] 3C432 IC emission from lobes AGN central source TSZ (ktcmb ) 3 γ FIC (α 1) min α 1) / 2 E X (min measure TCMB(z)

25 SZE and TCMB(z) Clusters RGs Probe energy release mechanisms at high-z with the SZE (Colafrancesco et al. 2010)

26 SZE and Dark Matter nature

27 1ES Dark Matter Hot gas

28 SZDM from 1ES

29 Neutralino mass (ν=223 GHz) Frequency (Mχ= 20 GeV) Isolating SZDM at 223 GHz [S.C. et al. 2007]

30 Cosmology vs. Astrophysics

31 SZ & Cosmology: astrophysical caveats X-ray gas models overpredict SZE Gas pressure gas emissivity [Diego & Partridge 2009; Bonamente et al. 2007] [Malu et al. 2010; Massardi et al. 2010] Estd. ATCA+ROSAT Lack of detailed knowledge of cluster physics is a limitation to the use of SZE for cosmology Obsv. X-ray gas modeling Gas clumpiness Non-thermal phenomena ATCA+Chandra

32 mm frequency Herschel SPIRE view of Bullet cluster 250 µm 350 µm 500 µm Large impact of point sources at mm frequency [Zemkov et al. 2010]

33 Spatially resolved spectroscopic SZE RXJ

34 Spatially resolved spectroscopic SZE RXJ Single-T gas Multi-T gas AGN non-th

35 News and Views New ideas New technology

36 SZE probe in cluster atmospheres x0 = x0 ( Pe ) x0 = x0 ( Pe ) SZth Degenerate w.r.t. Vp, ECR, MDM, PWHICM i( x) Slope = x Unbiased probe at ~x0 SZwarm SZkin SZrel Continuous spectroscopy SZDM Wide ν-band spectroscopy High-ν spectroscopy [Colafrancesco, Prokhorov, Dogiel 2009] = hν KTCMB

37 Observational requirements Thermal SZE spectra ) A low-ν band to determine the verall amplitude of the SZE that is roportional to y = dl n T mainly depending on τ = σt dl n insensitive to T) 3) A high-ν band to determine the electron temperature T from the shape of the SZ spectrum ( highly sensitive to T) 2) A medium-ν band to determine the crossover of the spectrum that allows to obtain information on - electron pressure Pe - TCMB(z) - Vpec ) Very high-ν band to monitor the oregrounds Galaxy, Point-like Sources) Bands:

38 Observational requirements Thermal SZE spectra ) A low-ν band to determine the verall amplitude of the SZE that is roportional to y = dl n T mainly depending on τ = σt dl n insensitive to T) Batm>10K 3) A high-ν band to determine the electron temperature T from the shape of the SZ spectrum ( highly sensitive to T) 2) A medium-ν band to determine the crossover of the spectrum that allows to obtain information on - electron pressure Pe - TCMB(z) - Vpec ) Very high-ν band to monitor the oregrounds Galaxy, Point-like Sources) Bands:

39 State of the Art so far SPT Deep integrations, high resolution, ~103 deg2 survey. - No access to positive peak of SZE (ν>300 GHz) - No spectroscopy. SZ + LABOCA - No spectroscopy GHz - Different instruments PLANCK In contrast, we would need Full sky, but shallow survey. A few thousand clusters with low-moderate S/N ratio. Low-Moderate spatial resolution Spectroscopic capabilities Wider & continuous frequency coverage Better calibration (no multi-band, no atmosphere) Better knowledge of foregrounds first time first time first time

40 SZE in Space PLANCK OLIMPO MILLIMETRON Millimetron 3m 3 m dish Passive cooling (50 K) Θ= arcmin Noise=18 mjy/ Hz Spectroscopy Large-survey mode Pointed mode MILLIMETRON 12m 12m dish 3m dish 12 m dish Active cooling (4 K) Θ< arcmin Noise<0.1 mjy/ Hz Spectroscopy Polarimetry Super VLBI Observatory mode Small-survey mode

41 SZE spectroscopy: precision COMA in SZE: Current data (Battistelli et al. 2003, ApJ 598, L75) MILLIMETRON (3m) 10 min. exposure R=20 OVRO WMAP MITO MILLIMETRON (12m) 10 min. exposure R=100 x hν / ktcmb [Colafrancesco 2004]

42 SZE spectroscopy: physics Low-resolution space spectrometer vs. ground based multiband (3-BP) 3-BP Millimetron (3 m.) Millimetron (12 m.) Spectroscopic capabilities will allow to separate the cluster parameters: nne e TTee Vpp TTCMB CMB - the main physical quantities of the cluster thermal plasma (density ne, temperature Te) - the cluster peculiar velocity Vp - the value of the CMB temperature TCMB(z) at the cluster redshift z All with good precision (independent derivation!)

43 SZE: resolving cluster atmospheres X-ray MS m. 12 m. 150 GHz 150 GHz 350 GHz 350 GHz R=100 Millimetron

44 SZE: spectro-polarimetry Polarizations arises as a natural outcome of electron-radiation scattering various polarizations Polarization due to transverse motion of clusters Polarization in galaxy clusters due to transverse motions of plasma within the cluster Polarization in galaxy clusters due to multiple scattering γ-e within the cluster Other polarization effects 0.1β t2τ 0.01β t τ kt τ me c 2 2

45 SZE polarization: general formalism Polarization due to galaxy clusters transverse motion Polarization due to transverse motions of plasma within the cluster Polarization due to multiple scattering γ-e within the cluster β tτ 2 β τ 2 t kt τ 2 mc 2

46 SZE: spectro-polarimetry kpsz Qp kpsz tpsz tpsz tpsz f(x) SZth SZkin Qp x [Sazonov & Sunyaev 1999] [Colafrancesco et al. 2010]

47 Cosmology & mm s DE ModG DM LSS SZE BH 5 THz 100 GHz SFR PA

48 THANKS for your attention