Planck meets the Lyman-α forest

Transcription

1 Planck meets the Lyman-α forest Jose Oñorbe Max Planck Institute for Astronomy Collaborators: J. Hennawi (MPIA), Z. Lukić (LBNL), A. Rorai (IoA), G. Kulkarni (IoA) June 15, 2016 Meeting on Fundamental Cosmology, Barcelona

2 The CMB constraints on Reioniation Planck Collaboration (2016a, 2016b) Jose Oñorbe 2

3 Reioniation sets up the Thermal State of the IGM Balance of photoheating and adiabatic cooling gives a T relationship: T ( ) = T 0 γ 1 (Hui & Gnedin, 1997) 7.0 = (Oñorbe+in prep) log10 (T/K) log p. d. f. T0/1E4 (K) HeII reioniation HI reioniation log 10 (ρ b / ρ b ) Measure thermal evolution of the IGM to constrain reioniation history 2 T IGM determines galaxy formation (minimum galaxy mass, halo baryon content) Jose Oñorbe 3

4 The Thermal History of the Universe: Jeans Scale Gas pressure can counterbalance gravitational collapse DM density gas density (Kulkarni,Oñorbe+2015) Gas traces large-scale distribution of dark matter, but small-scale fluctuations suppressed by pressure: λ Jeans = c s π/gρ 200ckpc In IGM sound crossing time comparable to the Hubble time λ P /c s t H pressure scale depends on the full thermal history: λ f (T [])d (Gnedin & Hui 1998) Jose Oñorbe 4

5 Thermal parameters affect the Lyman-α statistics Credit video: A. Rorai Lyman-α forest Power Spectrum Thermal broadening cut-off T = T 0 γ 1 Jose Oñorbe 5

6 Thermal parameters affect the Lyman-α statistics Credit video: A. Rorai Lyman-α forest Power Spectrum Pressure smoothing cut-off T = T 0 γ 1 Jose Oñorbe 5

7 Simulating the Lyman-α forest Low density hydro + gravity, CMB gives initial conditions Nyx massively parallel grid hydro code (Almgren+ 2013; Lukic+ 2015). A Mpc/h run costs cpu-hrs UV Background uniform and isotropic (Haardt & Madau 2012, Faucher-Giguere+2009) Jose Oñorbe 6

8 Problem with Standard UV models xe τe Haardt & Madau 2012 model τ = Haardt & Madau 2012 sim. τ = τ e () 0 n e( )d Jose Oñorbe 7

9 Problem with Standard UV models xe τe Standard UV models reionie and heat the gas too early!! Haardt & Madau 2012 model τ = Haardt & Madau 2012 sim. τ = T 0 /1E4 (K) Why? Overestimated λ mfp at high- Haard & Madau 2012 sim Jose Oñorbe 7

10 New Self-Consistent UVB Models (Oñorbe+2016a) xe τe early reion. middle reion. late reion γ T0 (10 4 K) Haardt & Madau 2012 late reion. middle reion. early reion. Bolton et al Becker et al (flat prior on γ) Becker et al (γ from Bolton et al. 2014) Boera et al (γ from Bolton et al. 2014) Lid et al Input free parameters for the model Ioniation History: reion, Total Heat Input: T Tables publicly available for your favorite hydro code Jose Oñorbe 8

11 New Self-Consistent UVB Models (Oñorbe+2016a) xe τe early reion. middle reion. late reion T( ) (10 4 K) λp (ckpc) Haardt & Madau 2012 sim. late reion. middle reion. early reion. Becker et al Boera et al Input free parameters for the model Ioniation History: reion, Total Heat Input: T Tables publicly available for your favorite hydro code Jose Oñorbe 8

12 New Self-Consistent UVB Models (Oñorbe+2016a) γ middle reion. cold HI THI = K middle reion. THI = K middle reion. warm HI THI = K middle reion. hot HI THI = K Bolton et al γ middle reion. No HeII THeII = 0. 0 K middle reion. cold HeII THeII = K middle reion. THeII = K middle reion. warm HeII THeII = K middle reion. hot HeII THeII = K Bolton et al T0 (10 4 K) Becker et al (flat prior on γ) Becker et al (γ from Bolton et al. 2014) Boera et al (γ from Bolton et al. 2014) Lid et al T0 (10 4 K) Becker et al (flat prior on γ) Becker et al (γ from Bolton et al. 2014) Boera et al (γ from Bolton et al. 2014) Lid et al Input free parameters for the model Ioniation History: reion, Total Heat Input: T Tables publicly available for your favorite hydro code Jose Oñorbe 8

13 New Planck constraints and Lyman-α statistics at high τ = xe τe (Oñorbe+2016b) T0 (10 4 K) Planck 2016 τ e value, T HI = K λp (ckpc) τ = Jose Oñorbe 9

14 New Planck constraints and Lyman-α statistics at high τ = xe τe (Oñorbe+2016b) T0 (10 4 K) λp (ckpc) THI = K THI = K THI = K THI = K Same ioniation history, different HI heat input Jose Oñorbe 9

15 New Planck constraints and Lyman-α statistics at high xe τe τ = τ = τ = τ = (Oñorbe+2016b) T0 (10 4 K) λp (ckpc) τ = τ = τ = τ = Same HI heat input, different ioniation history Jose Oñorbe 9

16 HI Reioniation Constraints from = 5 Lyman-α 10 0 =5.00 kp(k)/π Oñorbe+2016b 10-1 τ = Viel et al. 2013a k (s/km) Jose Oñorbe 10

17 HI Reioniation Constraints from = 5 Lyman-α 10 0 =5.00 kp(k)/π 10-1 T HI = K T HI = K T HI = K T HI = K Viel et al. 2013a Oñorbe+2016b k (s/km) = 5 observations point towards a hotter IGM (higher heat input during HI reioniation) Jose Oñorbe 10

18 HI Reioniation Constraints from = 5 Lyman-α 10 0 =5.00 kp(k)/π 10-1 τ = τ = τ = τ = Viel et al. 2013a k (s/km) Oñorbe+2016b = 5 observations point towards a hotter IGM or an earlier reioniation (2σ from Planck) Jose Oñorbe 10

19 At 6 the IGM is more sensitive to HI reioniation =6.00 = kp(k)/π 10-1 τ = τ = τ = τ = mock observations ±1σ k (s/km) kp(k)/π 10-1 THI = K THI = K THI = K THI = K mock observations ±1σ k (s/km) Data points: mock observations ( = 4) for the T HI = K model We have started to compile a sample of high S/N quasars at 6.1 Jose Oñorbe 11

20 Degeneracy with Cosmological Parameters 10 0 =5.00 =5.00 kp(k)/π kp(k)/π 10-1 A: σ8 = Ωm = B: σ8 = Ωm = C: σ8 = Ωm = D: σ8 = Ωm = Viel et al. 2013a 10-1 Planck 2015 τe, CDM Planck 2015 τe, 3.0 kev Thermal Planck 2015 τe, 2.0 kev Thermal Planck 2015 τe, kev Thermal Viel et al. 2013a k (s/km) k (s/km) hotter IGM denerated with Warm Dark matter effects but very different evolution Jose Oñorbe 12

21 Take away messages 1 The Lyman-α forest allows us to study the thermal state of the IGM HI and HeII reioniation 2 = 5 Lyman-α 1D Power spectrum points towards higher IGM temperatures or a higher τ e values for current Planck constraints. A = 6 measurement will be very helpful to confirm this picture. 3 Lower warm dark matter mass hotter IGM (or earlier reioniation) but different redshift evolution. Jose Oñorbe 13