Constraining the IGM thermal state and Cosmology

Transcription

1 Constraining the IGM thermal state and Cosmology Antonella Garzilli IEU, Ewha Womans University 29th November, 2013 with: Prof. Tom Theuns Dr. James Bolton Dr. Tae-Sun Kim Dr. Samuel Leach Dr. Matteo Viel

2 Structure formation

3 [Springel et al., 2003] IGM

4 Outline 1 IGM through Lyα forest 2 Wavelets Method 3 Results

5 Outline 1 IGM through Lyα forest 2 Wavelets Method 3 Results

6 λ α = 1216 Å Lyα forest

7 Typical normalized QSO-spectrum

8 IGM as a probe of galaxy and QSO evolution [Haardt & Madau, 2011] photo-ionization ε = + ν th Γ = + ν th photo-heating 4πj(ν) σ(ν)dν hν 4πj(ν) σ(ν)(hν hν th )dν hν [Becker et al., 2007] [Bolton et Haehnelt, 2007] [Faucher-Giguère et al., 2008b] [Carlverley et al, 2011] [Hui & Haiman, 2003]

9 IGM as a probe of Cosmology [Zaldarriaga et al., 2001] [Seljak et al., 2006] [Viel et al., 2009]

10 IGM Thermal state: Equation of state dn HI dt ρ dt dt = Γn HI + α R n e n HII εn HI Γn HI = α R n e n HII α R n 2 H n HI = α Rn H n H Γ ρ dt dt ε αρ2 Γ dt dt ε Γ ρ power law equation of state T = T 0 γ 1

11 T = T 0 γ 1 Effective Equation of State [Bolton et al., 2008]

12 Measuring γ: Inverted EOS? [Bolton et al., 2008] [Viel et al., 2009] [Calura et al., 2012] T = T 0 γ 1 γ < 1

13 Measuring γ: Theoretical expectations [McQuinn et al., 2009] [Compostella et al., 2013] γ 1.3

14 Thermal state of IGM [Schaye et al., 2000] [Schaye et al., 2000]

15 Current constraints on the IGM Thermal state [Schaye et al., 2000] [Ricotti et al., 2000] [McDonald et al., 2001] [Zaldarriaga et al., 2001] [Lidz et al., 2010] z = 2.4 T 0 = ± 500K γ = 1.46 ± 0.05 [Rudie et al., 2013] γ < 1 [Viel et al., 2009] [Calura et al., 2012]

16 Outline 1 IGM through Lyα forest 2 Wavelets Method 3 Results

17 Wavelets Morlet wavelet [Theuns & Zaroubi, 2000] [Zaldarriaga, 2002] ψ k (v) = A exp( ikv/2π) exp( v 2 /2s 2 ) s = 2π k

18 Wavelets

19 Wavelets and the Lyman α forest 0.9 < < 1.8 for z 3 [Lidz et al., 2010] [Zaldarriaga et al., 2001]

20 Linking theory with observations Observed Spectra 18 spectra from UVES of VLT [Kim et al., 2007] Metal cleaned Continuum fitted Normalized High S/N 50 Hydrodynamical Numerical simulations High resolution numerical simulations (gas + DM) Gadget 3 [Springel, 2005] particles 10 Mpc h 1 boxsize Uniform ultraviolet background [Haardt & Madau, 2001] Interpolation among cosmological and astrophysical parameters Exploration of likelihood function by Multinest [Feroz & Hobson, 2008]

21 Outline 1 IGM through Lyα forest 2 Wavelets Method 3 Results

22 Constraints on IGM thermal state wavelet filtering Flux PDF [Viel et al., 2009] wavelet filtering [Lidz et al., 2010] Garzilli et al, MNRAS, 424: , 2012

23 Constraints on IGM thermal state wavelet filtering wavelet filtering [Lidz et al., 2010]

24 Wavelets filtering & joint analysis [Lidz et al., 2010] [Becker et al., 2011] wavelet filtering wavelet + flux

25 Wavelets filtering & joint analysis II [McDonald et al., 2000] [Ricotti et al., 2000] [Schaye et al., 2000] wavelet+flux [Lidz et al., 2010] HeII reionization at z 6 [McQuinn et al., 2009] L1 [McQuinn et al., 2009] L1b

26

27 A new method for measuring the IGM temperature

28 Gaussian fitting τ e (v v 0 ) 2 2σ 2 σ T

29 Gaussian fitting [Schaye et al., 2000] FLO: From Line to Overdensity [Saitta et al., 2008]

30 Conclusion We implemented a wavelet analysis and applied it to high resolution QSO-spectra at z 3. Constraints of thermal state in agreement with previous results in literature Compatible with an additional source of heating at redshift z < 4