Lyman-alpha intensity mapping during the Epoch of Reionization Mário G. Santos CENTRA IST (Austin, May 15, 2012) Marta Silva, Mario G. Santos, Yan Gong, Asantha Cooray (2012), arxiv:1205.1493
Intensity mapping? Make 3d maps during EoR Not resolving galaxies Measure intensity over many small frequency bands and over a large area of the sky (low angular resolution) Each band will map into an effective Ly line redshift/position along line of sight If Ly is only signal we re done after beating noise Well, need to remove foregrounds, e.g. everything else that falls into the band (coming from lower redshifts) Then make 3d boxes at middle redshift, get 3d power spectrum and you re done! Galaxies Intensity
Sources of Ly emission Continuum Ly- emission from stars Scattering of Ly-n photons in the IGM Hydrogen Recombinations (galaxies and IGM) HI Collisional excitations (galaxies and IGM) Gas cooling (gravitational collapse) Powered by UV emission from stars X-ray emission from Quasars?
Galaxies / IGM First assumption - use a two-medium model: Galaxies Constant temperature Constant ionization fraction closed box IGM Temperature increasing Ionization fraction increasing Should be ionized around galaxies UV escape fraction from galaxies Reionization Ly- escape fraction (no scattering in IGM) HI glow around galaxies?
Ly- from Galaxies: Parameters Ionizing photon rate from stars - relate to Star Formation Rate: Ṅ ion = Q ion SFR Q ion ~ 5.38x10 60 UV photons/m Salpeter IMF Ionizing Fluxes from Shaerer 2002 (POP II, OB stars) 20% error? UV escape fraction: h fesc UV (M,z) =exp (z)m (z)i 20% uncertainty? Razoumov & Sommer-Larsen (2010)
Ly- from Galaxies: Parameters Average number of Ly photons per recombination: f rec ~ 0.66 (Gould & Weinberg, 1996) + 2-photon emission Ly escape fraction (related to dust absorption) f Ly esc (z) =C dust 10 3 (1 + z) Cdust ~ 3.34» ~ 2.57 Mass dependence? Hayes et al. (2011)
Ly- from Galaxies Hydrogen Recombinations: Ṅ Ly = f Ly esc A He f rec (1 f UV esc ) Ṅion L Gal rec 4.04 10 8 [1 f UV esc (M,z)]fesc Ly (z) SFR(M,z) M yr 1 L Collisions - Heating/excitations: he i 21.4eV SED from Maraston (2005) ~ 1% for Ly through excitations (Gould & Weinberg 96) L Gal exc 1.05 10 8 [1 f UV esc (M,z)]fesc Ly (z) SFR(M,z) M yr 1 L
Ly- from Galaxies Continuum emission: Average number of photons connect to UV emission/reionization: Q Ly 0.63 Q ion L Gal (SED from OB stars) cont 4.63 10 8 fesc Ly (z) SFR(M,z) M yr 1 L Cooling gas collapse (negligible): L Gal cool(m) 44fesc 1+ Ly M10 8 1+ 2.1 M 2 10 10 1+ 3 M 3 10 13 L
Galaxies - SFR 1.5 log 10 ( SFRD [M yr 1 Mpc 3 ] ) 2.0 2.5 3.0 3.5 4.0 4.5 6 7 8 9 10 11 12 13 14 z Top right: Solid lines - our model Dotted lines - catalogue from Guo et al. (2011) Top left: SFR density using our simulation (red points from Bouwens et al. 2011) Bottom: Obtained ionization fraction (x i ~ 0.9 at z=7 and τ~ 0.07) x i 1.0 0.8 0.6 0.4 0.2 0.0 6 7 8 9 10 11 12 13 14 z
Intensity from Galaxies 0 1 10 2 GAL : teo GAL : K98 log 10 [n(l >)(Mpc 3 )] 2 3 4 5 6 z = 6 z = 7 Ouchi2008: z = 5.7 Kashikawa2006: z = 5.7 Kashikawa2006: z = 6.6 40.0 40.5 41.0 41.5 42.0 42.5 43.0 43.5 44.0 log 10 [L Lyα (erg s 1 )] Luminosity functions Green/blue - with our SFR model Yellow/black/red - observations with Schechter function fits Ī Gal (z) = Z Mmax M min dm dn dm L Gal (M,z) 4 H(z) νiν[nwm 2 sr 1 ] Ly 10 3 SFR à H à Ly 7.0 7.5 8.0 8.5 9.0 9.5 10.0 10.5 11.0 z Total Ly intensity from galaxies blue - analytical calculation using our luminosities yellow - using the empirical relation from Jiang et al. (2011): L Gal K98 2.9 10 8 SFR(M,z) M yr 1 L
More Luminosity constraints (from Sobral et al. 2009)
Ly Power Spectrum from Galaxies Assume: I GAL = b Ly Ī GAL m (x) b Ly (z) = R Mmax M min R Mmax dm dn dm L GAL b(z,m) M min dm dn dm L GAL 10 1 z = 10 z = 9 z = 8 z = 7 5.0 LdbLyα/dL 10 0 blyα(z) 4.5 10 1 4.0 10 2 10 6 10 7 10 8 10 9 L Lyα [L ] 6.0 6.5 7.0 7.5 8.0 8.5 9.0 9.5 10.0 z
Ly Power Spectrum from Galaxies k 3 P(k)/2π 2 [nwm 2 sr 1 ] 2 10 1 10 2 10 3 10 4 10 5 cont rec exc total K98 z = 7 k 3 P(k)/2π 2 [nwm 2 sr 1 ] 2 10 1 10 2 10 3 10 4 10 5 10 6 10 7 cont rec exc total K98 z = 10 10 6 10 1 10 0 10 1 k[h/mpc] 10 8 10 1 10 0 10 1 k[h/mpc] Analytical calculation Continuum emission from stars dominates At k ~ 1 Mpc -1 (R ~ 9 Mpc), rms ~ 0.03 nwm -2 sr -1
Ly IGM intensity Analytical calculations Processes: Recombinations Radiative cooling Ly-n scattering Depends on: Ionization fraction Gas temperature matter density νiν[nwm 2 sr 1 ] 10 2 10 3 10 4 10 5 10 6 10 7 10 8 10 9 10 10 10 11 10 12 10 2 10 1 10 0 x i 10 2 T K = 20000 K : exc T K = 20000 K : rec T K = 50000 K : exc T K = 50000 K : rec T K (x i ) : exc T K (x i ) : rec Need to connect to UV photons that escape galaxy and SFR Need simulations! νiν[nwm 2 sr 1 ] 10 3 Total IGM : T K (x i ) IGM : T K = 20000 K 10 4 IGM : T K = 50000 K GAL GAL : e A(z) = ±0.2A(z) 10 1 10 0 x i
Seminumerical simulation 26 z=7 Modified version of SimFast21 (Santos et al. 2010, www.simfast21.org) Start with density field y[mpch 1 ] 0-26 -26 0 26 x[mpch 1 ] 0.8 0.4 0.0 0.4 0.8 1.2 1.6 2.0 δ
26 z=7 Get halos (Sheth & Tormen) Minimum 10 8 M Relate to SFR using previous model y[mpch 1 ] 0-26 -26 0 26 x[mpch 1 ] 4.0 3.6 3.2 2.8 2.4 2.0 1.6 1.2 0.8 0.4 0.0 Log SFR (M yr 1 )
Relate emission for UV, X- ray and Lyn photons to SFR Assume POP II type stars 26 z=7 Integrate temperature: X-ray heating (IGM), see Santos et al. 2008/2010 Photoionization heating (HII bubbles) Adiabatic cooling (no other cooling sources) y[mpch 1 ] 0 At same time generate HII bubbles in a given region using condition: N ion N HI +N HeI (with excursion-set algorithm, e.g. Furlanetto et al. 2006) Use f esc! Take into account Recombinations (using temperature, n_ HII ) Add back recombined HI to bubble -26-26 0 26 x[mpch 1 ] 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 x i =0.84
26 z=7 Use same prescription to relate Ly emission from Galaxies to SFR Calculate IGM Ly luminosity density from recombinations and excitations/heating (direct excitations negligible) y[mpch 1 ] 0 Calculate luminosity density from scattering of Lyn photons in the -26 IGM -26 0 26 x[mpch 1 ] 4.0 3.2 2.4 1.6 0.8 0.0 0.8 1.6 log10[νi ν (nwm 2 sr 1 )]
Ly at z=10 26 z=10 26 z=10 Note: Ionized bubbles contribute to IGM because they are not 100% ionized main contribution in IGM from excitations through heating y[mpch 1 ] y[mpch 1 ] 0-26 -26 26-26 0 26-26 0 26 x[mpch 1 ] x[mpch 1 ] 0 z=10 0.8 0.4 0.0 0.4 0.8 1.2 4.0 1.6 3.6 2.0 3.2 2.8 2.4 2.0 1.6 1.2 0.8 0.4 δ y[mpch 1 ] y[mpch 1 ] 0 0 z=7 SFR (M yr 1 ) -26-26 0 26-26 0 26 x[mpch 1 ] x[mpch 1 ]
Intensity 3d Power Spectrum Galaxies Source of emission in I (z=7) I (z=8) I (z=10) [nwm 2 sr 1 ] Recombinations 3.9 10 3 2.3 10 3 5.7 10 4 Excitations 1.4 10 3 8.0 10 4 2.0 10 4 Cooling 5.7 10 6 3.0 10 6 9.5 10 7 Continuum 7.3 10 3 5.7 10 3 2.9 10 3 Total 1.3 10 2 8.8 10 3 3.7 10 3 k 3 P(k)/2π 2 [nwm 2 sr 1 ] 2 10 3 10 1 10 1 10 3 10 5 10 7 10 9 10 11 exc cont cool rec total z = 7 Galaxies thin IGM thick lines 10 13 IGM 10 15 10 1 10 0 10 1 k[h/mpc] Source of emission in I (z=7) I (z=8) I (z=10) [nwm 2 sr 1 ] Recombinations 8.0 10 4 5.5 10 4 2.4 10 4 Excitations 5.2 10 3 1.9 10 3 2.3 10 4 Continuum 1.2 10 7 6.5 10 7 2.1 10 6 Total 6.0 10 3 2.5 10 3 4.7 10 4 k 3 P(k)/2π 2 [nwm 2 sr 1 ] 2 10 0 10 1 10 2 10 3 10 4 10 5 GAL IGM rms ~ 0.03 nwm -2 sr -1 Galaxies IGM 10 6 10 7 10 1 10 0 10 1 k[h/mpc]
Experimental issues Observations ~ 1 µm (z ~ 7) During the EoR we want to probe 3d modes: k ~ 0.05 Mpc -1 to 10 Mpc -1 Spatial scales: r ~ 0.5 Mpc to 125 Mpc Angular scales: µ ~ 10 to 1 deg (l ~ 150 to 6.5x10 4 ) Band: ± ~ 2A to 450A (dz ~ 0.0016 to 0.37 - careful with cosmological evolution ) Note: 450A for one redshift observation want many more! But Ly line width will wash out fluctuations along line of sight, so maybe no point to go below ± ~ 30A? (k < 0.7 Mpc -1 along line of sight) Ly\alpha widths (Ando et al. 2006)
Experimental issues Noise dominated by photon count from sky glow (earth observations) or Zodiacal light (space observations) Foregrounds: continuum emission and other lines (H?) from low-z galaxies Need many continuous slices/bands to fit-out the smooth foregrounds Also correlate with other low-z surveys to check contamination
Don t forget other lines! 21cm intensity evolution with redshift Sensitive to: IGM Gas density IGM temperature ionization fraction Star formation rate Lyman-α flux See Santos et al. 2008/2010 (simfast21.org) See also: - CO (Gong et al. 2011) - CII (Gong et al. 2011)
21cm/Ly maps at z=10 26 z=10 26 z=7 y[mpch 1 ] 0 y[mpch 1 ] 0-26 -26 0 26 x[mpch 1 ] -26-26 0 26 x[mpch 1 ] 0 5 10 15 20 25 30 35 40 45 50 δt b (mk) 4.0 3.2 2.4 1.6 0.8 0.0 0.8 1.6 log10[νi ν ]
21cm/Ly maps at z=7 26 z=7 26 z=7 y[mpch 1 ] 0 y[mpch 1 ] 0-26 -26 0 26 x[mpch 1 ] -26-26 0 26 x[mpch 1 ] 0 5 10 15 20 25 30 35 40 45 50 δt b (mk) 4.0 3.2 2.4 1.6 0.8 0.0 0.8 1.6 log10[νi ν (nwm 2 sr 1 )]
21cm/Ly cross-correlation 1.0 IGM+Galaxies Galaxies 0.5 r CII,HI (k) 0.0 0.5 1.0 10 1 10 0 10 1 k[h/mpc] z = 7 z = 8 z = 9 z = 10 Cross-correlation coefficient (dashed total, solid galaxies only) Transition from negative to positive related to typical bubble size (increases from z=10 to z=7)
Conclusions We considered emission from both Galaxies and IGM Signal from Galaxies dominate over IGM with 1.3x10-2 nwm -2 sr -1 at z=7 and 3.7x10-3 nwm -2 sr -1 at z=10 3d power spectrum rms ~ 0.03 nwm -2 sr -1 Cross-correlation with 21 cm signal can help with foregrounds and provide information about the ionization process Ly intensity mapping can provide a tomographic picture of the EoR but probably need to go to space