X-ray ionization of the intergalactic medium by quasars

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1 X-ray ionization of the intergalactic medium by quasars Luca Graziani In collaboration with: CRASH4 IGM reionisation by QSOs GAMESH, QSOs evolution & QSOs impact on SF B. Ciardi (MPA, Munich) A. Ferrara (SNS) R. Schneider (INAF-OAR, Italy) R. Valiante (INAF-OAR, Italy) S. Marassi (INAF-OAR, Italy) From wall to Web, MPG, July , Berlin, Germany

2 The FIRST team and collaborators Matteo de Bennassuti, PhD INAF/OAR Marco Limongi INAF/OAR Stefania Salvadori Kepteyn, Groningen Stefania Marassi, Pdoc INAF/OAR Simone Bianchi INAF/OAA Raffaella Schneider, PI INAF/OAR Roberto Maiolino Cambridge Andrea Ferrara Scuola Normale Rosa Valiante, Pdoc INAF/OAR Gen Chiaki Tokyo University Kazu Omukai Tohoku University

3 C.R.A.S.H. Cosmological RAdiative transfer Scheme for Hydrodynamics Multi-frequency RT code based on MC + Ray tracing. Describes 3D RT cosmological scenarios. Solves time dependent RT on cosmological scales Cosmic Reionization of H and He. Implements detailed H,He physics + metal ions. H-He ionising band: 13.6 ev - 200eV

4 CRASH4 Multi-frequency band RT: Extend up to soft x-rays: 10 KeV. Include Ly RT coupled with continuum. LW band and molecules: H2, CO. Dust photon scattering IS relevant. Secondary ionisation e e 30eV could collisionally ionise/excite the remaning neutral part.

5 HII ideal regions: H-only Ideal setup Ng=10-4 Include UV, UV+X H-only L = 1056 phot/sec Sidx= -1.5 T0= 100K H-only: x-rays create long lowionisation shells after UV I-front

6 HII ideal regions: H+He Ideal setup Ng=10-4 Include UV, UV+X H+He L = 1056 phot/sec Sidx= -1.5 T0= 100K Negligible impact on HeIII Sensitive on HII, HeII, T

7 Modelling dependence Ideal setup Ng=10-4 Include UV, UV+X H+He L = 1056 phot/sec Sidx= -1.5 T0= 100K Negligible impact of modelling in x but.. in T

8 Radiative Feedback in high-z QSO dominated environments

9 RT Feedback by ULAS J (Mortlock et al., 2011) Effects of x-rays on HII regions of high-z QSOs A. Ferrara (SNS) B. Ciardi (MPA) S. Gallerani (SNS) R. Schneider (OAR) R. Valiante (OAR) 1) Size of the HII region? (Also see Maselli 2007, Bolton 2011a ) 2) IGM heating? (Also see Koki s paper, Eide in prep., ) But also.. 3) Detectability of RRL on unresolved high density systems? (Manti et al. 2015, MNRAS) 4) Sensitive impact in T: affects Lya systems? Star formation in mini-halo type surrounding systems? (Graziani et al., 2015, MNRAS)

10 1) Size of HII regions 2 randomly selected LOS between min/max : high density systems along the observed LOS could introduce sensitive scatter in the semi-analytic estimates of HII region sizes. White et al vs d ~ 3.3 pmpc from spherical average

11 Size of HII regions 2 randomly selected LOS between min/max : high density systems along the observed LOS could introduce sensitive scatter in the semi-analytic estimates of HII region sizes. White et al vs d ~ 3.3 pmpc from spherical average

12 Size of HII regions 2 randomly selected LOS between min/max : high density systems along the observed LOS could introduce sensitive scatter in the semi-analytic estimates of HII region sizes. White et al vs d ~ 3.3 pmpc from spherical average But the scatter is relevant!

13 Size of HII regions But the scatter is relevant! And the definition of ionisation fronts could change when tracing UV or x-rays dominated regions! UV dominated

14 Size of HII regions But the scatter is relevant! And the definition of ionisation fronts could change when tracing UV or x-rays dominated regions! UV x-rays

15 Size of HII regions But the scatter is relevant! And the definition of ionisation fronts could change when tracing UV or x-rays dominated regions! X-rays only

16 Size of HII regions 2 randomly selected LOS between min/max : high density systems along the observed LOS could introduce sensitive scatter in the semi-analytic estimates of HII region sizes. White et al vs d ~ 3.3 pmpc from spherical average But the scatter is relevant! A region with 1 DLA + LLs is present here around d ~ 1.7 pmpc

17 HII size on a peculiar LOS! But on a peculiar LOS.. Rs < 2 pmpc! RT effects matter! (n, ( ),d)

18 HII size on a peculiar LOS! But on a peculiar LOS.. Rs < 2 pmpc! RT effects matter! (n, ( ),d)

19 HII size on a peculiar LOS Scatter induced by RT!! But on a peculiar LOS.. Rs < 2 pmpc! RT effects matter! (n, ( ),d)

20 2) High-z QSOs IGM heating Sensitive impact on T (large scales): the entire box is affected. Disjoined HII (fully ionised by UV front) and large, excited/heated regions by x-rays What feedback on other systems?? Impact on large scale reionisation simulations?? 21 cm?? but also RRL detectability?? Statistics of LOS showing dmax at certain T = 104K, K, 103 K..

21 4) QSOs RRLs with CRASH Radio Rec.Lines from obscured high-z QSOs with SKA S. Manti (SNS) S. Gallerani (SNS) A. Ferrara (SNS) C. Feruglio (SNS) G. Bernardi (SKA) Radio, mm, sub-mm photons are transparent to gas and dust while optical and x-rays are obscured. QSO x-rays could boost the number of H recombinations via secondary ionisations Evaluate the boost in the inner region of a QSO with CRASH. Track the H, He recombinations and post-process with detailed RRLs predictions.

22 QSOs RRLs with CRASH4 (preliminary) Evaluate the boost in the inner region of a QSO with CRASH. VALUES PREDICTED BY RT LARGER THAN SEMI ANALYTIC ESTIMATES b

23 GAMESH = GAMETE + CRASH + N-Body N-Body simulation: dynamical evolution of DM halos GAMETE simulation: Star formation, metal production CRASH simulation: RT, gas ionisation heating

24 CONCLUSIONS Multi-frequency RT code CRASH ready for x-rays reionization simulations including galaxies and QSOs self-consistently. Relative role of galaxies and QSOs on small scales must be tested statistically on large scales. Large shells at low ionization confirmed by models as tracer of x-rays radiation IGM heating significant from QSOs up to 1000K Proximity effects can be modelled with great level of details: x,t computed self-consistently as result of UV+x-rays bands New applications on radiative feedback modelling on SF systems and detectability with RRLs.