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 24-29 2016, Berlin, Germany
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
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
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.
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
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
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
Radiative Feedback in high-z QSO dominated environments
RT Feedback by ULAS J1120+0641 (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)
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. 2003 vs d ~ 3.3 pmpc from spherical average
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. 2003 vs d ~ 3.3 pmpc from spherical average
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. 2003 vs d ~ 3.3 pmpc from spherical average But the scatter is relevant!
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
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
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
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. 2003 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
HII size on a peculiar LOS! But on a peculiar LOS.. Rs < 2 pmpc! RT effects matter! (n, ( ),d)
HII size on a peculiar LOS! But on a peculiar LOS.. Rs < 2 pmpc! RT effects matter! (n, ( ),d)
HII size on a peculiar LOS Scatter induced by RT!! But on a peculiar LOS.. Rs < 2 pmpc! RT effects matter! (n, ( ),d)
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, 5 103 K, 103 K..
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.
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
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
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.