Daniele Sorini. Supervisor: Joseph Hennawi (MPIA) Collaborators: Jose Oñorbe (MPIA), Annalisa Pillepich (MPIA), Zarija Lukić (LBL)

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1 Daniele Sorini Supervisor: Joseph Hennawi (MPIA) Collaborators: Jose Oñorbe (MPIA), Annalisa Pillepich (MPIA), Zarija Lukić (LBL) From Wall to Web Berlin, July 2016

2 (b) (c) Galactic winds in the IGM log log ρ/< ρ> 1010T(K) AGN and Supernovaelog T(K) Feedback affect CGM density/temperature T(K) [Theuns+ 03; see ] also Kollmeier July (d) log10 T(K) (a) (d) No Feedback Feedback (d)(b) (c) (d (c) Feedback flux flux No Feedback 2 Galactic winds in the IGM Other unresolved physics in the CGM? Impact on Lyα forest flux statistics? (c)(a) velocity (km s-1) Daniele Sorini - Constraining Feedback with Lyα Statistics 1000 velocity (km s-1) Galactic winds in the IGM 1+ δ

3 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 3 P(k)(Mpc/h) Flux power spectrum for different feedback models Effect <~ 10% IGM: reionization unclear è Thermal state degenerate with feedback Around galaxies: CGM physics determines Lyα statistics (100,512) REF (100,512) AGN (25,512) REF (25,512) AGN [Viel+ 2013] k (h/mpc) Feedback effect on Lyα Flux Statistics in IGM < 1σ measurements [Theuns+ 03, Desjacques+ 04,Kollmeier+ 05, Viel+ 13]

4 The Large-scale Distribution of H i Flux Flux Flux Flux Flux Flux Flux der the larger-scale distribution H i around b galaxies with Dtran > the sampling of nately, atively poor in our sample A duebto thec survey 0121 of the KBSS fields (typically arcmin l cale is imposed by the footprint with A B of LRIS; C y centered on the bright QSO, the maximum arameter would be 2.15 pmpc at z = 2.3. Lyαb/g Quasar f/g imaged Quasar survey fields (see Table 1) were ments covering larger angular sizes and A B C thus Lyα J on on larger transverse scales. In Figures 9 widerbin sizes for absorbers with Dtran > to consider the large-scale distribution. This oise in the Lyβ bins with Dtran > 2 pmpc. Figures 9 Lyα max(n ) remains higher than the ate that Hi ue inthelyβ IGM (dark0 horizontal to line) out Velocity n begins to decline. For larger Dtran(km/s), the data A of random B Cplaces in ensities at or below that J Normalized Flux of the QSO spectra within ±1000 km s 1 of roduced in Figure 12. Q0821 BX pkpc z=2.25 QSO Q2343 BX pkpc z=2.11 b/g Quasar f/g Galaxy Q0100 BX pkpc z= Q1442 MD84 89 pkpc z=2.45 Q1623 BX pkpc z=2.18 ive Flux ing the degree Lyβ of scatter in max(nh i ) at fixed, Figure 13 shows max(nh i, 700 km s 1 ) n Dtran, aslyγ indicated. 0The top row of panels Lyα Velocity (km/s) an < 300 pkpc, while the bottom two rows larger Each panel1000 shows impact parameters. 1 Velocity (km/s) [Lau+ 15] [Rudie+ 12] υ [km s ] Smirnov probability that the two histograms e same parent only the- Constraining Figure 12. Lyαwith absorption within ±1000 km s 1 of the systemic redshift 2016 distribution. Notably, 4 o Daniele Sorini Feedback Lyα Statistics July

5 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 5 b/g Quasar f/g Quasar b/g Quasar f/g Galaxy Lyα flux statistics versus impact parameter [See also Rudie+ 12, 13] Previous work on covering factor and optically thick absorbers [e.g. Hennawi+ 06, 13; Rahmati+ 13; Fumagalli+ 14; Crighton+15]

6 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 6 ILLUSTRIS: z=2, L=75 cmpc/h = cmpc, LOW RES [Vogelsberger+ 14] NYX: z=2, L=100 cmpc/h = cmpc, N=4096 [Almgren+ 13, Lukić+ 15] Nyx reference run: NO FEEDBACK, no star formation Semianalytic feedback models painted on Nyx [See also Zjupa s poster]

7 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 7 Preliminary M h = M Sun M h = M Sun ILLUSTRIS: z=2, L=75 cmpc/h = cmpc, LOW RES [Vogelsberger+ 14] NYX: z=2, L=100 cmpc/h = cmpc, N=4096 [Almgren+ 13, Lukić+ 15] Nyx reference run: NO FEEDBACK, no star formation Semianalytic feedback models painted on Nyx

8 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 8 M h =10 12 M Sun b=50 kpc

9 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 9 M h =10 12 M Sun b=50 kpc

10 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 10 M h =10 12 M Sun b=50 kpc

11 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 11 OBS log(m/msun) >~ 12.5 QSO@ median z=2.3 b < 1 pmpc and l=2000 km/s SIMS z, l, M and b bins consistent with observations 1000 skewers for each b bin Preliminary [See also Meiksin+ 15]

12 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 12 OBS Median log(m/msun)=11.9 Star-forming median z=2.4 b < 2 pmpc and l=330 km/s SIMS z, l, M and b bins consistent with observations 1000 skewers for each b bin Preliminary [See also Meiksin+ 15, Turner+ 16]

13 24-29 July 2016 Daniele Sorini - Constraining Feedback with Lyα Statistics 13 CONCLUSIONS Mean flux/median optical depth sensitive to CGM temperature Cold feedback models favoured by observations OUTLOOK Compare with other simulations (e.g. Horizon) Consider other statistics (e.g. PDF, power spectrum ) Determine smallest number of skewers needed to set meaningful constraints on feedback