A Decade of WHIM search: Where do We Stand Where do We Go F. Nicastro (OAR-INAF) Y. Krongold, M. Elvis, S. Mathur 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 1
The Missing Baryons Problems McGaugh+1 Ω b WMAP h - =.6 h - =.456 ~ 5% Shull+1 ~ 3-4% (or more) of Baryons Still Missing at z~ Cosmological Baryon Fraction f b =.17 5/18/16 XMM-Newton: the Next Decade (F. Nicastro)
The WHIM in Hydro-dynamical simula6ons Britton+1 Cool-Phase: ~% Branchini+1 Warm-Phase: ~6% Hot-Phase: ~% 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 3
First Claimed WHIM Detections: Exceptional Outburst State (Nicastro+5, Nature, ApJ) However: - z(mkn 41) only.3 - Mkn 41 outbursts are unique + OII Kβ Controversial: - Not confirmed by XMM (though consistent with; Rassmussen+7) - Close to instrument systematics (Kaastra+6) Ω b (N OVII > 7 1 14 ) =.7 +3.8 1.9 1 [O / H ] 1 % ~ Ω Miss 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 4
A Serendipitous hot X-Ray/BLA PKS 558-54 (z=.137) Filament at z=.118? From X-rays è logt < 6.75; logn H =1.5±.3 (Z/Z.1 ) -1 From lack of OVI è logt > 6.5 From HI and T è Z = (1-4)% Z From Z and T è δ 3 and Theory From δ and N H è D=4-7 Mpc Combined Statistical Significance = 5.σ (5σ if FUSE systematics are included) [Nicastro+1] 5/18/16 (Nicastro+1) XMM-Newton: the Next Decade (F. Nicastro) 5
Galaxy concentrations as WHIM tracers But: N Right Ascension OVII ~ 8 x 1 16 cm -!!! Buote+9, Fang+1 H 356-39 Mkn 51 5/18/16 Ren, Fang & XMM-Newton: Buote, 14 the Next Decade (F. Nicastro) 6
OII Kβ @ z= Not OVII @ z=.3 <EW(OII Kβ)> = 14 ± 4 må.6 Nicastro+16, MNRAS, 457, 676 <EW(OII Kβ)> = 18 ± 5 må.4..8.6.4..7.6.5.4.1.8.3.8.6.4.6..4 1 3 4 1 3 4 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 7
The Case of H 356-39 & the z=-limm / z=.3-whim conspiracy z= OII Kβ or z.3 OVII Kα.15.1 z= OII Kα z= OIV Kα or z.3 OVI Kα.5 z= OI Kα or z.3 OIV Kα.15.1 EW(OII Kβ) = 18 ± 5 må vs <EW(OII Kβ)> AGN = 18 ± 5 må 1 3 4 Nicastro+16, MNRAS, 485, L13.5 z.3 WHIM not statistically required. If present must have: T 3x1 5 K b 1 km s-1 NOVII 4x1 15 cm - (<< 8x1 16 cm - of Fang+1) 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 8
Best WHIM Target in the Universe: 1ES 1553+113 z>.3 logt = 5. 5.5 6. 1 CV CIII CVI.1 CIV CII.1 4 6 8 1 1 1 OIII OIV OV OVII.1 OII OVI OVIII.1.1.1 4 6 8 1 1 HI 4 6 8 1 1 - z >.4 - F X ~ 1- mcrab - High S/N COS spectrum with 5 priors (HI Lyα with 4<b<8 km s -1 : BLAs - è 5. < logt < 5.5 è Mostly CV) 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 9
Tentative IGM IDs Nicastro+13 Redshift CV CVI OIV OV OVII BLA OVI (ma) CIV (ma).41±. NA NA NA NA.3σ 9.6σ <65 <13.133±. 3.8σ.7σ NA NA NA 5.4σ <14 <5.184±.1 3.6σ NA NA NA NA NA <11 NA.19±.1.σ NA NA 1.7σ NA 9.3σ 7.6σ NA.37±.1 3.9σ NA NA? NA 5,.σ <13 NA.31±.1 4.1σ 4.1σ NA? NA 8.1σ 3.6σ NA 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 1
Cool WHIM at z=.31: (6.3σ X-ray only) Nicastro+13 4 - -4 4 - -4 4 - -4.35.31.315.3 18 16 14 1 1 HI BLA From COS BLA and OVI b: è b th = 5 ± 7 km s -1 (b turb = 3 ± 14 km s -1 ) è logt = 5. ±.1 Fully Consistent with presence of CV, CVI, OV 4 - -4 4 - -4 8.315.311.3115.31 18 16 14 OVIa 1.315.311.3115.31 18 16 14 OVIb 1.315.311.3115.31 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 11
Best-Fitting WHIM Parameters Redshift logt N H (1 19 cm - ) n b (1-6 cm -3 ) Z/Z [= N H (X)/N H (FUV)].41±. 5.45 ±.5 3.8 ±.8 1..13, +.7, -.1 *.133±. 5.4, +., -.6 **. 15 NA.19±.1 5.5 ±.5 1.9 ± 1.8 17.4, +.4, -.3.37±.1 5.3 ±.1.3, +., -.1 19.7, +1.8, -..31±.1 5.5 ±.5 3.1, +1.6, -1.1 11.3, +.19, -. * No consistent X-Ray-FUV solution: BLA is too narrow and shallow to be imprinted by the X-ray absorber and OVI should be visible if logt<5. ** From N H (X) divided by the average <Z/Z > =.8 ±.4 determined for the z=.41,.19,.31 systems 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 1
Cool WHIM contains 15% of MBs 1 1 Ω b = 1 µm p ρ cr, i i N H Δl comoving σ Ωb = 1 1 [1 1/ K] 1/ ρ cr, K i i µm p [N H < N H i=1 Δl comoving >] dl comoving = c H(z) dz logt>5.5 WHIM? Missing.1 logt<5.5 WHIM.1 Ω b (5. < logt < 5.5;EW CV,OVII >1 m A o ) =.69 ±.18 = (15± 4)% Ω b 5% of Baryons are still Missing 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 13
XMM VLP: 1.6 Ms on 1ES 1553+113 1.9.8.7.6.5.4 logt = 5. 5.5 6. 1 CV CIII CVI.1 CIV CII.1 4 6 8 1 1 1 OV OIII OVII OIV.3.1 OII OVI OVIII..1.4.3..1 9 h at GTC SDSS u,g r,i,z 4.5 in r @ S/N=5 (.L* at z=.5) Allows Δz=.5.1.1.1 4 6 8 1 1 HI 4 6 8 1 1 With the sensitivity of the current 5 ks Chandra bound to detect only the cool WHIM in CV. ~1.6 Ms XMM è ~4x S/N in OVII è N OVII > 1 15 cm - è ~5-1 systems sampling the hot WHIM 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 14
4σ Detection of logt>5.5 WHIM in Multiple Lines 4 - -4 - -4 OIV Kα z= 4-4.4.5.6.7 Redshift z.4.5.6.7 4 - z=.54 logt = 5.7 -.1 +.5 K è b HI > 9 km s -1 + Tentatively confirms z=.43 OVII detects z=.37 OVII In the short-term, only ultra-deep XMM and Chandra observations can detect the missing 5% of baryons and solve the puzzle 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 15
The Long-term Future: Athena 6 AGNs Exposures: < T (ks) < 3 each -1 OVII-Forest - Total Exposure (in Msec)..3.4.5 Redshift 5 ks for F.5- =.1 mcrab along a random WHIM LOS from Cen+6: detects 5 Systems with logt = 5.-6.4 K, lognh = 18.7-19.4 (Z/Z )-1 cm- at z<.5 All in OVII-OVIII; in CV + OIV-OVI (Cool-Phase): excellent Density Diagnostics 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 16
Summary and Future - After proper ionization and metallicity correction, CV-OVI-BLA dominated cool WHIM contains ~ 15% of Baryons è 4-5 % of Baryons still Missing and likely to reside in logt>5.5 WHIM: detectable only with ultra-deep XMM and Chandra pointings - In the future Athena will enable: (a) accurate (few %) measure of the Cosmological Mass Density of Baryons in the Universe (b) study of the interplay between galaxy and AGN outflows and the IGM (feedback) (c) understanding of the role of shocks in the formation of structures in the Universe (d) mapping of the Universe s Dark-Matter concentrations 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 17