The Cool Portion of the WHIM & The Cold/Warm Milky Way CGM F. Nicastro (OAR-INAF) F. Senatore, Y. Krongold, M. Elvis, S. Mathur 8/25/15 Chandra Workshop 215 (F. Nicastro) 1
Outline Chandra Detection of the Cool Portion of the WHIM Mass Distribution Cold and Warm Baryons in-and-around the Galaxy Ubiquitous presence of z= OII absorption (OII Kβ) casts doubts on z=.3 WHIM discoveries 8/25/15 Chandra Workshop 215 (F. Nicastro) 2
The Missing Baryons Problems McGaugh+1 Ω b WMAP h -2 =.226 h -2 =.456 ~ 5% Shull+12 ~ 3-4% (or more) of Baryons Still Missing at z~ 8/25/15 Chandra Workshop 215 (F. Nicastro) Cosmological Baryon Fraction f b =.17 3
The WHIM SoluCon logt = 5. 5.5 6. 1 CIII CV.1 CIV CVI CII Cool-Phase: ~2% Warm-Phase: ~6%.1 1 OIII 4 6 8 1 12 OV OVII OIV Britton+12 Hot-Phase: ~2%.1 OII OVI OVIII.1 4 6 8 1 12.1.1 HI 4 6 8 1 12 8/25/15 Chandra Workshop 215 (F. Nicastro) 4
Best WHIM Target in the Universe: 1ES 1553+113 - z >.4 - F X ~ 1-2 mcrab 1ES 1553+115 - High S/N COS spectrum with 5 a-priori BLA signposts 8/25/15 Chandra Workshop 215 (F. Nicastro) 5
Cool WHIM at z=.312: (6.3σ X-ray only) Nicastro+13 4 2-2 -4 4 2-2 -4 4 2-2 -4.35.31.315.32 2 18 16 14 12 1 HI BLA From COS BLA and OVI b: è b th = 52 ± 7 km s -1 (b turb = 3 ± 14 km s -1 ) è logt = 5.2 ±.1 Fully Consistent with presence of CV, CVI, OV 4 2-2 -4 4 2-2 -4 8.315.311.3115.312 2 18 16 14 OVIa 12.315.311.3115.312 2 18 16 14 OVIb 12.315.311.3115.312 8/25/15 Chandra Workshop 215 (F. Nicastro) 6
1 1 Metallicities and Cosmological Mass Density of the Cool WHIM Ω b = 1 µm p ρ cr, i i N H Δl comoving dl comoving = c H(z) dz σ Ωb = 1 1 [1 1/ K] 1/2 ρ cr, logt>5.5 WHIM? Missing K i i µm p [N H < N H i=1 Δl comoving >] 2.1 logt<5.5 WHIM.1 Ω b (5. < logt < 5.5;EW CV,OVII >1 m A o ) =.55±.18 = (12 ± 4)% Ω b Ω b (5. < logt < 5.5;EW CV,OVII >1 m A o ) =.69 ±.18 = (15± 4)% Ω b 8/25/15 Chandra Workshop 215 (F. Nicastro) 7
Bound to Detect the Cool WHIM (CV) N Ion 1.1 1 2 N σ Δλ S / N f 1 i λ 2 i (1+ z) 1 3σ Column Density Threshold 1 logt = 5. 5.5 6. 1 CV CIII CVI.1 CIV CII.1 4 6 8 1 12 1 OIII OIV OV OVII.1 OII OVI OVIII.1.1.1.1 4 6 8 1 12 HI.4.3.2.1 4 6 8 1 12 With the sensitivity of the current 5 ks Chandra bound to detect only the cool WHIM in CV. ~3x exposure with XMM è 1x S/N in OVII è N OVII > 1 14 cm -2 è ~5 systems sampling the hot WHIM 8/25/15 Chandra Workshop 215 (F. Nicastro) 8
Summary - The cool portion of the WHIM has been detected in UV and X-rays - High metallicity (~.3 on average), consistent with feedback models - CV-OVI-BLA dominated WHIM contains ~ 15% of Baryons è 4-5 % of Baryons still Missing and likely to reside in logt>5.5 WHIM: detectable with our 1.6 Ms XMM VLP 8/25/15 Chandra Workshop 215 (F. Nicastro) 9
The Milky Way as Lab: Internal and External Probes 2 X-Ray Binaries wit RGS spectra with SNRE > 1 @ 22.2 A: probe the Disk 28 AGNs from Gupta+11: HETG/LETG spectra with low SNRE (1-8 @ 22.2 A) except Mkn 421 (1) and PKS 2155-34 (8): probe small portions of Disk and the Halo/CGM 8/25/15 "The Metal Enrichment of Diffuse Gas in the Universe" (Sexten, F. Nicastro) 1
Spectral Features: OI OII Kα Ubituitous; OII Kβ >3σ in 6 spectra.6.4.2.8.6.4.2.7.6.5.4.1.8.3.8.6.4.6.2.4 21 22 23 24 21 22 23 24 8/25/15 "The Metal Enrichment of Diffuse Gas in the Universe" (Sexten, F. Nicastro) 11
EWs and N H X 12 1 8 6 4 2 8 6 OI Kα correlates with N H X in X-Ray Binaries but not in AGNs 1 Saturation? Different Absorbers? 4 2 6 4 2 1 1 1 8/25/15 "The Metal Enrichment of Diffuse Gas in the Universe" (Sexten, F. Nicastro) 12
Line Saturation 1 8 Unsaturated <EW(OII Kα)> gal = 46 ± 8 ma <EW(OII Kα)> exgal = 13 ± 6 ma 6 OII is heavily saturated against both Galactic and extragalactic Lines of Sight. 4 However: stronger towards Galactic X-Ray Binaries 2 Fully Saturated è b and/or N OII must differ 2 4 6 8 8/25/15 "The Metal Enrichment of Diffuse Gas in the Universe" (Sexten, F. Nicastro) 13
Curves of Growth: b & N OII Line-of-Sight N OII b in 1 17 cm 2 in km s 1 Galactic Lines of Sight 4U 1728-16 9 +1 4 12 +14 17 V*V 821 Ara 4.9 ±.8 2 ± 6 18CB 1.62 ±.8 182 +7 4 Extragalactic Lines of Sight Mkn 421.42 +.11.9 4 +4 3 PKS 2155-34.3 +.7.11 4 +4 9 8CLETG 4 +9 3 6 +16 15 <b> Gal = 17 ± 4 km s -1 <b> Exgal = 5 ±1 km s -1 Either: Smaller Portion of Disk Or: Two Distinct Absorbers 8/25/15 "The Metal Enrichment of Diffuse Gas in the Universe" (Sexten, F. Nicastro) 14
The Disk CNMM & The Disk+Halo/ CGM WIMM 1 Disk & Halo WIM Warm Ionized Metal Medium: <T Halo > WIMM = 29 ± 9 K <Z Halo > WIMM =.3 ±.2 Z.1.1 <T Disk > WIMM = 3 ± 1 K <Z Disk > WIMM =.8 ±.1 Z.1.1 Disk CNM 1 1 Cold Neutral Metal Medium: <T disk > CNMM = 3 1 K <Z Disk > CNMM =.8 ±.2 Z <N OI > = (1. ±.4) 1 18 cm -2 <b> CNMM = 28 ± 5 km s -1 è > 22 Clouds kpc -1 with D<5 pc and n H >.1 cm -3 8/25/15 "The Metal Enrichment of Diffuse Gas in the Universe" (Sexten, F. Nicastro) 15
Metallicity of T<~1 4 K CGM at z<1 (Lehner+13) [O/H] Milky Way WIMM Inflow Outflow 8/25/15 "The Metal Enrichment of Diffuse Gas in the Universe" (Sexten, F. Nicastro) 16
Galaxy concentrations as WHIM tracers But: N Right Ascension OVII ~ 2 x 1 16 cm -2!!! Buote+9, Fang+1 H 2356-39 Mkn 51 8/25/15 "The Ren, Metal Fang Enrichment & Buote, of 214 Diffuse Gas in the Universe" (Sexten, F. Nicastro) 17
OII Kβ @ z= Not OVII @ z=.3.6.4.2.8.6.4.2.7.6.5.4.1.8.3.8.6.4.6.2.4 21 22 23 24 21 22 23 24 8/25/15 "The Metal Enrichment of Diffuse Gas in the Universe" (Sexten, F. Nicastro) 18
Conclusions Two distinct OI-OII components: the CNMM and the WIMM. The CNMM is confined in the disk of our Galaxy and has: T CNMM 3 1 K, <Z> CNMM =.8 ±.2 Z, <b> CNMM = 28 ± 5 km s 1 The CNMM must be patchy and made up of > 22 clouds kpc 1, with D < 5 pc each. The WIMM has <T> WIMM = 3 ± 1 K and permeates the whole Galaxy. We find: <Z Halo > WIMM =.3 ±.2 Z, <b Halo > WIMM =48 ± 6 km s 1 <Z Disk > WIMM =.8 ±.1 Z, <b Disk > WIMM = 1 ± 1 km s 1 We estimate: M CNMM < 8 1 8 M M WIMM ~ 8.2 1 9 M (only 1% in the disk). OII Kβ from the WIMM invalidates OVII Kα WHIM detection at z=.3 8/25/15 "The Metal Enrichment of Diffuse Gas in the Universe" (Sexten, F. Nicastro) 19